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https://gea.esac.esa.int/archive/documentation/GDR2/Data_processing/chap_cu3ast/sec_cu3ast_intro/ssec_cu3ast_intro_convention.html
|
3.1.2 Conventions, notations, nomenclature, and definitions
Author(s): Uli Bastian
The Gaia data processing, like any other complex multi-partner project, needs a set of agreed conventions and notations to be followed by all partners. Such conventions are needed to ease communication, to avoid misunderstandings and to streamline the distributed development of software for shared usage.
The DPAC consortium maintains a set of internal documents intending to collect all the necessary conventions. However, it is neither needed nor useful to expose the users of the Gaia Catalogue(s) to the full set of conventions. Instead, it is better to restrict the documentation to those which are actually of interest to the external users. Also, it is not useful to concentrate their description in one place. Rather they should be introduced where needed.
So, for instance, the definitions and notations for angular coordinates, time scales and epochs, as well as relativistic reference frames are given in the following subsections where they first appear. The agreed fundamental physical and mathematical constants are briefly described in Section 3.1.8.
The present subsection mentions only a few overarching aspects.
Physical units: The SI system
This section is mainly based on the ‘Units home page’ of the National Institute of Standards and Technology (see the NIST website), which generally agrees with IAU recommendations For interested users we recommend to read Thompson and Taylor (2008). In summary, The Gaia collaboration uses ‘acceptable SI units’ (as defined below) as default, plus a few extensions also described below. Following Thompson and Taylor (2008), we interpret the term ‘SI units’ as the seven SI base units (kg, m, s, mol, A, K, cd; see Section 4.1 in Thompson and Taylor (2008)), plus the 20 SI derived units (N, V, Hz, Gy, W, etc.; see Section 4.2 in Thompson and Taylor (2008)), plus the two SI supplementary units (rad and sr; Section 4.2.2 in Thompson and Taylor (2008)), including multiples and sub-multiples of these units formed by using SI prefixes (${\rm M}=10^{6}$, ${\rm k}=10^{3}$, $\mu=10^{-6}$, etc.; Table 5 in Thompson and Taylor (2008)). The term ‘acceptable SI units’ is taken to denote the ‘SI units’ (as defined above), plus those units accepted by the CIPM (Comité International des Poids et Mesures) for use with the SI (notably angular degree, arcminute, arcsecond, minute, hour, and day; Tables 6 and 7 in Thompson and Taylor (2008)), plus those units temporarily accepted for use with the SI (Table 9 and Section 5.2 in Thompson and Taylor (2008)), including multiples and sub-multiples of these units. We also follow Thompson and Taylor (2008) and the IAU by recognizing that the use of time intervals expressed in units of Julian years (year), distances in units of parsecs (pc) or astronomical units (au), and source brightness/luminosity in units of magnitudes (mag) is allowed. The use of the non-SI unit Å is ‘temporarily accepted’ by Thompson and Taylor (2008) and ‘deprecated’ by the IAU; we propose that this unit is not used.
Notation of units
The interested reader is strongly advised to consult Thompson and Taylor (2008); we simply list a few specific remarks which are relevant in the light of Gaia:
• The angular units degree, arcminute, arcsecond may be abbreviated as ‘deg’, ‘arcmin’, ‘arcsec’ or denoted by the conventional symbols ${}^{\circ}$ ${}^{\prime}$ ${}^{\prime\prime}$.
• Sub-multiples of the arcsecond are denoted by ‘mas’ ($10^{-3}$ arcseconds, 1 milli-arcsecond) and ‘$\mu$as’ ($10^{-6}$ arcseconds, 1 micro-arcsecond). In an ASCII-environment ‘$\mu$as’ is allowed to degenerate into ‘muas’.
• The unit of a Julian year is denoted as ‘year’, in line with Thompson and Taylor (2008), §5.1.1. In theory, some confusion could arise when using ‘y’ instead of ‘year’. For instance the SI unit ‘Gy’ (Gray, for absorbed radiation dose) could be mis-interpreted as $10^{9}$ years. To add to this confusion, we note that the (‘temporarily accepted’) radiation unit ‘rad’ (not to be confused with radian) is defined as ‘cGy’, i.e., centi-Gray. Although in the light of Gaia, this sort of confusion is generally not expected, the unit ‘year’ should either be spelt out explicitly, or be abbreviated solely by ‘a’ (from Latin ‘annum’, following ISO and Section 8.1 of Thompson and Taylor (2008).
• The use of the phrase/unit ‘micron’ to denote $\mu$m is not allowed; this unit should be denoted as ‘$\mu$m’ (or as ‘micrometer’ in full or ‘mum’ in abbreviation in an ASCII-environment).
• Note the distinction between a bit (b) and a byte (B, meaning eight bits). Thus: 1 kb denotes one kilobit ($10^{3}$ bit) and 1 kB denotes one kilobyte ($10^{3}$ byte).
• Note the distinction between binary and decimal prefixes. For example, one kilobit (kb) denotes $10^{3}=1000$ bit but one kibibit (Kib) denotes $2^{10}=1024$ bit. The prefix kilobinary, or kibi or Ki, means $2^{10}$. More examples of binary prefixes, e.g. Mi=$2^{20}\sim 10^{6}$, Gi=$2^{30}\sim 10^{9}$ and a complete list can be found here.
Acronyms
A list of acronyms and abbreviations used in the Gaia collaboration is maintained in the internal “Glossary of acronyms” text file and is available here: Glossary of acronyms file.
| 2019-03-24T15:30:23 |
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|
https://www.usgs.gov/center-news/volcano-watch-coexisting-volcanoes
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# Volcano Watch - Coexisting with volcanoes
Release Date:
Volcanoes have been in the news a lot lately: Etna (Italy), Reventador (Ecuador), Pago (New Britain, Papua New Guinea), Popocatepetl (Mexico)-even our own Mauna Loa. We usually hear about volcanoes only when one is erupting or getting ready to erupt. As a consequence, the news often makes volcanoes look pretty negative.
That's understandable, of course, for some eruptions can cause loss of life and destruction of property. We need to know about that!
But there is another side to volcanoes, a quiet side that generally gets lost in all the doom and gloom. It is this side that attracts people, makes for good living, provides natural resources for society, and inspires awe in those fortunate enough to observe volcanoes in all their glory. And, at most volcanoes, this side prevails for much of the time.
Let's take Hawaii. All of the islands were made by volcanoes. There wouldn't be a Hawaii without volcanoes. Even the coral reefs are built on volcanic rocks. Long after the islands formed, continued volcanic activity has given them features that we consider beneficial to society. Imagine a Waikiki without Diamond Head, a Mauna Kea without the cinder cones that dot its flanks, or a lower Puna without Kapoho Cone. Hilo Bay exists only because Mauna Loa erupted the Panaewa lava flow about 1,400 years ago. Kiholo Bay was enhanced by a Mauna Loa flow in 1859. The list goes on and on.
Think of all the benefits to society from an erupting volcano in Hawaii, such as Kilauea or, potentially, Mauna Loa. Increased visitation and the needs of those visitors come to mind immediately. Watching lava flows and fountains imparts residents and visitors alike with inspiration, wonder, awe, curiosity, and adventure. Such intangibles are positive additions to our lifestyle, to be balanced against vog and the destruction of property. On balance, most of us would probably agree that we're fortunate to have Kilauea and Mauna Loa on our island, though we temper this feeling with the terrible reality of the loss of communities, such as Kapoho and Kalapana.
A volcano has to destroy in order to create. This is the yin and yang of volcanoes. A new lava flow may form a bay but has to destroy the beach and whatever else was there first. Volcanic ash has to cover the ground surface before it can create fertile soil.
Destruction usually happens quickly, even by our time scales. A few seconds to a few days-that's all it takes. But it takes decades or centuries to rebound. This is a time scale hard for us to grasp, one so long and drawn out that we lose track of what is happening. We get out of the habit of thinking about our surroundings as volcanic-until the next eruption starts.
It is possible to minimize problems of eruptions with severe (some would say enlightened) land-use restrictions. Such restrictions require tough choices by society, especially given the generally infrequent occurrence of eruptions on a human time scale. It makes sense to restrict land use in valleys draining a volcano that has a mudflow every few decades, but if that land is fertile or beautiful, what do we do?
Throughout the world, societies on or near a volcano have generally made another choice-simply to coexist with the volcano. The choice has generally been made implicitly; little understanding of the volcano goes into such a decision, and people live there without much knowledge of the hazard but often with a mystical sense of what can happen. Rarely do communities, such as those at the foot of Sakurajima volcano in Kyushu, Japan, make an explicit plan to deal with a volcano, with full knowledge of what could happen in a large eruption.
Such coexistence, whether implicit or explicit, works well most of the time. The benefits of the volcano can be utilized with the understanding that an eruption might change things for the worse, at least over the short haul. An impending eruption is indeed cause for some, at times considerable, concern. But many positive opportunities will likely be found over the long haul, after the eruption has ended. It is not yin or yang, but both.
### Volcano Activity Update
Eruptive activity of Kilauea Volcano continued unabated at the Puu Oo vent during the past week. Lava flows through a tube system from the vent to the sea. Lava enters the ocean only at the Wilipea and West Highcastle lava deltas. The Laeapuki ocean entry of the east arm of the Mother's Day flow stopped last week, but another lobe is nearing the coast west of Laeapuki. Numerous surface breakouts are observed in the coastal flats makai of Paliuli. The public is reminded that the ocean entry areas are extremely hazardous, with explosions accompanying sudden collapses of the new land. The steam clouds are highly acidic and laced with glass particles. The National Park Service has erected a rope barricade to delineate the edge of the restricted area. Do not venture beyond this rope boundary and onto the lava deltas and benches.
There were no felt earthquakes in the week ending on December 5.
Mauna Loa is not erupting. The summit region continues to inflate, but no earthquakes were located in the area for the last seven days.
| 2019-11-21T19:55:44 |
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|
https://zims-en.kiwix.campusafrica.gos.orange.com/wikipedia_en_all_nopic/A/Logical_equivalence
|
# Logical equivalence
In logic and mathematics, statements ${\displaystyle p}$ and ${\displaystyle q}$ are said to be logically equivalent, if they are provable from each other under a set of axioms,[1] or have the same truth value in every model.[2] The logical equivalence of ${\displaystyle p}$ and ${\displaystyle q}$ is sometimes expressed as ${\displaystyle p\equiv q}$,[3] ${\displaystyle {\textsf {E}}pq}$, or ${\displaystyle p\iff q}$, depending on the notation being used. However, these symbols are also used for material equivalence, so proper interpretation would depend on the context. Logical equivalence is different from material equivalence, although the two concepts are intrinsically related.
## Logical equivalences
In logic, many common logical equivalences exist and are often listed as laws or properties. The following tables illustrate some of these.
### General logical equivalences[4]
EquivalenceName
${\displaystyle p\wedge \top \equiv p}$
${\displaystyle p\vee \bot \equiv p}$
Identity laws
${\displaystyle p\vee \top \equiv \top }$
${\displaystyle p\wedge \bot \equiv \bot }$
Domination laws
${\displaystyle p\vee p\equiv p}$
${\displaystyle p\wedge p\equiv p}$
Idempotent laws
${\displaystyle \neg (\neg p)\equiv p}$Double negation law
${\displaystyle p\vee q\equiv q\vee p}$
${\displaystyle p\wedge q\equiv q\wedge p}$
Commutative laws
${\displaystyle (p\vee q)\vee r\equiv p\vee (q\vee r)}$
${\displaystyle (p\wedge q)\wedge r\equiv p\wedge (q\wedge r)}$
Associative laws
${\displaystyle p\vee (q\wedge r)\equiv (p\vee q)\wedge (p\vee r)}$
${\displaystyle p\wedge (q\vee r)\equiv (p\wedge q)\vee (p\wedge r)}$
Distributive laws
${\displaystyle \neg (p\wedge q)\equiv \neg p\vee \neg q}$
${\displaystyle \neg (p\vee q)\equiv \neg p\wedge \neg q}$
De Morgan's laws
${\displaystyle p\vee (p\wedge q)\equiv p}$
${\displaystyle p\wedge (p\vee q)\equiv p}$
Absorption laws
${\displaystyle p\vee \neg p\equiv \top }$
${\displaystyle p\wedge \neg p\equiv \bot }$
Negation laws
### Logical equivalences involving conditional statements
1. ${\displaystyle p\implies q\equiv \neg p\vee q}$
2. ${\displaystyle p\implies q\equiv \neg q\implies \neg p}$
3. ${\displaystyle p\vee q\equiv \neg p\implies q}$
4. ${\displaystyle p\wedge q\equiv \neg (p\implies \neg q)}$
5. ${\displaystyle \neg (p\implies q)\equiv p\wedge \neg q}$
6. ${\displaystyle (p\implies q)\wedge (p\implies r)\equiv p\implies (q\wedge r)}$
7. ${\displaystyle (p\implies q)\vee (p\implies r)\equiv p\implies (q\vee r)}$
8. ${\displaystyle (p\implies r)\wedge (q\implies r)\equiv (p\vee q)\implies r}$
9. ${\displaystyle (p\implies r)\vee (q\implies r)\equiv (p\wedge q)\implies r}$
### Logical equivalences involving biconditionals
1. ${\displaystyle p\iff q\equiv (p\implies q)\wedge (q\implies p)}$
2. ${\displaystyle p\iff q\equiv \neg p\iff \neg q}$
3. ${\displaystyle p\iff q\equiv (p\wedge q)\vee (\neg p\wedge \neg q)}$
4. ${\displaystyle \neg (p\iff q)\equiv p\iff \neg q}$
## Examples
### In logic
The following statements are logically equivalent:
1. If Lisa is in Denmark, then she is in Europe (a statement of the form ${\displaystyle d\implies e}$).
2. If Lisa is not in Europe, then she is not in Denmark (a statement of the form ${\displaystyle \neg e\implies \neg d}$).
Syntactically, (1) and (2) are derivable from each other via the rules of contraposition and double negation. Semantically, (1) and (2) are true in exactly the same models (interpretations, valuations); namely, those in which either Lisa is in Denmark is false or Lisa is in Europe is true.
(Note that in this example, classical logic is assumed. Some non-classical logics do not deem (1) and (2) to be logically equivalent.)
### In mathematics
In mathematics, two statements ${\displaystyle p}$ and ${\displaystyle q}$ are often said to be logically equivalent, if they are provable from each other given a set of axioms and presuppositions. For example, the statement "${\displaystyle n}$ is divisible by 6" can be regarded as equivalent to the statement "${\displaystyle n}$ is divisible by 2 and 3", since one can prove the former from the latter (and vice versa) using some knowledge from basic number theory.[1]
## Relation to material equivalence
Logical equivalence is different from material equivalence. Formulas ${\displaystyle p}$ and ${\displaystyle q}$ are logically equivalent if and only if the statement of their material equivalence (${\displaystyle p\iff q}$) is a tautology.[5]
The material equivalence of ${\displaystyle p}$ and ${\displaystyle q}$ (often written as ${\displaystyle p\iff q}$) is itself another statement in the same object language as ${\displaystyle p}$ and ${\displaystyle q}$. This statement expresses the idea "'${\displaystyle p}$ if and only if ${\displaystyle q}$'". In particular, the truth value of ${\displaystyle p\iff q}$ can change from one model to another.
On the other hand, the claim that two formulas are logically equivalent is a statement in the metalanguage, which expresses a relationship between two statements ${\displaystyle p}$ and ${\displaystyle q}$. The statements are logically equivalent if, in every model, they have the same truth value.
## References
1. "The Definitive Glossary of Higher Mathematical Jargon — Equivalent Claim". Math Vault. 2019-08-01. Retrieved 2019-11-24.
2. Mendelson, Elliott (1979). Introduction to Mathematical Logic (2 ed.). p. 56.
3. "Mathematics | Propositional Equivalences". GeeksforGeeks. 2015-06-22. Retrieved 2019-11-24.
4. "Mathematics | Propositional Equivalences". GeeksforGeeks. 2015-06-22. Retrieved 2019-11-24.
5. Copi, Irving; Cohen, Carl; McMahon, Kenneth (2014). Introduction to Logic (New International Edition ed.). Pearson. p. 348.CS1 maint: extra text (link)
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.
| 2021-11-27T12:32:54 |
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https://www.usgs.gov/publications/alaska
|
January 1, 2019
Alaska is the largest state in the Nation, almost one-fifth the size of the combined lower 48 United States, and is rich in natural capital resources. Alaska is often identified as being on the front lines of climate change since it is warming faster than any other state and faces a myriad of issues associated with a changing climate. The cost of infrastructure damage from a warming climate is projected to be very large, potentially ranging from $110 to$270 million per year, assuming timely repair and maintenance. Although climate change does and will continue to dramatically transform the climate and environment of the Arctic, proactive adaptation in Alaska has the potential to reduce costs associated with these impacts. This includes the dissemination of several tools, such as guidebooks to support adaptation planning, some of which focus on Indigenous communities. While many opportunities exist with a changing climate, economic prospects are not well captured in the literature at this time.
As the climate continues to warm, there is likely to be a nearly sea ice-free Arctic during the summer by mid-century. Ocean acidification is an emerging global problem that will intensify with continued carbon dioxide (CO2) emissions and negatively affects organisms. Climate change will likely affect management actions and economic drivers, including fisheries, in complex ways. The use of multiple alternative models to appropriately characterize uncertainty in future fisheries biomass trajectories and harvests could help manage these challenges. As temperature and precipitation increase across the Alaska landscape, physical and biological changes are also occurring throughout Alaska’s terrestrial ecosystems. Degradation of permafrost is expected to continue, with associated impacts to infrastructure, river and stream discharge, water quality, and fish and wildlife habitat.
Longer sea ice-free seasons, higher ground temperatures, and relative sea level rise are expected to exacerbate flooding and accelerate erosion in many regions, leading to the loss of terrestrial habitat in the future and in some cases requiring entire communities or portions of communities to relocate to safer terrain. The influence of climate change on human health in Alaska can be traced to three sources: direct exposures, indirect effects, and social or psychological disruption. Each of these will have different manifestations for Alaskans when compared to residents elsewhere in the United States. Climate change exerts indirect effects on human health in Alaska through changes to water, air, and soil and through ecosystem changes affecting disease ecology and food security, especially in rural communities.
Alaska’s rural communities are predominantly inhabited by Indigenous peoples who may be disproportionately vulnerable to socioeconomic and environmental change; however, they also have rich cultural traditions of resilience and adaptation. The impacts of climate change will likely affect all aspects of Alaska Native societies, from nutrition, infrastructure, economics, and health consequences to language, education, and the communities themselves.
The profound and diverse climate-driven changes in Alaska’s physical environment and ecosystems generate economic impacts through their effects on environmental services. These services include positive benefits directly from ecosystems (for example, food, water, and other resources), as well as services provided directly from the physical environment (for example, temperature moderation, stable ground for supporting infrastructure, and smooth surface for overland transportation). Some of these effects are relatively assured and in some cases are already occurring. Other impacts are highly uncertain, due to their dependence on the structure of global and regional economies and future human alterations to the environment decades into the future, but they could be large.
In Alaska, a range of adaptations to changing climate and related environmental conditions are underway and others have been proposed as potential actions, including measures to reduce vulnerability and risk, as well as more systemic institutional transformation.
| 2022-05-20T05:35:35 |
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http://trilinos.sandia.gov/packages/docs/dev/packages/ifpack/doc/html/classIfpack__SILU.html
|
IFPACK Development
Ifpack_SILU Class Reference
A wrapper to SuperLU 4.0's supernodal ILUT w/ partial pivoting. More...
#include <Ifpack_SILU.h>
Inheritance diagram for Ifpack_SILU:
[legend]
Collaboration diagram for Ifpack_SILU:
[legend]
List of all members.
## Public Member Functions
Constructors and destructors.
Ifpack_SILU (Epetra_RowMatrix *A)
Constructor.
~Ifpack_SILU ()
Destructor.
Construction methods
int Initialize ()
Initialize the preconditioner, does not touch matrix values.
bool IsInitialized () const
Returns true if the preconditioner has been successfully initialized.
int Compute ()
Compute ILU factors L and U using the specified graph, diagonal perturbation thresholds and relaxation parameters.
bool IsComputed () const
If factor is completed, this query returns true, otherwise it returns false.
int SetParameters (Teuchos::ParameterList ¶meterlist)
Set parameters using a Teuchos::ParameterList object.
int SetUseTranspose (bool UseTranspose_in)
If set true, transpose of this operator will be applied.
Mathematical functions.
int Apply (const Epetra_MultiVector &X, Epetra_MultiVector &Y) const
int Multiply (bool Trans, const Epetra_MultiVector &X, Epetra_MultiVector &Y) const
int ApplyInverse (const Epetra_MultiVector &X, Epetra_MultiVector &Y) const
Returns the result of a Epetra_Operator inverse applied to an Epetra_MultiVector X in Y.
double Condest (const Ifpack_CondestType CT=Ifpack_Cheap, const int MaxIters=1550, const double Tol=1e-9, Epetra_RowMatrix *Matrix_in=0)
Computes the estimated condition number and returns the value.
double Condest () const
Returns the computed estimated condition number, or -1.0 if not computed.
Query methods
const char * Label () const
Returns a character string describing the operator.
int SetLabel (const char *Label_in)
Sets label for this object.
double NormInf () const
Returns 0.0 because this class cannot compute Inf-norm.
bool HasNormInf () const
Returns false because this class cannot compute an Inf-norm.
bool UseTranspose () const
Returns the current UseTranspose setting.
const Epetra_MapOperatorDomainMap () const
Returns the Epetra_Map object associated with the domain of this operator.
const Epetra_MapOperatorRangeMap () const
Returns the Epetra_Map object associated with the range of this operator.
const Epetra_CommComm () const
Returns the Epetra_BlockMap object associated with the range of this matrix operator.
const Epetra_RowMatrixMatrix () const
Returns a reference to the matrix to be preconditioned.
virtual ostream & Print (ostream &os) const
Prints on stream basic information about this object.
virtual int NumInitialize () const
Returns the number of calls to Initialize().
virtual int NumCompute () const
Returns the number of calls to Compute().
virtual int NumApplyInverse () const
Returns the number of calls to ApplyInverse().
virtual double InitializeTime () const
Returns the time spent in Initialize().
virtual double ComputeTime () const
Returns the time spent in Compute().
virtual double ApplyInverseTime () const
Returns the time spent in ApplyInverse().
virtual double InitializeFlops () const
Returns the number of flops in the initialization phase.
virtual double ComputeFlops () const
Returns the number of flops in the computation phase.
virtual double ApplyInverseFlops () const
Returns the number of flops in the application of the preconditioner.
## Detailed Description
A wrapper to SuperLU 4.0's supernodal ILUT w/ partial pivoting.
The Ifpack_SILU class is a wrapper to SuperLU 4.0's supernodal ILUT w/ partial pivoting.
Date:
Definition at line 83 of file Ifpack_SILU.h.
## Member Function Documentation
int Ifpack_SILU::ApplyInverse ( const Epetra_MultiVector & X, Epetra_MultiVector & Y ) const [virtual]
Returns the result of a Epetra_Operator inverse applied to an Epetra_MultiVector X in Y.
In this implementation, we use several existing attributes to determine how virtual method ApplyInverse() should call the concrete method Solve(). We pass in the UpperTriangular(), the Epetra_CrsMatrix::UseTranspose(), and NoDiagonal() methods. The most notable warning is that if a matrix has no diagonal values we assume that there is an implicit unit diagonal that should be accounted for when doing a triangular solve.
Parameters:
X - (In) A Epetra_MultiVector of dimension NumVectors to solve for. Out Y - (Out) A Epetra_MultiVector of dimension NumVectors containing result.
Returns:
Integer error code, set to 0 if successful.
Implements Ifpack_Preconditioner.
Definition at line 354 of file Ifpack_SILU.cpp.
int Ifpack_SILU::SetUseTranspose ( bool UseTranspose_in ) [inline, virtual]
If set true, transpose of this operator will be applied.
This flag allows the transpose of the given operator to be used implicitly. Setting this flag affects only the Apply() and ApplyInverse() methods. If the implementation of this interface does not support transpose use, this method should return a value of -1.
Parameters:
UseTranspose_in - (In) If true, multiply by the transpose of operator, otherwise just use operator.
Returns:
Always returns 0.
Implements Epetra_Operator.
Definition at line 139 of file Ifpack_SILU.h.
The documentation for this class was generated from the following files:
| 2014-03-08T19:46:54 |
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|
https://pdglive.lbl.gov/DataBlock.action?node=B062RS2&home=BXXX005
|
# ${{\boldsymbol N}{(1520)}}$ INELASTIC POLE RESIDUE
The normalized residue'' is the residue divided by $\Gamma _{pole}$/2.
# Normalized residue in ${{\boldsymbol N}}$ ${{\boldsymbol \pi}}$ $\rightarrow$ ${{\boldsymbol N}{(1520)}}$ $\rightarrow$ ${{\boldsymbol \Delta}}{{\boldsymbol \pi}}$ , ${\boldsymbol D}{\mathrm -wave}$ INSPIRE search
MODULUS PHASE ($^\circ{}$) DOCUMENT ID TECN COMMENT
$0.25 \pm0.03$ 105+-18
2015 A
DPWA Multichannel
• • • We do not use the following data for averages, fits, limits, etc. • • •
$0.25 \pm0.03$ 100+-20
2012 A
DPWA Multichannel
References:
SOKHOYAN 2015A
EPJ A51 95 High-Statistics Study of the Reaction ${{\mathit \gamma}}$ ${{\mathit p}}$ $\rightarrow$ ${{\mathit p}}$2 ${{\mathit \pi}^{0}}$
ANISOVICH 2012A
EPJ A48 15 Properties of Baryon Resonances from a Multichannel Partial Wave Analysis
| 2020-10-24T11:57:50 |
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https://bison.inl.gov/Documentation/source/kernels/KKSPhaseChemicalPotential.aspx
|
# KKSPhaseChemicalPotential
KKS model kernel to enforce the pointwise equality of phase chemical potentials dFa/dca = dFb/dcb. The non-linear variable of this kernel is ca.
Enforces the point wise equality of the phase chemical potentials
\frac{dF_a}{dc_a}=\frac{dF_b}{dc_b}.
The non-linear variable of this Kernel is .
### Residual
R=\frac{dF_a}{dc_a} - \frac{dF_b}{dc_b}
### Jacobian
For the Jacobian we need to calculate
J=\frac \partial{\partial u_j}\left( \frac{dF_a}{dc_a} - \frac{dF_b}{dc_b} \right).
#### On-Diagonal
J = \phi_j \left( \frac{\partial2 F_a}{\partial c_a2} - \frac{\partial^2 F_b}{\partial c_a \partial c_b} \right)
#### Off-Diagonal
With the union of the argument vectors of and (represented in the code by _coupled_moose_vars[]) we get
\sum_i \left( \frac{\partial2 F_a}{\partial c_a \partial q_i}\frac{\partial q_i}{\partial u_j} - \frac{\partial2 F_b}{\partial c_b \partial q_i}\frac{\partial q_i}{\partial u_j} \right).
Again the is non-zero only if , which is the case if is the argument selected through jvar.
J = \frac{\partial2 F_a}{\partial c_a \partial q_\text{jvar}}\phi_j - \frac{\partial2 F_b}{\partial c_b \partial q_\text{jvar}}\phi_j.
Note that in the code jvar is not an index into _coupled_moose_vars[] but has to be resolved through the _jvar_map.
## Input Parameters
• variableThe name of the variable that this Kernel operates on
C++ Type:NonlinearVariableName
Description:The name of the variable that this Kernel operates on
• cbPhase b concentration
C++ Type:std::vector
Description:Phase b concentration
• fa_nameBase name of the free energy function Fa (f_name in the corresponding derivative function material)
C++ Type:MaterialPropertyName
Description:Base name of the free energy function Fa (f_name in the corresponding derivative function material)
• fb_nameBase name of the free energy function Fb (f_name in the corresponding derivative function material)
C++ Type:MaterialPropertyName
Description:Base name of the free energy function Fb (f_name in the corresponding derivative function material)
### Required Parameters
• args_aVector of further parameters to Fa (optional, to add in second cross derivatives of Fa)
C++ Type:std::vector
Description:Vector of further parameters to Fa (optional, to add in second cross derivatives of Fa)
• args_bVector of further parameters to Fb (optional, to add in second cross derivatives of Fb)
C++ Type:std::vector
Description:Vector of further parameters to Fb (optional, to add in second cross derivatives of Fb)
• blockThe list of block ids (SubdomainID) that this object will be applied
C++ Type:std::vector
Description:The list of block ids (SubdomainID) that this object will be applied
### Optional Parameters
• enableTrueSet the enabled status of the MooseObject.
Default:True
C++ Type:bool
Description:Set the enabled status of the MooseObject.
• save_inThe name of auxiliary variables to save this Kernel's residual contributions to. Everything about that variable must match everything about this variable (the type, what blocks it's on, etc.)
C++ Type:std::vector
Description:The name of auxiliary variables to save this Kernel's residual contributions to. Everything about that variable must match everything about this variable (the type, what blocks it's on, etc.)
• use_displaced_meshFalseWhether or not this object should use the displaced mesh for computation. Note that in the case this is true but no displacements are provided in the Mesh block the undisplaced mesh will still be used.
Default:False
C++ Type:bool
Description:Whether or not this object should use the displaced mesh for computation. Note that in the case this is true but no displacements are provided in the Mesh block the undisplaced mesh will still be used.
• control_tagsAdds user-defined labels for accessing object parameters via control logic.
C++ Type:std::vector
Description:Adds user-defined labels for accessing object parameters via control logic.
• seed0The seed for the master random number generator
Default:0
C++ Type:unsigned int
Description:The seed for the master random number generator
• diag_save_inThe name of auxiliary variables to save this Kernel's diagonal Jacobian contributions to. Everything about that variable must match everything about this variable (the type, what blocks it's on, etc.)
C++ Type:std::vector
Description:The name of auxiliary variables to save this Kernel's diagonal Jacobian contributions to. Everything about that variable must match everything about this variable (the type, what blocks it's on, etc.)
• implicitTrueDetermines whether this object is calculated using an implicit or explicit form
Default:True
C++ Type:bool
Description:Determines whether this object is calculated using an implicit or explicit form
• vector_tagsnontimeThe tag for the vectors this Kernel should fill
Default:nontime
C++ Type:MultiMooseEnum
Description:The tag for the vectors this Kernel should fill
• extra_vector_tagsThe extra tags for the vectors this Kernel should fill
C++ Type:std::vector
Description:The extra tags for the vectors this Kernel should fill
• matrix_tagssystemThe tag for the matrices this Kernel should fill
Default:system
C++ Type:MultiMooseEnum
Description:The tag for the matrices this Kernel should fill
• extra_matrix_tagsThe extra tags for the matrices this Kernel should fill
C++ Type:std::vector
Description:The extra tags for the matrices this Kernel should fill
| 2020-11-29T08:25:37 |
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|
https://math.libretexts.org/Bookshelves/Algebra/Map%3A_College_Algebra_(OpenStax)/01%3A_Prerequisites
|
# 1: Prerequisites
$$\newcommand{\vecs}[1]{\overset { \scriptstyle \rightharpoonup} {\mathbf{#1}} }$$
$$\newcommand{\vecd}[1]{\overset{-\!-\!\rightharpoonup}{\vphantom{a}\smash {#1}}}$$
In this chapter, we will review sets of numbers and properties of operations used to manipulate numbers. This understanding will serve as prerequisite knowledge throughout our study of algebra and trigonometry.
Thumbnail: A shortcut called FOIL is sometimes used to find the product of two binomials. It is called FOIL because we multiply the first terms, the outer terms, the inner terms, and then the last terms of each binomial.
## Contributors
• Lynn Marecek (Santa Ana College) and MaryAnne Anthony-Smith (formerly of Santa Ana College). This content produced by OpenStax and is licensed under a Creative Commons Attribution License 4.0 license.
| 2019-12-14T02:33:10 |
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https://runescapeclassic.fandom.com/wiki/Experience
|
## FANDOM
4,034 Pages
Killing monsters and fulfilling certain tasks will grant players experience (also known as exp, xp, or experience points), which they accumulate to increase skill levels. Training skills generically is the typical way to gain experience, however quests often reward some. To reach level 99 in a skill, the player needs to reach 13,034,431 XP. Half of that amount is nearly enough for level 92, and a quarter of it barely reaches level 85. To reach level 99 in all 18 skills, the player will have accumulated 234,619,758 exp.
## Hits
The Hits skill is a special case, since all accounts start with level 10 and 1,000 experience (after character classes were removed). This isn't enough for level 10 in other skills, however. When RuneScape 2 was released, accounts that had not reached 1154 Hits XP for true level 10 had their Hitpoints level in RS2 set to the correct value for 1000 XP — level 9.
## Maximum experience in a single skill
Unlike RS2, RuneScape Classic does not have an experience cap at 200 million. Instead, it is not possible to exceed 536,870,911 ($\frac{2^{31} - 1}{4}$) experience in a single skill because of data type limits.
Passing the maximum XP results in an integer overflow, and the displayed value will wrap around to a very large negative number. It is possible to continue gaining experience afterwards. Going from negative experience to positive does not cause the level to reset to level 1. Only one person is currently known to have negative experience (in Thieving).
The reason for the limit being a quarter of the usual maximum for 32-bit singed integers (2,147,483,647) is precision. The number is divided by four before being displayed in order to allow for a limit set of possible experience values below 0 (0.25, 0.5, and 0.75). For example, killing a chicken gives 6.5 Hits XP, but the number beyond the decimal point is not displayed on screen.
## Experience table
The following table shows the relationship between skill level, the experience required for that level, and the difference in experience from the previous level:
Level Exp Exp Diff Level Exp Exp Diff Level Exp Exp Diff Level Exp Exp Diff
1 0 0 26 8,740 898 51 111,945 10,612 76 1,336,443 126,022
2 83 83 27 9,730 990 52 123,660 11,715 77 1,475,581 139,138
3 174 91 28 10,824 1,094 53 136,594 12,934 78 1,629,200 153,619
4 276 102 29 12,031 1,207 54 150,872 14,278 79 1,798,808 169,608
5 388 112 30 13,363 1,332 55 166,636 15,764 80 1,986,068 187,260
6 512 124 31 14,833 1,470 56 184,040 17,404 81 2,192,818 206,750
7 650 138 32 16,456 1,623 57 203,254 19,214 82 2,421,087 228,269
8 801 151 33 18,247 1,791 58 224,466 21,212 83 2,673,114 252,027
9 969 168 34 20,224 1,977 59 247,886 23,420 84 2,951,373 278,259
10 1,154 185 35 22,406 2,182 60 273,742 25,856 85 3,258,594 307,221
11 1,358 204 36 24,815 2,409 61 302,288 28,546 86 3,597,792 339,198
12 1,584 226 37 27,473 2,658 62 333,804 31,516 87 3,972,294 374,502
13 1,833 249 38 30,408 2,935 63 368,599 34,795 88 4,385,776 413,482
14 2,107 274 39 33,648 3,240 64 407,015 38,416 89 4,842,295 456,519
15 2,411 304 40 37,224 3,576 65 449,428 42,413 90 5,346,332 504,037
16 2,746 335 41 41,171 3,947 66 496,254 46,826 91 5,902,831 556,499
17 3,115 369 42 45,529 4,358 67 547,953 51,699 92 6,517,253 614,422
18 3,523 408 43 50,339 4,810 68 605,032 57,079 93 7,195,629 678,376
19 3,973 450 44 55,649 5,310 69 668,051 63,019 94 7,944,614 748,985
20 4,470 497 45 61,512 5,863 70 737,627 69,576 95 8,771,558 826,944
21 5,018 548 46 67,983 6,471 71 814,445 76,818 96 9,684,577 913,019
22 5,624 606 47 75,127 7,144 72 899,257 84,812 97 10,692,629 1,008,052
23 6,291 667 48 83,014 7,887 73 992,895 93,638 98 11,805,606 1,112,977
24 7,028 737 49 91,721 8,707 74 1,096,278 103,383 99 13,034,431 1,228,825
25 7,842 814 50 101,333 9,612 75 1,210,421 114,143 Level 99 is the max
Community content is available under CC-BY-SA unless otherwise noted.
| 2020-02-18T13:45:22 |
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https://blogs.nasa.gov/sofia/2022/08/26/sofia-finds-more-water-in-the-moons-southern-hemisphere/moretus-final/
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# Water Abundances in the Moon’s Moretus Crater Region
The image shows flux data obtained by SOFIA’s FORCAST instrument overlaid on an orthographic projection of the Moon, creating a map of water abundances in the Moretus Crater region. Surface lunar features are clearly visible within the flux data. In this image, lighter colors correspond to a higher flux, and darker corresponds to a lower flux. Credit: Honniball et al. and Applied Coherent Technology Corp. The Moon reference image is constructed using the LRO-WAC albedo mosaic.
| 2022-09-24T23:47:56 |
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http://supercgis.com/standard-error/relation-of-standard-deviation-to-standard-error.html
|
Home > Standard Error > Relation Of Standard Deviation To Standard Error
# Relation Of Standard Deviation To Standard Error
## Contents
doi: 10.1136/bmj.331.7521.903PMCID: PMC1255808Statistics NotesStandard deviations and standard errorsDouglas G Altman, professor of statistics in medicine1 and J Martin Bland, professor of health statistics21 Cancer Research UK/NHS Centre for Statistics in Medicine, Statements, such as average 3.4 cm (±1.2), are ambiguous and should not be used. Representative Sample A subset of a statistical population that accurately reflects ... The 95% confidence interval for the average effect of the drug is that it lowers cholesterol by 18 to 22 units. http://supercgis.com/standard-error/reporting-standard-error-versus-standard-deviation.html
Later sections will present the standard error of other statistics, such as the standard error of a proportion, the standard error of the difference of two means, the standard error of Clark-Carter D. The standard deviation of the age for the 16 runners is 10.23, which is somewhat greater than the true population standard deviation σ = 9.27 years. This often leads to confusion about their interchangeability. More Bonuses
## Standard Error To Standard Deviation Calculator
Sokal and Rohlf (1981)[7] give an equation of the correction factor for small samples ofn<20. The standard error of a proportion and the standard error of the mean describe the possible variability of the estimated value based on the sample around the true proportion or true The data set is ageAtMar, also from the R package openintro from the textbook by Dietz et al.[4] For the purpose of this example, the 5,534 women are the entire population
For example, the U.S. JSTOR2682923. ^ Sokal and Rohlf (1981) Biometry: Principles and Practice of Statistics in Biological Research , 2nd ed. Assuming a normal distribution, around 68% of daily price changes are within one SD of the mean, with around 95% of daily price changes within two SDs of the mean. Standard Error Calculator The sample standard deviation s = 10.23 is greater than the true population standard deviation σ = 9.27 years.
Sampling is a term used in statistics that describes methods of selecting a pre-defined representative number of data from a larger data population. Calculate Standard Error From Standard Deviation In Excel The mean age was 23.44 years. It will be shown that the standard deviation of all possible sample means of size n=16 is equal to the population standard deviation, σ, divided by the square root of the http://ncalculators.com/math-worksheets/calculate-standard-deviation-standard-error.htm doi: 10.1007/s11999-011-1908-9PMCID: PMC3148365In Brief: Standard Deviation and Standard ErrorDavid J.
Standard error of the mean (SEM) This section will focus on the standard error of the mean. Standard Error Of The Mean For example, the sample mean is the usual estimator of a population mean. When the sampling fraction is large (approximately at 5% or more) in an enumerative study, the estimate of the standard error must be corrected by multiplying by a "finite population correction"[9] Relevant details of the t distribution are available as appendices of many statistical textbooks, or using standard computer spreadsheet packages.
## Calculate Standard Error From Standard Deviation In Excel
Assets Under Management - AUM The market value of assets that an investment company manages on behalf of investors. directory In it, you'll get: The week's top questions and answers Important community announcements Questions that need answers see an example newsletter By subscribing, you agree to the privacy policy and terms Standard Error To Standard Deviation Calculator Discover how the different techniques used to select representative samples and unbiased samples are often exploited and ... Convert Standard Deviation To Standard Error In Excel The formula for the SEM is the standard deviation divided by the square root of the sample size.
Perspect Clin Res. 3 (3): 113–116. http://supercgis.com/standard-error/relationship-between-standard-deviation-and-standard-error-of-measurement.html For example, the sample mean is the usual estimator of a population mean. Journal of the Royal Statistical Society. The data set is ageAtMar, also from the R package openintro from the textbook by Dietz et al.[4] For the purpose of this example, the 5,534 women are the entire population Convert Standard Error To Variance
They may be used to calculate confidence intervals. Standard deviation (s) = Standard Error * √n = 20.31 x √9 = 20.31 x 3 s = 60.93 variance = σ2 = 60.932 = 3712.46 For more information for dispersion The mean age was 33.88 years. this contact form With n = 2 the underestimate is about 25%, but for n = 6 the underestimate is only 5%.
The survey with the lower relative standard error can be said to have a more precise measurement, since it has proportionately less sampling variation around the mean. How To Calculate Standard Error Of The Mean Understand the basics of calculation and interpretation of standard deviation and how it is used to measure risk in the investment ... The unbiased estimate of population variance calculated from a sample is: [xi is the ith observation from a sample of the population, x-bar is the sample mean, n (sample size) -1
## The margin of error of 2% is a quantitative measure of the uncertainty – the possible difference between the true proportion who will vote for candidate A and the estimate of
The effect of the FPC is that the error becomes zero when the sample size n is equal to the population size N. It is rare that the true population standard deviation is known. Read Answer >> What is the difference between a simple random sample and a stratified random sample? Standard Error Of Estimate First, take the square of the difference between each data point and the sample mean, finding the sum of those values.
Note: the standard error and the standard deviation of small samples tend to systematically underestimate the population standard error and deviations: the standard error of the mean is a biased estimator For the age at first marriage, the population mean age is 23.44, and the population standard deviation is 4.72. However, the SD may be more or less depending on the dispersion of the additional data added to the sample. navigate here Correction for finite population The formula given above for the standard error assumes that the sample size is much smaller than the population size, so that the population can be considered
The standard deviation of the sample mean is $\sigma/\sqrt{n}$ where $\sigma$ is the (population) standard deviation of the data and $n$ is the sample size - this may be what you're For a value that is sampled with an unbiased normally distributed error, the above depicts the proportion of samples that would fall between 0, 1, 2, and 3 standard deviations above Another way of considering the standard error is as a measure of the precision of the sample mean.The standard error of the sample mean depends on both the standard deviation and For illustration, the graph below shows the distribution of the sample means for 20,000 samples, where each sample is of size n=16.
For an upcoming national election, 2000 voters are chosen at random and asked if they will vote for candidate A or candidate B. Text is available under the Creative Commons Attribution-ShareAlike License; additional terms may apply.
| 2017-06-29T02:11:35 |
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|
http://astronomy.wikia.com/wiki/Weakly_interacting_massive_particles
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## FANDOM
420 Pages
Includes CC-BY-SA content from Wikipedia's Weakly interacting massive particles article (authors)
In particle physics and astrophysics, weakly interacting massive particles, or WIMPs, are among the leading hypothetical particle physics candidates for dark matter. The term “WIMP” is given to a dark matter particle that was produced by falling out of thermal equilibrium with the hot dense plasma of the early universe, although it is often used to refer to any dark matter candidate that interacts with standard particles via a force similar in strength to the weak nuclear force. Its name comes from the fact that obtaining the correct abundance of dark matter today via thermal production requires a self-annihilation cross section of $\langle \sigma v \rangle \simeq 3 \times 10^{-26} \mathrm{cm}^{3} \;\mathrm{s}^{-1}$, which is roughly what is expected for a new particle in the 100 GeV mass range that interacts via the electroweak force. Because supersymmetric extensions of the standard model of particle physics readily predict a new particle with these properties, this apparent coincidence is known as the “WIMP miracle”, and a stable supersymmetric partner has long been a prime WIMP candidate. However, recent null results from direct detection experiments including LUX and SuperCDMS, along with the failure to produce evidence of supersymmetry in the Large Hadron Collider (LHC) experiment. Experimental efforts to detect WIMPs include the search for products of WIMP annihilation, including gamma rays, neutrinos and cosmic rays in nearby galaxies and galaxy clusters; direct detection experiments designed to measure the collision of WIMPs with nuclei in the laboratory, as well as attempts to directly produce WIMPs in colliders, such as the LHC.
## Theoretical framework and propertiesEdit
WIMP-like particles are predicted by R-parity-conserving supersymmetry, a popular type of extension to the standard model of particle physics, although none of the large number of new particles in supersymmetry have been observed. WIMP-like particles are also predicted by universal extra dimension and little Higgs.
Model parity candidate
SUSY R-parity lightest supersymmetric particle (LSP)
UED KK-parity lightest Kaluza-Klein particle (LKP)
little Higgs T-parity lightest T-odd particle (LTP)
The main theoretical characteristics of a WIMP are:
Because of their lack of electromagnetic interaction with normal matter, WIMPs would be dark and invisible through normal electromagnetic observations. Because of their large mass, they would be relatively slow moving and therefore "cold". Their relatively low velocities would be insufficient to overcome the mutual gravitational attraction, and as a result WIMPs would tend to clump together. WIMPs are considered one of the main candidates for cold dark matter, the others being massive compact halo objects (MACHOs) and axions. (These names were deliberately chosen for contrast, with MACHOs named later than WIMPs. Also, in contrast to MACHOs, there are no known stable particles within the standard model of particle physics that have all the properties of WIMPs. The particles that have little interaction with normal matter, such as neutrinos, are all very light, and hence would be fast moving, or "hot".
## WIMPs as dark matterEdit
Although the existence of WIMPs in nature is hypothetical at this point, it would resolve a number of astrophysical and cosmological problems related to dark matter. There is near consensus today among astronomers that most of the mass in the Universe is dark. Simulations of a universe full of cold dark matter produce galaxy distributions that are roughly similar to what is observed. By contrast, hot dark matter would smear out the large-scale structure of galaxies and thus is not considered a viable cosmological model.
The WIMP fits the model of a relic dark matter particle from the early Universe, when all particles were in a state of thermal equilibrium. For sufficiently high temperatures, such as those existing in the early Universe, the dark matter particle and its antiparticle would have been both forming from and annihilating into lighter particles. As the Universe expanded and cooled, the average thermal energy of these lighter particles decreased and eventually became insufficient to form a dark matter particle-antiparticle pair. The annihilation of the dark matter particle-antiparticle pairs, however, would have continued, and the number density of dark matter particles would have begun to decrease exponentially. Eventually, however, the number density would become so low that the dark matter particle and antiparticle interaction would cease, and the number of dark matter particles would remain (roughly) constant as the Universe continued to expand. Particles with a larger interaction cross section would continue to annihilate for a longer period of time, and thus would have a smaller number density when the annihilation interaction ceases. Based on the current estimated abundance of dark matter in the Universe, if the dark matter particle is such a relic particle, the interaction cross section governing the particle-antiparticle annihilation can be no larger than the cross section for the weak interaction. If this model is correct, the dark matter particle would have the properties of the WIMP.
## Experimental detectionEdit
Because WIMPs may only interact through gravitational and weak forces, they are extremely difficult to detect. However, there are many experiments underway to attempt to detect WIMPs both directly and indirectly. Direct detection refers to the observation of the effects of a WIMP-nucleus collision as the dark matter passes through a detector in an Earth laboratory. Indirect detection refers to the observation of annihilation or decay products of WIMPs far away from Earth.
Indirect detection efforts typically focus on locations where WIMP dark matter is thought to accumulate the most: in the centers of galaxies and galaxy clusters, as well as in the smaller satellite galaxies of the Milky Way. These are particularly useful since they tend to contain very little baryonic matter, reducing the expected background from standard astrophysical processes. Typical indirect searches look for excess gamma rays, which are predicted both as final-state products of annihilation, or are produced as charged particles interact with ambient radiation via inverse Compton scattering. The spectrum and intensity of a gamma ray signal depends on the annihilation products, and must be computed on a model-by-model basis. Experiments that have placed bounds on WIMP annihilation, via the non-observation of an annihilation signal, include the Fermi-LAT gamma ray telescope and the VERITAS ground-based gamma ray observatory. Although the annihilation of WIMPs into standard model particles also predicts the production of high-energy neutrinos, their interaction rate is too low to reliably detect a dark matter signal at present. Future observations from the IceCube observatory in Antarctica may be able to differentiate WIMP-produced neutrinos from standard astrophysical neutrinos; however, at present, only 37 cosmological neutrinos have been observed, making such a distinction impossible.
Another type of indirect WIMP signal could come from the Sun. Halo WIMPs may, as they pass through the Sun, interact with solar protons, helium nuclei as well as heavier elements. If a WIMP loses enough energy in such an interaction to fall below the local escape velocity, it would not have enough energy to escape the gravitational pull of the Sun and would remain gravitationally bound. As more and more WIMPs thermalize inside the Sun, they begin to annihilate with each other, forming a variety of particles, including high-energy neutrinos. These neutrinos may then travel to the Earth to be detected in one of the many neutrino telescopes, such as the Super-Kamiokande detector in Japan. The number of neutrino events detected per day at these detectors depends on the properties of the WIMP, as well as on the mass of the Higgs boson. Similar experiments are underway to detect neutrinos from WIMP annihilations within the Earth and from within the galactic center.
While most WIMP models indicate that a large enough number of WIMPs must be captured in large celestial bodies for these experiments to succeed, it remains possible that these models are either incorrect or only explain part of the dark matter phenomenon. Thus, even with the multiple experiments dedicated to providing indirect evidence for the existence of cold dark matter, direct detection measurements are also necessary to solidify the theory of WIMPs.
Although most WIMPs encountering the Sun or the Earth are expected to pass through without any effect, it is hoped that a large number of dark matter WIMPs crossing a sufficiently large detector will interact often enough to be seen—at least a few events per year. The general strategy of current attempts to detect WIMPs is to find very sensitive systems that can be scaled up to large volumes. This follows the lessons learned from the history of the discovery and (by now) routine detection of the neutrino.
### Cryogenic crystal detectorsEdit
A technique used by the Cryogenic Dark Matter Search (CDMS) detector at the Soudan Mine relies on multiple very cold germanium and silicon crystals. The crystals (each about the size of a hockey puck) are cooled to about 50 mK. A layer of metal (aluminium and tungsten) at the surfaces is used to detect a WIMP passing through the crystal. This design hopes to detect vibrations in the crystal matrix generated by an atom being "kicked" by a WIMP. The tungsten transition edge sensors (TES) are held at the critical temperature so they are in the superconducting state. Large crystal vibrations will generate heat in the metal and are detectable because of a change in resistance. CRESST, CoGeNT, and EDELWEISS run similar setups.
### Noble gas scintillatorsEdit
Another way of detecting atoms "knocked about" by a WIMP is to use scintillating material, so that light pulses are generated by the moving atom and detected, often with PMTs. Experiments such as DEAP at SNOLAB, DarkSide, or WARP at the LNGS plan to instrument a very large target mass of liquid argon for sensitive WIMP searches. ZEPLIN, and XENON used xenon to exclude WIMPs at higher sensitivity until superseded in sensitivity by LUX in 2013. Larger ton-scale expansions of these xenon detectors have been approved for construction. PandaX is also using xenon. Neon may used in future studies.
### Crystal scintillatorsEdit
Instead of a liquid noble gas, an in principle simpler approach is the use of a scintillating crystal such as NaI(Tl). This approach is taken by DAMA/LIBRA, an experiment that observed an annular modulation of the signal consistent with WIMP detection (see #Recent Limits). Several experiments are attempting to replicate those results, including ANAIS and DM-Ice, which is codeploying NaI crystals with the IceCube detector at the South Pole. KIMS is approaching the same problem using CsI(Tl) as a scintillator.
### Bubble chambersEdit
The PICASSO (Project In Canada to Search for Supersymmetric Objects) experiment is a direct dark matter search experiment that is located at SNOLAB in Canada. It uses bubble detectors with Freon as the active mass. PICASSO is predominantly sensitive to spin-dependent interactions of WIMPs with the fluorine atoms in the Freon. COUPP, a similar experiment using trifluoroiodomethane(CF3I), published limits for mass above 20 GeV in 2011.
A bubble detector is a radiation sensitive device that uses small droplets of superheated liquid that are suspended in a gel matrix. It uses the principle of a bubble chamber but, since only the small droplets can undergo a phase transition at a time, the detector can stay active for much longer periods.When enough energy is deposited in a droplet by ionizing radiation, the superheated droplet becomes a gas bubble. The bubble development is accompanied by an acoustic shock wave that is picked up by piezo-electric sensors. The main advantage of the bubble detector technique is that the detector is almost insensitive to background radiation. The detector sensitivity can be adjusted by changing the temperature, typically operated between 15 °C and 55 °C. There is another similar experiment using this technique in Europe called SIMPLE.
PICASSO reports results (November 2009) for spin-dependent WIMP interactions on 19F, for masses of 24 Gev new stringent limits have been obtained on the spin-dependent cross section of 13.9 pb (90% CL). The obtained limits restrict recent interpretations of the DAMA/LIBRA annual modulation effect in terms of spin dependent interactions.
PICO is an expansion of the concept planned in 2015.
### Other Edit
Time Project Chambers (TPC) filled with low pressure gases are being studied for WIMP detection. The Directional Recoil Identification From Tracks (DRIFT) collaboration is attempting to utilize the predicted directionality of the WIMP signal. DRIFT uses a carbon disulfide target, that allows WIMP recoils to travel several millimetres, leaving a track of charged particles. This charged track is drifted to an MWPC readout plane that allows it to be reconstructed in three dimensions and determine the origin direction. DMTPC is a similar experiment with CF4 gas.
## Recent limitsEdit
In February 2010, researchers at CDMS-II announced that they had observed two events that may have been caused by WIMP-nucleus collisions. CoGeNT, a smaller detector using a single germanium puck, designed to sense WIMPs with smaller masses, reported hundreds of detection events in 56 days. Juan Collar, who presented the results to a conference at the University of California, was quoted: "If it's real, we're looking at a very beautiful dark-matter signal".
Annual modulation is one of the predicted signatures of a WIMP signal, and on this basis the DAMA collaboration has claimed a positive detection. Other groups, however, have not confirmed this result. The CDMS data made public in May 2004 exclude the entire DAMA signal region given certain standard assumptions about the properties of the WIMPs and the dark matter halo. CDMS and EDELWEISS would be expected to observe a significant number of WIMP-nucleus scatters if the DAMA signal were in fact caused by WIMPs.
Current limits from LUX and other searches are in disagreement with any WIMP interpretation of these results. With 370 kilograms of xenon it is more sensitive than XENON or CDMS.
| 2017-06-28T21:00:08 |
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https://par.nsf.gov/biblio/10310557-vector-output-relu-neural-network-problems-copositive-programs-convex-analysis-two-layer-networks-polynomial-time-algorithms
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Vector-output ReLU Neural Network Problems are Copositive Programs: Convex Analysis of Two Layer Networks and Polynomial-time Algorithms
We describe the convex semi-infinite dual of the two-layer vector-output ReLU neural network training problem. This semi-infinite dual admits a finite dimensional representation, but its support is over a convex set which is difficult to characterize. In particular, we demonstrate that the non-convex neural network training problem is equivalent to a finite-dimensional convex copositive program. Our work is the first to identify this strong connection between the global optima of neural networks and those of copositive programs. We thus demonstrate how neural networks implicitly attempt to solve copositive programs via semi-nonnegative matrix factorization, and draw key insights from this formulation. We describe the first algorithms for provably finding the global minimum of the vector output neural network training problem, which are polynomial in the number of samples for a fixed data rank, yet exponential in the dimension. However, in the case of convolutional architectures, the computational complexity is exponential in only the filter size and polynomial in all other parameters. We describe the circumstances in which we can find the global optimum of this neural network training problem exactly with soft-thresholded SVD, and provide a copositive relaxation which is guaranteed to be exact for certain classes of problems, and which more »
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Publication Date:
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10310557
Journal Name:
International Conference on Learnining Representations (ICLR)
National Science Foundation
##### More Like this
1. We develop a convex analytic approach to analyze finite width two-layer ReLU networks. We first prove that an optimal solution to the regularized training problem can be characterized as extreme points of a convex set, where simple solutions are encouraged via its convex geometrical properties. We then leverage this characterization to show that an optimal set of parameters yield linear spline interpolation for regression problems involving one dimensional or rank-one data. We also characterize the classification decision regions in terms of a kernel matrix and minimum 1-norm solutions. This is in contrast to Neural Tangent Kernel which is unable to explain predictions of finite width networks. Our convex geometric characterization also provides intuitive explanations of hidden neurons as auto-encoders. In higher dimensions, we show that the training problem can be cast as a finite dimensional convex problem with infinitely many constraints. Then, we apply certain convex relaxations and introduce a cutting-plane algorithm to globally optimize the network. We further analyze the exactness of the relaxations to provide conditions for the convergence to a global optimum. Our analysis also shows that optimal network parameters can be also characterized as interpretable closed-form formulas in some practically relevant special cases.
2. We develop exact representations of training twolayer neural networks with rectified linear units (ReLUs) in terms of a single convex program with number of variables polynomial in the number of training samples and the number of hidden neurons. Our theory utilizes semi-infinite duality and minimum norm regularization. We show that ReLU networks trained with standard weight decay are equivalent to block 1 penalized convex models. Moreover, we show that certain standard convolutional linear networks are equivalent semidefinite programs which can be simplified to 1 regularized linear models in a polynomial sized discrete Fourier feature space.
3. We study training of Convolutional Neural Networks (CNNs) with ReLU activations and introduce exact convex optimization formulations with a polynomial complexity with respect to the number of data samples, the number of neurons, and data dimension. More specifically, we develop a convex analytic framework utilizing semi-infinite duality to obtain equivalent convex optimization problems for several two- and three-layer CNN architectures. We first prove that two-layer CNNs can be globally optimized via an 2 norm regularized convex program. We then show that multi-layer circular CNN training problems with a single ReLU layer are equivalent to an 1 regularized convex program that encourages sparsity in the spectral domain. We also extend these results to three-layer CNNs with two ReLU layers. Furthermore, we present extensions of our approach to different pooling methods, which elucidates the implicit architectural bias as convex regularizers.
4. We develop a convex analytic framework for ReLU neural networks which elucidates the inner workings of hidden neurons and their function space characteristics. We show that neural networks with rectified linear units act as convex regularizers, where simple solutions are encouraged via extreme points of a certain convex set. For one dimensional regression and classification, as well as rank-one data matrices, we prove that finite two-layer ReLU networks with norm regularization yield linear spline interpolation. We characterize the classification decision regions in terms of a closed form kernel matrix and minimum L1 norm solutions. This is in contrast to Neural Tangent Kernel which is unable to explain neural network predictions with finitely many neurons. Our convex geometric description also provides intuitive explanations of hidden neurons as auto encoders. In higher dimensions, we show that the training problem for two-layer networks can be cast as a finite dimensional convex optimization problem with infinitely many constraints. We then provide a family of convex relaxations to approximate the solution, and a cutting-plane algorithm to improve the relaxations. We derive conditions for the exactness of the relaxations and provide simple closed form formulas for the optimal neural network weights in certain cases. We alsomore »
5. Understanding the fundamental mechanism behind the success of deep neural networks is one of the key challenges in the modern machine learning literature. Despite numerous attempts, a solid theoretical analysis is yet to be developed. In this paper, we develop a novel unified framework to reveal a hidden regularization mechanism through the lens of convex optimization. We first show that the training of multiple threelayer ReLU sub-networks with weight decay regularization can be equivalently cast as a convex optimization problem in a higher dimensional space, where sparsity is enforced via a group 1- norm regularization. Consequently, ReLU networks can be interpreted as high dimensional feature selection methods. More importantly, we then prove that the equivalent convex problem can be globally optimized by a standard convex optimization solver with a polynomial-time complexity with respect to the number of samples and data dimension when the width of the network is fixed. Finally, we numerically validate our theoretical results via experiments involving both synthetic and real datasets.
| 2022-11-30T01:11:48 |
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https://www.abs.gov.au/methodologies/labour-force-status-families-methodology/jun-2020
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This is not the latest release View the latest release
# Labour Force Status of Families methodology
Reference period
June 2020
Released
16/10/2020
## Introduction
Labour force estimates of families are produced from data collected in the monthly Labour Force Survey (LFS) in June. Since these products are all based on data collected in the LFS, the methodology of publication Labour Force, Australia is relevant to all three publications. Additional information is provided in Labour Statistics: Concepts, Sources and Methods.
## What is a family?
A family is defined as two related people who live in the same household. This includes all families such as couples with and without children, including same-sex couples, couples with dependants, single mothers or fathers with children, and siblings living together. At least one person in the family has to be 15 years or over. A household may contain more than one family.
### More on how families are defined
#### Family composition
The primary relationships that define family units are couple relationships and parent-child relationships. From these, there are three main types of families: couple families, one parent families, and other families.
• Couple families are based around two people in a couple relationship who usually live together in the same household. Couples can be same-sex or opposite-sex, and their dependants or children may also be members of the couple family if they all reside in the same household.
• One parent families are based around a person who is not in a couple relationship with anyone who usually lives in the same household, but has at least one child who usually lives in the household regardless of the age of the child. These households can include other related individuals. While couple families can be made up of couples with or without children - one parent families necessarily include children.
• Other families are defined as a group of other related individuals residing in the same household. These individuals do not form a couple or parent-child relationship with any other person in the household and are not related to any couple or one-parent families that might also be in the same household.
In some cases, a household will contain more than one family. Multi-generational households or households with many family members may be split into smaller family units. For example, a single mother with a baby living with her parents forms two families in the one household. The parents are one couple family and the daughter and her baby form one lone parent family.
#### What is not a family?
People who live alone or who live in households with non-relatives, such as students sharing a flat (with no couple relationships), are not considered to be in a family. Family members who usually live across different households are also not included. These statistics are intended to reflect families who usually live together in the same household.
There are special cases for when a child under 15 years old is living with non-relatives. In these cases, the child is considered to be dependent, so they form a child dependency relationship with the oldest member of the household (the family head), thereby forming a one parent family.
#### What is a dependant?
Families can be classed as having, or not having, dependants. There are two kinds of dependants:
• children under 15 years, and
• dependent students aged 15 to 24 years who are attending school or studying full-time at a tertiary education institution and living with their parents/guardians.
These children are considered to be financially dependent on the parent or parents that they usually live with, which is why they are referred to as 'dependants'. However, they have to be usually living in the same household; full-time students who have left home to study and live by themselves are not considered to be part of the family in that household, even if they remain financially dependent on their parents.
Children aged over 15 years who are not full-time students are not considered dependent on their parents, even if they still live at home. It is also possible to have one parent families without dependants, (such as, an 80 year old mother living with her 55 year old daughter).
It is important to consider whether children in a household are dependent on their parents when looking at these estimates, as the labour force characteristics will vary between families who have dependants and those that do not.
## Scope
Family data was collected for people who were usual residents of private dwellings and whose family relationships could be derived. Children under 15 are included in scope, and their characteristics are used in the classification of parent-child relationships and family type.
People interviewed in the LFS who were classed as visitors to private dwellings, and those living in non-private dwellings (including hotels, motels, hospitals and other institutions) were excluded. People living in remote Aboriginal and Torres Strait Islander communities were also excluded. After these exclusions were applied, the estimates in this publication for June 2020 cover approximately 80% of the survey sample.
## Benchmarking and estimation
The estimates are calculated in such a way as to sum to independent counts of people and households (benchmarks). These benchmarks are updated based on Estimated Resident Population (ERP) data.
For all data published in this release, estimates have been compiled using benchmarks that have been rebased to the results of the 2016 Census. These benchmarks have been revised to include the ERP data as at June 2020. For more details on population benchmarks, see the Methodology of Labour Force, Australia.
## Survey output
A number of spreadsheets are available from the Data downloads section of this publication. They present tables of estimates and their corresponding relative standard errors (RSEs).
For users who wish to undertake more detailed analysis, the underlying microdata is available in ABS TableBuilder. For more details, refer to Microdata, Labour Force Status of Families, Australia. For more information see also About TableBuilder.
Special tabulations are available on request. Subject to confidentiality and sampling variability constraints, tabulations can be produced from the survey incorporating data items, populations and geographic area selections to meet individual requirements. These will be provided in electronic form. All enquiries should be made to the National Information and Referral Service at [email protected] or to [email protected]
## Reliability of estimates
Since the estimates in this publication are based on information obtained from occupants of a sample of households, they are subject to sampling variability. That is, they may differ from those estimates that would have been produced if all households had been included in the survey or a different sample was selected.
Some of the estimates contained in the tables have a relative standard error (RSE) of 50 per cent or greater. These estimates are marked as unreliable for general use. Estimates with an RSE of between 25 and 50 per cent are also marked and should be used with caution.
The data in these tables are as reported by any responsible adult aged 15 years and over who were usual residents of private dwellings and were selected in the LFS.
The data used to compile families statistics can be based on complicated family relationships and this adds complexity around interpreting the aggregated estimates.
### More on reliability of estimates
#### Non-sampling error
Non-sampling error may occur in any collection, whether it is based on a sample or a full count such as a census. Sources of non-sampling error include non-response, errors in reporting by respondents or recording of answers by interviewers and errors in coding and processing data. Every effort is made to reduce non-sampling error by careful design and testing of questionnaires, training and supervision of interviewers, and extensive editing and quality control procedures at all stages of data processing
#### Sampling error
Sampling error is the difference between the published estimates, derived from a sample of persons, and the value that would have been produced if the total population (as defined by the scope of the survey) had been included in the survey. One measure of the sampling error is given by the standard error (SE), which indicates the extent to which an estimate might have varied by chance because only a sample of persons was included. There are about two chances in three (67%) that a sample estimate will differ by less than one SE from the number that would have been obtained if all households had been surveyed, and about 19 chances in 20 (95%) that the difference will be less than two SEs.
Another measure of the likely difference is the relative standard error (RSE), which is obtained by expressing the SE as a percentage of the estimate.
$$\large{RSE\%=(\frac{SE}{estimate})\times100}$$
RSEs for Labour Force Status of Families estimates have been calculated using the Jackknife method of variance estimation. This involves the calculation of 30 'replicate' estimates based on 30 different subsamples of the obtained sample. The variability of estimates obtained from these subsamples is used to estimate the sample variability surrounding the main estimate.
The Excel spreadsheets in the Data downloads section contain all the tables produced for this release and the calculated RSEs for each of the estimates.
Only estimates (numbers or percentages) with RSEs less than 25% are considered sufficiently reliable for most analytical purposes. However, estimates with larger RSEs have been included. Estimates with an RSE in the range 25% to 50% should be used with caution while estimates with RSEs greater than 50% are considered too unreliable for general use. All cells in the Excel spreadsheets with RSEs greater than 25% contain a comment indicating the size of the RSE. These cells can be identified by a red indicator in the corner of the cell. The comment appears when the mouse pointer hovers over the cell.
Another measure is the Margin of Error (MOE), which shows the largest possible difference that could be between the estimate due to sampling error and what would have been produced had all persons been included in the survey with a given level of confidence. It is useful for understanding and comparing the accuracy of proportion estimates.
Where provided, MOEs for estimates are calculated at the 95% confidence level. At this level, there are 19 chances in 20 that the estimate will differ from the population value by less than the provided MOE. The 95% MOE is obtained by multiplying the SE by 1.96.
$$\large{MOE=SE\times1.96}$$
#### Calculation of standard error
Standard errors can be calculated using the estimates (counts or percentages) and the corresponding RSEs. Since the RSE is obtained by expressing the standard error as a percentage of the estimate, recalculating the standard error is obtained by multiplying the estimate by the RSE.
#### Proportions and percentages
Proportions and percentages formed from the ratio of two estimates are also subject to sampling errors. The size of the error depends on the accuracy of both the numerator and the denominator. A formula to approximate the RSE of a proportion is given below. This formula is only valid when x is a subset of y:
$$\large{RSE(\frac{x}{y})\approx\sqrt{[RSE(x)]^2-[RSE(y)]^2}}$$
#### Differences
The difference between two survey estimates (counts or percentages) can also be calculated from published estimates. Such an estimate is also subject to sampling error. The sampling error of the difference between two estimates depends on their SEs and the relationship (correlation) between them. An approximate SE of the difference between two estimates (x-y) may be calculated by the following formula:
$$\large {SE(x-y)\approx\sqrt{[SE(x)]^2+[SE(y)]^2}}$$
While this formula will only be exact for differences between separate and uncorrelated characteristics or sub populations, it provides a good approximation for the differences likely to be of interest in this publication.
#### Significance testing
A statistical significance test for a comparison between estimates can be performed to determine whether it is likely that there is a difference between the corresponding population characteristics. The SE of the difference between two corresponding estimates (x and y) can be calculated using the formula shown above in the Differences section. This SE is then used to calculate the following test statistic:
$$\LARGE{(\frac{x-y}{SE(x-y)})}$$
If the value of this test statistic is greater than 1.96 then there is evidence, with a 95% level of confidence, of a statistically significant difference in the two populations with respect to that characteristic. Otherwise, it cannot be stated with confidence that there is a real difference between the populations with respect to that characteristic.
## Glossary
Since these products are all based on data collected in the LFS, the Glossary of publication Labour Force, Australia and information is provided in Labour Statistics: Concepts, Sources and Methods, may be of assistance. Further information is also available in the ABS Family, Household and Income Unit Variables Standard.
The following glossary items relate specifically to family characteristics.
### Show all
#### Child
A person of any age who is a natural, adopted, step, or foster son or daughter of a couple or lone parent, usually resident in the same household.
All children under 15 years who usually reside in a household must form a parent-child relationship with at least one other member of the household. In households where there is no reported parent or guardian, the child is classified as having a parent-child relationship with the next most appropriate adult. This can include parent-child relationships with other relatives (such as aunts, uncles or grandparents) or with unrelated individuals (a nominal guardian).
In order to be classified as a child, the person can have no partner or child of his or her own usually resident in the household.
There are three types of child identified in the 'Relationship in household' classification:
• Child under 15 years
• Dependent student
• Non-dependent child
The differentiation of children into these three types is based upon the dependency criterion and is designed to identify families with different structures and needs. Dependency as used in these standards refers to economic dependency and is applied only to the population of people who could be described as 'children'. It is thus not intended to measure an aged or disabled person's dependency.
See Dependant, Dependent Student and Non-dependent Child.
#### Couple relationship
A couple relationship is defined as two people usually residing in the same household who share a social, economic and emotional bond usually associated with marriage and who consider their relationship to be a marriage or marriage-like union. This relationship is identified by the presence of a registered marriage or de facto marriage.
In practice, a de facto marriage exists between couples when their relationship to each other is reported as partner, lover, boyfriend, girlfriend, or as a common law (or de facto) husband, wife or spouse.
A 'couple relationship' includes same-sex couples.
#### Dependant
A dependant is a family member who is either:
• under 15 years of age;
• aged 15–19 years and attending school or aged 15–24 years and attending a tertiary education institution full time (i.e. dependent students).
In order to be classified as a dependant, the person must have no partner or child of his/her own usually resident in the household. A separate family in the household is formed in this instance.
#### Dependent student
A full time student aged 15-24 years, living in the same usual residence as his or her natural, step, foster or adoptive parent.
#### Family
Two or more persons, one of whom is at least 15 years of age, who are related by blood, marriage (registered or de facto), adoption, step or fostering, and who are usually resident in the same household. The basis of a family is formed by identifying the presence of a couple relationship, lone parent-child relationship or other blood relationship. Some households will therefore contain more than one family.
Consider, for example, if two elderly brothers are living with the family of the daughter of one of the brothers. The daughter's family forms the basic family of the household and the two brothers are both allocated to this family unit as related individuals. The two brothers do not form a separate family in their own right in addition to the daughter's family, because they are related to a couple family or one-parent family already present in the household. However, if the two brothers were living in a dwelling with a family to whom they were not related, they would then form a family in their own right and be classified as an 'other family'.
See Other Families.
#### Family composition
The categories for family composition are:
• Couple family
• Couple family with dependants
• Couple family with children under 15 years
• Couple family without children under 15 years, but with dependent students
• Couple family without dependants
• Couple family without dependants, but with children 15 years or older (ie non-dependent child)
• Couple family without children
• One parent family
• One parent family with dependants
• One parent family with children under 15 years
• One parent family without children under 15 years, but with dependent students
• One parent family without dependants, but with children 15 years or older (ie non-dependent child)
• Other families
#### Father
A male parent with dependants and/or children. The relationship between a father and a child/dependant can be formed via a natural, adoptive, step, foster or child dependency relationship.
#### Hours worked
The number of hours actually worked during the reference week.
#### Household
One or more persons usually resident in the same private dwelling.
#### Husband/partner
A person in a couple relationship with another person usually resident in the same household. The couple relationship may be in either a registered or de facto marriage and includes same-sex couples. In an opposite sex couple, this is the male partner (ie husband). In a same-sex couple, it is the eldest partner (and can be female or male).
#### Jobless family
A jobless family is a family where no persons in the family aged 15 years or over are employed. This includes dependants and non-dependent children.
In a jobless family, all of the family members are either unemployed and/or not in the labour force.
Families that have no employed members but do have members that are classified as undetermined in the scope of the labour force survey, such as members of the permanent Australian defence force, are not included in the number of jobless families.
#### Lone parent family
See One Parent family.
#### Long-term job seekers
Refers to unemployed persons who have been actively seeking work for one year or more.
#### Mother
A female parent with dependants and/or children, or non-dependent children. The relationship between a mother and a child/dependant can be formed via a natural, adoptive, step, foster or child dependency relationship.
#### Non-dependent child
Non-dependent children are defined as children over the age of 15 years who are not studying full-time.
In order to be classified as a child, the person must have no partner or child of his/her own usually resident in the household. A separate family in the household is formed in this instance.
The types of parent-child relationships which can be formed are via a natural, adoptive, step, or foster relationship.
Dependency, as used in these classifications, refers to economic dependency and is only applied to the part of the population that can be described as ‘children’.
The dependency criterion is based on the barriers to full time employment: age and student status. Essentially, once a child turns 15 years and becomes eligible to be included in the labour force, they lose their dependency status unless they are attending school or a tertiary educational institution full-time, are aged 15 to 24 years old and live in the same household as their parents/ guardian.
See Child.
#### Non-private dwelling
An establishment which provides a communal type of accommodation, such as a hotel, motel, hospital or other institution. Family data is not collected from non-private dwellings.
#### Not determined
Where a person has an unknown labour force status, or was a permanent member of the Australian defence force (out of scope for labour force survey).
#### One parent family
A family consisting of one parent with at least one dependant or non-dependent child (regardless of age) who is also usually resident in the family. This family type may or may not include other related individuals.
#### Opposite-sex couple
Two persons of the opposite sex who are in a couple relationship and are usually resident in the same household.
#### Other families
A family of related individuals residing in the same household. These individuals do not form a couple or parent-child relationship with any other person in the household and are not relateded to any couple or one parent family in the household (if present).
If two brothers, for example, are living together and neither is a partner, a lone parent or a child to anyone else in the household, and neither is related to any person in the household who are in a couple or one-parent family (if present), then they are classified as an other family. However, if the two brothers share the household with the daughter of one of the brothers and her husband, then both brothers are included in the couple family and classified as other related individuals.
#### Private dwelling
A residential structure which is self-contained, owned or rented by the occupants, and intended solely for residential use. A private dwelling may be a flat, part of a house, or even a room, but can also be a house attached to, or rooms above shops or offices. Family data is only collected from private dwellings.
#### Relationship in household
The relationship of each person residing in the same household. This is typically in relation to the family reference person (previously referred to as the "head" of the family). The family reference person is typically a parent of children in the household or a husband/partner in a family formed around a couple relationship.
#### Same-sex couple
Two persons of the same sex who are in a couple relationship and are usually resident in the same household.
#### Short-term job seekers
Refers to unemployed persons who have been actively seeking work for less than 12 months.
#### Social marital status
Social marital status is the relationship status of an individual with reference to another person who is usually resident in the household. A marriage exists when two people live together as husband and wife, or partners, regardless of whether the marriage is formalised through registration. Individuals are, therefore, regarded as married if they are in a de facto marriage, or if they are living with the person to whom they are registered as married.
#### Tertiary education institution
A Technical and Further Education (TAFE) college, university, or other educational institution, excluding primary schools and secondary schools (i.e. High School).
#### Usual resident
A person who usually lives in that particular dwelling and regards it as their own or main home.
#### Wife/partner
A person in a couple relationship with another person usually resident in the same household. The couple relationship may be in either a registered or de facto marriage and includes same-sex couples. In an opposite sex couple, this is the female partner (ie wife). In a same-sex couple, it is the youngest partner (and can be male or female).
## Acknowledgement
ABS surveys draw extensively on information provided freely by individuals, businesses, governments and other organisations. Their continued cooperation is very much appreciated: without it, the wide range of statistics published by the ABS would not be available. Information received by the ABS is treated in strict confidence as required by the Census and Statistics Act, 1905.
## History of changes
### Comparability with previous estimates
Care should be taken when comparing the latest estimates from this issue of the publication against earlier estimates published in previous issues. Estimates from previous issues have not been recompiled using the latest population and household benchmarks.
### Improvements to family estimates
From October 2008, the method of producing family estimates from the LFS was improved to include the following:
• an expanded scope to include households containing permanent members of the defence forces;
• an increased range of families in the LFS sample contributing to the family estimates; and
• improvements to the weighting method by utilising independent population benchmarks (of people and households), ensuring the estimates more closely reflect the Australian population.
For more information, see the Information Paper: Improvements to Family Estimates from the Labour Force Survey, 2008
| 2021-10-28T21:14:41 |
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|
https://par.nsf.gov/biblio/10121815-quantifying-thermal-sunyaevzeldovich-effect-excess-millimetre-emission-quasar-environments
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Quantifying the thermal Sunyaev–Zel’dovich effect and excess millimetre emission in quasar environments
ABSTRACT
In this paper, we probe the hot, post-shock gas component of quasar-driven winds through the thermal Sunyaev–Zel’dovich (tSZ) effect. Combining data sets from the Atacama Cosmology Telescope, the Herschel Space Observatory, and the Very Large Array, we measure average spectral energy distributions of 109 829 optically selected, radio quiet quasars from 1.4 to 3000 GHz in six redshift bins between 0.3 < z < 3.5. We model the emission components in the radio and far-infrared, plus a spectral distortion from the tSZ effect. At z > 1.91, we measure the tSZ effect at 3.8σ significance with an amplitude corresponding to a total thermal energy of 3.1 × 1060 erg. If this energy is due to virialized gas, then our measurement implies quasar host halo masses are ∼6 × 1012 h−1 M⊙. Alternatively, if the host dark matter halo masses are ∼2 × 1012 h−1 M⊙ as some measurements suggest, then we measure a >90 per cent excess in the thermal energy over that expected due to virialization. If the measured SZ effect is primarily due to hot bubbles from quasar-driven winds, we find that $(5^{+1.2}_{-1.3}$) per cent of the quasar bolometric luminosity couples to the intergalactic medium over a fiducial quasar lifetime of 100 Myr. An additional source of tSZ may be correlated structure, and further work more »
Authors:
; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; more »
Publication Date:
NSF-PAR ID:
10121815
Journal Name:
Monthly Notices of the Royal Astronomical Society
Volume:
490
Issue:
2
Page Range or eLocation-ID:
p. 2315-2335
ISSN:
0035-8711
Publisher:
Oxford University Press
1. ABSTRACT The infrared (IR) spectral energy distributions (SEDs) of main-sequence galaxies in the early Universe (z > 4) is currently unconstrained as IR continuum observations are time-consuming and not feasible for large samples. We present Atacama Large Millimetre Array Band 8 observations of four main-sequence galaxies at z ∼ 5.5 to study their IR SED shape in detail. Our continuum data (rest-frame 110 $\rm \mu m$, close to the peak of IR emission) allows us to constrain luminosity-weighted dust temperatures and total IR luminosities. With data at longer wavelengths, we measure for the first time the emissivity index at these redshifts to provide more robust estimates of molecular gas masses based on dust continuum. The Band 8 observations of three out of four galaxies can only be reconciled with optically thin emission redward of rest-frame $100\, {\rm \mu m}$. The derived dust peak temperatures at z ∼ 5.5 ($30\!-\!43\, {\rm K}$) are elevated compared to average local galaxies, however, $\sim 10\, {\rm K}$ below what would be predicted from an extrapolation of the trend at z < 4. This behaviour can be explained by decreasing dust abundance (or density) towards high redshifts, which would cause the IR SED at the peakmore »
| 2022-10-04T13:13:20 |
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|
https://math.wikia.org/wiki/Function_transformations
|
## FANDOM
1,168 Pages
Transformations of functions include reflections, stretches, compressions, and shifts.
## Types of transformation
### Reflections
A function $y=f(x)$ can be reflected across the x-axis by multiplying $y$ by -1 to give $-y=f(x)$ or $y=-f(x)$ .
A function can also be reflected across the y-axis by multiplying $x$ by -1, giving $y=f(-x)$ .
A function can be reflected across the line $y=x$ by swapping $x$ and $y$ in the equation, yielding $x=f(y)$ (if $y$ can be isolated, this is equivalent to $y=f^{-1}(x)$ .
### Stretches and compressions
Multiplying $y$ by any constant $a$ will stretch the graph vertically by a factor of the reciprocal of $a$ . Likewise, multiplying $x$ by any constant will do the same horizontally.
### Shifts
Subtracting any constant $k$ from $y$ (or adding it to $f(x)$) will shift the graph up by $k$ units. Subtracting a constant from $x$ (giving $y=f(x-h)$ will shift the graph $h$ units to the right.
Community content is available under CC-BY-SA unless otherwise noted.
| 2019-12-10T08:32:41 |
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|
https://pos.sissa.it/256/137/
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Volume 256 - 34th annual International Symposium on Lattice Field Theory (LATTICE2016) - Hadron Spectroscopy and Interactions
Charmonium and charmed meson spectroscopy from lattice QCD
D. Tims,* G. Cheung, C. O'Hara, G. Moir, M.J. Peardon, S. Ryan, C. Thomas on behalf of the Hadron Spectrum Collaboration
*corresponding author
Full text: pdf
Pre-published on: February 01, 2017
Published on: March 24, 2017
Abstract
Spectra of highly excited hidden and open-charm mesons calculated on dynamical lattice QCD ensembles with a pion mass of $M_{\pi}\sim 240$ MeV are presented and compared to previous results obtained on a lattice where $M_{\pi}\sim400$ MeV. The distillation technique was employed in order to compute the necessary correlation functions, allowing the use of a large basis of interpolating operators with various spatial structures. This basis included operators proportional to the gluonic field strength, allowing the identification of possible hybrid states. We conclude that reducing the light quark mass has little effect on the overall pattern and structure of the spectra.
DOI: https://doi.org/10.22323/1.256.0137
How to cite
Metadata are provided both in "article" format (very similar to INSPIRE) as this helps creating very compact bibliographies which can be beneficial to authors and readers, and in "proceeding" format which is more detailed and complete.
Open Access
Copyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.
| 2020-11-24T13:10:06 |
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|
https://www.nist.gov/pml/photoionization-co2-arpes/photoionization-co2-experimental-procedure
|
An official website of the United States government
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Secure .gov websites use HTTPS
A lock ( ) or https:// means you’ve safely connected to the .gov website. Share sensitive information only on official, secure websites.
# Photoionization of CO2 - Experimental Procedure
## Share
This experiment was carried out on the 5 m normal incidence monochromator fitted to a beamline at the Daresbury SRS, providing a photon flux of ≈ 1010 photons/s within a bandpass of 0.1 Å in the spectral region from 650 Å to 840 Å [24]. The light was brought into the experimental chamber by a 2 mm internal diameter glass capillary light guide whose capillary aperture was placed close to the exit slit of the monochromator. In addition to offering a low-loss transport for the vacuum ultraviolet radiation, the capillary also served to maintain a pressure differential between the experimental chamber and the ultra high vacuum of the optical monochromator. A schematic diagram of the experimental apparatus is shown in Fig. 1. The light guide extends from the exit slit, EX in Fig. 1, to the interaction region above the gas entrance tube, GS in Fig. 1, and can be as long as 30 cm dependent upon exact placement of the experimental chamber with respect to the monochromator.
The electron spectrometer system comprises two 100 mm mean radius hemispherical analyzers, one rotatable about the incoming light beam as an axis and the other fixed, contained in a chamber shielded from magnetic fields by three layers of µ-metal. The radiation from the monochromator is polarized, its polarization depending upon the optics of the monochromator and the subtended angles of acceptance of the synchrotron radiation. In our configuration, the light is polarized with between 75 % and 80 % of the light intensity having its electric field vector E perpendicular to the plane of the paper in Fig. 1. In this configuration, the fixed analyzer accepts electrons ejected parallel to the E of the incident radiation. The fixed analyzer is ES-2 in Fig. 1. The other electron spectrometer is rotatable about an axis defined by the direction of the light and hence collects electron in the plane of the E. This movement allows the angular distribution of the photoelectrons to be explored completely and is sufficient to determine the angular asymmetry parameter for the scattering process. The entrance lenses for the spectrometers are three element zoom lenses based upon the design of Harting and Read [25]. The entrance cone to the lens system has a small aperture, usually about 1 mm in our experiments, which acts as the limiting aperture for determining both the energy and angular resolution of the system. The zoom lens focuses the electrons from a small interaction volume determined by the size of the light beam exiting the capillary and the size of the gas jet exiting the gas entrance tube onto the entrance plane of the hemispheres. The pass energy of the electron analyzer and focus voltages are set by external controls. The pass energy remains fixed for a particular set of experiments, and the other voltages are appropriately varied to scan the electron energy spectrum as required by using an automated data control system. The electrons are dispersed upon passing through the analyzer hemispheres and focused on the hemisphere exit plane. Since the apparatus was first described in the literature, the electron spectrometers have been fitted with position sensitive detectors which are placed near the exit focal plane of the hemispheres [26]. This allows for the simultaneous detection of a range of energies in the photoelectron spectra and thereby improves the data quality for a given period of data accumulation, compared to using a conventional electron multiplier behind an exit slit.
The polarization of the incoming light was measured using a three mirror polarizer with tungsten mesh and plate photodiodes which could be rotated with the rotatable analyzer through 90° in order to determine the light polarization. The polarization detection device was constructed based upon considerations given by Horton et al. [27]. The polarization was checked frequently since small movements in the storage ring beam position, and the mirrors focusing the light onto the entrance slit of the monochromator, can have a marked effect on the polarization. It was found that, provided the pre-mirror adjustments were kept optimized for maximum photon flux at the exit slit of the monochromator, the polarization would remain stable during the accumulation of a particular data set. The tungsten wire mesh at the entrance of the polarizer served as a photocathode for monitoring the intensity of the incoming light beam. A tungsten plate serving as a second photocathode collected the beam remaining after three reflections of the beam. The ratios of these photocurrents as a function of the angular position of the movable electron spectrometer provided the data necessary to determine the polarization of the light.
Calibration of the energy response of the analyzers was performed using the known values of the cross section and asymmetry parameters for argon or helium gas and following standard procedures outlined in the literature [28-30]. For all the spectra reported here the electron spectrometer resolution was determined from the rare gas calibration to be 41 meV for the fixed analyzer and 46 meV for the rotatable analyzer. The 5 m monochromator resolution was 0.1 Å (≈ 2 meV) for the measurements taken at wavelengths shorter than 750 Å. At wavelengths longer than this, where the structure in the absorption spectrum is less dense the resolution requirements could be relaxed and a wavelength resolution of 0.2 Å was used. The data were accumulated by simultaneously taking photoelectron spectra at two angles with respect to the polarization direction by utilizing both electron spectrometer systems. Since the two analyzers could be positioned at different angles, a particular data point did not require rotation of the movable electron spectrometer system. The wavelength on the monochromator was then incremented by 0.1 Å and another set of photoelectron spectra taken. The light polarization was checked periodically by a 90° rotation of the movable electron spectrometer. During data accumulation, the time spent at a particular electron kinetic energy was determined by integration of the light flux signal to some predetermined amount so that all the points in a particular data set would be correctly normalized to the same total light flux.
The differential cross section for photoabsorption in the dipole approximation for a randomly oriented gas may be expressed as
$${{\textstyle{\rm d}\sigma_v}\over{\textstyle{\rm d}\Omega}} = {{\textstyle\sigma_v}\over{\textstyle 4\pi}} ~ \left[ 1 + {\textstyle\beta_v\over \textstyle 4}~(3P \cos 2\theta +1)\right]$$
where θ is the angle between the major polarization axis and the ejected electron, P is the degree of polarization of the incoming light, Ω is the solid angle of collection of the photoelectrons, and σv is the partial cross section for the vibrational-electronic channel corresponding to the photoelectron being detected. The total cross section for a particular electronic channel is the sum of the partial cross sections of the individually resolved vibrational channels. The vibrational branching ratio is defined as the partial cross section for that channel divided by the total cross section for the electronic state. The number of photoelectrons per steradian per unit light flux, dN/dΩ is proportional to the differential cross section and hence we can recast the above equation into one that refers to the measurable parameters of the experiment:
$${{\textstyle{\rm d}N_v}\over{\textstyle{\rm d}\Omega}} = {{\textstyle N_v}\over{\textstyle 4\pi}} ~ \left[ 1+{\textstyle\beta_v\over \textstyle 4}~(3P\cos 2\theta +1)\right] ~.$$
Nv is the total number of electrons detected in a particular vibrational channel summed over the all solid angles. Measurements were made simultaneously at θ=0° and θ=90° and hence βv and Nv could be directly deduced from the two spectra [31]. The branching ratio for a particular transition is the ratio of Nv with respect to the sum of all the Nv for a particular electronic excitation. The data reported here were taken only for transitions that left the CO2+ molecule in the X 2Πg ground electronic state. Altogether about 1500 data sets were taken in the wavelength region 650 Å to 890 Å.
Figure 2 shows the photoionization efficiency (relative photoionization cross section) for CO2+ in the wavelength region of interest in the present study. The data were taken using a rotationally cooled sample of CO2 and a laboratory light source coupled to a quadrupole mass filter [16, 32]. A one meter near-normal incidence monochromator provided dispersed radiation with a wavelength resolution of 0.12 Å. This rotationally-cooled spectrum shows more detailed and sharper structure, particularly near ionization onset, than does the spectrum obtained by Berkowitz [33] with a slightly better wavelength resolution of 0.07 Å. The spectrum shows members of the TO series that have as limits the A state of CO2+ vibrational levels. The notation A nv(TO) n = 4,5, ... etc., means the level is a member of the TO series having the nv vibrational level of the A state of CO2+ as its limit. The symbol B n0(s,d) n = 3,4,...etc. is a Rydberg level of quantum number n having as its series limit the B state of CO2+ in the vibrational ground state. The s or d refers to the Hennings sharp or diffuse series. The notation A 3v(L) v = 0,... refers to a level of the Lindholm series with principal quantum number 3 that has the A state as its limit and has a vibrational excitation of v in the symmetric stretch mode.
## Contacts
Created August 25, 2009, Updated June 2, 2021
| 2022-06-27T17:36:46 |
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https://wiki.cosmos.esa.int/planck-legacy-archive/index.php?title=Power_spectra&diff=prev&oldid=6211
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# Difference between revisions of "Power spectra"
This is the page regarding the HFI-based power spectra
We call intra-frequency checks those performed between detectors (or sets of) in the same frequency bands, which thus respond similarly to the sky emission. Interfrequency-checks on the other hand correspond to checks between detector in different frequency bands, imposing further reliance on a sky model to perform the test.
## Intra-frequency checks
These compare the power spectra between various detector sets operating within the same frequency channel. They see the same sky, and should therefore give consistent results, up to the noise level, and up to color corrections due to their somewhat different spectral band passes. These corrections are rather small if one restricts the comparison to specific portions of the sky, for instance dominated by extra-Galactic components, like it is done for extracting the CMB power spectrum in the likelihood analysis where \$f_{sky} \sim 0.4\$.
The pictures shows in grey the prior deduced from the beam parameters uncertainty analysis. At 217 GHz, the distance between PSB and SWB suggests an accounted for effect (fortunately small enough for the likelihood analysis). The relative calibration appear to be at the 0.1% level.
This shows that whatever systematic effect might remain, it has to be common to all detectors within a frequency band to a very high level of accuracy.
## Inter-frequency checks
(Planck) High Frequency Instrument
Cosmic Microwave background
| 2022-05-26T18:37:54 |
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https://www.stats.gov.sa/en/statistical-knowledge/36
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# Statistics and Its Relation to Mathematical Economics
Assuming that mathematical economics is the application of mathematics to express theories and relations among economic phenomena variables, taking the advantage that using the mathematical approach to express economic problems would make it easier and simpler when presenting such problems, thus achieving accurate results in a neutral and clear manner when it comes to analyzing facts. Hence, the mathematical approach mainly depends, when presenting and mathematically expressing such problems, on the statistical method and its theories.
Economic modeling, including developing hypotheses, conducting statistical tests and forecasting the targeted economic variables, would, in particular, depend on such statistical method and its theories to identify trends and disseminate outputs.
Lately, the relationship between statistics and econometrics has been acknowledged, especially by economists who see that realistic assumptions should be considered when developing mathematical modeling to minimize the gap between the model theorem and realistic application thereof.
Statistical Survey:
37101
| 2020-07-14T16:56:40 |
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https://www.ecb.europa.eu/pub/financial-stability/macroprudential-bulletin/focus/2022/html/ecb.mpbu202210_focus3.en.html
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# Gauging the sensitivity of loan-service-to-income (LSTI) ratios to increases in interest rates
Prepared by Emil Bandoni, Barbara Jarmulska and Jan Hannes Lang
Against the backdrop of increasing interest rates in the euro area, it is important to understand how household LSTI ratios could be affected. To answer this question, it is useful to recall that at a given point in time the LSTI ratio consists of two payment parts: the amortisation of the loan principle and the interest payment on the outstanding loan balance: $LSTIT=LTITδT+iT$.
Factors that influence the LSTI interest rate sensitivity include the initial loan-to-income (LTI) ratio, the loan maturity, the interest rate fixation period and the initial interest rate. The definition of the LSTI ratio above suggests that the higher the LTI ratio at the time of interest rate resetting, the higher the LSTI sensitivity will be to a given interest rate increase.[1] In turn, the LTI ratio at the time of interest rate resetting will be higher: (1) the higher the LTI ratio at origination; (2) the lower the amortisation rate, which will depend on the loan maturity;[2] and (3) the less time that has elapsed since the loan origination, which is determined by the interest rate fixation period.[3] All three factors give rise to a higher outstanding loan balance when repricing takes place and therefore result in a larger LSTI increase for a given change in the interest rate (Chart A, panel a). Finally, a lower interest rate at origination will lead to a higher LSTI interest rate sensitivity for a given market rate, as the change in the interest rate at the time of repricing will be larger.
Given the heterogeneous impact of interest rate changes on LSTI ratios depending on the underlying lending standards, loan-level simulations are crucial to detect pockets of vulnerabilities. Simulations based on aggregate data will not be meaningful for identifying vulnerabilities, as the aggregate household debt-to-income ratio (~1 in the euro area) is many times lower than LTI ratios at the micro level (with values that are usually between 2 and 8). Although comprehensive loan-level data for households are not available for the euro area, European DataWarehouse (EDW) data on the universe of securitised household mortgage loans can be used to gain at least a partial view of pockets of vulnerabilities. With these data, the framework outlined above allows us to simulate shocked LSTIs based on the mortgage loan characteristics, including the LTI ratio and interest rate at origination, maturity, interest fixation period and amortisation type. Chart A, panel b shows a simulated distribution of LSTI increases if interest rates increase by 200 basis points from end-2021 levels. Based on this exercise, we find that LSTI increases would be manageable for most loans but pockets of vulnerabilities exist, where LSTIs of existing loans could increase by more than 8 percentage points. The granularity of the data also makes it possible to analyse expected LSTI changes across countries and over time, or to focus on a subset of exposures.
1. We assume a fixed interest rate until time T. For a given LTI ratio, amortisation rate and market interest rate at time T this will imply: $∆LSTIT=LTITδT+iT-LTITδT+i0=LTITiT-i0$. Clearly, the higher the LTI ratio at time T, the larger the increase in the LSTI ratio will be for a given change in the interest rate. Moreover, the lower the initial interest rate at loan origination (time 0), the larger the change in the interest rate will be at the time of resetting for a given market interest rate.
2. A longer maturity implies a lower amortisation rate and therefore a smaller share of initial debt that is paid back in each period.
3. This implies fewer periods during which a given share of the initial debt (amortisation rate) is paid back.
| 2022-12-01T14:23:36 |
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http://www.nist.gov/manuscript-publication-search.cfm?pub_id=907710
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# Publication Citation
NIST Authors in Bold
Author(s): Howard S. Cohl; On Parameter Differentiation for Integral Representations of Associated Legendre Functions May 24, 2011 For integral representations of associated Legendre functions in terms of modified Bessel functions, we establish justification for differentiation under the integral sign with respect to parameters. With this justification, derivatives for associated Legendre functions of the first and second kind with respect to the degree are evaluated at odd-half-integer degrees, for general complex-orders, and derivatives with respect to the order are evaluated at integer-orders, for general complex-degrees. We also discuss the properties of the complex function $f:\C\setminus\{-1,1\}\to\C$ given by $f(z)=z/(\sqrt{z+1}\sqrt{z-1})$. Symmetry, Integrability and Geometry: Methods and Applications (SIGMA) 7 16 pp. Legendre functions; modified Bessel functions; derivatives Math, Modeling Click here to retrieve PDF version of paper (166KB)
| 2013-05-23T00:26:58 |
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https://par.nsf.gov/biblio/10005866-measurement-differential-production-cross-sections-bosons-association-jets-pp-collisions
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Measurement of differential production cross sections for $Z/γ*$ bosons in association with jets in $pp¯$ collisions at $s=1.96 TeV$
Authors:
; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; more »
Publication Date:
NSF-PAR ID:
10005866
Journal Name:
Physical Review D
Volume:
91
Issue:
1
ISSN:
1550-7998
Publisher:
American Physical Society
| 2022-09-27T14:46:29 |
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https://www.cdc.gov/cancer/uscs/technical_notes/criteria/age-adjusted-incidence-rates.htm
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# Criteria for Reporting Age-Adjusted Cancer Incidence Rates for U.S. Census Regions and Divisions
The annual age-adjusted cancer incidence rates for some U.S. Census regions and divisions are not available because the data from the cancer registries of some states in those regions or divisions do not meet the eligibility criteria for inclusion in this report. In contrast, the annual age-adjusted cancer death rates are available for all states in every Census region or division. However, the age-adjusted incidence rate for Census regions or divisions in which the data of less than 100% of the cancer registries meet eligibility criteria can be estimated by assuming that the incidence-to-mortality ratio for states without eligible cancer registry data in that Census region or division equals the incidence-to-mortality ratio for states with eligible cancer registry data in that Census region or division.
Let
M1 = age-adjusted death rate in states with eligible cancer registries
M0 = age-adjusted death rate in states without eligible cancer registries
I1 = age-adjusted incidence rate in states with eligible cancer registries
I0 = age-adjusted incidence rate in states without eligible cancer registries (incidence data are not available)
P1 = Proportion of the population in the Census region or division that resides in states with eligible cancer registries
R = ($M0M1$)
Îtotal = age-adjusted incidence rate for the entire Census region or division
where “eligible” refers to the state and metropolitan area cancer registries that meet this report’s data quality criteria for all invasive cancer sites combined.
Since we are assuming that $I1M1=I0M0$, the estimate of the age-adjusted incidence rate for states without eligible cancer registries is $I0=I1M0M1=I1R$. Thus, an estimate of the age-adjusted incidence rate for 100% of the Census region or division is computed as the following weighted average—
Îtotal = P1I1 + (1 – P1)I0 = P1I1 + (1 – P1)I1R = I1[P1+(1 – P1)R]
As an example, consider invasive female breast cancer in a hypothetical Census region with seven states. Incidence data for five states that cover 86.3% of the population (P1 = 0.863) are eligible for inclusion in the calculation of the regional incidence rate; data for two states are not eligible. The female breast cancer death rate for the five eligible states is $M1=27.3105$, and the rate for the two ineligible states is $M0=27.7105$.
The age-adjusted incidence rate for states with eligible cancer registries is $I1=145.1105$.
The age-adjusted incidence rate for female invasive breast cancer in the entire Census region (in other words, corrected for the data not available from the ineligible registries) is
$I^total=145.1105×0.863+0.13727.727.3=145.39105$
The underlying assumptions for this method are that the age-adjusted death rates for states with and without eligible cancer registries are accurate and that the incidence-to-mortality ratio for states without eligible cancer registries in that Census region or division equals the incidence-to-mortality ratio for states with eligible cancer registries in that Census region or division.
For each Census region or division in which less than 100% of the registries provided data eligible for this report, we used the above-described method to estimate the age-adjusted incidence rates (Îtotal) for the six major cancer sex-site groups: breast (female only), prostate, male and female colorectal, and male and female lung and bronchus. If the estimate of the age-adjusted incidence rate for each of the six cancer sites for that Census region or division falls within the confidence interval of the observed age-adjusted incidence rate for states with eligible cancer registries, then the observed age-adjusted incidence rates for all cancer sites are published. If one or more of the six estimates of age-adjusted incidence rates falls outside the confidence interval, then the observed age-adjusted cancer incidence rates are not reported for that U.S. Census region or division.
We emphasize, however, that all cancer incidence rates in this report are based exclusively on data obtained from states with eligible cancer registries and are not the estimates of the age-adjusted incidence rates calculated using the methods described above.
Page last reviewed: May 29, 2019
| 2020-05-27T07:12:26 |
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https://lammps.sandia.gov/doc/pair_gran.html
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# pair_style gran/hooke command¶
Accelerator Variants: gran/hooke/omp
# pair_style gran/hooke/history command¶
Accelerator Variants: gran/hooke/history/omp, gran/hooke/history/kk
# pair_style gran/hertz/history command¶
Accelerator Variants: gran/hertz/history/omp
## Syntax¶
pair_style style Kn Kt gamma_n gamma_t xmu dampflag keyword
• style = gran/hooke or gran/hooke/history or gran/hertz/history
• Kn = elastic constant for normal particle repulsion (force/distance units or pressure units - see discussion below)
• Kt = elastic constant for tangential contact (force/distance units or pressure units - see discussion below)
• gamma_n = damping coefficient for collisions in normal direction (1/time units or 1/time-distance units - see discussion below)
• gamma_t = damping coefficient for collisions in tangential direction (1/time units or 1/time-distance units - see discussion below)
• xmu = static yield criterion (unitless value between 0.0 and 1.0e4)
• dampflag = 0 or 1 if tangential damping force is excluded or included
• keyword = limit_damping
limit_damping value = none
limit damping to prevent attractive interaction
Note
Versions of LAMMPS before 9Jan09 had different style names for granular force fields. This is to emphasize the fact that the Hertzian equation has changed to model polydispersity more accurately. A side effect of the change is that the Kn, Kt, gamma_n, and gamma_t coefficients in the pair_style command must be specified with different values in order to reproduce calculations made with earlier versions of LAMMPS, even for monodisperse systems. See the NOTE below for details.
## Examples¶
pair_style gran/hooke/history 200000.0 NULL 50.0 NULL 0.5 1
pair_style gran/hooke 200000.0 70000.0 50.0 30.0 0.5 0
pair_style gran/hooke 200000.0 70000.0 50.0 30.0 0.5 0 limit_damping
## Description¶
The gran styles use the following formulas for the frictional force between two granular particles, as described in (Brilliantov), (Silbert), and (Zhang), when the distance r between two particles of radii Ri and Rj is less than their contact distance d = Ri + Rj. There is no force between the particles when r > d.
The two Hookean styles use this formula:
$F_{hk} = (k_n \delta \mathbf{n}_{ij} - m_{eff} \gamma_n\mathbf{ v}_n) - (k_t \mathbf{ \Delta s}_t + m_{eff} \gamma_t \mathbf{v}_t)$
The Hertzian style uses this formula:
$F_{hz} = \sqrt{\delta} \sqrt{\frac{R_i R_j}{R_i + R_j}} F_{hk} = \sqrt{\delta} \sqrt{\frac{R_i R_j}{R_i + R_j}} \Big[ (k_n \delta \mathbf{n}_{ij} - m_{eff} \: \gamma_n \mathbf{ v}_n) - (k_t \mathbf{ \Delta s}_t + m_{eff} \: \gamma_t \mathbf{v}_t) \Big]$
In both equations the first parenthesized term is the normal force between the two particles and the second parenthesized term is the tangential force. The normal force has 2 terms, a contact force and a damping force. The tangential force also has 2 terms: a shear force and a damping force. The shear force is a “history” effect that accounts for the tangential displacement between the particles for the duration of the time they are in contact. This term is included in pair styles hooke/history and hertz/history, but is not included in pair style hooke. The tangential damping force term is included in all three pair styles if dampflag is set to 1; it is not included if dampflag is set to 0.
The other quantities in the equations are as follows:
• $$\delta$$ = d - r = overlap distance of 2 particles
• $$K_n$$ = elastic constant for normal contact
• $$K_t$$ = elastic constant for tangential contact
• $$\gamma_n$$ = viscoelastic damping constant for normal contact
• $$\gamma_t$$ = viscoelastic damping constant for tangential contact
• $$m_{eff} = M_i M_j / (M_i + M_j) =$$ effective mass of 2 particles of mass M_i and M_j
• $$\mathbf{\Delta s}_t =$$ tangential displacement vector between 2 particles which is truncated to satisfy a frictional yield criterion
• $$n_{ij} =$$ unit vector along the line connecting the centers of the 2 particles
• $$V_n =$$ normal component of the relative velocity of the 2 particles
• $$V_t =$$ tangential component of the relative velocity of the 2 particles
The $$K_n$$, $$K_t$$, $$\gamma_n$$, and $$\gamma_t$$ coefficients are specified as parameters to the pair_style command. If a NULL is used for $$K_t$$, then a default value is used where $$K_t = 2/7 K_n$$. If a NULL is used for $$\gamma_t$$, then a default value is used where $$\gamma_t = 1/2 \gamma_n$$.
The interpretation and units for these 4 coefficients are different in the Hookean versus Hertzian equations.
The Hookean model is one where the normal push-back force for two overlapping particles is a linear function of the overlap distance. Thus the specified $$K_n$$ is in units of (force/distance). Note that this push-back force is independent of absolute particle size (in the monodisperse case) and of the relative sizes of the two particles (in the polydisperse case). This model also applies to the other terms in the force equation so that the specified $$\gamma_n$$ is in units of (1/time), $$K_t$$ is in units of (force/distance), and $$\gamma_t$$ is in units of (1/time).
The Hertzian model is one where the normal push-back force for two overlapping particles is proportional to the area of overlap of the two particles, and is thus a non-linear function of overlap distance. Thus Kn has units of force per area and is thus specified in units of (pressure). The effects of absolute particle size (monodispersity) and relative size (polydispersity) are captured in the radii-dependent pre-factors. When these pre-factors are carried through to the other terms in the force equation it means that the specified $$\gamma_n$$ is in units of (1/(time*distance)), $$K_t$$ is in units of (pressure), and $$\gamma_t$$ is in units of (1/(time*distance)).
Note that in the Hookean case, $$K_n$$ can be thought of as a linear spring constant with units of force/distance. In the Hertzian case, $$K_n$$ is like a non-linear spring constant with units of force/area or pressure, and as shown in the (Zhang) paper, $$K_n = 4G / (3(1-\nu))$$ where $$\nu =$$ the Poisson ratio, G = shear modulus = $$E / (2(1+\nu))$$, and E = Young’s modulus. Similarly, $$K_t = 4G / (2-\nu)$$. (NOTE: in an earlier version of the manual, we incorrectly stated that $$K_t = 8G / (2-\nu)$$.)
Thus in the Hertzian case $$K_n$$ and $$K_t$$ can be set to values that corresponds to properties of the material being modeled. This is also true in the Hookean case, except that a spring constant must be chosen that is appropriate for the absolute size of particles in the model. Since relative particle sizes are not accounted for, the Hookean styles may not be a suitable model for polydisperse systems.
Note
In versions of LAMMPS before 9Jan09, the equation for Hertzian interactions did not include the $$\sqrt{r_i r_j / (r_i + r_j)}$$ term and thus was not as accurate for polydisperse systems. For monodisperse systems, $$\sqrt{ r_i r_j /(r_i+r_j)}$$ is a constant factor that effectively scales all 4 coefficients: $$K_n, K_t, \gamma_n, \gamma_t$$. Thus you can set the values of these 4 coefficients appropriately in the current code to reproduce the results of a previous Hertzian monodisperse calculation. For example, for the common case of a monodisperse system with particles of diameter 1, all 4 of these coefficients should now be set 2x larger than they were previously.
Xmu is also specified in the pair_style command and is the upper limit of the tangential force through the Coulomb criterion Ft = xmu*Fn, where Ft and Fn are the total tangential and normal force components in the formulas above. Thus in the Hookean case, the tangential force between 2 particles grows according to a tangential spring and dash-pot model until Ft/Fn = xmu and is then held at Ft = Fn*xmu until the particles lose contact. In the Hertzian case, a similar analogy holds, though the spring is no longer linear.
Note
Normally, xmu should be specified as a fractional value between 0.0 and 1.0, however LAMMPS allows large values (up to 1.0e4) to allow for modeling of systems which can sustain very large tangential forces.
The effective mass m_eff is given by the formula above for two isolated particles. If either particle is part of a rigid body, its mass is replaced by the mass of the rigid body in the formula above. This is determined by searching for a fix rigid command (or its variants).
For granular styles there are no additional coefficients to set for each pair of atom types via the pair_coeff command. All settings are global and are made via the pair_style command. However you must still use the pair_coeff for all pairs of granular atom types. For example the command
pair_coeff * *
should be used if all atoms in the simulation interact via a granular potential (i.e. one of the pair styles above is used). If a granular potential is used as a sub-style of pair_style hybrid, then specific atom types can be used in the pair_coeff command to determine which atoms interact via a granular potential.
If two particles are moving away from each other while in contact, there is a possibility that the particles could experience an effective attractive force due to damping. If the limit_damping keyword is used, this option will zero out the normal component of the force if there is an effective attractive force.
Styles with a gpu, intel, kk, omp, or opt suffix are functionally the same as the corresponding style without the suffix. They have been optimized to run faster, depending on your available hardware, as discussed on the Speed packages doc page. The accelerated styles take the same arguments and should produce the same results, except for round-off and precision issues.
These accelerated styles are part of the GPU, USER-INTEL, KOKKOS, USER-OMP and OPT packages, respectively. They are only enabled if LAMMPS was built with those packages. See the Build package doc page for more info.
You can specify the accelerated styles explicitly in your input script by including their suffix, or you can use the -suffix command-line switch when you invoke LAMMPS, or you can use the suffix command in your input script.
See the Speed packages doc page for more instructions on how to use the accelerated styles effectively.
## Mixing, shift, table, tail correction, restart, rRESPA info¶
The pair_modify mix, shift, table, and tail options are not relevant for granular pair styles.
These pair styles write their information to binary restart files, so a pair_style command does not need to be specified in an input script that reads a restart file.
These pair styles can only be used via the pair keyword of the run_style respa command. They do not support the inner, middle, outer keywords.
The single() function of these pair styles returns 0.0 for the energy of a pairwise interaction, since energy is not conserved in these dissipative potentials. It also returns only the normal component of the pairwise interaction force. However, the single() function also calculates 10 extra pairwise quantities. The first 3 are the components of the tangential force between particles I and J, acting on particle I. The fourth is the magnitude of this tangential force. The next 3 (5-7) are the components of the relative velocity in the normal direction (along the line joining the 2 sphere centers). The last 3 (8-10) the components of the relative velocity in the tangential direction.
These extra quantities can be accessed by the compute pair/local command, as p1, p2, …, p10.
## Restrictions¶
All the granular pair styles are part of the GRANULAR package. It is only enabled if LAMMPS was built with that package. See the Build package doc page for more info.
These pair styles require that atoms store torque and angular velocity (omega) as defined by the atom_style. They also require a per-particle radius is stored. The sphere atom style does all of this.
This pair style requires you to use the comm_modify vel yes command so that velocities are stored by ghost atoms.
These pair styles will not restart exactly when using the read_restart command, though they should provide statistically similar results. This is because the forces they compute depend on atom velocities. See the read_restart command for more details.
## Default¶
none
(Brilliantov) Brilliantov, Spahn, Hertzsch, Poschel, Phys Rev E, 53, p 5382-5392 (1996).
(Silbert) Silbert, Ertas, Grest, Halsey, Levine, Plimpton, Phys Rev E, 64, p 051302 (2001).
(Zhang) Zhang and Makse, Phys Rev E, 72, p 011301 (2005).
| 2021-05-16T18:35:10 |
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|
https://pos.sissa.it/256/103/
|
Volume 256 - 34th annual International Symposium on Lattice Field Theory (LATTICE2016) - Hadron Spectroscopy and Interactions
Including heavy spin effects in a lattice QCD study of static-static-light-light tetraquarks
P. Bicudo, J. Scheunert, M. Wagner*
*corresponding author
Full text: pdf
Pre-published on: 2016-12-27 09:53:30
Published on: 2017-03-24 10:20:24
Abstract
In previous works we predicted the existence of a $\bar b \bar b u d$ tetraquark with quantum numbers $I(J^P) = 0(1^+)$ using the static approximation for the $\bar b$ quarks and neglecting heavy spin effects. Since the binding energy is of the same order as expected for these heavy spin effects, it is essential to include them in the computation. Here we present a corresponding method and show evidence that binding is only slightly weakened and that the $\bar b \bar b u d$ tetraquark persists.
Open Access
Copyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.
| 2017-11-22T14:33:48 |
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|
https://finalfantasy.fandom.com/wiki/Apocalypse_(Final_Fantasy_VII)
|
## FANDOM
38,268 Pages
The Apocalypse is a weapon for Cloud in Final Fantasy VII. It is acquired late in the game, and provides triple AP growth to its three Materia slots. It is one of only two pieces of equipment, along with the Scimitar for Cid, that provide triple AP to Materia. It can be equipped to Cloud or thrown, or sold for 1 gil.
## ObtainedEdit
Apocalypse is found in the final room of the optional dungeon Ancient Forest, which is unlocked either with a green/black/gold Chocobo or by defeating the Ultimate Weapon. This makes it a rare weapon that can be acquired later in the game.
## StatsEdit
Attack 88 110 43 x3 Element: Cut Spirit +16 Triple AP
As the Apocalypse has a base Attack stat bonus of 88, the base damage for physical attacks when it is equipped is the following formula:
$\text{Base Damage} = \text{(88 + Strength)} + \frac{\text{(88 + Strength)} + \text{Level}}{32} \times \frac{\text{(88 + Strength)} \times \text{Level}}{32}$
where "Level" is Cloud's current level and "Strength" is his Strength stat. The x3 also has an Attack% (Accuracy) of 110%, and grants a +43 bonus to Cloud's Magic stat when casting spells. Apocalypse also grants +16 to Cloud's Spirit stat, boosting resistance to magic damage.
## UseEdit
Apocalypse has very strong stats, with a high Attack stat, and one of the highest Magic stats of a weapon for Cloud, tied with Ragnarok and outclassed only by Ultima Weapon. However, by far is main draw is the triple AP bonus to its three equipped Materia, which hastens grinding. It is one of two weapons in the game, along with Cid's Scimitar, that provide triple AP.
Apocalypse's Materia slots are all unlinked, meaning none of them can benefit from Support Materia, such as All. To make grinding easier, the player may wish to equip Cloud with Slash-All or the Independent Materia Mega All, which allow his attacks to hit all targets. Though a drawback of using these Materia is that they could take a slot from another Materia to be leveled instead, there are benefits to mastering these Materia to give them to other characters.
Apocalypse can be used as the optimal way to grind Materia in the Northern Cave. In the Water Crossing and Water Path, Movers and Magic Pots give a significant amount of AP upon defeat. If bringing Cloud with Apocalypse, Cid with Scimitar, another character with a double AP weapon, and all characters equipped with Rune Armlet armor (which provide double AP to four Materia slots), the player can rapidly master Materia.
As a pure weapon, Apocalypse is outclassed by Heaven's Cloud, Ragnarok, and Ultima Weapon. Due to its triple AP bonus, however, it should be kept and used specifically for farming Materia.
## EtymologyEdit
Apocalypse (Ancient Greek: ἀποκάλυψις apokálypsis, from ἀπό and καλύπτω meaning "uncovering"), translated literally from Greek, is a disclosure of knowledge, i.e., a lifting of the veil or revelation. In religious contexts it is usually a disclosure of something hidden. Today, it is commonly used in reference to any prophetic revelation or so-called end time scenario, or to the end of the world in general.
Community content is available under CC-BY-SA unless otherwise noted.
| 2020-07-09T02:31:08 |
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|
https://firas.moosvi.com/oer/physics_bank/content/public/006.Force/Newton%27s%20Second%20Law/Blocks%20on%20a%20Table/Blocks%20on%20a%20Table.html
|
# Blocks on a Table#
Blocks A, B, and C are on a frictionless table, connected by massless strings. Block A has mass 4 $$M$$, block B has mass 23 $$M$$, and block C has mass 8 $$M$$.
Block C is pulled to the right by a large force $$F_A$$ that causes the entire system to accelerate.
Which of the following statements is true?
## Part 1#
Which of the following statements is true?
### Answer Section#
• Block A experiences the greatest net force.
• Block B experiences the greatest net force.
• Block C experiences the greatest net force.
• More information is needed to answer this question.
• The net force on all the blocks is the same.
## Attribution#
Problem is licensed under the CC-BY-NC-SA 4.0 license.
| 2022-10-01T15:28:17 |
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|
https://simulationresearch.lbl.gov/modelica/userGuide/performance.html
|
# 3. Simulation Performance¶
This section provides tips for how to implement numerically efficient models.
## 3.1. Control input signal of equipment¶
Most equipment models that take a real-valued control signals as an input, such as flow machines (fans and pumps), have a boolean parameter filteredSpeed, and all actuators have a boolean parameter filteredOpening. If set to true, which is the default setting, then the control input signal is sent to a 2nd order low pass filter that changes a step signal to a smooth signal. This typically improves the robustness of the simulation.
To see the effect of the filter, consider the model below in which fanS is configured with filteredSpeed=false, and fanC is configured with filteredSpeed=true. Both fans are connected to a step input signal. The configuration of fanS causes the fan speed to instantly change from 0 to 1. In large system models, this can lead to high computing time or to convergence problems. The fanC avoids this problem because the speed of the fan varies continuously, thereby making it easier for the solver to compute a solution. In this model, we set the parameter raiseTime=30 seconds.
Fig. 3.1 Schematic diagram of fans that are configured with filteredSpeed=false (fanS) and filteredSpeed=true (fanC).
Fig. 3.2 Mass flow rate of the two fans for a step input signal at 0 seconds.
For fans and pumps, the dynamics introduced by the filter can be thought of as approximating the rotational inertia of the fan rotor and the inertia of the fluid in the duct or piping network. The default value is raiseTime=30 seconds.
For actuators, the raise time approximates the travel time of the valve lift. The default value is raiseTime=120 seconds.
Note
When changing filteredSpeed (or filteredOpening), or when changing the value of raiseTime, the dynamic response of the closed loop control changes. Therefore, control gains may need to be retuned to ensure satisfactory closed loop control performance.
For further information, see the User’s Guide of the flow machine package, and the User’s Guide of the actuator package.
## 3.2. Fluid flow systems¶
### 3.2.1. Breaking algebraic loops¶
In fluid flow systems, flow junctions where mass flow rates separate and mix can couple non-linear systems of equations. This leads to larger systems of coupled equations that need to be solved, which often causes larger computing time and can sometimes cause convergence problems. To decouple these systems of equations, in the model of a flow junction (Buildings.Fluid.FixedResistances.Junction), or in models for fans or pumps (such as the model Buildings.Fluid.Movers.SpeedControlled_y), the parameter dynamicBalance can be set to true. This adds a control volume at the fluid junction that can decouple the system of equations.
### 3.2.2. Reducing nonlinear equations of serially connected flow resistances¶
In fluid flow systems, if multiple components are connected in series, then computing the pressure drop due to flow friction in the individual components can lead to coupled nonlinear systems of equations. While this is no problem for small models, the iterative solution can lead to higher computing time, particularly in large models where other equations may be part of the residual function.
For illustration, consider the simple system shown below in which the flow resistances res1 and res2 compute the mass flow rate as $$\dot m = k \, \sqrt{\Delta p}$$ if the parameter from_dp is set to true, or otherwise compute the pressure drop between their inlet and outlet as $$\Delta p = (\dot m / k)^2$$. (Both formulations are implemented using regularization near zero.)
Fig. 3.3 Schematic diagram of two flow resistances in series that connect a source and a volume.
Depending on the configuration of the individual component models, simulating this system model may require the iterative solution of a nonlinear equation to compute the mass flow rate or the pressure drop. To avoid a nonlinear equation, use any of the measures below.
• Set the parameter res2(dp_nominal=0), and add the pressure drop to the parameter dp_nominal of the model res1. This will eliminate the equation that computes the flow friction in res2, thereby avoiding a nonlinear equation. The same applies if there are multiple components in series, such as a pre-heat coil, a heating coil and a cooling coil.
• Set from_dp=false in all components, which is the default setting. This will cause Modelica to use a function that computes the pressure drop as a function of the mass flow rate. Therefore, a code translator is likely to generate an equation that solves for the mass flow rate, and it then uses the mass flow rate to compute the pressure drop of the components that are connected in series.
Control valves also allow lumping the pressure drop into the model of the valve. Consider the situation where a fixed flow resistance is in series with a control valve as shown below.
Fig. 3.4 Schematic diagram of a fixed flow resistance and a valve in series that connect a source and a volume.
Suppose the parameters are
Buildings.Fluid.FixedResistances.PressureDrop res(
redeclare package Medium = Medium,
m_flow_nominal=0.2,
dp_nominal=10000);
Buildings.Fluid.Actuators.Valves.TwoWayLinear val(
redeclare package Medium = Medium,
m_flow_nominal=0.2,
dpValve_nominal=5000);
To avoid a nonlinear equation, the flow resistance could be deleted as shown below.
Fig. 3.5 Schematic diagram of a valve that connects a source and a volume.
If the valve is configured as
Buildings.Fluid.Actuators.Valves.TwoWayLinear val(
redeclare package Medium = Medium,
m_flow_nominal=0.2,
dpValve_nominal=5000,
dpFixed_nominal=10000);
then the valve will compute the composite flow coefficient $$\bar k$$ as
$\bar k = \frac{1}{\sqrt{1/k_v(y) + 1/k_f}}$
where $$k_v(y) = \dot m(y)/\sqrt{\Delta p}$$ is the flow coefficient of the valve at the lift $$y$$, and $$k_f$$ is equal to the ratio m_flow_nominal/sqrt(dpFixed_nominal). The valve model then computes the pressure drop using $$\bar k$$ and the same equations as described above for the fixed resistances. Thus, the composite model has the same valve authority and mass flow rate, but a nonlinear equation can be avoided.
For more details, see the User’s Guide of the actuator package.
### 3.2.3. Prescribed mass flow rate¶
For some system models, the mass flow rate can be prescribed by using an idealized pump or fan (model Buildings.Fluid.Movers.FlowControlled_m_flow) or a source element that outputs the required mass flow rate (such as the model Buildings.Fluid.Sources.MassFlowSource_T). Using these models avoids having to compute the intersection of the fan curve and the flow resistance. In some situations, this can lead to faster and more robust simulation.
Warning
If you prescribe the mass flow rate, make sure the pump (or fan) does not work agains a closed valve (or damper). Otherwise, it will force the flow through the component, which leads to very large pressure drops.
### 3.2.4. Avoiding events¶
In Modelica, the time integration is halted whenever a Real elementary operation such as $$x>y$$, where $$x$$ and $$y$$ are variables of type Real, changes its value. In this situation, an event occurs and the solver determines a small interval in time in which the relation changes its value. This can increase computing time. An example where such an event occurs is the following relation that computes the enthalpy of the medium that streams through port_a as
if port_a.m_flow > 0 then
h_a = inStream(port_a.h_outflow);
else
h_a = port_a.h_outflow;
end if;
or, equivalently,
h_a = if port_a.m_flow > 0 then inStream(port_a.h_outflow) else port_a.h_outflow;
When simulating a model that contains such code, a time integrator will iterate to find the time instant where port_a.m_flow crosses zero. If the modeling assumptions allow approximating this equation in a neighborhood around port_a.m_flow=0, then replacing this equation with an approximation that does not require an event iteration can reduce computing time. For example, the above equation could be approximated as
T_a = Modelica.Fluid.Utilities.regStep(
port_a.m_flow, inStream(port_a.h_outflow), port_a.h_outflow,
m_flow_nominal*1E-4);
where m_flow_nominal is a parameter that is set to a value that is close to the mass flow rate that the model has at full load. If the magnitude of the flow rate is larger than 1E-4 times the typical flow rate, the approximate equation is the same as the exact equation, and below that value, an approximation is used. However, for such small flow rates, not much energy is transported and hence the error introduced by the approximation is generally negligible.
In some cases, adding dynamics to the model can further improve the computing time, because the return value of the function Modelica.Fluid.Utilities.regStep() above can change abruptly if its argument port_a.m_flow oscillates in the range of +/- 1E-4*m_flow_nominal, for example due to numerical noise. Adding dynamics may be achieved using a formulation such as
hMed = Modelica.Fluid.Utilities.regStep(
port_a.m_flow, inStream(port_a.h_outflow), port_a.h_outflow,
m_flow_nominal*1E-4);
der(h)=(hMed-h)/tau;
where tau>0 is a time constant. See, for example, Buildings.Fluid.Sensors.SpecificEnthalpyTwoPort for a robust implementation.
Note
In the package Buildings.Utilities.Math the functions and blocks whose names start with smooth can be used to avoid events.
## 3.3. Examples for how to debug and correct slow simulations¶
### 3.3.1. State events¶
This section shows how a simulation that stalls due to events can be debugged to find the root cause, and then corrected. While the details may differ from one tool to another, the principle is the same. In our situation, we attempted to simulate Buildings.Examples.DualFanDualDuct for one year in Dymola 2016 FD01 using the model from Buildings version 3.0.0. We run
simulateModel("Buildings.Examples.DualFanDualDuct.ClosedLoop",
tolerance=1e-06, resultFile="DualFanDualDuctClosedLoop");
and plotted the computing time and the number of events. Around $$t=0.95e7$$ seconds, there was a spike as shown in the figure below.
Fig. 3.6 Computing time and number of events.
As the number of events increased drastically, we enabled in Dymola in Simulation -> Setup, under the tab Debug the entry Events during simulation and simulated the model from $$t=0.9e7$$ to $$t=1.0e7$$ seconds. It turned out that setting the start time to $$t=0.9e7$$ seconds was sufficient to reproduce the behavior; otherwise we would have had to set it to an earlier time. Inspecting Dymola’s log file dslog.txt when the simulation stalls shows that its last entries are
Expression TRet.T > amb.x_pTphi.T became true ( (TRet.T)-(amb.x_pTphi.T) = 2.9441e-08 )
Iterating to find consistent restart conditions.
during event at Time : 9267949.854873843
Expression TRet.T > amb.x_pTphi.T became false ( (TRet.T)-(amb.x_pTphi.T) = -2.94411e-08 )
Iterating to find consistent restart conditions.
during event at Time : 9267949.855016639
Expression TRet.T > amb.x_pTphi.T became true ( (TRet.T)-(amb.x_pTphi.T) = 2.94407e-08 )
Iterating to find consistent restart conditions.
during event at Time : 9267949.855208419
Expression TRet.T > amb.x_pTphi.T became false ( (TRet.T)-(amb.x_pTphi.T) = -2.94406e-08 )
Iterating to find consistent restart conditions.
during event at Time : 9267949.855351238
Hence, there is an event every few milliseconds, which explains why the simulation does not appear to be progessing. The solver does the right thing, it stops the integration, handles the event, and restarts the integration, just to encounter another event a few milliseconds later. Hence, we go back to our system model and follow the output signal of TRet.T of the return air temperature sensor, which shows that it is used in the economizer control to switch the sign of the control gain because the economizer can provide heating or cooling, depending on the ambient and return air temperature. The problematic model is shown in the figure below.
Fig. 3.7 Block diagram of part of the economizer control that computes the outside air damper control signal. This implementation triggers many events.
The events are triggered by the inequality block which changes the control, which then in turn seems to cause a slight change in the return air temperature, possibly due to numerical noise or maybe because the return fan may change its operating point as the dampers are adjusted, and hence change the heat added to the medium. Regardless, this is a bad implementation that also would cause oscillatory behavior in a real system if the sensor signal had measurement noise. Therefore, this equality comparison must be replaced by a block with hysteresis, which we did as shown in the figure below. We selected a hysteresis of $$0.2$$ Kelvin, and now the model runs fine for the whole year.
Fig. 3.8 Block diagram of part of the revised economizer control that computes the outside air damper control signal.
### 3.3.2. State variables that dominate the error control¶
In a development version of the model Buildings.Examples.DualFanDualDuct.ClosedLoop (commit ef410ee), the simulation time was very slow during part of the simulation, as shown in Fig. 3.9.
Fig. 3.9 Computing time and number of events.
The number of state events did not increase in that time interval. To isolate the problem, we enabled in Dymola under Simulation -> Setup the option to log which states dominate the error (see Debug tab).
Running the simulation again gave the following output:
Integration terminated successfully at T = 1.66e+07
Limit stepsize, Dominate error, Exceeds 10% of error Component (#number)
0 1 6 cooCoi.temSen_1.T (# 1)
36 0 140 cooCoi.temSen_2.T (# 2)
37 0 0 cooCoi.ele[1].mas.T (# 3)
45 0 0 cooCoi.ele[2].mas.T (# 4)
51 0 0 cooCoi.ele[3].mas.T (# 5)
53 0 0 cooCoi.ele[4].mas.T (# 6)
13555 13201 19064 fanSupHot.filter.x[1] (# 7)
11905 2170 12394 fanSupHot.filter.x[2] (# 8)
400 47 419 fanSupCol.filter.x[1] (# 9)
420 71 521 fanSupCol.filter.x[2] (# 10)
5082 2736 6732 fanRet.filter.x[1] (# 11)
1979 25 4974 fanRet.filter.x[2] (# 12)
38 0 3 TPreHeaCoi.T (# 13)
30 0 1 TRet.T (# 14)
38 0 3 TMix.T (# 15)
80 0 0 TCoiCoo.T (# 16)
305 22 275 cor.vavHot.filter.x[1] (# 18)
Hence, the state variables in the highlighted lines limit the step size significantly more often than other variables. Therefore, we removed these state variables by setting in the fan models the parameter filteredSpeed=false. After this change, the model simulates without problems.
## 3.4. Numerical solvers¶
Dymola 2021 is configured to use dassl as a default solver with a tolerance of 1E-4. We recommend to change this setting to radau with a tolerance of around 1E-6, as this generally leads to faster and more robust simulation for thermo-fluid flow systems.
Note that this is the error tolerance of the local integration time step. Most ordinary differential equation solvers only control the local integration error and not the global integration error. As a rule of thumb, the global integration error is one order of magnitude larger than the local integration error. However, the actual magnitude of the global integration error depends on the stability of the differential equation. As an extreme case, if a system is chaotic and uncontrolled, then the global integration error will grow rapidly.
| 2020-12-02T06:06:45 |
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|
https://alldimensions.fandom.com/wiki/TREEVERSE
|
## FANDOM
2,681 Pages
TREEVERSE is one of the biggest finitely-sized verses. Although it is very big, it only contains $g_{n^2}$ galaxies, with hypergroups, each containing $\frac{g_{n^2}}{n^2}$ galaxies. It also exists in all dimensions, except dimensions below 2nd, and has a different property of each dimension's TREEVERSE. In it's planets with life, you can find lots of trees and TREES. TREES are trees that can reach 200-1200 meters of height. It can contain other verses, like there are [n, n2, n3...nn] Rainbowlineverses, Udekaverses, Vendekaverses and if the right dimensionality (5D+), they can contain the Multiverses. It also contains some (10-100) Zverses.
It's biggest stars are the ꦋ-class stars, with a diameter from 12 741 to 617 194 solar diameters. The smallest types of stars are ䷨-class stars, with a diameter from 493-611 kilometers. As this verse's size is extremely really big, you may think that some of it's verses are exactly identical to ours, but no, but it can allow a Earth where humans exist, but have a different history. Only 92n-129n Tree-verse clusters (clusters that the closest verse needs to be <82.3 of itself verses apart, and contain 10+ of the same kind of verses) allow the existance of verses exactly identical to ours.
There are $\frac{n*g_{n}}{\left[n,\operatorname{ceil}\left(\frac{n}{2}\right)\right]}$TREEVERSES in a Barrel.
## TREEYUM
In $100\frac{1}{\prod_{o=1}^n\frac{n}{o}}\%$ of planets of TREEVERSE, there is a element called TREEYUM (T), a element found mostly 74-394 km below the planet's surface. It is a lot harder than diamond, and nearly unbreakable. It is not radioactive, as 3/56, of its isotopes are stable, and it has a orange color. It has 83 electrons, 59 protons, 3 neutrons and 7 exotic protons. To be solid, it needs to be in contact with other materials (at least 6-8 nm away from them), otherwise its going to be gas, but it liquifies at 0.0000000000032 °K and solidifies at 1.71*10-31 °K when not in contact with other materials. As it is harder than diamond, it is used on 2.8km- skyscrapers, because it cannot held the pressure so it will fall, so upyte is used.
## TREETITE
TREETITE is a synthetic material created by TREEVERSIANS, it has a HEP (Heptadecimal) color. The formula for TREETITE is $\operatorname{T_2V_7CoHe_{33}Sg_{HEP color}}$ , base 17. The seaborgium is the HEP color, so HEP #176D1G will have 176D1G17 atoms, or 2037772 seaborgium atoms. It is used in spaceships, because TREETITE can survive (be solid) becoming gas when not in contact with other materials, but as TREETITE is more breakable than TREEYUM, it is only used in spaceships.
SPOILER: It will appear in BFBFBFBFB 11, when Joshua Ray Barkfelt takes the last #00GG00 TREETITE, but it was actually #00GG01 so team Nugcfycycyrxxdxdtxxidtxezaaqgcycouvyv5756889990987654321HIiiihvfyversemuiviverse.......verse………^…^…^^…^^o lose.
## TREEMIUM
TREEMIUM is a mineral and element found in the core of $\frac{100}{\sum_{g=0}^{n}ng^{2}} \%$ of the planets of TREEVERSE, and $\frac{100}{n\uparrow\uparrow 3}$ have the element 152 or less kilometers above it's core. It is found in TREEVITE rocks, containing minerals like $\operatorname{Gd_2H}$, $\operatorname{DyNe_3}$, $\operatorname{Nd_2Sb_3}$ and $\operatorname{M_3}$ (tri-TREEMIUM). It's symbol is M, and it's used to make TREEKITE. It is very rare in the TIC (TREEVERSE's interclusteral commerce)[1], because of the location of TREEMIUM. It also has a blue/purple color, but the purple color is rarer than the blue one.
## TREEKITE
TREEKITE is a synthetic material created by TREEVERSIANS, made to resemble TREEMIUM, and being cheaper, because you can make it by putting $\operatorname{T_2PCs_3}$ (solid) in $\operatorname{KCl_3}$ (liquid), giving $\operatorname{TCs_3K}$ and $\operatorname{M_2}$ , then the $\operatorname{TCs_3K}$ is removed from the mix. In the TIC, it costs ᐕ371.28 (371.28 riennans) per rock, 78.2% less than normal TREEMIUM (ᐕ1703.12 per rock). It is normally blue, but you can can change its color to green by throwing $\operatorname{M_2}$ into $\operatorname{W_2O_3}$ (liquid), it will react with the ditungsten trioxide and form $\operatorname{WO_2M_4}$, and its color will be green, that costs ᐕ439.03 per rock.
## Unite
Unite is a rare rock found below 193 meters below some planet's surfaces, but found in $\frac{1}{173*10^{15}}$ parts per million, that means, it is 7 times more rare than Radon on Earth[2]. It is not an element, but a junction of elements. It's chemical formula is $\operatorname{HHe_2Li_3Be_4\cdots Lv_{116}Ts_{117}Og_{118}}$, aka 118Ut (the 3rd, most common, the 1st most common is 38Ut and the 2nd is 143Ut). The 118Ut costs ᐕ82712.49 per rock, and 38Ut costs ᐕ33925.28 per rock.
### Umite
The Umite was created by the Treckimea humans, and is the highest Unite rock someone in 1000000000 ly from the Trackimea cluster has ever created. It is 38319124Ut. It was created with some help of the squares, and it is one of the 612 out of 90000001 types of Unite (10000000Ut to 100000000Ut) that isn't radioative.
### Upyte
The Upyte is a synthetic type of Unite, and it is the most common kind of one. It is very strong (stronger than TREEYUM!), so it is used on building skyscrapers. Treckimea humans that have gone to Tyàts also passed that material to squares. They only used it in houses.
##
1. The TIC was created and only used by the inhabitants of the cluster where the TREEVERSIAN colonizers of Tyàts came from (aka Treckimea).
Community content is available under CC-BY-SA unless otherwise noted.
| 2019-11-13T13:30:39 |
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|
https://par.nsf.gov/biblio/10340397-memory-hard-puzzles-standard-model-applications-memory-hard-functions-resource-bounded-locally-decodable-codes
|
Memory-Hard Puzzles in the Standard Model with Applications to Memory-Hard Functions and Resource-Bounded Locally Decodable Codes
We formally introduce, define, and construct {\em memory-hard puzzles}. Intuitively, for a difficulty parameter $t$, a cryptographic puzzle is memory-hard if any parallel random access machine (PRAM) algorithm with small'' cumulative memory complexity ($\ll t^2$) cannot solve the puzzle; moreover, such puzzles should be both easy'' to generate and be solvable by a sequential RAM algorithm running in time $t$. Our definitions and constructions of memory-hard puzzles are in the standard model, assuming the existence of indistinguishability obfuscation (\iO) and one-way functions (OWFs), and additionally assuming the existence of a {\em memory-hard language}. Intuitively, a language is memory-hard if it is undecidable by any PRAM algorithm with small'' cumulative memory complexity, while a sequential RAM algorithm running in time $t$ can decide the language. Our definitions and constructions of memory-hard objects are the first such definitions and constructions in the standard model without relying on idealized assumptions (such as random oracles). We give two applications which highlight the utility of memory-hard puzzles. For our first application, we give a construction of a (one-time) {\em memory-hard function} (MHF) in the standard model, using memory-hard puzzles and additionally assuming \iO and OWFs. For our second application, we show any cryptographic puzzle (\eg, memory-hard, time-lock) more »
Authors:
; ;
Award ID(s):
Publication Date:
NSF-PAR ID:
10340397
Journal Name:
Security and Cryptography for Networks
3. Memory-hard functions (MHFs) are a key cryptographic primitive underlying the design of moderately expensive password hashing algorithms and egalitarian proofs of work. Over the past few years several increasingly stringent goals for an MHF have been proposed including the requirement that the MHF have high sequential space-time (ST) complexity, parallel space-time complexity, amortized area-time (aAT) complexity and sustained space complexity. Data-Independent Memory Hard Functions (iMHFs) are of special interest in the context of password hashing as they naturally resist side-channel attacks. iMHFs can be specified using a directed acyclic graph (DAG) $G$ with $N=2^n$ nodes and low indegree and the complexity of the iMHF can be analyzed using a pebbling game. Recently, Alwen et al. [CCS'17] constructed an DAG called DRSample which has aAT complexity at least $\Omega\left( N^2/\log N\right)$. Asymptotically DRSample outperformed all prior iMHF constructions including Argon2i, winner of the password hashing competition (aAT cost $\mathcal{O}\left(N^{1.767}\right)$), though the constants in these bounds are poorly understood. We show that the the greedy pebbling strategy of Boneh et al. [ASIACRYPT'16] is particularly effective against DRSample e.g., the aAT cost is $\mathcal{O}\left( N^2/\log N\right)$. In fact, our empirical analysis {\em reverses} the prior conclusion of Alwen et al. that DRSample providesmore »
| 2023-01-27T14:29:54 |
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|
http://dlmf.nist.gov/23.10
|
# §23.10 Addition Theorems and Other Identities
###### Contents
23.10.1
23.10.2
23.10.3
For further addition-type identities for the -function see Lawden (1989, §6.4).
If , then
23.10.5
and
## §23.10(ii) Duplication Formulas
23.10.7
(23.10.8) continues to hold when , , are permuted cyclically.
23.10.9
## §23.10(iv) Homogeneity
For any nonzero real or complex constant
23.10.17
23.10.18
23.10.19
Also, when is replaced by the lattice invariants and are divided by and , respectively.
For these results and further identities see Lawden (1989, §6.6) and Apostol (1990, p. 14).
| 2014-03-11T02:54:51 |
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|
http://trilinos.sandia.gov/packages/docs/r10.8/packages/teuchos/browser/doc/html/example_2BLAS_2cxx__main_8cpp_source.html
|
Teuchos Package Browser (Single Doxygen Collection) Version of the Day
example/BLAS/cxx_main.cpp
Go to the documentation of this file.
00001 /*
00003 // ***********************************************************************
00004 //
00005 // Teuchos: Common Tools Package
00006 // Copyright (2004) Sandia Corporation
00007 //
00008 // Under terms of Contract DE-AC04-94AL85000, there is a non-exclusive
00009 // license for use of this work by or on behalf of the U.S. Government.
00010 //
00011 // Redistribution and use in source and binary forms, with or without
00012 // modification, are permitted provided that the following conditions are
00013 // met:
00014 //
00015 // 1. Redistributions of source code must retain the above copyright
00016 // notice, this list of conditions and the following disclaimer.
00017 //
00018 // 2. Redistributions in binary form must reproduce the above copyright
00019 // notice, this list of conditions and the following disclaimer in the
00020 // documentation and/or other materials provided with the distribution.
00021 //
00022 // 3. Neither the name of the Corporation nor the names of the
00023 // contributors may be used to endorse or promote products derived from
00024 // this software without specific prior written permission.
00025 //
00026 // THIS SOFTWARE IS PROVIDED BY SANDIA CORPORATION "AS IS" AND ANY
00027 // EXPRESS OR IMPLIED WARRANTIES, INCLUDING, BUT NOT LIMITED TO, THE
00028 // IMPLIED WARRANTIES OF MERCHANTABILITY AND FITNESS FOR A PARTICULAR
00029 // PURPOSE ARE DISCLAIMED. IN NO EVENT SHALL SANDIA CORPORATION OR THE
00030 // CONTRIBUTORS BE LIABLE FOR ANY DIRECT, INDIRECT, INCIDENTAL, SPECIAL,
00031 // EXEMPLARY, OR CONSEQUENTIAL DAMAGES (INCLUDING, BUT NOT LIMITED TO,
00032 // PROCUREMENT OF SUBSTITUTE GOODS OR SERVICES; LOSS OF USE, DATA, OR
00033 // PROFITS; OR BUSINESS INTERRUPTION) HOWEVER CAUSED AND ON ANY THEORY OF
00034 // LIABILITY, WHETHER IN CONTRACT, STRICT LIABILITY, OR TORT (INCLUDING
00035 // NEGLIGENCE OR OTHERWISE) ARISING IN ANY WAY OUT OF THE USE OF THIS
00036 // SOFTWARE, EVEN IF ADVISED OF THE POSSIBILITY OF SUCH DAMAGE.
00037 //
00038 // Questions? Contact Michael A. Heroux ([email protected])
00039 //
00040 // ***********************************************************************
00042 */
00043
00044 #include "Teuchos_BLAS.hpp"
00045 #include "Teuchos_Version.hpp"
00046
00047 int main(int argc, char* argv[])
00048 {
00049 std::cout << Teuchos::Teuchos_Version() << std::endl << std::endl;
00050
00051 // Creating an instance of the BLAS class for double-precision kernels looks like:
00052 Teuchos::BLAS<int, double> blas;
00053
00054 // This instance provides the access to all the BLAS kernels listed in Figure \ref{blas_kernels}:
00055 const int n = 10;
00056 double alpha = 2.0;
00057 double x[ n ];
00058 for ( int i=0; i<n; i++ ) { x[i] = i; }
00059 blas.SCAL( n, alpha, x, 1 );
00060 int max_idx = blas.IAMAX( n, x, 1 );
00061 std::cout<< "The index of the maximum magnitude entry of x[] is the "
00062 << max_idx <<"-th and x[ " << max_idx-1 << " ] = "<< x[max_idx-1]
00063 << std::endl;
00064
00065 return 0;
00066 }
| 2014-07-30T15:31:33 |
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|
https://www.nist.gov/mml/csd/chemical-informatics-group/lennard-jones-fluid-properties
|
An official website of the United States government
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# Lennard-Jones Fluid Properties
## Share
The purpose of these pages is to provide some explicit results from molecular dynamics and Monte Carlo simulations for the Lennard-Jones fluid. It is intended to provide guides for testing codes. Reproducing these results is a test of the correctness of codes, either written by the user or obtained elsewhere. The explicit conditions for each of the sets of results are supplied so that meaningful comparisons of your results with the ones listed here are possible.
The information presented here has been organized into eight different pages. It is available as web pages or as a single excel file.
1. MD: NVE Molecular dynamics results at liquid-like densities along an isotherm of reduced temperature 0.85. Mean values and standard deviations of temperature, energy, pressure, and diffusion coefficient are reported.
2. LAMMPS-MD: NVT Molecular dynamics results at vapor- and liquid-like densities along isotherms of reduced temperature 0.65 - 1.20. Mean values and standard error of temperature, energy, and pressure are reported.
3. MC: NVT Monte Carlo results at both liquid- and vapor-like densities along two isotherms of reduced temperature 0.85 and 0.90. Mean values and standard deviations of energy and pressure are reported.
4. SAT-TMMC: Liquid-vapor coexistence properties obtained by grand-canonical transition-matrix Monte Carlo and histogram re-weighting [1]. Mean values and standard deviations of the saturation pressure and coexisting liquid and vapor densities, energies, and activities are reported.
A. LJ Potential truncated at 3σ, with analytic long-range corrections, over the reduced temperature range 0.70 to 1.20 at increments of 0.05.
B. LJ Potential with linear force shift at 2.5σ, over the reduced temperature range 0.65 to 0.90 at increments of 0.05.
C. LJ Potential with linear force shift at 3.0σ, over the reduced temperature range 0.70 to 1.00 at increments of 0.05.
D. LJ Potential with linear force shift at 3.5σ, over the reduced temperature range 0.70 to 1.15 at increments of 0.05.
E. LJ Potential with linear force shift at 4.0σ, over the reduced temperature range 0.60 to 1.20 at increments of 0.05.
F. LJ Potential cut, with no tail correction, at 5.0σ, over the reduced temperature range 0.60 to 1.25 at increments of 0.05.
5. EOS-TMMC: Equations of state (pressure as a function density) generated by grand-canonical transition-matrix Monte Carlo over the temperature range 0.70 to 1.20 and 1.35 - 1.50 at increments of 0.05. For a given density, the mean pressure and its standard deviation are reported. CPU timings and downloadable raw simulation data (particle number probability distributions) are provided here.
6. SAT-EOS: Liquid-vapor coexistence properties as determined from an empirical fit of a large amount of simulation data [2]. The data serve as an approximate guide for liquid-vapor coexistence properties at temperatures other than those investigated in Item 3. Furthermore, the empirical fit should not be used in the vicinity of the critical point.
7. SURFACE TENSION: Surface tension of the Lennard-Jones fluid at various temperatures calculated using explicit molecular dynamics of the liquid-vapor interface and the combination of finite-size scaling and grand-canonical transition-matrix Monte Carlo. The influence of truncation is also investigated in this section.
8. VAPOR-EOS-TMMC: Vapor-phase properties for the Lennard-Jones fluid, linear-force shifted at r=2.5σ obtained by grand-canonical transition-matrix Monte Carlo and histogram re-weighting [1] over the reduced temperature range 0.65 to 0.90 at increments of 0.05. Mean values and standard deviations of the saturation pressure and coexisting liquid and vapor densities, energies, and activities are reported.
As is usually the case, temperature, density (number density), pressure, etc., are given in reduced units (denoted by *). That is, these properties are expressed in terms of the characteristic energy, ε, and length scale, σ, defined by the Lennard-Jones potential:
$$\Large V_{LJ} \left( r \right) = 4 \epsilon \left[ \left(\dfrac{\sigma}{r}\right)^{12} -\left(\dfrac{\sigma}{r}\right)^{6} \right]$$
Therefore, the reduced temperature T*, density ρ*, and pressure p* are kBT/ε, ρσ3, pσ3/ε, respectively. The critical parameters for the pure LJ fluid have been determined to be Tc* = 1.3120(7), ρc* = 0.316(1), and pc* = 0.1279(6) [3].
For computational expediency, the potential and force are usually truncated at some cutoff distance rc. That is, the effective potential V(r) is
$$\Large V\left( r \right) = \begin{cases} V_{LJ} \left( r \right) & r \leq r_c \\ 0 & r > r_c \end{cases}$$
In this work, the cutoff distance is taken to be 3σ, unless noted otherwise. An approximate correction for this truncation to the energy and pressure of the system can be obtained by assuming the spatial correlations beyond the cutoff distance are unity. The reader is referred to Refs. [4] and [5] for these so-called "standard long range corrections" (sLRC). It should be noted that this not a good assumption in inhomogeneous fluids. For completeness, the working expressions for obtaining the long range corrections to the potential energy per particle and virial pressure are provided below:
$$\Large U_{LRC} = \dfrac{1}{2} 4 \pi \rho \int _{r_c} ^{\infty} dr~r^2~V_{LJ} \left( r \right)$$
$$\Large p_{LRC} = -\left( \dfrac{1}{2} \right) \left( \dfrac{1}{3} \right) 4 \pi \rho^2 \int _{r_c} ^{\infty} dr~r^2~r~ \dfrac{dV_{LJ} \left( r \right)}{dr}$$
where ρ is the bulk number density, VLJ(r) is the Lennard-Jones potential energy, and rc is the truncation (cutoff) distance. A subtle point to note is that the above pressure correction does not account for impulsive effects at rc where the potential energy (and therefore the force) changes discontinuously. This is particularly important when trying to simulate directly interfacial phenomena [6]. Finally, it should be mentioned that other truncation and long range correction schemes for dealing with non-bonded interactions exist [4-8]. In some cases, the truncation schemes can yield critical properties that differ from those quoted above [8].
In future versions, coordinate sets will be available for which the potential energy per particle and the virial are specified. This information can be used to test energy/force routines.
### References
1. J. R. Errington, J. Chem. Phys. 118, 9915 (2003).
2. J. K. Johnson, J. A. Zollweg, and K. E. Gubbins, Mol. Phys. 78, 591 (1993).
3. J. J. Potoff and A. Z. Panagiotopoulos, J. Chem. Phys. 109, 10914 (1998).
4. M. P. Allen and D. J. Tildesley, Computer Simulation of Liquids (Oxford University Press, New York, 1989).
5. D. Frenkel and B. Smit, Understanding Molecular Simulation, 2nd ed. (Academic, San Diego, 2002)., pp.37-38.
6. A. Trkohymchuk and J. Alejandre, J. Chem. Phys. 111, 8510 (1999).
7. D. N. Theodorou and U. W. Suter, J. Chem. Phys. 82, 955 (1985).
8. B. Smit, J. Chem. Phys. 96, 8639 (1992).
Created July 27, 2012, Updated June 2, 2021
| 2023-01-29T18:12:37 |
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|
http://legisquebec.gouv.qc.ca/en/showversion/cr/P-40.1,%20r.%203?code=se:79_6_8&pointInTime=20210720
|
### P-40.1, r. 3 - Regulation respecting the application of the Consumer Protection Act
79.6.8. The notice provided for in paragraph b of section 187.9 of the Act must be sent to the consumer between the 90th and the 60th day preceding the coming into force of the amendment.
O.C. 994-2018, s. 47.
In force: 2019-08-01
79.6.8. The notice provided for in paragraph b of section 187.9 of the Act must be sent to the consumer between the 90th and the 60th day preceding the coming into force of the amendment.
O.C. 994-2018, s. 47.
| 2021-09-16T15:37:45 |
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http://scstatehouse.gov/sess120_2013-2014/SJ13/20130227.htm
|
South Carolina General Assembly
120th Session, 2013-2014
Journal of the Senate
Wednesday, February 27, 2013
(Statewide Session)
Indicates Matter Stricken
Indicates New Matter
The Senate assembled at 2:00 P.M., the hour to which it stood adjourned, and was called to order by the PRESIDENT.
A quorum being present, the proceedings were opened with a devotion by the Chaplain as follows:
The Psalmist declared:
"Your word is a lamp to my feet and a light for my path."
(Psalm 119:105)
Join me as we bow in prayer, please:
Holy God, how challenging and difficult are the issues that confront these leaders in this day and time. The resulting pressures on them and their aides have to be so great. We ask, O Lord, that You clearly illumine the way which these Senators are to follow, that You light their paths in a manner that results in their arriving at the best decisions and actions for everyone in South Carolina. And may these leaders themselves always feel confident of Your gracious guidance. We pray this in Your loving name, dear Lord.
Amen.
The PRESIDENT called for Petitions, Memorials, Presentments of Grand Juries and such like papers.
The following were received and referred to the appropriate committee for consideration:
Document No. 4334
Agency: Board of Architectural Examiners
Chapter: 11
Statutory Authority: 1976 Code Sections 40-1-70 and 40-3-60
SUBJECT: Officers, Meetings, Applications and Fees, Renewals, and Continuing Education
Received by Lieutenant Governor February 27, 2013
Referred to Labor, Commerce and Industry Committee
Legislative Review Expiration February 3, 2014
Document No. 4335
Agency: Board of Cosmetology
Chapter: 35
Statutory Authority: 1976 Code Sections 40-1-70, 40-13-60, and 40-13-80
Received by Lieutenant Governor February 27, 2013
Referred to Labor, Commerce and Industry Committee
Legislative Review Expiration February 3, 2014
Document No. 4336
Agency: Board of Cosmetology
Chapter: 35
Statutory Authority: 1976 Code Sections 40-1-70 and 40-13-60
SUBJECT: Requirements of Licensure in the Field of Cosmetology (Educational Requirements)
Received by Lieutenant Governor February 27, 2013
Referred to Labor, Commerce and Industry Committee
Legislative Review Expiration February 3, 2014
Document No. 4337
Agency: Board of Cosmetology
Chapter: 35
Statutory Authority: 1976 Code Sections 40-1-70 and 40-13-60
SUBJECT: Requirements of Licensure in the Field of Cosmetology (Sanitation and Salons)
Received by Lieutenant Governor February 27, 2013
Referred to Labor, Commerce and Industry Committee
Legislative Review Expiration February 3, 2014
Document No. 4338
Agency: Manufactured Housing Board
Chapter: 79
Statutory Authority: 1976 Code Sections 40-1-70 and 40-29-200(B)(1)
SUBJECT: Financial Responsibility
Received by Lieutenant Governor February 27, 2013
Referred to Labor, Commerce and Industry Committee
Legislative Review Expiration February 3, 2014
REGULATION RESUBMITTED
Document No. 4168
Agency: South Carolina Perpetual Care Cemetery Board
Chapter: 21
Statutory Authority: 1976 Code Sections 40-8-10, et seq.
SUBJECT: Perpetual Care Cemetery Board
Received by Lieutenant Governor January 8, 2013
Referred to Labor, Commerce and Industry Committee
Legislative Review Expiration May 8, 2013
Senate Referred to LCI Committee February 2, 2011
Senate Requested Withdrawal May 5, 2011
120 Day Period Tolled
Withdrawn and Resubmitted January 10, 2012
Senate Committee Requested Withdrawal January 10, 2012
120 Day Period Tolled
Withdrawn due to end of two-year session June 8, 2012
Resubmitted with no substantive changes January 8, 2013
Received by Lt. Gov & Speaker May 5, 2013
Senate Committee Requested Withdrawal February 21, 2013
120 Day Period Tolled
Withdrawn and Resubmitted February 27, 2013
REGULATIONS WITHDRAWN AND RESUBMITTED
Document No. 4282
Agency: Board of Chiropractic Examiners
Chapter: 25
Statutory Authority: 1976 Code Sections 40-1-70 and 40-9-30
SUBJECT: Requirements of Licensure for Chiropractors
Received by Lieutenant Governor January 8, 2013
Referred to Medical Affairs Committee
Legislative Review Expiration May 8, 2013
Committee Requested Withdrawal February 21, 2013
120 Day Period Tolled
Withdrawn and Resubmitted February 26, 2013
Document No. 4328
Agency: Occupational Therapy Board
Chapter: 94
Statutory Authority: 1976 Code Sections 40-1-70 and 40-36-10, et seq.
SUBJECT: Requirements of Licensure for Occupational Therapists
Received by Lieutenant Governor January 30, 2013
Referred to Labor, Commerce and Industry Committee
Legislative Review Expiration May 30, 2013
Committee Requested Withdrawal February 21, 2013
120 Day Period Tolled
Withdrawn and Resubmitted Feruary 27, 2013
Leave of Absence
On motion of Senator BRYANT, at 2:05 P.M., Senator VERDIN was granted a leave of absence for today.
Leave of Absence
On motion of Senator COURSON, at 2:05 P.M., Senator GREGORY was granted a leave of absence for today.
Leave of Absence
At 3:30 P.M., Senator GROOMS requested a leave of absence beginning at 3:45 P.M. and lasting until 10:00 P.M.
Leave of Absence
On motion of Senator SETZLER, at 6:00 P.M., Senator MATTHEWS was granted a leave of absence for the balance of the day.
Doctor of the Day
Senators BRYANT and O'DELL introduced Dr. Marshall Meadors of Anderson, S.C., Doctor of the Day.
S. 137 (Word version) Sens. Cromer, Grooms
S. 237 (Word version) Sen. Young
S. 382 (Word version) Sens. Pinckney, Hembree, Cromer, Matthews
S. 401 (Word version) Sen. Coleman
Privilege of the Chamber
On motion of Senator BRYANT, Chairman of the Committee on Invitations, and on behalf of Senator SHEALY, with unanimous consent, the Privilege of the Chamber, to that area behind the rail, was granted to Richard Culliver and his family.
At 2:22 P.M., Senator COURSON asked unanimous consent to make a motion to invite the House of Representatives to attend the Senate Chamber for the purpose of ratifying Acts at 3:00 P.M.
There was no objection and a message was sent to the House accordingly.
Expression of Personal Interest
Senator GROOMS rose for an Expression of Personal Interest.
Point of Order
Senator LEATHERMAN raised a Point of Order under Rule 13 that the time limitation for an Expression of Personal Interest was five minutes.
The PRESIDENT stated that the time had expired.
Expression of Personal Interest
Senator SHANE MARTIN rose for an Expression of Personal Interest.
Expression of Personal Interest
Senator BRIGHT rose for an Expression of Personal Interest.
RECALLED, AMENDED AND READ THE SECOND TIME
S. 352 (Word version) -- Senators Massey and Nicholson: A BILL TO AMEND SECTION 7-7-390, AS AMENDED, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO THE DESIGNATION OF VOTING PRECINCTS IN MCCORMICK COUNTY, SO AS TO ADD THE "MONTICELLO" PRECINCT, TO DESIGNATE A MAP NUMBER ON WHICH THE NAMES OF THESE PRECINCTS MAY BE FOUND AND MAINTAINED BY THE OFFICE OF RESEARCH AND STATISTICS OF THE STATE BUDGET AND CONTROL BOARD, AND TO CORRECT ARCHAIC LANGUAGE.
Senator LARRY MARTIN asked unanimous consent to make a motion to recall the Bill from the Committee on Judiciary.
The Bill was recalled from the Committee on Judiciary.
Senator LARRY MARTIN asked unanimous consent to make a motion to take the Bill up for immediate consideration.
There was no objection.
The Senate proceeded to a consideration of the Bill. The question then was the second reading of the Bill.
Senators MASSEY and NICHOLSON proposed the following amendment (JUD0352.001), which was adopted:
Amend the bill, as and if amended, page 1, by striking lines 27 and 28, in Section 7-7-390, as contained in SECTION 1, and inserting therein the following:
/ "Section 7-7-390. In McCormick County there are the following voting precincts numbered and named as follows: /
Renumber sections to conform.
Amend title to conform.
The question then was the second reading of the Bill.
The "ayes" and "nays" were demanded and taken, resulting as follows:
Ayes 42; Nays 0; Abstain 1
AYES
Alexander Allen Bennett
Bright Bryant Campbell
Campsen Cleary Coleman
Corbin Courson Cromer
Davis Fair Ford
Grooms Hayes Hembree
Hutto Jackson Johnson
Leatherman Lourie Malloy
Martin, Larry Martin, Shane Massey
Matthews McElveen McGill
Nicholson O'Dell Peeler
Pinckney Rankin Reese
Scott Shealy Thurmond
Turner Williams Young
Total--42
NAYS
Total--0
ABSTAIN
Sheheen
Total--1
The Bill was read the second time, passed and ordered to a third reading.
INTRODUCTION OF BILLS AND RESOLUTIONS
The following were introduced:
S. 433 (Word version) -- Senators Peeler, Leatherman, Courson, Hayes, L. Martin, Alexander, Fair, Grooms, Verdin, Cromer, O'Dell, Rankin, Bryant, Campsen, Cleary, Campbell, Massey, Bright, Davis, S. Martin, Gregory, Bennett, Corbin, Hembree, Shealy, Thurmond, Turner and Young: A SENATE RESOLUTION TO RECOGNIZE AND HONOR WESLEY DONEHUE FOR AGGRESSIVELY PURSUING HIS GOALS AND FOR HIS DEDICATION AND COMMITMENT TO COMMUNITY AFFAIRS, AND TO CONGRATULATE HIM FOR BEING NAMED TO THE 2013 STATE NEWSPAPER'S 20 UNDER 40.
l:\s-res\hsp\001done.mrh.hsp.docx
Senators PEELER and CAMPSEN spoke on the Resolution.
S. 434 (Word version) -- Senator Nicholson: A SENATE RESOLUTION TO EXTEND HEARTIEST CONGRATULATIONS AND BEST WISHES TO MR. LUTHER C. SHELTON, JR. ON THE OCCASION OF HIS NINETIETH BIRTHDAY AND TO WISH HIM MANY MORE YEARS OF HEALTH AND HAPPINESS.
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S. 435 (Word version) -- Senator Verdin: A SENATE RESOLUTION TO HONOR THE LIFE OF HEAVEN CAROL PHIPPS, INFANT DAUGHTER OF TONYA PHIPPS AND STEVE NELSON, TO EXPRESS PROFOUND SORROW OF THE MEMBERS OF THE SENATE UPON HER UNTIMELY DEATH, AND TO EXTEND DEEPEST SYMPATHY TO HER LOVING FAMILY.
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S. 436 (Word version) -- Senators Leatherman and Malloy: A BILL TO AMEND THE CODE OF LAWS OF SOUTH CAROLINA, 1976, BY ADDING SECTION 59-40-237 SO AS TO ALLOW A LOCAL SCHOOL DISTRICT TO SPONSOR A CHARTER SCHOOL LOCATED IN A CONTIGUOUS SCHOOL DISTRICT IF THE SCHOOL SERVES PREDOMINANTLY AT-RISK STUDENTS.
l:\council\bills\nl\13032dg13.docx
Read the first time and referred to the Committee on Education.
S. 437 (Word version) -- Senators Cleary, Reese, Rankin, Campsen, Hembree, Davis, McGill, Thurmond, Campbell and Cromer: A BILL TO AMEND SECTION 12-43-220, AS AMENDED, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO VALUATION AND CLASSIFICATION OF PROPERTY FOR PURPOSES OF THE PROPERTY TAX, SO AS TO PROVIDE THAT THE OWNER-OCCUPANT OF RESIDENTIAL PROPERTY QUALIFIES FOR THE FOUR PERCENT ASSESSMENT RATIO ALLOWED OWNER-OCCUPIED RESIDENTIAL PROPERTY, IF THE OWNER IS OTHERWISE QUALIFIED AND THE RESIDENCE IS NOT RENTED FOR MORE THAN ONE HUNDRED DAYS A YEAR, AND TO DELETE OTHER REFERENCES TO RENTAL OF THESE RESIDENCES; AND TO AMEND SECTION 12-54-240, RELATING TO DISCLOSURE OF RECORDS, REPORTS, AND RETURNS WITH THE DEPARTMENT OF REVENUE, SO AS TO PROVIDE VERIFICATION THAT THE FEDERAL SCHEDULE E CONFORMS WITH THE SAME DOCUMENT REQUIRED BY A COUNTY ASSESSOR IS NOT PROHIBITED.
l:\council\bills\nl\13162dg13.docx
Read the first time and referred to the Committee on Finance.
S. 438 (Word version) -- Senators L. Martin and Campbell: A BILL TO AMEND THE CODE OF LAWS OF SOUTH CAROLINA, 1976, BY ADDING SECTION 8-15-70 SO AS TO PROVIDE FOR THE FAIR AND OPEN COMPETITION IN GOVERNMENTAL CONTRACTS BY STIPULATING THAT STATE OR LOCAL ENTITIES, OFFICIALS, AND EMPLOYEES, IN REGARD TO A PUBLIC BUILDING, MAY NOT REQUIRE OR PROHIBIT A BIDDER, OFFEROR, CONTRACTOR, OR SUBCONTRACTOR FROM ENTERING INTO OR ADHERING TO AN AGREEMENT WITH ONE OR MORE LABOR ORGANIZATIONS IN REGARD TO THE PROJECT AND MAY NOT OTHERWISE DISCRIMINATE AGAINST A BIDDER, OFFEROR, CONTRACTOR, OR SUBCONTRACTOR FOR BECOMING OR REFUSING TO BECOME A SIGNATORY TO AN AGREEMENT WITH ONE OR MORE LABOR ORGANIZATIONS IN REGARD TO THE PROJECT, TO PROVIDE THAT STATE AND LOCAL ENTITIES, OFFICIALS, AND EMPLOYEES SHALL NOT AWARD A GRANT, TAX ABATEMENT, OR TAX CREDIT CONDITIONED UPON THE INCLUSION OF SUCH AGREEMENTS IN THE AWARD, AND TO PROVIDE EXCEPTIONS TO AND EXEMPTIONS FROM THESE PROVISIONS.
l:\council\bills\dka\3089sd13.docx
Read the first time and referred to the Committee on Finance.
S. 439 (Word version) -- Senators Fair, Hutto and Jackson: A BILL TO AMEND SECTION 63-13-40, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO CRIMINAL BACKGROUND CHECKS FOR EMPLOYMENT IN CHILDCARE FACILITIES, SO AS TO ALSO PROHIBIT SUCH EMPLOYMENT OF A PERSON WHO HAS BEEN CONVICTED OF UNLAWFUL CONDUCT TOWARD A CHILD, CRUELTY TO CHILDREN, OR CHILD ENDANGERMENT.
l:\council\bills\nbd\11138vr13.docx
Read the first time and referred to the Committee on Judiciary.
S. 440 (Word version) -- Senators Fair, Hutto and Jackson: A BILL TO AMEND THE CODE OF LAWS OF SOUTH CAROLINA, 1976, BY ADDING SECTION 63-19-1435 SO AS TO PROVIDE THAT THE USE OF RESTRAINTS ON JUVENILES APPEARING IN COURT ARE PROHIBITED UNLESS THE RESTRAINTS ARE NECESSARY TO PREVENT HARM OR IF THE JUVENILE IS A FLIGHT RISK AND THERE ARE NO LESS RESTRICTIVE ALTERNATIVES AVAILABLE; TO GIVE A JUVENILE'S ATTORNEY THE RIGHT TO BE HEARD BEFORE THE COURT ORDERS THE USE OF RESTRAINTS; AND IF RESTRAINTS ARE ORDERED, TO REQUIRE THE COURT TO MAKE FINDINGS OF FACT IN SUPPORT OF THE ORDER.
l:\council\bills\nbd\11144ac13.docx
Read the first time and referred to the Committee on Judiciary.
S. 441 (Word version) -- Senators Fair, Hutto and Jackson: A BILL TO AMEND THE CODE OF LAWS OF SOUTH CAROLINA, 1976, BY ADDING SECTION 16-15-386 SO AS TO CREATE THE OFFENSE OF SEXTING FOR A PERSON LESS THAN EIGHTEEN YEARS OF AGE; TO PROVIDE FOR CIVIL FINES AND COSTS FOR COMMITTING A FIRST OR SECOND OFFENSE; TO PROVIDE FOR A MISDEMEANOR AND A CRIMINAL FINE AND COSTS FOR COMMITTING THREE OR MORE OFFENSES; TO PROHIBIT THE ARREST OR PLACEMENT IN THE CUSTODY OF THE DEPARTMENT OF JUVENILE JUSTICE OR OTHER CONFINEMENT FOR COMMITTING A FIRST OR SECOND OFFENSE, WITH CERTAIN EXCEPTIONS; TO PROHIBIT PROSECUTION OF A PERSON WHO HAS COMMITTED A FIRST OR SECOND SEXTING OFFENSE UNDER THIS SECTION OF COMMITTING CERTAIN OTHER CRIMES; TO PROHIBIT PLACEMENT ON THE SEX OFFENDER REGISTRY FOR COMMITTING AN OFFENSE UNDER THIS SECTION; TO PROVIDE FOR CONTEMPT OF COURT AND REQUIRED COMMUNITY SERVICE FOR FAILURE TO PAY FINES FOR FIRST AND SECOND OFFENSES; AND TO VEST EXCLUSIVE JURISDICTION TO HEAR ALLEGED OFFENSES IN THE MUNICIPAL AND MAGISTRATES COURT.
l:\council\bills\nbd\11126vr13.docx
Read the first time and referred to the Committee on Judiciary.
S. 442 (Word version) -- Senators Fair, Hutto and Jackson: A BILL TO AMEND SECTION 63-13-20, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO THE DEFINITION OF TERMS USED IN THE REGULATION OF CHILDCARE FACILITIES, SO AS TO DEFINE "SCHOOL VACATION AND SCHOOL HOLIDAY CAMPS FOR CHILDREN"; AND BY ADDING SECTION 63-13-220 SO AS TO MAKE CERTAIN EMPLOYEE CRIMINAL BACKGROUND CHECKS PROVISIONS APPLICABLE TO EMPLOYEES AND VOLUNTEERS WHO WORK AT SCHOOL VACATION AND SCHOOL HOLIDAY CAMPS; TO HAVE A CAREGIVER PRESENT AT ALL TIMES AT SCHOOL VACATION AND SCHOOL HOLIDAY CAMPS WHO IS CERTIFIED IN BASIC FIRST AID AND INFANT-CHILD CARDIOPULMONARY RESUSCITATION; AND TO HAVE A LIFEGUARD PRESENT AT ALL TIMES FOR SCHOOL VACATION AND SCHOOL HOLIDAY CAMPS THAT ALLOW CHILDREN TO HAVE ACCESS TO A BODY OF WATER.
l:\council\bills\nbd\11141vr13.docx
Read the first time and referred to the Committee on Judiciary.
S. 443 (Word version) -- Senators Fair, Hutto and Jackson: A BILL TO AMEND SECTION 19-1-180, AS AMENDED, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO THE ADMISSIBILITY OF OUT-OF-COURT STATEMENTS MADE BY CHILDREN UNDER CERTAIN CIRCUMSTANCES, SO AS TO ALLOW THE ADMISSIBILITY OF HEARSAY STATEMENTS MADE TO FORENSIC INTERVIEWERS; TO DEFINE FORENSIC INTERVIEWER; AND TO PROVIDE FOR TRAINING AND CONTINUING EDUCATION REQUIREMENTS FOR FORENSIC INTERVIEWERS.
l:\council\bills\nbd\11139vr13.docx
Read the first time and referred to the Committee on Judiciary.
S. 444 (Word version) -- Senators O'Dell and Sheheen: A JOINT RESOLUTION PROPOSING AN AMENDMENT TO SECTION 7, ARTICLE VI OF THE CONSTITUTION OF SOUTH CAROLINA, 1895, RELATING TO THE CONSTITUTIONAL OFFICERS OF THIS STATE, SO AS TO DELETE THE ADJUTANT GENERAL FROM THE LIST OF STATE OFFICERS WHICH THE CONSTITUTION REQUIRES TO BE ELECTED; AND TO AMEND SECTION 4, ARTICLE XIII, RELATING TO THE ADJUTANT AND INSPECTOR GENERAL, SO AS TO DELETE AN OBSOLETE REFERENCE TO INSPECTOR GENERAL, TO MAKE A CONFORMING CHANGE TO THE RANK OF THE ADJUTANT GENERAL, TO PROVIDE THAT BEGINNING UPON THE EXPIRATION OF THE TERM OF THE ADJUTANT GENERAL SERVING IN OFFICE ON THE DATE OF THE RATIFICATION OF THIS AMENDMENT, THE ADJUTANT GENERAL MUST BE APPOINTED BY THE GOVERNOR UPON THE ADVICE AND CONSENT OF THE SENATE FOR A FOUR-YEAR TERM COMMENCING ON THE FIRST WEDNESDAY FOLLOWING THE SECOND TUESDAY IN JANUARY FOLLOWING THE GENERAL ELECTION, WHICH MARKS THE MIDTERM OF THE GOVERNOR, EXCEPT THAT THE INITIAL TERM OF THE FIRST ADJUTANT GENERAL APPOINTED PURSUANT TO THIS AMENDMENT MUST BE FOR TWO YEARS SO AS TO ALLOW SUBSEQUENT TERMS TO BE STAGGERED WITH THAT OF THE GOVERNOR, AND TO PROVIDE THAT THE GENERAL ASSEMBLY SHALL PROVIDE BY LAW FOR THE DUTIES, COMPENSATION, AND QUALIFICATIONS FOR THE OFFICE, THE PROCEDURES BY WHICH THE APPOINTMENT IS MADE, AND THE PROCEDURES BY WHICH THE ADJUTANT GENERAL MAY BE REMOVED FROM OFFICE.
l:\council\bills\ggs\22530zw13.docx
Read the first time and referred to the Committee on Judiciary.
S. 445 (Word version) -- Senators O'Dell, Sheheen and Setzler: A BILL TO AMEND SECTION 1-3-240, AS AMENDED, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO THE REMOVAL OF OFFICERS BY THE GOVERNOR, SO AS TO ADD THE ADJUTANT GENERAL TO THE LIST OF OFFICERS OR ENTITIES THE GOVERNING BOARD OF WHICH MAY BE REMOVED BY THE GOVERNOR ONLY FOR CERTAIN REASONS CONSTITUTING CAUSE; TO AMEND SECTION 25-1-320, RELATING TO THE STATE ADJUTANT GENERAL, SO AS TO PROVIDE THAT BEGINNING UPON THE EXPIRATION OF THE TERM OF THE ADJUTANT GENERAL SERVING IN OFFICE ON THE DATE OF THE 2014 GENERAL ELECTION, THE ADJUTANT GENERAL MUST BE APPOINTED BY THE GOVERNOR UPON THE ADVICE AND CONSENT OF THE SENATE FOR A FOUR-YEAR TERM COMMENCING ON THE FIRST WEDNESDAY FOLLOWING THE SECOND TUESDAY IN JANUARY THAT FOLLOWS THE GENERAL ELECTION THAT MARKS THE MIDTERM OF THE GOVERNOR, EXCEPT THAT THE INITIAL TERM OF THE FIRST ADJUTANT GENERAL APPOINTED PURSUANT TO THIS ACT MUST BE FOR TWO YEARS SO AS TO ALLOW SUBSEQUENT TERMS TO BE STAGGERED WITH THAT OF THE GOVERNOR, AND TO ESTABLISH CERTAIN QUALIFICATIONS FOR THE OFFICE OF ADJUTANT GENERAL; TO AMEND SECTION 25-1-340, AS AMENDED, RELATING TO VACANCIES IN THE OFFICE OF ADJUTANT GENERAL, SO AS TO DELETE A REFERENCE TO THE ELIGIBILITY REQUIREMENTS OF CONSTITUTIONAL OFFICERS; AND TO PROVIDE THAT THE ABOVE PROVISIONS ARE EFFECTIVE UPON THE RATIFICATION OF AMENDMENTS TO SECTION 7, ARTICLE VI, AND SECTION 4, ARTICLE XIII OF THE CONSTITUTION OF THIS STATE DELETING THE REQUIREMENT THAT THE STATE ADJUTANT GENERAL BE ELECTED BY THE QUALIFIED ELECTORS OF THIS STATE.
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Read the first time and referred to the Committee on Judiciary.
S. 446 (Word version) -- Senator Massey: A BILL TO RATIFY AN AMENDMENT TO SECTION 8, ARTICLE IV OF THE CONSTITUTION OF SOUTH CAROLINA, 1895, RELATING TO THE ELECTION, QUALIFICATIONS, AND TERM OF THE LIEUTENANT GOVERNOR, TO PROVIDE THAT THE LIEUTENANT GOVERNOR MUST BE ELECTED JOINTLY WITH THE GOVERNOR IN A MANNER PRESCRIBED BY LAW; TO ADD SECTION 37 TO ARTICLE III OF THE CONSTITUTION OF THIS STATE, TO PROVIDE THAT THE SENATE SHALL ELECT FROM AMONG ITS MEMBERS A PRESIDENT TO PRESIDE OVER THE SENATE AND TO PERFORM OTHER DUTIES AS PROVIDED BY LAW; TO DELETE SECTIONS 9 AND 10 OF ARTICLE IV OF THE CONSTITUTION OF THIS STATE, RELATING TO THE LIEUTENANT GOVERNOR BEING PRESIDENT OF THE SENATE AND, WHILE PRESIDING IN THE SENATE, HAVING NO VOTE, UNLESS THE SENATE IS EQUALLY DIVIDED, TO REMOVE INCONSISTENT PROVISIONS; TO AMEND SECTION 11 OF ARTICLE IV OF THE CONSTITUTION OF THIS STATE, RELATING TO THE REMOVAL OF THE LIEUTENANT GOVERNOR FROM OFFICE BY IMPEACHMENT, DEATH, RESIGNATION, DISQUALIFICATION, DISABILITY, OR REMOVAL FROM THE STATE, TO PROVIDE THAT THE GOVERNOR SHALL APPOINT, WITH THE ADVICE AND CONSENT OF THE SENATE, A SUCCESSOR TO FULFILL THE UNEXPIRED TERM; AND TO AMEND SECTION 12 OF ARTICLE IV OF THE CONSTITUTION OF THIS STATE, RELATING TO THE DISABILITY OF THE GOVERNOR, TO CONFORM APPROPRIATE REFERENCES.
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Read the first time and referred to the Committee on Judiciary.
S. 447 (Word version) -- Senator Fair: A BILL TO AMEND THE CODE OF LAWS OF SOUTH CAROLINA, 1976, SO AS TO ENACT THE "SOUTH CAROLINA STOP METHAMPHETAMINE PRODUCTION ACT"; BY ADDING SECTION 44-53-362 SO AS TO PROVIDE A PRACTITIONER WITH CONTROLLED SUBSTANCES PRESCRIPTIVE AUTHORITY IMMUNITY FROM CIVIL AND CRIMINAL LIABILITY FOR PRESCRIBING SUCH DRUG IN THE ABSENCE OF GROSS NEGLIGENCE; TO AMEND SECTION 44-53-230, RELATING TO DRUGS DESIGNATED AS SCHEDULE III CONTROLLED SUBSTANCES, SO AS TO INCLUDE EPHEDRINE, PSEUDOEPHEDRINE, AND PHENYLPROPANOLAMINE IN THIS DESIGNATION; TO AMEND SECTION 44-53-376, RELATING TO THE CRIMINAL OFFENSE OF DISPOSING OF WASTE FROM THE PRODUCTION OF METHAMPHETAMINE, SO AS TO REQUIRE A LOCAL GOVERNMENTAL ENTITY THAT LOCATES OR SEIZES A METHAMPHETAMINE LABORATORY OR DUMPSITE TO REPORT SUCH ACTION TO THE STATE LAW ENFORCEMENT DIVISION; TO AMEND SECTION 44-53-398, AS AMENDED, RELATING TO THE OVER-THE-COUNTER SALE AND PURCHASE OF EPHEDRINE, PSEUDOEPHEDRINE, AND PHENYLPROPANOLAMINE, INCLUDING, AMONG OTHER THINGS, REQUIREMENTS FOR PACKAGING, RETAIL SALE AND PURCHASE AMOUNTS, AND LOGGING AND TRANSMITTING SALES AND PURCHASE INFORMATION, SO AS TO DELETE ALL PROVISIONS REGULATING THE SALE AND PURCHASE REQUIREMENTS OF THESE CONTROLLED SUBSTANCES EXCEPT THE FELONY CRIMINAL OFFENSE, PENALTIES FOR VIOLATIONS, AND LEGITIMATE MEDICAL EXCEPTIONS FOR POSSESSION, MANUFACTURING, DELIVERING, DISTRIBUTING, DISPENSING, ADMINISTERING, PURCHASING, OR SELLING THESE CONTROLLED SUBSTANCES; TO AMEND SECTION 44-53-1640, RELATING TO THE DEPARTMENT OF HEALTH AND ENVIRONMENTAL CONTROL PRESCRIPTION MONITORING PROGRAM FOR SCHEDULE II, III, AND IV CONTROLLED SUBSTANCES, SO AS TO PROVIDE THAT INFORMATION SUBMITTED TO THIS MONITORING PROGRAM MUST BE SUBMITTED IN ACCORDANCE WITH CERTAIN NATIONAL PHARMACY AUTOMATION AND EXCHANGE OF INFORMATION STANDARDS; TO AMEND SECTION 44-53-1650, RELATING TO THE CONFIDENTIALITY OF INFORMATION SUBMITTED TO THE PRESCRIPTION MONITORING PROGRAM, INCLUDING PROCEDURES FOR RELEASING THIS INFORMATION, SO AS TO PROVIDE THAT LAW ENFORCEMENT MAY OBTAIN INFORMATION ON EPHEDRINE, PSEUDOEPHEDRINE, OR PHENYLPROPANOLAMINE SALES AND PURCHASES WITHOUT CONDUCTING A SPECIFIC DRUG RELATED INVESTIGATION ON A DESIGNATED PERSON; TO AMEND CHAPTER 32, TITLE 56, RELATING TO THE MOTOR VEHICLE DAMAGE DISCLOSURE ACT, SO AS TO REQUIRE A PERSON SELLING A MOTOR VEHICLE THAT WAS THE SITE OF A METHAMPHETAMINE LABORATORY OR DUMPSITE TO DISCLOSE THIS INFORMATION IN WRITING TO THE PURCHASER OF THE VEHICLE; TO AMEND SECTION 63-7-920, RELATING TO CHILD ABUSE AND NEGLECT INVESTIGATIONS AND PLACEMENT, SO AS TO PROHIBIT THE DEPARTMENT OF SOCIAL SERVICES FROM PLACING A CHILD WHO HAS BEEN EXPOSED TO METHAMPHETAMINE USE, MANUFACTURE, SALE, DISTRIBUTION, OR TRAFFICKING WITH A RELATIVE OR ASSOCIATE INVOLVED IN SUCH ILLEGAL ACTIVITY; AND TO REPEAL SECTION 23-3-1200 RELATING TO THE STATE LAW ENFORCEMENT DIVISION SERVING AS THE DEPOSITORY OF CERTAIN SCHEDULE II CONTROLLED SUBSTANCE INFORMATION.
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Read the first time and referred to the Committee on Medical Affairs.
S. 448 (Word version) -- Senator Alexander: A BILL TO AMEND THE CODE OF LAWS OF SOUTH CAROLINA, 1976, BY ADDING SECTION 40-47-938 SO AS TO PROVIDE CIRCUMSTANCES IN WHICH A PHYSICIAN MAY ENTER A SUPERVISORY RELATIONSHIP WITH A PHYSICIAN ASSISTANT; TO AMEND SECTION 40-47-910, RELATING TO DEFINITIONS IN THE PHYSICIAN ASSISTANTS PRACTICE ACT, SO AS TO ADD AND REVISE CERTAIN DEFINITIONS; TO AMEND SECTION 40-47-940, RELATING TO APPLICATION FOR LICENSURE, SO AS TO DELETE CERTAIN APPLICATION REQUIREMENTS; TO AMEND SECTION 40-47-945, RELATING TO CONDITIONS FOR GRANTING PERMANENT LICENSURE, SO AS TO DELETE REQUIREMENTS THAT AN APPLICANT APPEAR BEFORE THE BOARD WITH HIS SUPERVISING PHYSICIAN AND HIS SCOPE OF PRACTICE GUIDELINES, AND TO DELETE THE PROHIBITION AGAINST THE APPROVAL OF A SUPERVISING PHYSICIAN OF ON-THE-JOB TRAINING OR TASKS NOT LISTED ON THE APPLICATION FOR LIMITED LICENSURE AS A PHYSICIAN ASSISTANT; TO AMEND SECTION 40-47-955, RELATING TO PHYSICAL PRESENCE REQUIREMENTS OF THE SUPERVISING PHYSICIAN OF A PHYSICIAN ASSISTANT, SO AS TO DELETE EXISTING REQUIREMENTS CONCERNING ON-SITE SETTINGS AND TO PROVIDE WHERE AND HOW A PHYSICIAN ASSISTANT MAY PRACTICE, TO REVISE PROVISIONS CONCERNING OFF-SITE SETTINGS, AND TO REVISE CERTAIN REQUIREMENTS OF A SUPERVISING PHYSICIAN; TO AMEND SECTION 40-47-960, RELATING TO MINIMUM REQUIREMENTS FOR SCOPE OF PRACTICE GUIDELINES FOR PHYSICIAN ASSISTANTS, SO AS TO INCLUDE THE IMMEDIATE CONSULTATION BETWEEN THE PHYSICIAN ASSISTANT AND HIS PRIMARY OR SUPERVISING PHYSICIAN; TO AMEND SECTION 40-47-965, RELATING TO THE AUTHORITY OF A PHYSICIAN ASSISTANT TO REQUEST OR RECEIVE PROFESSIONAL SAMPLES OF DRUGS AUTHORIZED UNDER HIS SCOPE OF PRACTICE GUIDELINES, SO AS TO DELETE THE PROHIBITION AGAINST REQUESTING OR RECEIVING PROFESSIONAL SAMPLES OF SCHEDULE II CONTROLLED SUBSTANCES; TO AMEND SECTION 40-47-970, RELATING TO THE PRESCRIBING OF DRUGS BY A PHYSICIAN ASSISTANT, SO AS TO AS TO DELETE A PROHIBITION AGAINST PRESCRIBING SCHEDULE II CONTROLLED SUBSTANCES; TO AMEND SECTION 40-47-975, RELATING TO THE AUTHORITY OF A SUPERVISING PHYSICIAN TO REQUEST PERMISSION FROM THE BOARD FOR A PHYSICIAN ASSISTANT UNDER HIS SUPERVISION TO RECEIVE ON-THE-JOB TRAINING, SO AS TO DELETE EXISTING LANGUAGE AND PROVIDE THAT A SUPERVISING PHYSICIAN MAY DETERMINE WHETHER A PHYSICIAN ASSISTANT UNDER HIS SUPERVISION NEEDS ADDITIONAL TRAINING OR EDUCATION, THAT THE PHYSICIAN AND PHYSICIAN ASSISTANT MAY JOINTLY DETERMINE THE MEANS OF PROVIDING THIS TRAINING OR EDUCATION, AND THAT CERTAIN RELATED INFORMATION MUST BE SUBMITTED TO THE BOARD OF MEDICAL EXAMINERS AND THE PHYSICIAN ASSISTANT COMMITTEE FOR THE APPROVAL OF EACH; TO AMEND SECTION 40-47-995, RELATING TO THE TERMINATION OF A SUPERVISORY RELATIONSHIP BETWEEN A PHYSICIAN AND PHYSICIAN ASSISTANT, SO AS TO PROVIDE THAT UPON THIS TERMINATION THE PRACTICE OF THE PHYSICIAN ASSISTANT MUST CEASE UNTIL NEW SCOPE OF PRACTICE GUIDELINES, RATHER THAN A NEW APPLICATION, ARE SUBMITTED BY A NEW SUPERVISING PHYSICIAN TO THE BOARD; AND TO REPEAL SECTION 40-47-980 RELATING TO THE TREATMENT OF PATIENTS IN CHRONIC CARE AND LONG-TERM CARE FACILITIES.
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Read the first time and referred to the Committee on Medical Affairs.
S. 449 (Word version) -- Fish, Game and Forestry Committee: A JOINT RESOLUTION TO APPROVE REGULATIONS OF THE DEPARTMENT OF NATURAL RESOURCES, RELATING TO SEASONS, LIMITS, METHODS OF TAKE AND SPECIAL USE RESTRICTIONS ON WILDLIFE MANAGEMENT AREAS, DESIGNATED AS REGULATION DOCUMENT NUMBER 4297, PURSUANT TO THE PROVISIONS OF ARTICLE 1, CHAPTER 23, TITLE 1 OF THE 1976 CODE.
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Read the first time and ordered placed on the Calendar without reference.
S. 450 (Word version) -- Senators Hutto, Alexander, Allen, Bennett, Bright, Bryant, Campbell, Campsen, Cleary, Coleman, Corbin, Courson, Cromer, Davis, Fair, Ford, Gregory, Grooms, Hayes, Hembree, Jackson, Johnson, Leatherman, Lourie, Malloy, L. Martin, S. Martin, Massey, Matthews, McElveen, McGill, Nicholson, O'Dell, Peeler, Pinckney, Rankin, Reese, Scott, Setzler, Shealy, Sheheen, Thurmond, Turner, Verdin, Williams and Young: A SENATE RESOLUTION TO COMMEND MAYOR RICHARD ALTON MCCOLLUM OF BAMBERG FOR HIS LIFETIME OF DEDICATED PUBLIC SERVICE, TO CONGRATULATE HIM UPON HIS RETIREMENT AS MAYOR OF BAMBERG, AND TO WISH HIM MUCH SUCCESS AND FULFILLMENT IN ALL HIS FUTURE ENDEAVORS.
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S. 451 (Word version) -- Senators Bright, Bryant, Davis, Corbin, Grooms and Shealy: A BILL TO AMEND CHAPTER 2, TITLE 12 OF THE 1976 CODE, RELATING TO TAXATION, BY ADDING SECTION 12-2-110, TO PROVIDE THAT PRIVATE CHILDCARE FACILITIES, PRIVATE SCHOOLS, AND HOME SCHOOLS BE TAXED IN THE SAME MANNER AS A PUBLIC FACILITY PROVIDING LIKE SERVICES.
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Senator BRIGHT spoke on the Bill.
Read the first time and referred to the Committee on Finance.
S. 452 (Word version) -- Senators Scott, Alexander, Allen, Bennett, Bright, Bryant, Campbell, Campsen, Cleary, Coleman, Corbin, Courson, Cromer, Davis, Fair, Ford, Gregory, Grooms, Hayes, Hembree, Hutto, Jackson, Johnson, Leatherman, Lourie, Malloy, L. Martin, S. Martin, Massey, Matthews, McElveen, McGill, Nicholson, O'Dell, Peeler, Pinckney, Rankin, Reese, Setzler, Shealy, Sheheen, Thurmond, Turner, Verdin, Williams and Young: A SENATE RESOLUTION TO RECOGNIZE AND HONOR RENOWNED NEW YORK CITY RESTAURATEUR MELBA WILSON FOR HER SUCCESSFUL CAREER, TO WELCOME HER TO THE PALMETTO STATE, AND TO EXTEND THANKS FOR HER PARTICIPATION IN THE FIRST ANNUAL SOUTH CAROLINA CORNBREAD FESTIVAL.
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S. 453 (Word version) -- Senator Setzler: A SENATE RESOLUTION TO RECOGNIZE AND HONOR JOHN QUINCY "JOHNNY" HUDSON, JR. OF AIKEN COUNTY AND TO COMMEND HIM FOR FORTY YEARS OF DEVOTED SERVICE AS AN ELECTED MEMBER OF THE WAGENER TOWN COUNCIL AND FOR HIS LIFELONG DEDICATION TO SERVING OTHERS.
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S. 454 (Word version) -- Senators Bright and Bryant: A BILL TO AMEND SECTION 16-23-420 OF THE 1976 CODE, RELATING TO POSSESSION OF A FIREARM ON ANY PREMISES OR PROPERTY OWNED, OPERATED, OR CONTROLLED BY A PRIVATE OR PUBLIC COLLEGE, UNIVERSITY, TECHNICAL COLLEGE, OR OTHER POST-SECONDARY INSTITUTION, TO PROVIDE THAT A PERSON AUTHORIZED TO CARRY A CONCEALED WEAPON PURSUANT TO ARTICLE 4, CHAPTER 31, TITLE 23, WHO IS A REGISTERED STUDENT, EMPLOYEE, OR FACULTY MEMBER OF THE INSTITUTION, MAY POSSESS A FIREARM ON ANY PREMISES OR PROPERTY OWNED, OPERATED, OR CONTROLLED BY THE INSTITUTION, AND A PRIVATE COLLEGE, UNIVERSITY, TECHNICAL COLLEGE, OR OTHER POST-SECONDARY INSTITUTION MAY POST A SIGN STATING "NO CONCEALABLE WEAPONS ALLOWED" WHICH SHALL CONSTITUTE NOTICE TO A PERSON HOLDING A PERMIT ISSUED PURSUANT TO ARTICLE 4, CHAPTER 31, TITLE 23 THAT CONCEALABLE WEAPONS NOT BE BROUGHT UPON THE PREMISES.
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Senator BRIGHT spoke on the Bill.
Read the first time and referred to the Committee on Judiciary.
S. 455 (Word version) -- Senators Bright and Bryant: A BILL TO AMEND SECTION 23-31-215 OF THE 1976 CODE, RELATING TO ISSUANCE OF A CONCEALED WEAPONS PERMIT, TO PROVIDE THAT A CONCEALED WEAPONS PERMIT IS VALID UNTIL THE SOUTH CAROLINA LAW ENFORCEMENT DIVISION DETERMINES THE RENEWAL APPLICATION IS DENIED.
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Senator BRIGHT spoke on the Bill.
Read the first time and referred to the Committee on Judiciary.
H. 3378 (Word version) -- Reps. Sandifer, Whitmire and Gambrell: A BILL TO AMEND THE CODE OF LAWS OF SOUTH CAROLINA, 1976, BY ADDING SECTION 6-1-90 SO AS TO ENACT THE "VOLUNTEER SERVICE PERSONNEL APPRECIATION ACT" AND TO ALLOW THE GOVERNING BODY OF A LOCAL GOVERNMENT TO AUTHORIZE THE DISTRIBUTION OF CERTAIN REWARDS TO THREE ENUMERATED CATEGORIES OF VOLUNTEER SERVICE PERSONNEL SO LONG AS ALL PERSONNEL IN A RESPECTIVE CATEGORY ARE TREATED EQUALLY.
Read the first time and referred to the Committee on Judiciary.
H. 3525 (Word version) -- Reps. Hayes, Barfield, Clemmons, H. A. Crawford, George, Goldfinch, Hardee, Hardwick and Ryhal: A CONCURRENT RESOLUTION TO REQUEST THAT THE DEPARTMENT OF TRANSPORTATION NAME THE INTERSECTION LOCATED AT THE JUNCTURE OF SOUTH CAROLINA HIGHWAYS 9 AND 410 IN HORRY COUNTY "LIEUTENANT JOHN RONALD FLOYD INTERSECTION" AND ERECT APPROPRIATE MARKERS OR SIGNS AT THIS INTERSECTION THAT CONTAIN THE WORDS "LIEUTENANT JOHN RONALD FLOYD INTERSECTION".
The Concurrent Resolution was introduced and referred to the Committee on Transportation.
H. 3574 (Word version) -- Medical, Military, Public and Municipal Affairs Committee: A JOINT RESOLUTION TO APPROVE REGULATIONS OF THE DEPARTMENT OF LABOR, LICENSING AND REGULATION - PANEL FOR DIETETICS, RELATING TO DEFINITIONS, DESIGNATED AS REGULATION DOCUMENT NUMBER 4237, PURSUANT TO THE PROVISIONS OF ARTICLE 1, CHAPTER 23, TITLE 1 OF THE 1976 CODE.
Read the first time and referred to the Committee on Medical Affairs.
H. 3614 (Word version) -- Reps. Rutherford, Alexander, Allison, Anderson, Anthony, Atwater, Bales, Ballentine, Bannister, Barfield, Bedingfield, Bernstein, Bingham, Bowen, Bowers, Branham, Brannon, G. A. Brown, R. L. Brown, Chumley, Clemmons, Clyburn, Cobb-Hunter, Cole, H. A. Crawford, K. R. Crawford, Crosby, Daning, Delleney, Dillard, Douglas, Edge, Erickson, Felder, Finlay, Forrester, Funderburk, Gagnon, Gambrell, George, Gilliard, Goldfinch, Govan, Hamilton, Hardee, Hardwick, Harrell, Hart, Hayes, Henderson, Herbkersman, Hiott, Hixon, Hodges, Horne, Hosey, Howard, Huggins, Jefferson, Kennedy, King, Knight, Limehouse, Loftis, Long, Lowe, Lucas, Mack, McCoy, McEachern, M. S. McLeod, W. J. McLeod, Merrill, Mitchell, D. C. Moss, V. S. Moss, Munnerlyn, Murphy, Nanney, Neal, Newton, Norman, Ott, Owens, Parks, Patrick, Pitts, Pope, Powers Norrell, Putnam, Quinn, Ridgeway, Riley, Rivers, Robinson-Simpson, Ryhal, Sabb, Sandifer, Sellers, Simrill, Skelton, G. M. Smith, G. R. Smith, J. E. Smith, J. R. Smith, Sottile, Southard, Spires, Stavrinakis, Stringer, Tallon, Taylor, Thayer, Toole, Vick, Weeks, Wells, Whipper, White, Whitmire, Williams, Willis and Wood: A CONCURRENT RESOLUTION TO CONGRATULATE AUTHOR LOVELL KOBIE WILKERSON III OF RICHLAND COUNTY ON THE PUBLICATION OF HIS NEW CHILDREN'S BOOK, QUEEN INFINITY, AND TO HONOR MR. WILKERSON AS RECIPIENT OF THE MOONBEAM CHILDREN'S BOOK AWARD BRONZE MEDAL FOR READING SKILLS AND LITERACY FOR QUEEN INFINITY.
The Concurrent Resolution was adopted, ordered returned to the House.
REPORTS OF STANDING COMMITTEES
Senator COURSON from the Committee on Education submitted a favorable report on:
S. 10 (Word version) -- Senators L. Martin and Fair: A JOINT RESOLUTION TO AUTHORIZE SCHOOL TRUSTEES OF A SCHOOL DISTRICT, IN FISCAL YEAR 2012-2013, TO SELL OR LEASE SCHOOL PROPERTY, REAL OR PERSONAL, IN THE SCHOOL DISTRICT AT ANY TIME THEY DEEM IT EXPEDIENT TO DO SO AND APPLY THE PROCEEDS OF THE SALE OR LEASE TO THE SCHOOL FUND OF THE DISTRICT.
Ordered for consideration tomorrow.
Senator FAIR from the Committee on Corrections and Penology polled out S. 146 favorable with amendment:
S. 146 (Word version) -- Senator Fair: A BILL TO AMEND CHAPTER 1, TITLE 24, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO THE DEPARTMENT OF CORRECTIONS, SO AS TO DEVOLVE ITS DUTIES, FUNCTIONS, AND RESPONSIBILITIES UPON THE DEPARTMENT OF COMMUNITY AND INSTITUTIONAL CORRECTIONS; BY ADDING CHAPTER 2 TO TITLE 24 SO AS TO ESTABLISH THE SOUTH CAROLINA DEPARTMENT OF COMMUNITY AND INSTITUTIONAL CORRECTIONS; TO AMEND SECTION 24-19-10, AS AMENDED, 24-19-20, 24-19-30, 24-19-40, 24-19-50, 24-19-60, 24-19-110, AS AMENDED, AND 24-19-160, RELATING TO THE CORRECTION AND TREATMENT OF YOUTHFUL OFFENDERS, SO AS TO SUBSTITUTE THE TERM "DEPARTMENT OF CORRECTIONS" FOR THE TERM "DEPARTMENT OF COMMUNITY AND INSTITUTIONAL CORRECTIONS", TO SUBSTITUTE THE TERM "YOUTHFUL OFFENDER DIVISION" FOR THE TERM "YOUTHFUL OFFENDER PAROLE AND REENTRY SERVICES DIVISION, TO DELETE THE TERM "TREATMENT" AND ITS DEFINITION, TO PROVIDE A DEFINITION FOR THE TERM "CRIMINOGENIC RISKS AND NEEDS", TO PROVIDE THAT THE DIVISION OF YOUTHFUL OFFENDER PAROLE AND REENTRY SERVICES SHALL CONSIDER ITS CLIENTS CRIMINOGENIC RISKS AND TO REVISE THE PROVISIONS RELATING TO THE HOUSING AND TREATMENT OF YOUTHFUL OFFENDERS, TO SUBSTITUTE THE TERM "DEPARTMENT OF PROBATION, PAROLE AND PARDON SERVICES" FOR THE TERM "DEPARTMENT OF COMMUNITY AND INSTITUTIONAL CORRECTIONS", TO MAKE TECHNICAL CHANGES, AND TO SUBSTITUTE THE TERM "PROBATION, PAROLE, AND PARDON SERVICES BOARD" FOR THE TERM "PAROLE AND PARDON SERVICES BOARD"; AND TO AMEND CHAPTER 21, TITLE 24, RELATING TO THE DEPARTMENT OF PROBATION, PAROLE AND PARDON SERVICES, SO AS TO DEVOLVE ITS DUTIES, FUNCTIONS, AND RESPONSIBILITIES UPON THE DEPARTMENT OF COMMUNITY AND INSTITUTIONAL CORRECTIONS, TO REVISE THE DEFINITION OF THE TERM "HEARING OFFICER", TO SUBSTITUTE THE TERM "BOARD OF PROBATION, PAROLE AND PARDON SERVICES" FOR THE TERM "BOARD OF PAROLE AND PARDON SERVICES", TO REVISE THE BOARD'S DUTIES, AND TO PROVIDE THAT CERTAIN YOUTHFUL OFFENDERS SHALL NOT BE REQUIRED TO PAY SUPERVISION FEES.
Poll of the Corrections and Penology Committee
Polled 11; Ayes 11; Nays 0; Not Voting 6
AYES
Fair Campbell Massey
Martin, Shane Davis Johnson
McElveen Shealy Thurmond
Turner Young
Total--11
NAYS
Total--0
NOT VOTING
Pinckney Williams Nicholson
Gregory Matthews Allen
Total--6
Ordered for consideration tomorrow.
Senator LEATHERMAN from the Committee on Finance submitted a favorable with amendment report on:
S. 163 (Word version) -- Senators Campbell, McGill, O'Dell and Cleary: A BILL TO AMEND SECTION 12-62-50 OF THE 1976 CODE, RELATING TO THE TAX REBATE TO A MOTION PICTURE PRODUCTION COMPANY BY THE SOUTH CAROLINA FILM COMMISSION, TO PROVIDE THAT THE REBATE MAY NOT EXCEED TWENTY PERCENT OF THE TOTAL AGGREGATE PAYROLL FOR PERSONS SUBJECT TO INCOME TAX WITHHOLDINGS OF SOUTH CAROLINA AND MAY NOT EXCEED TWENTY-FIVE PERCENT FOR RESIDENTS OF SOUTH CAROLINA AND FOR PERSONS EMPLOYED WITH THE PRODUCTION WHEN TOTAL PRODUCTION COSTS IN THIS STATE EQUAL OR EXCEED ONE MILLION DOLLARS DURING THE TAXABLE YEAR; AND TO AMEND SECTION 12-62-60, RELATING TO REBATES TO MOTION PICTURE PRODUCTION COMPANIES, TO PROVIDE THAT THE DEPARTMENT MAY REBATE UP TO THIRTY PERCENT OF THE EXPENDITURES IN SOUTH CAROLINA IF THERE IS A MINIMUM IN-STATE EXPENDITURE OF ONE MILLION DOLLARS.
Ordered for consideration tomorrow.
Senator LEATHERMAN from the Committee on Finance submitted a favorable with amendment report on:
S. 234 (Word version) -- Senator Coleman: A BILL TO AMEND THE CODE OF LAWS OF SOUTH CAROLINA, 1976, BY ADDING CHAPTER 67 TO TITLE 12 SO AS TO ENACT THE "SOUTH CAROLINA ABANDONED BUILDINGS REVITALIZATION ACT" WHICH PROVIDES THAT A TAXPAYER MAKING INVESTMENTS OF A CERTAIN SIZE IN REHABILITATING AN ABANDONED BUILDING MAY AT HIS OPTION RECEIVE SPECIFIED INCOME TAX CREDITS OR CREDITS AGAINST THE PROPERTY TAX LIABILITY.
Ordered for consideration tomorrow.
Senator LEATHERMAN from the Committee on Finance submitted a favorable with amendment report on:
S. 237 (Word version) -- Senators Shealy, Setzler, Courson, Turner, Cromer and Massey: A BILL TO AMEND SECTION 10-1-161 OF THE 1976 CODE, RELATING TO STATE CAPITOL BUILDING FLAGS FLOWN AT HALF-STAFF, TO PROVIDE THAT FLAGS ATOP THE STATE CAPITOL BUILDING MUST BE LOWERED TO HALF-STAFF FOR MEMBERS OF THE UNITED STATES MILITARY SERVICES, WHO WERE RESIDENTS OF THIS STATE AND WHO LOST THEIR LIVES IN THE LINE OF DUTY, ON THE DAY WHEN THEIR NAMES ARE RELEASED TO THE GENERAL PUBLIC, AND THE FLAGS SHALL REMAIN AT HALF-STAFF UNTIL AT LEAST DAWN THE SECOND DAY AFTER FUNERAL SERVICES ARE CONDUCTED.
Ordered for consideration tomorrow.
Senator LEATHERMAN from the Committee on Finance submitted a favorable with amendment report on:
S. 294 (Word version) -- Senator Cleary: A BILL TO AMEND SECTION 6-4-10, AS AMENDED, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO THE EXPENDITURE OF LOCAL ACCOMMODATION TAX REVENUES, SO AS TO CLARIFY THAT IN CERTAIN SITUATIONS, FUNDS MAY BE USED FOR BEACH RENOURISHMENT, AND TO ALLOW A MUNICIPALITY OR COUNTY, IN CERTAIN SITUATIONS, UPON A TWO-THIRDS VOTE OF THE MEMBERSHIP OF THE LOCAL GOVERNING BODY, TO HOLD THE FUNDS FOR MORE THAN TWO YEARS IF THE FUNDS ARE DESIGNATED FOR THE CONTROL AND REPAIR OF WATERFRONT EROSION, INCLUDING BEACH RENOURISHMENT.
Ordered for consideration tomorrow.
Senator LEATHERMAN from the Committee on Finance submitted a favorable with amendment report on:
S. 303 (Word version) -- Senator Campsen: A BILL TO AMEND SECTION 12-37-220, AS AMENDED, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO PROPERTY TAX EXEMPTIONS, SO AS TO INCLUDE CERTAIN TRUSTS IN EXEMPTING PROPERTY USED FOR THE HOLDING OF ITS MEETINGS WHEN NO PROFIT OR BENEFIT INURES TO THE BENEFIT OF ANY STOCKHOLDER OR INDIVIDUAL; AND TO AMEND SECTION 12-24-40, AS AMENDED, RELATING TO EXEMPTIONS FROM DEED RECORDING FEES, SO AS TO EXEMPT TRANSFERS FROM A TRUST ESTABLISHED FOR THE BENEFIT OF A RELIGIOUS ORGANIZATION TO THE RELIGIOUS ORGANIZATION.
Ordered for consideration tomorrow.
Senator LEATHERMAN from the Committee on Finance submitted a favorable with amendment report on:
S. 351 (Word version) -- Senator O'Dell: A JOINT RESOLUTION TO AUTHORIZE THE STATE BUDGET AND CONTROL BOARD TO TRANSFER OWNERSHIP OF THE BELTON NATIONAL GUARD ARMORY TO THE CITY OF BELTON.
Ordered for consideration tomorrow.
Senator COURSON from the Committee on Education submitted a favorable report on:
S. 391 (Word version) -- Senators Matthews, Courson, Hayes, Jackson, Setzler, Williams, Nicholson and Scott: A SENATE RESOLUTION TO STRONGLY ENCOURAGE THE BOARD OF TRUSTEES OF SOUTH CAROLINA STATE UNIVERSITY TO DELAY ITS SEARCH AND SELECTION OF A PRESIDENT OF THE UNIVERSITY UNTIL AFTER THE MEMBERS TO SEATS REPRESENTING THE FIFTH, SIXTH, AND SEVENTH CONGRESSIONAL DISTRICTS AND AT-LARGE SEATS NINE, ELEVEN, AND TWELVE ARE ELECTED DURING THE 2013 SOUTH CAROLINA LEGISLATIVE SESSION.
Ordered for consideration tomorrow.
Senator COURSON from the Committee on Education submitted a favorable with amendment report on:
H. 3453 (Word version) -- Reps. Bingham, Allison, Anthony, Hayes and Atwater: A JOINT RESOLUTION TO REQUIRE LOCAL SCHOOL DISTRICTS TO DECIDE AND NOTIFY TEACHERS OF THEIR EMPLOYMENT FOR THE 2013-2014 SCHOOL YEAR BY MAY 15, 2013; TO PROVIDE THAT A CONTINUING-CONTRACT TEACHER WHO IS BEING RECOMMENDED FOR FORMAL EVALUATION THE FOLLOWING SCHOOL YEAR MUST BE NOTIFIED IN WRITING ON OR BEFORE THE DATE THE SCHOOL DISTRICT ISSUES THE WRITTEN OFFER OF EMPLOYMENT OR REEMPLOYMENT; TO REQUIRE TEACHERS WHO ARE REEMPLOYED BY WRITTEN NOTIFICATION TO NOTIFY THE DISTRICT BOARD OF THEIR ACCEPTANCE WITHIN TEN DAYS OF RECEIPT OF WRITTEN NOTIFICATION OF EMPLOYMENT; AND TO ALLOW DISTRICTS TO UNIFORMLY NEGOTIATE SALARIES OF CERTAIN RETIRED TEACHERS BELOW THE DISTRICT SALARY SCHEDULE.
Ordered for consideration tomorrow.
Invitations Accepted
On motion of Senator BRYANT, with unanimous consent, the following invitations were polled favorably from the Committee on Invitations and ordered placed on the Calendar:
Poll of the Invitations Committee
Polled 11; Ayes 11; Nays 0; Not Voting 0
AYES
Bryant Alexander McGill
Reese Ford Verdin
Campsen Cromer Malloy
Cleary Johnson
Total--11
NAYS
Total--0
Tuesday, March 5, 2013, 6:00 P.M. - 8:00 P.M.
Members of the Senate and Staff, Reception, The Clarion, by the ALEC
Wednesday, March 6, 2013, 8:00 A.M.- 10:00 A.M.
Members of the Senate and Staff, Breakfast, Room 112, Blatt Building, by the PIEDMONT MUNICIPAL POWER SYSTEM
Wednesday, March 6, 2013, 12:00 P.M. - 2:00 P.M.
Members of the Senate and Staff, Luncheon, State House Grounds, by the SC FIREFIGHTERS ASSOCIATION
Wednesday, March 6, 2013, 6:00 P.M. - 8:00 P.M.
Members of the Senate and Staff, Reception, Municipal Association of SC, by the AMERICAN ADVERTISING FEDERATION
Wednesday, March 6, 2013, 6:00 P.M. - 8:00 P.M.
Members of the Senate and Staff, Reception, The Palmetto Club, by the COLLEGE OF CHARLESTON
Thursday, March 7, 2013, 8:00 A.M. - 10:00 A.M.
Member of the Senate, Breakfast, Room 112, Blatt Building, by the CAMO COALITION AND SC WILDLIFE
Tuesday, March 12, 2013, 6:00 - 8:00 P.M.
Members of the Senate, Reception, The Marriott, by the GOVERNOR'S SCHOOL FOR MATH & SCIENCE TOWNES AWARD
Tuesday, March 19, 2013, 6:00 P.M. - 8:00 P.M.
Members of the Senate and Staff, Reception, Columbia Museum of Art, by the FLORENCE COUNTY NIGHT
Wednesday, March 20, 2013, 8:00 A.M. - 10:00 A.M.
Members of the Senate, Breakfast, Room 112, Blatt Building, by the SC CLEAN ENERGY BUSINESS ALLIANCE
Wednesday, March 20, 2013, 12:00 P.M. - 2:00 P.M. Members of the Senate, Luncheon, Room 112, Blatt Building, by the NATIONAL FEDERATION OF THE BLIND
Wednesday, March 20, 2013, 6:00 P.M. - 8:00 P.M.
Members of the Senate, Reception, Seawells, by the SC SUMMARY COURT JUDGES ASSOCIATION
Wednesday, March 20, 2013, 7:00 P.M. - 9:00 P.M.
Members of the Senate, Reception, Blue Marlin Vista Room, by the ALCOA MT. HOLLY
Thursday, March 21, 2013, 8:00 A.M. - 10:00 A.M.
Members of the Senate and Staff, Breakfast, Room 112, Blatt Building, by the SC VOCATIONAL REHABILITATION ASSOCIATION
Appointments Reported
Senator LARRY MARTIN from the Committee on Judiciary submitted a favorable report on:
Initial Appointment, South Carolina State Ethics Commission, with the term to commence June 30, 2008, and to expire June 30, 2013
5th Congressional District:
Twana N. Burris-Alcide, 591 Lakeside Drive, Rock Hill, SC 29730 VICE Vacant
Initial Appointment, South Carolina Board of Juvenile Parole, with the term to commence July 1, 2012, and to expire June 30, 2016
At-Large:
Barbara W. Mishoe, 154 South Main Street, Greeleyville, SC 29056 VICE New Seat
Initial Appointment, South Carolina Board of Juvenile Parole, with the term to commence July 1, 2012, and to expire June 30, 2016
Robert J. Reid, 19 Dingle Street, Charleston, SC 29403 VICE New Seat
Initial Appointment, South Carolina Board of Juvenile Parole, with the term to commence July 1, 2011, and to expire June 30, 2015
At-Large:
Carla J. Smalls, 261 Caedmons Creek Drive, Irmo, SC 29063 VICE New Seat
Initial Appointment, South Carolina Board of Juvenile Parole, with the term to commence July 1, 2010, and to expire June 30, 2014
At-Large:
Frank D. Wideman, 126 Stratford Road, Greenwood, SC 29649 VICE New Seat
Senator COURSON from the Committee on Education submitted a favorable report on:
Reappointment, South Carolina Public Charter School District Board of Trustees, with the term to commence May 3, 2011, and to expire May 3, 2014
Governor Appointed:
Donald L. McLaurin, 13 Water Street, Charleston, SC 29401
HOUSE CONCURRENCES
The following Resolutions were returned from the House with concurrence and received as information:
S. 251 (Word version) -- Senators Scott, Massey, Alexander, Allen, Bennett, Bright, Bryant, Campbell, Campsen, Cleary, Coleman, Corbin, Courson, Cromer, Davis, Fair, Ford, Gregory, Grooms, Hayes, Hembree, Hutto, Jackson, Johnson, Leatherman, Lourie, Malloy, L. Martin, S. Martin, Matthews, McElveen, McGill, Nicholson, O'Dell, Peeler, Pinckney, Rankin, Reese, Setzler, Shealy, Sheheen, Thurmond, Turner, Verdin, Williams and Young: A CONCURRENT RESOLUTION TO REQUEST THAT THE DEPARTMENT OF TRANSPORTATION NAME THE PORTION OF PLEASANT LANE ROAD IN EDGEFIELD COUNTY FROM ITS INTERSECTION WITH UNITED STATES HIGHWAY 25 TO ITS INTERSECTION WITH UNITED STATES HIGHWAY 378 "MAMIE J. REARDEN HIGHWAY" AND ERECT APPROPRIATE MARKERS OR SIGNS ALONG THIS PORTION OF HIGHWAY THAT CONTAIN THE WORDS "MAMIE J. REARDEN HIGHWAY".
S. 324 (Word version) -- Senator L. Martin: A CONCURRENT RESOLUTION TO REQUEST THAT THE DEPARTMENT OF TRANSPORTATION NAME THE BRIDGE OVER HIGHWAY 123 AT THE INTERSECTION OF HIGHWAY 123 AND ROAD 37-18 AS THE SAMUEL MAVERICK BRIDGE AND ERECT APPROPRIATE MARKERS OR SIGNS AT THE BRIDGE THAT CONTAIN THE WORDS "SAMUEL MAVERICK BRIDGE".
THE SENATE PROCEEDED TO A CALL OF THE UNCONTESTED LOCAL AND STATEWIDE CALENDAR.
The following Joint Resolution was read the third time and ordered sent to the House of Representatives:
S. 418 (Word version) -- Transportation Committee: A JOINT RESOLUTION TO APPROVE REGULATIONS OF THE DEPARTMENT OF TRANSPORTATION, RELATING TO SPECIFIC INFORMATION SERVICE SIGNING, DESIGNATED AS REGULATION DOCUMENT NUMBER 4312, PURSUANT TO THE PROVISIONS OF ARTICLE 1, CHAPTER 23, TITLE 1 OF THE 1976 CODE.
S. 127 (Word version) -- Senators Alexander and Ford: A BILL TO AMEND ARTICLE 6, CHAPTER 38, TITLE 44 OF THE 1976 CODE, RELATING TO HEAD AND SPINAL CORD INJURIES, BY ADDING ARTICLE 6 TO CREATE THE SOUTH CAROLINA BRAIN INJURY LEADERSHIP COUNCIL, TO PROVIDE FOR THE RESPONSIBILITIES AND DUTIES OF THE COUNCIL, TO PROVIDE FOR THE COMPOSITION AND APPOINTMENT OF THE COUNCIL, AND TO PROVIDE FOR THE POWERS AND AUTHORITY OF THE COUNCIL.
The Senate proceeded to a consideration of the Bill, the question being the adoption of the amendment proposed by the Committee on Medical Affairs.
The Committee on Medical Affairs proposed the following amendment (S-127), which was adopted:
Amend the bill, as and if amended, page 2, by striking lines 12-18 and inserting:
/ public policy concerning brain injuries to state policymakers; and
(7) serve as the statewide advisory board for implementing the federal Traumatic Brain Injury Act and applying for federal traumatic brain injury funding.
Section 44-38-630. (A) The members of the South Carolina Brain Injury Leadership Council should have knowledge or expertise in the area of brain injury or related services. The Council shall be comprised of representatives of the following agencies and organizations, shall be appointed by the director of the agency or organization and shall serve ex officio: /
Amend the bill further, page 3, by striking line 16 and inserting:
/ SECTION 2. Section 44-20-225 is repealed.
SECTION 3. This act takes effect upon approval by the Governor. /
Renumber sections to conform.
Amend title to conform.
Senator ALEXANDER explained the committee amendment.
The question then was second reading of the Bill.
The "ayes" and "nays" were demanded and taken, resulting as follows:
Ayes 41; Nays 0
AYES
Alexander Allen Bennett
Bright Bryant Campbell
Campsen Cleary Coleman
Corbin Courson Cromer
Davis Fair Grooms
Hayes Hutto Jackson
Johnson Leatherman Lourie
Malloy Martin, Larry Martin, Shane
Massey Matthews McElveen
McGill Nicholson O'Dell
Peeler Pinckney Rankin
Reese Scott Shealy
Sheheen Thurmond Turner
Williams Young
Total--41
NAYS
Total--0
Statement by Senator SETZLER
I was out of the Chamber at the time the vote was taken on this Bill. I was attending an economic development event in my district, but, had I been here, I would have voted in favor of the second reading of the Bill.
There being no further amendments, the Bill was read the second time, passed and ordered to a third reading.
S. 428 (Word version) -- Medical Affairs Committee: A JOINT RESOLUTION TO APPROVE REGULATIONS OF THE DEPARTMENT OF HEALTH AND ENVIRONMENTAL CONTROL, RELATING TO SOUTH CAROLINA IMMUNIZATION REGISTRY, DESIGNATED AS REGULATION DOCUMENT NUMBER 4259, PURSUANT TO THE PROVISIONS OF ARTICLE 1, CHAPTER 23, TITLE 1 OF THE 1976 CODE.
The Senate proceeded to a consideration of the Resolution, the question being the second reading of the Joint Resolution.
The "ayes" and "nays" were demanded and taken, resulting as follows:
Ayes 38; Nays 5
AYES
Alexander Allen Bennett
Campbell Campsen Cleary
Coleman Corbin Courson
Cromer Davis Fair
Ford Grooms Hayes
Hembree Hutto Jackson
Johnson Leatherman Lourie
Malloy Martin, Larry Matthews
McElveen McGill Nicholson
O'Dell Peeler Pinckney
Rankin Reese Scott
Shealy Sheheen Thurmond
Turner Williams
Total--38
NAYS
Bright Bryant Martin, Shane
Massey Young
Total--5
Statement by Senator SETZLER
I was out of the Chamber at the time the vote was taken on this Resolution. I was attending an economic development event in my district, but, had I been here, I would have voted in favor of the second reading of the Resolution.
The Joint Resolution was read the second time and ordered placed on the Third Reading Calendar.
S. 429 (Word version) -- Medical Affairs Committee: A JOINT RESOLUTION TO APPROVE REGULATIONS OF THE DEPARTMENT OF LABOR, LICENSING AND REGULATION - PANEL FOR DIETETICS, RELATING TO DEFINITIONS, DESIGNATED AS REGULATION DOCUMENT NUMBER 4237, PURSUANT TO THE PROVISIONS OF ARTICLE 1, CHAPTER 23, TITLE 1 OF THE 1976 CODE.
The Senate proceeded to a consideration of the Resolution, the question being the second reading of the Joint Resolution.
The "ayes" and "nays" were demanded and taken, resulting as follows:
Ayes 42; Nays 1
AYES
Alexander Allen Bennett
Bright Campbell Campsen
Cleary Coleman Corbin
Courson Cromer Davis
Fair Ford Grooms
Hayes Hembree Hutto
Jackson Johnson Leatherman
Lourie Malloy Martin, Larry
Martin, Shane Massey Matthews
McElveen McGill Nicholson
O'Dell Peeler Pinckney
Rankin Reese Scott
Shealy Sheheen Thurmond
Turner Williams Young
Total--42
NAYS
Bryant
Total--1
Statement by Senator SETZLER
I was out of the Chamber at the time the vote was taken on this Resolution. I was attending an economic development event in my district, but, had I been here, I would have voted in favor of the second reading of the Resolution.
The Joint Resolution was read the second time and ordered placed on the Third Reading Calendar.
SENT TO THE HOUSE
S. 64 (Word version) -- Senator Scott: A CONCURRENT RESOLUTION TO CONGRATULATE HARRISON REARDEN FOR HIS MANY YEARS OF PUBLIC SERVICE AND REQUEST THAT THE DEPARTMENT OF TRANSPORTATION NAME THE INTERCHANGE LOCATED AT THE INTERSECTION OF SOUTH CAROLINA HIGHWAY 277 AND FONTAINE ROAD IN RICHLAND COUNTY "HARRISON REARDEN INTERCHANGE" AND ERECT APPROPRIATE MARKERS OR SIGNS AT THIS INTERCHANGE THAT CONTAIN THE WORDS "HARRISON REARDEN INTERCHANGE".
The Senate proceeded to a consideration of the Concurrent Resolution, the question being the adoption of the amendment proposed by the Committee on Transportation.
The Committee on Transportation proposed the following amendment (64R001.LKG), which was adopted:
Amend the concurrent resolution, as and if amended, page 2, after line 8, by adding:
/ Whereas, among numerous other citations, Mr. Rearden was awarded the state's highest honor, the Order of the Palmetto, by Governor Carroll Campbell, and he was awarded the Order of the Silver Crescent by Governor Jim Hodges; and /
Renumber sections to conform.
Amend title to conform.
There being no further amendments, the Concurrent Resolution was adopted, as amended and ordered sent to the House with amendments.
CARRIED OVER
S. 6 (Word version) -- Senator Peeler: A BILL TO AMEND SECTION 40-11-260, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO FINANCIAL STATEMENTS AND NET WORTH REQUIREMENTS FOR GENERAL CONTRACTORS AND MECHANICAL CONTRACTORS, SO AS TO ADJUST THE NET WORTH REQUIREMENTS FOR LICENSURE AND LICENSE RENEWAL, AND TO DELETE OBSOLETE LANGUAGE.
On motion of Senator O'DELL, the Bill was carried over.
Expression of Personal Interest
Senator SCOTT rose for an Expression of Personal Interest.
THE CALL OF THE UNCONTESTED CALENDAR HAVING BEEN COMPLETED, THE SENATE PROCEEDED TO THE MOTION PERIOD.
On motion of Senator PEELER, the Senate agreed to dispense with the Motion Period.
RATIFICATION OF ACTS
Pursuant to an invitation the Honorable Speaker and House of Representatives appeared in the Senate Chamber on February 27, 2013, at 3:45 P.M. and the following Acts and Joint Resolution were ratified:
(R2, S. 91 (Word version)) -- Senator Gregory: AN ACT TO AMEND SECTION 50-11-310, AS AMENDED, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO THE HUNTING AND TAKING OF ANTLERED DEER, SO AS TO DELETE A PROHIBITION ON BAITING DEER IN GAME ZONES 1 AND 2.
L:\COUNCIL\ACTS\91HTC13.DOCX
(R3, S. 165 (Word version)) -- Senators Campsen and Grooms: AN ACT TO AMEND SECTION 50-15-65, AS AMENDED, CODE OF LAWS OF SOUTH CAROLINA, 1976, RELATING TO MANAGEMENT AND CONTROL OF ALLIGATORS ON PRIVATE LANDS, SO AS TO EXTEND THE HUNTING SEASON OF ALLIGATORS ON PRIVATE LANDS TO MAY THIRTY-FIRST.
L:\COUNCIL\ACTS\165AB13.DOCX
(R4, S. 244 (Word version)) -- Senators McGill, Cleary and Campsen: AN ACT TO AMEND THE CODE OF LAWS OF SOUTH CAROLINA, 1976, BY REPEALING SECTION 50-11-940 RELATING TO THE DESIGNATION OF CERTAIN PROPERTY OF THE BELLE W. BARUCH FOUNDATION IN GEORGETOWN COUNTY AS A BIRD AND GAME REFUGE; AND BY REPEALING SECTION 50-11-941 PROVIDING THAT PROVISIONS OF SECTION 50-11-940 MUST NOT BE CONSTRUED TO BE IN CONFLICT WITH THE LAST WILL AND TESTAMENT OF BELLE W. BARUCH.
L:\COUNCIL\ACTS\244AC13.DOCX
(R5, S. 379 (Word version)) -- Senator Sheheen: AN ACT TO AMEND ACT 930 OF 1970, AS AMENDED, RELATING TO THE SCHOOL DISTRICT BOARD OF TRUSTEES FOR KERSHAW COUNTY, SO AS TO REVISE THE SPECIFIC ELECTION DISTRICTS FROM WHICH THE MEMBERS OF THE KERSHAW COUNTY SCHOOL DISTRICT BOARD OF TRUSTEES SHALL BE ELECTED BEGINNING WITH SCHOOL TRUSTEE ELECTIONS IN 2014, AND TO PROVIDE FOR DEMOGRAPHIC INFORMATION IN REGARD TO THESE NEWLY DRAWN ELECTION DISTRICTS.
L:\COUNCIL\ACTS\379ZW13.DOCX
(R6, H. 3180 (Word version)) -- Reps. Pope and V.S. Moss: A JOINT RESOLUTION TO AUTHORIZE THE STATE BUDGET AND CONTROL BOARD TO TRANSFER OWNERSHIP OF CLOVER NATIONAL GUARD ARMORY IN CLOVER, SOUTH CAROLINA, TO THE TOWN OF CLOVER.
L:\COUNCIL\ACTS\3180DG13.DOCX
Expression of Personal Interest
Senator CROMER rose for an Expression of Personal Interest.
Remarks by Senator CROMER
Thank you, Mr. PRESIDENT. I would like the other Senators representing Lexington to join me here at the podium. I will begin my introduction while my colleagues make their way here.
I met the Longstreet's a little over a year ago while out campaigning
-- knocking on doors and burning up the shoe leather, Senator from Edgefield. I had no idea where this couple lived, but I had spoken and corresponded with them prior to this meeting. I got to spend about an hour, hour and a half with this wonderful family in their home.
I would like to have them stand right now -- David and Karen Longstreet. It was January of 2012, and, I believe, it was on New Year's Day. They were on their way to a church service. They went through an intersection and at that moment another driver, who had been out partying all night the night before, t-boned their van and killed their precious little six-year-old girl, Emma. Chief Green, who is also here, told me earlier that one of his deputies actually witnessed the accident.
We have a Bill coming up -- the Ignition Interlock Bill -- and I know that's why you're here today. Senators LARRY MARTIN, SHEALY, SETZLER, MASSEY, LOURIE, FAIR and myself are sponsoring an amendment to name this bill "Emma's Law." We are doing that for you.
This family has suffered a tremendous loss. They still have three fine young boys that are doing great. David and Karen, our thoughts and prayers are with you and your family. We appreciate you being here today to try and help us shepherd this Bill forward.
The Senator from Richland, Senator LOURIE, is principal sponsor of this very important legislation. I sponsored the amendment to the original legislation last year and sadly, it didn't quite make it through. Hopefully we will get through it this year and we'll see some purpose for what happened to young Emma.
Let me add that the gentleman who hit them that morning already had a prior DUI offense. That is one of the reasons we are asking that enrollment in an Ignition Interlock Program be required on a first offense so that tragedies like this might be avoided in the future.
I would just like to say to the Longstreets, God bless you.
Thank you.
On motion of Senator SHANE MARTIN, with unanimous consent, the remarks of Senator CROMER were ordered printed in the Journal.
THE SENATE PROCEEDED TO THE INTERRUPTED DEBATE.
RETURNED TO THE STATUS OF SPECIAL ORDER
S. 137 (Word version) -- Senators Lourie, L. Martin, Hayes, Fair, Davis, Ford, Cromer and Grooms: A BILL TO AMEND SEVERAL SECTIONS OF TITLE 56, RELATING TO IGNITION INTERLOCK DEVICES, TO PROVIDE FOR THE ISSUANCE OF AN IGNITION INTERLOCK LICENSE AND ITS CONTENTS AND THE RESTRICTIONS RELATED TO THE LICENSE, TO PROVIDE FOR PENALTIES RELATED TO IGNITION INTERLOCK DEVICES, TO REVISE THE PENALTY IMPOSED UPON A PERSON WHO REFUSES TO BE SUBJECTED TO A CHEMICAL TEST, TO PROVIDE FOR ENROLLMENT IN THE IGNITION INTERLOCK DEVICE PROGRAM UNDER CERTAIN CIRCUMSTANCES, AND TO MAKE TECHNICAL CHANGES.
(Abbreviated Title)
The Senate proceeded to a consideration of the Bill, the question being the adoption of the amendment proposed by the Committee on Judiciary.
The Committee on Judiciary proposed the following amendment (JUD0137.001), which was adopted:
Amend the bill, as and if amended, by striking all after the enacting words and inserting:
/ SECTION 1. Section 56-1-286 of the 1976 Code is amended to read:
"Section 56-1-286. (A) The Department of Motor Vehicles must shall suspend the driver's license, permit, or nonresident operating privilege of, or deny the issuance of a license or permit to a person under the age of twenty-one who drives a motor vehicle and has an alcohol concentration of two one-hundredths of one percent or more. In cases in which a law enforcement officer initiates suspension proceedings for a violation of this section, the officer has elected to pursue a violation of this section and is subsequently prohibited from prosecuting the person for a violation of Section 63-19-2440, 63-19-2450, 56-5-2930, or 56-5-2933, arising from the same incident.
(B) A person under the age of twenty-one who drives a motor vehicle in this State is considered to have given consent to chemical tests of his the person's breath or blood for the purpose of determining the presence of alcohol.
(C) A law enforcement officer who has arrested a person under the age of twenty-one for a violation of Chapter 5 of this title (Uniform Act Regulating Traffic on Highways), or any other traffic offense established by a political subdivision of this State, and has reasonable suspicion that the person under the age of twenty-one has consumed alcoholic beverages and driven a motor vehicle may order the testing of the person arrested to determine the person's alcohol concentration.
A law enforcement officer may detain and order the testing of a person to determine the person's alcohol concentration if the officer has reasonable suspicion that a motor vehicle is being driven by a person under the age of twenty-one who has consumed alcoholic beverages.
The person tested or giving samples for testing may have a qualified person of his the person's choice conduct additional tests at the person's expense and must be notified in writing of that right. A person's request or failure to request additional blood tests is not admissible against the person in any proceeding. The person's failure or inability of the person tested to obtain additional tests does not preclude the admission of evidence relating to the tests or samples taken at the officer's direction of the officer. The officer must shall provide affirmative assistance to the person to contact a qualified person to conduct and obtain additional tests. Affirmative assistance shall, at a minimum, include providing transportation for the person to the nearest medical facility which provides blood tests to determine a person's alcohol concentration. If the medical facility obtains the blood sample but refuses or fails to test the blood to determine the person's alcohol concentration, SLED must the State Law Enforcement Division shall test the blood and provide the result to the person and to the officer. Failure to provide affirmative assistance upon request to obtain additional tests bars the admissibility of the breath test result in any a judicial or administrative proceeding.
(E) A qualified person and his the person's employer who obtain samples or administer the tests or assist in obtaining samples or administering of tests at the direction of the primary investigating officer officer's direction are immune from civil and criminal liability unless the obtaining of samples or the administering of tests is performed in a negligent, reckless, or fraudulent manner. A person may not be required by the officer ordering the tests to obtain or take any sample of blood or urine.
(F) If Except as provided in subsection (H), if a person refuses upon the request of the primary investigating officer officer's request to submit to chemical tests as provided in subsection (C), the department must shall suspend his the person's license, permit, or any nonresident operating privilege, or deny the issuance of a license or permit to him the person for:
(1) six months; or
(2) one year, if the person, within the five years preceding the violation of this section, has been previously convicted of violating Section 56-5-2930, 56-5-2933, or 56-5-2945, or any other a law of this State or another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or another drug other drugs, or the person has had a previous suspension imposed pursuant to Section 56-1-286, 56-5-2950, or 56-5-2951, or 56-5-2990.
(G) If Except as provided in subsection (H), if a person submits to a chemical test and the test result indicates an alcohol concentration of two one-hundredths of one percent or more, the department must shall suspend his the person's license, permit, or any nonresident operating privilege, or deny the issuance of a license or permit to him the person for:
(1) three months; or
(2) six months, if the person, within the five years preceding the violation of this section, has been previously convicted of violating Section 56-5-2930, 56-5-2933, or 56-5-2945, or any other a law of this State or another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or another drug other drugs, or the person has had a previous suspension imposed pursuant to Section 56-1-286, 56-5-2950, or 56-5-2951, or 56-5-2990.
(H) In lieu of serving the remainder of a suspension or denial of the issuance of a license or permit, a person may enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension or denial of the issuance of a license or permit, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle equal to the length of time remaining on the person's suspension or denial of the issuance of a license or permit. If the length of time remaining is less than three months, the ignition interlock device is required to be affixed to the motor vehicle for three months. Once a person has enrolled in the Ignition Interlock Device Program and obtained an ignition interlock restricted license, the person is subject to Section 56-5-2941 and cannot subsequently choose to serve the suspension.
(H)(I) A person's driver's license, permit, or nonresident operating privilege must be restored when the person's period of suspension under pursuant to subsection (F) or (G), or ignition interlock restricted license requirement pursuant to subsection (H), has concluded, even if the person has not yet completed the Alcohol and Drug Safety Action Program in which he the person is enrolled. After the person's driving privilege is restored, he must the person shall continue to participate in the Alcohol and Drug Safety Action Program in which he the person is enrolled. If the person withdraws from or in any way stops making satisfactory progress toward the completion of the Alcohol and Drug Safety Action Program, the person's license must be suspended until he the person completes the Alcohol and Drug Safety Action Program. A person must shall be attending or have completed an Alcohol and Drug Safety Action Program pursuant to Section 56-5-2990 before his the person's driving privilege can may be restored at the conclusion of the suspension period or ignition interlock restricted license requirement.
(I)(J) A test may not be administered or samples taken unless, upon activation of the video recording equipment and prior to the commencement of the testing procedure, the person has been given a written copy of and verbally informed that:
(1) he the person does not have to take the test or give the samples but that his the person's privilege to drive must be suspended or denied for at least six months with the option of ending the suspension or denial if the person enrolls in the Ignition Interlock Device Program, if he the person refuses to submit to the tests, and that his the person's refusal may be used against him the person in court;
(2) his the person's privilege to drive must be suspended for at least three months with the option of ending the suspension if the person enrolls in the Ignition Interlock Device Program, if he the person takes the test or gives the samples and has an alcohol concentration of two one-hundredths of one percent or more;
(3) he the person has the right to have a qualified person of his the person's own choosing conduct additional independent tests at his the person's expense;
(4) he the person has the right to request an administrative a contested case hearing within thirty days of the issuance of the notice of suspension; and
(5) he must the person shall enroll in an Alcohol and Drug Safety Action Program within thirty days of the issuance of the notice of suspension if he the person does not request an administrative a contested case hearing or within thirty days of the issuance of notice that the suspension has been upheld at the administrative contested case hearing.
The primary investigating officer must notify promptly shall promptly notify the department of the a person's refusal of a person to submit to a test requested pursuant to this section as well as the test result of any a person who submits to a test pursuant to this section and registers an alcohol concentration of two one-hundredths of one percent or more. The notification must be in a manner prescribed by the department.
(J)(K) If the test registers an alcohol concentration of two one-hundredths of one percent or more or if the person refuses to be tested, the primary investigating officer must shall issue a notice of suspension, and the suspension is effective beginning on the date of the alleged violation of this section. The person, within thirty days of the issuance of the notice of suspension, must shall enroll in an Alcohol and Drug Safety Action Program pursuant to Section 56-5-2990 if he the person does not request an administrative hearing. If the person does not request an administrative hearing and does not enroll in an Alcohol and Drug Safety Action Program within thirty days, the suspension remains in effect, and a temporary alcohol license must not be issued. If the person drives a motor vehicle during the period of suspension without a temporary alcohol license, the person must be penalized for driving while his the person's license is suspended pursuant to Section 56-1-460.
(K)(L) Within thirty days of the issuance of the notice of suspension the person may:
(1) obtain a temporary alcohol license by filing with the Department of Motor Vehicles a form for this purpose. A one-hundred-dollar fee must be assessed for obtaining a temporary alcohol license. Twenty-five dollars of the fee collected by the Department of Motor Vehicles must be distributed to the Department of Public Safety for supplying and maintaining all necessary vehicle videotaping equipment. The remaining seventy-five dollars must be placed by the Comptroller General into a special restricted account to be used by the Department of Motor Vehicles to defray its the Department of Motor Vehicle's expenses. The temporary alcohol license allows the person to drive a motor vehicle without any restrictive conditions pending the outcome of the contested case hearing provided for in this section or the final decision or disposition of the matter; and
(2) request a contested case hearing before the Office of Motor Vehicle Hearings pursuant to its rules of procedure.
At the contested case hearing if:
(a) the suspension is upheld, the person must shall enroll in an Alcohol and Drug Safety Action Program and his the person's driver's license, permit, or nonresident operating privilege must be suspended or the person must be denied the issuance of a license or permit for the remainder of the suspension periods provided for in subsections (F) and (G); or
(b) the suspension is overturned, the person must have his person's driver's license, permit, or nonresident operating privilege must be reinstated.
(L)(M) The periods of suspension provided for in subsections (F) and (G) begin on the day the notice of suspension is issued, or at the expiration of any other suspensions, and continue until the person applies for a temporary alcohol license and requests an administrative hearing.
(M)(N) If a person does not request a contested case hearing, he shall have the person has waived his the person's right to the hearing and his the person's suspension must not be stayed but shall continue for the periods provided for in subsections (F) and (G).
(N)(O) The notice of suspension must advise the person of the requirement to enroll in an Alcohol and Drug Safety Action Program and of his the person's right to obtain a temporary alcohol license and to request a contested case hearing. The notice of suspension also must advise the person that, if he the person does not request a contested case hearing within thirty days of the issuance of the notice of suspension, he must the person shall enroll in an Alcohol and Drug Safety Action Program, and he the person waives his the person's right to the contested case hearing, and the suspension continues for the periods provided for in subsections (F) and (G).
(O)(P) A contested case hearing must be held after the request for the hearing is received by the Office of Motor Vehicle Hearings. The scope of the hearing is limited to whether the person:
(1) was lawfully arrested or detained;
(2) was given a written copy of and verbally informed of the rights enumerated in subsection (I)(J);
(3) refused to submit to a test pursuant to this section; or
(4) consented to taking a test pursuant to this section, and the:
(a) reported alcohol concentration at the time of testing was two one-hundredths of one percent or more;
(b) individual who administered the test or took samples was qualified pursuant to this section;
(c) test administered and samples taken were conducted pursuant to this section; and
(d) the machine was operating properly.
Nothing in this section prohibits the introduction of evidence at the contested case hearing on the issue of the accuracy of the breath test result.
The Department of Motor Vehicles and the arresting officer shall have the burden of proof in contested case hearings conducted pursuant to this section. If neither the Department of Motor Vehicles nor the arresting officer appears at the contested case hearing, the hearing officer shall rescind the suspension of the person's license, permit, or nonresident's operating privilege regardless of whether the person requesting the contested case hearing or the person's attorney appears at the contested case hearing.
A written order must be issued to all parties either reversing or upholding the suspension of the person's license, permit, or nonresident's operating privilege, or denying the issuance of a license or permit. If the suspension is upheld, the person must receive credit for the number of days his the person's license was suspended before he the person received a temporary alcohol license and requested the contested case hearing.
(P)(Q) A contested case hearing is a contested proceeding under the Administrative Procedures Act, and a person has a right to appeal the decision of the hearing officer pursuant to that act to the Administrative Law Court in accordance with its appellate rules. The filing of an appeal shall stay the suspension until a final decision is issued.
(Q)(R) A person who is unconscious or otherwise in a condition rendering him incapable of refusal is considered to be informed and not to have withdrawn the consent provided for in subsection (B) of this section.
(R)(S) When a nonresident's privilege to drive a motor vehicle in this State has been suspended under the procedures of this section, the department shall give written notice of the action taken to the motor vehicle administrator of the state of the person's residence and of any state in which he has a license or permit.
(S)(T) A person required to submit to a test must be provided with a written report including the time of arrest, the time of the tests, and the results of the tests before any proceeding in which the results of the tests are used as evidence. A person who obtains additional tests shall furnish a copy of the time, method, and results of any additional tests to the officer before any trial, hearing, or other proceeding in which the person attempts to use the results of the additional tests as evidence.
(T)(U) A person whose driver's license or permit is suspended under this section is not required to file proof of financial responsibility.
(U)(V) The department shall administer the provisions of this section, not including subsection (D), and shall promulgate regulations necessary to carry out its provisions.
(V)(W) Notwithstanding any other provision of law, no suspension imposed pursuant to this section is counted as a demerit or result in any insurance penalty for automobile insurance purposes if at the time he the person was stopped, the person whose license is suspended had an alcohol concentration that was less than eight one-hundredths of one percent."
SECTION 2. Section 56-1-400 of the 1976 Code is amended to read:
(B)(1) A person who does not own a vehicle, as shown in the Department of Motor Vehicles' records, and who certifies that he the person:
(a) cannot obtain a vehicle owner's permission to have an ignition interlock device installed on a vehicle;
(b) will not be driving any a vehicle other than the one a vehicle owned by his the person's employer; and
(c) that he will not own a vehicle during the interlock period, may petition the Department of Motor Vehicles department, on a form provided by it the department, for issuance of a an ignition interlock restricted license containing an ignition interlock device restriction, that permits the person to operate a vehicle specified by the employee according to the employer's needs as contained in the employer's statement during the days and hours specified in the employer's statement without having to show that an ignition interlock device has been installed.
(2) The form must contain:
(a) identifying information about the employer's noncommercial vehicles that the person will be operating;
(b) a statement that explains the circumstances in which the person will be operating the employer's vehicles; and
(c) the notarized signature of the person's employer.
(3) This subsection does not apply to a person who is self-employed or to a person who is employed by a business owned in whole or in part by the person or a member of the person's household or immediate family unless during the defense of a criminal charge, the court finds that the vehicle's ownership by the business serves a legitimate business purpose and that titling and registration of the vehicle by the business was not done to circumvent the intent of this section.
(4) Whenever the person operates the employer's vehicle pursuant to this subsection, the person shall have with the person a copy of the form specified by this subsection.
(5) The determination of eligibility for this the waiver is subject to periodic review at the discretion of the Department of Motor Vehicles department. The Department of Motor Vehicles must department shall revoke a license waiver issued pursuant to this exemption if it the department determines that the person has been driving a vehicle other than the one vehicle owned by his the person's employer or has been operating the person's employer's vehicle outside the locations, days, or hours specified by the employer in the department's records. The person may seek relief from the Department of Motor Vehicle's department's determination by filing a request for a contested case hearing with the Office of Motor Vehicle Hearings pursuant to the Administrative Procedures Act and the rules of procedure for the Office of Motor Vehicle Hearings. However, the filing of a request for a contested case hearing will not stay the revocation of the waiver pending the hearing.
(C) Any A person whose license has been suspended or revoked for an offense within the jurisdiction of the court of general sessions shall provide the Department of Motor Vehicles department with proof that the fine owed by the person has been paid before the Department of Motor Vehicles department may return or issue the person a license. Proof that the fine has been paid may be a receipt from the clerk of court of the county in which the conviction occurred stating that the fine has been paid in full."
SECTION 3. Section 56-1-460 of the 1976 Code is amended to read:
"Section 56-1-460. (A)(1) Except as provided in item (2), a person who drives a motor vehicle on any a public highway of this State when his the person's license to drive is canceled, suspended, or revoked must, upon conviction, be punished as follows:
(a) for a first offense, fined three hundred dollars or imprisoned for up to thirty days, or both;
(b) for a second offense, fined six hundred dollars or imprisoned for up to sixty consecutive days, or both; and
(c) for a third and or subsequent offense, fined one thousand dollars and imprisoned for up to ninety days or confined to a person's place of residence pursuant to the Home Detention Act for not less than ninety days nor more than six months. No portion of a term of imprisonment or confinement under home detention may be suspended by the trial judge. For purposes of this item, a person sentenced to confinement pursuant to the Home Detention Act is required to pay for the cost of such confinement.
(d) Notwithstanding the provisions of Sections 22-3-540, 22-3-545, 22-3-550, and 14-25-65, an offense punishable under this item may be tried in magistrates or municipal court.
(e)(i) A person convicted of a first or second offense of this item, as determined by the records of the department, and who is employed or enrolled in a college or university at any time while his the person's driver's license is suspended pursuant to this item, may apply for a route restricted driver's license permitting him the person to drive only to and from work or his the person's place of education and in the course of his the person's employment or education during the period of suspension. The department may issue the route restricted driver's license only upon a showing by the person that he the person is employed or enrolled in a college or university and that he the person lives further than one mile from his the person's place of employment or place of education.
(ii) When the department issues a route restricted driver's license, it shall designate reasonable restrictions on the times during which and routes on which the person may operate a motor vehicle. A person holding a route restricted driver's license pursuant to this item must shall report to the department immediately any change in his the person's employment hours, place of employment, status as a student, or residence.
(iii) The fee for a route restricted driver's license issued pursuant to this item is one hundred dollars, but no additional fee is due when changes occur in the place and hours of employment, education, or residence. Of this fee, eighty dollars must be placed by the Comptroller General into a special restricted account to be used by the Department of Motor Vehicles to defray its the Department of Motor Vehicle's expenses. The remainder of the fees collected pursuant to this item must be credited to the Department of Transportation State Non-Federal Aid Highway Fund.
(iv) The operation of a motor vehicle outside the time limits and route imposed by a route restricted license by the person issued that license is a violation of subsection (A)(1).
(2) A person who drives a motor vehicle on any a public highway of this State when his the person's license has been suspended or revoked pursuant to the provisions of Section 56-5-2990 or 56-5-2945 must, upon conviction, be punished as follows:
(a) for a first offense, fined three hundred dollars or imprisoned for not less than ten nor more than thirty days;
(b) for a second offense, fined six hundred dollars or imprisoned for not less than sixty days nor more than six months;
(c) for a third and or subsequent offense, fined one thousand dollars and imprisoned for not less than six months nor more than three years;
(d) noNo portion of the minimum sentence imposed under pursuant to this item may be suspended.
(C) One hundred dollars of each fine imposed pursuant to this section must be placed by the Comptroller General into a special restricted account to be used by the Department of Public Safety for the Highway Patrol."
SECTION 4. Section 56-1-748 of the 1976 Code is amended to read:
"Section 56-1-748. (A) No person issued a restricted driver's license under the provisions of Section 56-1-170(B) 56-1-170, Section 56-1-320(A) 56-1-320, Section 56-1-740(B) 56-1-740, 56-1-745, Section 56-1-746 (D) 56-1-746, Section 56-5-750(G) 56-5-750, Section 56-9-430(B) 56-9-430, Section 56-10-260(B) 56-10-260, Section 56-10-270(C) 56-10-270, or Section 56-5-2951(H) 56-5-2951 shall subsequently be eligible for issuance of a restricted driver's license under these provisions.
(B) A person who obtains a route restricted driver's license and who is required to attend an Alcohol and Drug Safety Action Program or a court ordered drug program as a condition of reinstatement of the person's driving privileges may use the route restricted driver's license to attend the Alcohol and Drug Safety Action Program classes or court ordered drug program in addition to the other permitted uses of the route restricted driver's license."
SECTION 5. Section 56-1-1310 of the 1976 Code is repealed.
SECTION 6. Section 56-1-1320 of the 1976 Code is amended to read:
(B) Ninety-five dollars of the collected fee must be credited to the State's General Fund of the State for use of the Department of Public Safety in the hiring, training, and equipping of members of the South Carolina Highway Patrol and Transportation Police and in the operations of the South Carolina Highway Patrol and Transportation Police."
SECTION 7. Section 56-1-1350 of the 1976 Code is repealed.
SECTION 8. Section 56-5-2941 of the 1976 Code is amended to read:
"Section 56-5-2941. (A) Except as otherwise provided in this section, in addition to the penalties required and authorized to be imposed against a person violating the provisions of Section 56-5-2930, 56-5-2933, or 56-5-2945, or violating the provisions of another law of any other another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or other drugs Pursuant to Sections 56-5-2945 and 56-5-2990, the Department of Motor Vehicles must shall require the a person, if he is a subsequent offender and who is a resident of this State, and who has violated the provisions of Section 56-5-2930, 56-5-2933, 56-5-2945, 56-5-2947, or a law of another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or other drugs, to have installed on any motor vehicle the person drives an ignition interlock device designed to prevent driving of the motor vehicle if the person has consumed alcoholic beverages. This section does not apply to a person convicted of a first offense violation of Section 56-5-2930 or 56-5-2933, unless the person refused to submit to a breath test pursuant to Section 56-5-2950 or submitted to a breath test pursuant to Section 56-5-2950 and had an alcohol concentration of twelve one hundredths of one percent or more. The Department of Motor Vehicles department may waive the requirements of this section if it finds the department determines that the offender person has a medical condition that makes him the person incapable of properly operating the installed device. If the department grants a medical waiver, the department shall suspend the person's driver's license for the length of time that the person would have been required to hold an ignition interlock restricted license pursuant to Sections 56-5-2945 and 56-5-2990. The department may withdraw the waiver at any time that the department becomes aware that the person's medical condition has improved to the extent that the person has become capable of properly operating an installed device. The department also shall require a person who has enrolled in the Ignition Interlock Device Program in lieu of the remainder of a driver's license suspension or denial of the issuance of a driver's license or permit pursuant to Section 56-1-286 or 56-5-2951 to have an ignition interlock device installed on any motor vehicle the person drives.
The length of time that an interlock a device is required to be affixed to a motor vehicle following the completion of a period of license suspension imposed on the offender person is two years for a second offense, three years for a third offense, and the remainder of the offender's person's life for a fourth or subsequent offense is set forth in Sections 56-1-286, 56-5-2945, 56-5-2947, 56-5-2951, and 56-5-2990.
(B) Notwithstanding the pleadings, for purposes of a second or a subsequent offense, the specified length of time that an interlock a device is required to be affixed to a motor vehicle is based on the Department of Motor Vehicle's records for offenses pursuant to Section 56-1-286, 56-5-2930, 56-5-2933, or 56-5-2945, 56-5-2947, 56-5-2950, or 56-5-2951.
(B)(C) If a person who is a subsequent offender and a resident of this State is convicted of violating the provisions of a law of any other another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or other drugs, and, as a result of the conviction, the person is subject to an ignition interlock device requirement in the other state, the person is subject to the requirements of this section for the length of time that would have been required for an offense committed in South Carolina, or for the length of time that is required by the other state, whichever is longer.
(C)(D) If a person from another state becomes a resident of South Carolina while subject to an ignition interlock device requirement in another state, the person may only obtain a South Carolina driver's license if the person enrolls in the South Carolina ignition interlock device program Ignition Interlock Device Program pursuant to this section. The person is subject to the requirements of this section for the length of time that would have been required for an offense committed in South Carolina, or for the length of time that is required by the other state, whichever is longer.
(D)(E) The offender shall person must be subject to an Ignition Interlock Device Point System managed by the Department of Probation, Parole and Pardon Services. An offender receiving A person accumulating a total of:
(1) two points or more, but less than three points, will must have their the length of time that the interlock device is required extended by two months.;
(2) An offender receiving a total of three points or more, but less than four points, will must have their the length of time that the interlock device is required extended by four months, and must shall submit to a substance abuse assessment pursuant to Section 56-5-2990, and shall successfully complete the plan of education and treatment, or both, as recommended by the certified substance abuse program. Should the individual person not complete the recommended plan, or not make progress toward completing the plan, the Department of Motor Vehicles must shall suspend the individual's driver's person's ignition interlock restricted license until the plan is completed or progress is being made toward completing the plan.;
(3) An offender receiving a total of four points or more shall must have their the person's ignition interlock restricted license suspended for a period of one year six months, and shall submit to a substance abuse assessment pursuant to Section 56-5-2990, and shall successfully complete the plan of education and treatment, or both, as recommended by the certified substance abuse program. Completion of the plan is mandatory as a condition of reinstatement of the person's driving privileges Should the person not complete the recommended plan or not make progress toward completing the plan, the Department of Motor Vehicles shall leave the person's ignition interlock restricted license in suspended status, or, if the license has already been reinstated following the six-month suspension, shall resuspend the person's ignition interlock restricted license until the plan is completed or progress is being made toward completing the plan. The Department of Alcohol and Other Drug Abuse Services is responsible for notifying the Department of Motor Vehicles of an individual's a person's completion and compliance with education and treatment programs. Upon reinstatement of driving privileges following the six-month suspension, the Department of Probation, Parole and Pardon Services shall reset the person's point total to zero points, and the person shall complete the remaining period of time on the ignition interlock device.
(E)(F) The cost of the interlock device must be borne by the offender person. However, if the offender believes he person is indigent and cannot afford the cost of the ignition interlock device, the offender person may submit an affidavit of indigency to the Department of Probation, Parole and Pardon Services for a determination of indigency as it pertains to the cost of the ignition interlock device. The affidavit of indigency form must be made publicly accessible on the Department of Probation, Parole and Pardon Services' Internet web site. If the Department of Probation, Parole and Pardon Services determines that the offender person is indigent as it pertains to the ignition interlock device, it the Department of Probation, Parole and Pardon Services may authorize an interlock a device to be affixed to the motor vehicle and the cost of the initial installation and standard use of the ignition interlock device to be paid for by the Ignition Interlock Device Fund managed by the Department of Probation, Parole and Pardon Services. Funds remitted to the Department of Probation, Parole and Pardon Services for the Ignition Interlock Device Fund also may be used by the Department of Probation, Parole and Pardon Services to support the Ignition Interlock Device Program. For purposes of this section, a person is indigent if the person is financially unable to afford the cost of the ignition interlock device. In making a determination whether a person is indigent, all factors concerning the person's financial conditions should be considered including, but not limited to, income, debts, assets, number of dependants dependents claimed for tax purposes, living expenses, and family situation. A presumption that the person is indigent is created if the person's net family income is less than or equal to the poverty guidelines established and revised annually by the United States Department of Health and Human Services published in the Federal Register. 'Net income' means gross income minus deductions required by law. The determination of indigency is subject to periodic review at the discretion of the Department of Probation, Parole and Pardon Services.
(F)(G) The ignition interlock service provider must shall collect and remit monthly to the Ignition Interlock Device Fund a fee as determined by the Department of Probation, Parole and Pardon Services not to exceed three hundred sixty thirty dollars per year month for each year month the person is required to drive a vehicle with an ignition interlock a device. Any A ignition service provider failing who fails to properly remit funds to the Ignition Interlock Device Fund may be decertified as an ignition interlock a service provider by the Department of Probation, Parole and Pardon Services. If a service provider is decertified for failing to remit funds to the Ignition Interlock Device Fund, the cost for removal and replacement of an ignition interlock a device must be borne by the service provider.
(G)(H)(1) The offender must person shall have the interlock device inspected every sixty days to verify that the device is affixed to the motor vehicle and properly operating, and to allow for the preparation of an ignition interlock device inspection report by the service provider indicating the offender's person's alcohol content at each attempt to start and running re-test retest during each sixty-day period. Failure of the person to have the interlock device inspected every sixty days must result in one ignition interlock device point.
(2) Only a service provider authorized by the Department of Probation, Parole and Pardon Services to perform inspections on ignition interlock devices may conduct inspections. The service provider immediately must shall report any devices that fail inspection to the Department of Probation, Parole and Pardon Services. The report must contain the person's name of the offender, identify the vehicle upon which the failed device is installed, and the reason for the failed inspection, and.
(3) If the inspection report reflects that the person has failed to complete a running retest, the person must be assessed one ignition interlock device point.
(4) The inspection report must indicate the offender's person's alcohol content at each attempt to start and running re-test retest during each sixty-day period. Failure of the offender to have the interlock device inspected every sixty days will result in one ignition interlock device point. Upon review of the ignition interlock device inspection report, if the report reflects that the offender attempted to start the motor vehicle with an alcohol concentration of two one-hundredths of one percent or more, the offender is assessed one-half interlock device point. Upon review of the interlock device inspection report, if If the report reflects that the offender person violated a running re-test retest by having an alcohol concentration of:
(a) between two one-hundredths of one percent or more and but less than four one-hundredths of one percent, the offender is person must be assessed one-half ignition interlock device point.;
(b) Upon review of the interlock device inspection report, if the report reflects that the offender person violated a running re-test retest by having an alcohol concentration between four one-hundredths of one percent or more and but less than fifteen one-hundredths of one percent, the offender is person must be assessed one ignition interlock device point.; or
(c) Upon review of the interlock device inspection report, if the report reflects that the offender person violated a running re-test retest by having an alcohol concentration above fifteen one-hundredths of one percent or more, the offender is person must be assessed two ignition interlock device points.
(5) An individual A person may appeal any interlock device points received to an administrative hearing officer with the Department of Probation, Parole and Pardon Services through a process established by the Department of Probation, Parole and Pardon Services. The administrative hearing officer's decision on appeal shall be is final and no appeal from such decision shall be is allowed.
(H)(I) Ten Five years from the date of the person's last conviction driver's license reinstatement and every five years thereafter a fourth or subsequent offender whose license has been reinstated pursuant to Section 56-1-385 may apply to the Department of Probation, Parole and Pardon Services for removal of the ignition interlock device and the removal of the restriction from his the person's driver's license. The Department of Probation, Parole and Pardon Services may, for good cause shown, remove the device and remove the restriction notify the Department of Motor Vehicles that the person is eligible to have the restriction removed from the offender's person's license.
(I)(J)(1) Except as otherwise provided in this section, it is unlawful for a person issued a driver's license with an ignition interlock restriction who is subject to the provisions of this section to drive a motor vehicle that is not equipped with a properly operating, certified ignition interlock device. A person who violates this section must be punished in the manner provided by law subsection:
(a) for a first offense, is guilty of a misdemeanor, and, upon conviction, must be fined not less than five hundred dollars, or be imprisoned not more than ninety days, or be confined to the person's place of residence pursuant to the Home Detention Act for six months. The person must have the length of time that the ignition interlock device is required extended by six months;
(b) for a second offense, is guilty of a misdemeanor, and, upon conviction, must be fined not less than one thousand dollars, or be imprisoned not more than three years, or be confined to the person's place of residence pursuant to the Home Detention Act for one year. The person must have the length of time that the ignition interlock device is required extended by one year; and
(c) for a third or subsequent offense, is guilty of a felony, and, upon conviction, must be fined not less than fine thousand dollars, or be imprisoned not more than ten years, or be confined to the person's place of residence pursuant to the Home Detention Act for three years. The person must have the length of time that the ignition interlock device is required extended by three years.
(2) No portion of the minimum sentence imposed pursuant to this subsection may be suspended.
(3) Notwithstanding any other provision of law, a first or second offense punishable pursuant to this subsection may be tried in summary court.
(J)(K)(1) An offender that A person who is required in the course and scope of his the person's employment to drive a motor vehicle owned by the offender's person's employer may drive his the employer's motor vehicle without installation of an ignition interlock device, provided that the offender's person's use of the employer's motor vehicle is solely for the employer's business purposes. This subsection does not apply to an offender a person who is self-employed or to an offender a person who is employed by a business owned in whole or in part by the offender person or a member of the offender's person's household or immediate family unless during the defense of a criminal charge, the court finds that the vehicle's ownership by the business serves a legitimate business purpose and that titling and registration of the vehicle by the business was not done to circumvent the intent of this section.
(2) Whenever the person operates the employer's vehicle pursuant to this subsection, the person shall have with the person a copy of the Department of Motor Vehicle's form specified by Section 56-1-400(B).
(3) This subsection will be construed in parallel with the requirements of subsection 56-1-400(B). A waiver issued pursuant to this subsection will be subject to the same review and revocation as described in subsection 56-1-400(B).
(K)(L) It is unlawful for a person to tamper with or disable, or attempt to tamper with or disable, an ignition interlock device installed on a motor vehicle pursuant to this section. Obstructing or obscuring the camera lens of an ignition interlock device constitutes tampering. A person who violates this subsection is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days, or both.
(L)(M) It is unlawful for a person to knowingly rent, lease, or otherwise provide an offender a person who is subject to the provisions of this section with a motor vehicle without a properly operating, certified ignition interlock device. A person who violates this subsection is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days, or both.
(M)(N) It is unlawful for an offender a person who is subject to the provisions of this section to solicit or request another person, or for a person to solicit or request another person on behalf of an offender a person who is subject to the provisions of this section, to engage an ignition interlock device to start a motor vehicle with a device installed pursuant to this section. A person who violates this subsection is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days, or both.
(N)(O) It is unlawful for another person to engage an ignition interlock device to start a motor vehicle with a device installed pursuant to this section. A person who violates this subsection is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days, or both.
(O)(P) Only ignition interlock devices certified by the Department of Probation, Parole and Pardon Services may be used to fulfill the requirements of this section.
(1) The Department of Probation, Parole and Pardon Services must shall certify whether a device meets the accuracy requirements and specifications provided in guidelines or regulations adopted by the National Highway Traffic Safety Administration, as amended from time to time. All devices certified to be used in South Carolina must be set to prohibit the starting of a motor vehicle when an alcohol concentration of two one-hundredths of one percent or more is measured and all running re-tests retests must record violations of an alcohol concentration of two one-hundredths of one percent or more, and must capture a photographic image of the driver as the driver is operating the ignition interlock device. The photographic images recorded by the ignition interlock device may be used by the Department of Probation, Parole and Pardon Services to aid in the Department of Probation, Parole and Pardon Services' management of the Ignition Interlock Device Program; however, neither the Department of Probation, Parole and Pardon Services, the Department of Probation, Parole and Pardon Services' employees, nor any other political subdivision of this State may be held liable for any injury caused by a driver or other person who operates a motor vehicle after the use or attempted use of an ignition interlock device.
(2) The Department of Probation, Parole and Pardon Services shall maintain a current list of certified ignition interlock devices and their manufacturers. The list must be updated at least quarterly. If a particular certified device fails to continue to meet federal requirements, the device must be decertified, may not be used until it is compliant with federal requirements, and must be replaced with a device that meets federal requirements. The cost for removal and replacement must be borne by the manufacturer of the noncertified device.
(3) Only ignition interlock installers certified by the Department of Probation, Parole and Pardon Services may install and service ignition interlock devices required pursuant to this section. The Department of Probation, Parole and Pardon Services shall maintain a current list of vendors that are certified to install the devices.
(P)(Q) In addition to availability under the Freedom of Information Act, any Department of Probation, Parole and Pardon Services policy concerning ignition interlock devices must be made publicly accessible on the Department of Probation, Parole and Pardon Service's Services' Internet web site.
(Q)(R) The Department of Probation, Parole and Pardon Services shall develop policies including, but not limited to, the certification, use, maintenance, and operation of ignition interlock devices and the Ignition Interlock Device Fund."
SECTION 9. Section 56-5-2942 of the 1976 Code is amended to read:
"Section 56-5-2942. (A) A person who is convicted of or pleads guilty or nolo contendere to a second or subsequent violation of Section 56-5-2930, 56-5-2933, or 56-5-2945 must have all motor vehicles owned by or registered to him the person immobilized if the person is a resident of this State, unless the vehicle has been confiscated pursuant to Section 56-5-6240 or the person is a holder of a valid ignition interlock restricted license.
(B) For purposes of this section, 'immobilized' and 'immobilization' mean suspension and surrender of the registration and motor vehicle license plate.
(C) Upon receipt of a conviction by the department from the court for a second or subsequent violation of Section 56-5-2930, 56-5-2933, or 56-5-2945, the department must shall determine all vehicles registered to the convicted person, both solely and jointly, and suspend all vehicles registered to the person, unless the person is a holder of a valid ignition interlock restricted license.
(D) Upon notification by a court in this State or by any other another state of a conviction for a second or subsequent violation of Section 56-5-2930, 56-5-2933, or 56-5-2945, the department must shall require the person, unless the person is a holder of a valid ignition interlock restricted license, convicted to surrender all license plates and vehicle registrations subject to immobilization pursuant to this section. The immobilization is for a period of thirty days to take place during the driver's license suspension pursuant to a conviction for a second or subsequent violation of Section 56-5-2930, 56-5-2933, or 56-5-2945. The department must shall maintain a record of all vehicles immobilized pursuant to this section.
(E) An immobilized motor vehicle must be released to the holder of a bona fide lien on the motor vehicle when possession of the motor vehicle is requested, as provided by law, by the lienholder for the purpose of foreclosing on and satisfying the lien.
(F) An immobilized motor vehicle may be released by the department without legal or physical restraints to a person who has not been convicted of a second or subsequent violation of Section 56-5-2930, 56-5-2933, or 56-5-2945, if that person is a registered owner of the motor vehicle or a member of the household of a registered owner. The vehicle must be released if an affidavit is submitted by that person to the department stating that:
(1) he the person regularly drives the motor vehicle subject to immobilization;
(2) the immobilized motor vehicle is necessary to his the person's employment, transportation to an educational facility, or for the performance of essential household duties;
(3) no other motor vehicle is available for the person's use;
(4) the person will not authorize the use of the motor vehicle by any other person known by him the person to have been convicted of a second or subsequent violation of Section 56-5-2930, 56-5-2933, or 56-5-2945; or
(5) the person will report immediately to a local law enforcement agency any unauthorized use of the motor vehicle by a person known by him the person to have been convicted of a second or subsequent violation of Section 56-5-2930, 56-5-2933, or 56-5-2945.
(G) The department may issue a determination permitting or denying the release of the vehicle based on the affidavit submitted pursuant to subsection (F). A person may seek relief from a department determination immobilizing a motor vehicle or denying the release of the motor vehicle by filing a request for a contested case hearing with the Office of Motor Vehicle Hearings pursuant to the Administrative Procedures Act and the rules of procedure for the Office of Motor Vehicle Hearings.
(H) A person who drives an immobilized motor vehicle except as provided in subsections (E) and (F) is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days.
(I) A person who fails to surrender registrations and license plates pursuant to this section is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days.
(J) A fee of fifty dollars must be paid to the department for each motor vehicle that was suspended before any of the suspended registrations and license plates may be registered or before the motor vehicle may be released pursuant to subsection (F). This fee must be placed by the Comptroller General into a special restricted interest bearing account to be used by the Department of Motor Vehicles to defray its the Department of Motor Vehicle's expenses.
(K) For purposes of this article, a conviction of or plea of nolo contendere to Section 56-5-2933 is considered a prior offense of Section 56-5-2930."
SECTION 10. Section 56-5-2945 of the 1976 Code is amended to read:
"Section 56-5-2945. (A) A person who, while under the influence of alcohol, drugs, or the combination of alcohol and drugs, drives a motor vehicle and when driving a motor vehicle does any act forbidden by law or neglects any duty imposed by law in the driving of the motor vehicle, which act or neglect proximately causes great bodily injury or death to a another person other than himself, is guilty of the offense of felony driving under the influence, and, upon conviction, must be punished:
(1) by a mandatory fine of not less than five thousand one hundred dollars nor more than ten thousand one hundred dollars and mandatory imprisonment for not less than thirty days nor more than fifteen years when great bodily injury results;
(2) by a mandatory fine of not less than ten thousand one hundred dollars nor more than twenty-five thousand one hundred dollars and mandatory imprisonment for not less than one year nor more than twenty-five years when death results.
A part of the mandatory sentences required to be imposed by this section must not be suspended, and probation must not be granted for any portion.
(B) As used in this section, 'great bodily injury' means bodily injury which creates a substantial risk of death or which causes serious, permanent disfigurement, or protracted loss or impairment of the function of any bodily member or organ.
(C)(1) The Department of Motor Vehicles must shall suspend the driver's license of a person who is convicted or who receives sentence upon a plea of guilty or nolo contendere pursuant to this section for a period to include a period of incarceration plus three years for a conviction of Section 56-5-2945 when 'great bodily injury' occurs and five years when a death occurs. This period of incarceration shall must not include any portion of a suspended sentence such as probation, parole, supervised furlough, or community supervision. For suspension purposes of this section, convictions arising out of a single incident shall must run concurrently.
(2) After the person is released from prison, the person shall enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle for three years when 'great bodily injury' results and five years when a death occurs.
(C)(D) One hundred dollars of each fine imposed pursuant to this section must be placed by the Comptroller General into a special restricted account to be used by the Department of Public Safety for the Highway Patrol."
SECTION 11. Section 56-5-2947 of the 1976 Code is amended to read:
"Section 56-5-2947. (A) A person eighteen years of age or over older is guilty of child endangerment when:
(1) the person is in violation of violates:
(a) Section 56-5-750;
(b) Section 56-5-2930;
(c) Section 56-5-2933; or
(d) Section 56-5-2945; and
(2) the person has one or more passengers under younger than sixteen years of age in the motor vehicle when the violation occurs.
If more than one passenger under younger than sixteen years of age is in the vehicle when a violation of subsection (A)(1) occurs, the person may be charged with only one violation of this section.
(B) Upon conviction, the person must be punished by:
(1) a fine of fined not more than one-half of the maximum fine allowed for committing the violation enumerated in subsection (A)(1), when the person is fined for that offense;
(2) a term of imprisonment of imprisoned not more than one-half of the maximum term of imprisonment allowed for committing the violation enumerated listed in subsection (A)(1), when the person is imprisoned for the offense; or
(3) both a fine and imprisonment fined and imprisoned as prescribed in items (1) and (2) when the person is fined and imprisoned for the offense.
(C) No portion of the penalty assessed under pursuant to subsection (B) may be suspended or revoked and probation may not be awarded.
(D)(1) In addition to imposing the penalties for offenses enumerated listed in subsection (A)(1) and the penalties contained in subsection (B), the Department of Motor Vehicles must shall suspend the person's driver's license for sixty days.
(2) The person shall enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle for three months.
(3) Sections 56-1-1320 and 56-5-2990 as they relate to enrollment in an alcohol and drug safety action program and to the issuance of a provisional driver's license will not be effective until the sixty-day suspension ignition interlock restricted license period is completed.
(E) A person may be convicted under pursuant to this section for child endangerment in addition to being convicted for an offense enumerated listed in subsection (A)(1).
(F) The court that has jurisdiction over an offense enumerated listed in subsection (A)(1) has jurisdiction over the offense of child endangerment.
(G) A first offense charge for a violation of this section may not be used as the only evidence for taking a child into protective custody pursuant to Sections 63-7-620(A) and 63-7-660."
SECTION 12. Section 56-5-2950 of the 1976 Code is amended to read:
(B) No tests may be administered or samples obtained unless, upon activation of the video recording equipment and prior to the commencement of the testing procedure, the person has been given a written copy of and verbally informed that:
(1) he the person does not have to take the test or give the samples, but that his the person's privilege to drive must be suspended or denied for at least six months with the option of ending the suspension if the person enrolls in the Ignition Interlock Device Program, if he the person refuses to submit to the test, and that his the person's refusal may be used against him the person in court;
(2) his the person's privilege to drive must be suspended for at least one month with the option of ending the suspension if the person enrolls in the Ignition Interlock Device Program, if he the person takes the test or gives the samples and has an alcohol concentration of fifteen one-hundredths of one percent or more;
(3) he the person has the right to have a qualified person of his the person's own choosing conduct additional independent tests at his the person's expense;
(4) he the person has the right to request an administrative a contested case hearing within thirty days of the issuance of the notice of suspension; and
(5) if he the person does not request an administrative a contested case hearing or if his the person's suspension is upheld at the administrative contested case hearing, he must the person shall enroll in an Alcohol and Drug Safety Action Program.
(C) A hospital, physician, qualified technician, chemist, or registered nurse who obtains the samples or conducts the test or participates in the process of obtaining the samples or conducting the test in accordance with this section is not subject to a cause of action for assault, battery, or another cause alleging that the drawing of blood or taking samples at the request of the arrested person or a law enforcement officer was wrongful. This release from liability does not reduce the standard of medical care required of the person obtaining the samples or conducting the test. This qualified release also applies to the employer of the person who conducts the test or obtains the samples.
(D) The person tested or giving samples for testing may have a qualified person of his the person's own choosing conduct additional tests at his the person's expense and must be notified in writing of that right. A person's request or failure to request additional blood or urine tests is not admissible against the person in the criminal trial. The failure or inability of the person tested to obtain additional tests does not preclude the admission of evidence relating to the tests or samples obtained at the direction of the law enforcement officer.
(E) The arresting officer must shall provide affirmative assistance to the person to contact a qualified person to conduct and obtain additional tests. Affirmative assistance, at a minimum, includes providing transportation for the person to the nearest medical facility which performs blood tests to determine a person's alcohol concentration. If the medical facility obtains the blood sample but refuses or fails to test the blood sample to determine the person's alcohol concentration, SLED must shall test the blood sample and provide the result to the person and to the arresting officer. Failure to provide affirmative assistance upon request to obtain additional tests bars the admissibility of the breath test result in any a judicial or administrative proceeding.
SLED must shall administer the provisions of this subsection and must shall make regulations necessary to carry out its this subsection's provisions. The costs of the tests administered at the direction of the law enforcement officer must be paid from the State's general fund of the state. However, if the person is subsequently convicted of violating Section 56-5-2930, 56-5-2933, or 56-5-2945, then, upon conviction, the person must shall pay twenty-five dollars for the costs of the tests. The twenty-five dollars must be placed by the Comptroller General into a special restricted account to be used by the State Law Enforcement Division to offset the costs of administration of the breath testing devices, breath testing site video program, and toxicology laboratory.
(F) A qualified person who obtains samples or administers the tests or assists in obtaining samples or the administration of tests at the direction of a law enforcement officer is released from civil and criminal liability unless the obtaining of samples or tests is performed in a negligent, reckless, or fraudulent manner. No person may be required by the arresting officer, or by another law enforcement officer, to obtain or take any sample of blood or urine.
(G) In the criminal prosecution for a violation of Section 56-5-2930, 56-5-2933, or 56-5-2945 the alcohol concentration at the time of the test, as shown by chemical analysis of the person's breath or other body fluids, gives rise to the following:
(1) if the alcohol concentration was at that time five one-hundredths of one percent or less, it is conclusively presumed that the person was not under the influence of alcohol;
(2) if the alcohol concentration was at that time in excess of five one-hundredths of one percent but less than eight one-hundredths of one percent, this fact does not give rise to any inference that the person was or was not under the influence of alcohol, but this fact may be considered with other evidence in determining the guilt or innocence of the person; or
(3) if the alcohol concentration was at that time eight one-hundredths of one percent or more, it may be inferred that the person was under the influence of alcohol.
The provisions of this section must not be construed as limiting the introduction of any other evidence bearing upon the question of whether or not the person was under the influence of alcohol, drugs, or a combination of them alcohol and drugs.
(H) A person who is unconscious or otherwise in a condition rendering him the person incapable of refusal is considered to be informed and not to have withdrawn the consent provided by subsection (A) of this section.
(I) A person required to submit to tests by the arresting law enforcement officer must be provided with a written report including the time of arrest, the time of the tests, and the results of the tests before any trial or other proceeding in which the results of the tests are used as evidence. A person who obtains additional tests must shall furnish a copy of the time, method, and results of any tests such tests to the officer before any a trial, hearing, or other proceeding in which the person attempts to use the results of the additional tests as evidence.
(J) Policies, procedures, and regulations promulgated by SLED may be reviewed by the trial judge or hearing officer on motion of either party. The failure to follow any of these policies, procedures, and regulations, or the provisions of this section, shall result in the exclusion from evidence of any test results, if the trial judge or hearing officer finds that this failure materially affected the accuracy or reliability of the test results or the fairness of the testing procedure and the court trial judge or hearing officer rules specifically as to the manner in which the failure materially affected the accuracy or reliability of the test results or the fairness of the procedure.
(K) If a state employee charged with the maintenance of breath testing devices in this State and the administration of breath testing policy is required to testify at an administrative a contested case hearing or court proceeding, the entity employing the witness may charge a reasonable fee to the defendant for these such services."
SECTION 13. Section 56-5-2951 of the 1976 Code is amended to read:
"Section 56-5-2951. (A) The Department of Motor Vehicles must shall suspend the driver's license, permit, or nonresident operating privilege of, or deny the issuance of a license or permit to, a person who drives a motor vehicle and refuses to submit to a test provided for in Section 56-5-2950 or has an alcohol concentration of fifteen one-hundredths of one percent or more. The arresting officer must shall issue a notice of suspension which is effective beginning on the date of the alleged violation of Section 56-5-2930, 56-5-2933, or 56-5-2945.
(B) Within thirty days of the issuance of the notice of suspension, the person may:
(1) obtain a temporary alcohol license by filing with from the Department of Motor Vehicles a form for this purpose. A one hundred dollar fee must be assessed for obtaining a temporary alcohol license. Twenty-five dollars of the fee must be distributed by the Department of Motor Vehicles to the Department of Public Safety for supplying and maintaining all necessary vehicle videotaping equipment. The remaining seventy-five dollars must be placed by the Comptroller General into a special restricted account to be used by the Department of Motor Vehicles to defray its the Department of Motor Vehicle's expenses. The temporary alcohol license allows the person to drive without any restrictive conditions pending the outcome of the contested case hearing provided for in subsection (F) or the final decision or disposition of the matter. If the suspension is upheld at the contested case hearing, the temporary alcohol license remains in effect until the Office of Motor Vehicle Hearings issues the hearing officer's decision and the Department of Motor Vehicles sends notice to the person that he the person is eligible to receive a restricted license pursuant to subsection (H); and
(2) request a contested case hearing before the Office of Motor Vehicle Hearings in accordance with its the Office of Motor Vehicle Hearings' rules of procedure.
At the contested case hearing if:
(a) the suspension is upheld, the person's driver's license, permit, or nonresident operating privilege must be suspended or the person must be denied the issuance of a license or permit for the remainder of the suspension period provided for in subsection (I). Within thirty days of the issuance of the notice that the suspension has been upheld, the person must shall enroll in an Alcohol and Drug Safety Action Program pursuant to Section 56-5-2990;
(b) the suspension is overturned, the person must have his the person's driver's license, permit, or nonresident operating privilege reinstated.
The provisions of this subsection do not affect the trial for a violation of Section 56-5-2930, 56-5-2933, or 56-5-2945.
(C) The period of suspension provided for in subsection (I) begins on the day the notice of suspension is issued, or at the expiration of any other suspensions, and continues until the person applies for a temporary alcohol license and requests a contested case hearing.
(D) If a person does not request a contested case hearing, he the person waives his the person's right to the hearing, and his the person's suspension must not be stayed but continues for the period provided for in subsection (I).
(E) The notice of suspension must advise the person:
(1) of his the person's right to obtain a temporary alcohol driver's license and to request a contested case hearing before the Office of Motor Vehicle Hearings.;
(2) The notice of suspension also must advise the person that, if he the person does not request a contested case hearing within thirty days of the issuance of the notice of suspension, he the person waives his the person's right to the administrative contested case hearing, and the suspension continues for the period provided for in subsection (I).; and
(3) The notice of suspension also must advise the person that if the suspension is upheld at the contested case hearing or if he the person does not request a contested case hearing, he the person must shall enroll in an Alcohol and Drug Safety Action Program.
(F) A contested case hearing must be held after the request for the hearing is received by the Office of Motor Vehicle Hearings. The scope of the hearing is limited to whether the person:
(1) was lawfully arrested or detained;
(2) was given a written copy of and verbally informed of the rights enumerated in Section 56-5-2950;
(3) refused to submit to a test pursuant to Section 56-5-2950; or
(4) consented to taking a test pursuant to Section 56-5-2950, and the:
(a) reported alcohol concentration at the time of testing was fifteen one-hundredths of one percent or more;
(b) individual who administered the test or took samples was qualified pursuant to Section 56-5-2950;
(c) tests administered and samples obtained were conducted pursuant to Section 56-5-2950; and
(d) machine was working properly.
Nothing in this section prohibits the introduction of evidence at the contested case hearing on the issue of the accuracy of the breath test result.
A written order must be issued to all parties either reversing or upholding the suspension of the person's license, permit, or nonresident's operating privilege, or denying the issuance of a license or permit. If the suspension is upheld, the person must receive credit for the number of days his the person's license was suspended before he the person received a temporary alcohol license and requested the contested case hearing.
The Department of Motor Vehicles and the arresting officer shall have the burden of proof in contested case hearings conducted pursuant to this section. If neither the Department of Motor Vehicles nor the arresting officer appears at the contested case hearing, the hearing officer shall rescind the suspension of the person's license, permit, or nonresident's operating privilege regardless of whether the person requesting the contested case hearing or the person's attorney appears at the contested case hearing.
(G) A contested case hearing is governed by the Administrative Procedures Act, and a person has a right to appeal the decision of the hearing officer pursuant to that act to the Administrative Law Court in accordance with its the Administrative Law Court's appellate rules. The filing of an appeal stays the suspension until a final decision is issued on appeal.
(H)(1) If the person did not request a contested case hearing or the suspension is upheld at the administrative contested case hearing, the person must shall enroll in an Alcohol and Drug Safety Action Program pursuant to Section 56-5-2990, and may apply for a restricted license if he the person is employed or enrolled in a college or university. The restricted license permits him the person to drive only to and from work and his the person's place of education and in the course of his the person's employment or education during the period of suspension. The restricted license also permits him the person to drive to and from the Alcohol Drug Safety Action Program classes or to a court-ordered drug program. The department may issue the restricted license only upon showing by the individual person that he the person is employed or enrolled in a college or university, that he the person lives further than one mile from his the person's place of employment, place of education, or location of his the person's Alcohol and Drug Safety Action Program classes, or the location of his the person's court-ordered drug program, and that there is no adequate public transportation between his the person's residence and his the person's place of employment, his the person's place of education, the location of his the person's Alcohol and Drug Safety Action Program classes, or the location of his the person's court-ordered drug program.
(2) If the department issues a restricted license pursuant to this subsection, it must the department shall designate reasonable restrictions on the times during which and routes on which the individual person may drive a motor vehicle. A change in the employment hours, place of employment, status as a student, status of attendance of Alcohol and Drug Safety Action Program classes, status of attendance of his the person's court-ordered drug program, or residence must be reported immediately to the department by the licensee person.
(3) The fee for a restricted license is one hundred dollars, but no additional fee may be charged because of changes in the place and hours of employment, education, or residence. Twenty dollars of this fee must be deposited in the state state's general fund, and eighty dollars must be placed by the Comptroller General into a special restricted account to be used by the Department of Motor Vehicles to defray the expenses of the Department of Motor Vehicles Vehicle's expenses.
(4) Driving a motor vehicle outside the time limits and route imposed by a restricted license by the person issued that license is a violation of Section 56-1-460.
(I)(1) The Except as provided in subsection (I)(3), the period of a driver's license, permit, or nonresident operating privilege suspension for, or denial of issuance of a license or permit to, an arrested person who has no previous convictions for violating Section 56-5-2930, 56-5-2933, or 56-5-2945, or any other a law of this State or another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or another drug other drugs within the ten years preceding a violation of this section, and who has had no previous suspension imposed pursuant to Section 56-5-2950 56-1-286, or 56-5-2951, or 56-5-2990, within the ten years preceding a violation of this section is:
(a) six months for a person who refuses to submit to a test pursuant to Section 56-5-2950; or
(b) one month for a person who takes a test pursuant to Section 56-5-2950 and has an alcohol concentration of fifteen one-hundredths of one percent or more.
(2) The period of a driver's license, permit, or nonresident operating privilege suspension for, or denial of issuance of a license or permit to, an arrested a person who has been convicted previously for violating Section 56-5-2930, 56-5-2933, or 56-5-2945, or any other another law of this State or another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or another drug within the ten years preceding a violation of this section, or who has had a previous suspension imposed pursuant to Section 56-5-2950 56-1-286, or 56-5-2951, or 56-5-2990, within the ten years preceding a violation of this section is:
(a) for a second offense, nine months if he the person refuses to submit to a test pursuant to Section 56-5-2950, or two months if he the person takes a test pursuant to Section 56-5-2950 and has an alcohol concentration of fifteen one-hundredths of one percent or more;
(b) for a third offense, twelve months if he the person refuses to submit to a test pursuant to Section 56-5-2950, or three months if he the person takes a test pursuant to Section 56-5-2950 and has an alcohol concentration of fifteen one-hundredths of one percent or more; and
(c) for a fourth or subsequent offense, fifteen months if he the person refuses to submit to a test pursuant to Section 56-5-2950, or four months if he the person takes a test pursuant to Section 56-5-2950 and has an alcohol concentration of fifteen one-hundredths of one percent or more.
(3) In lieu of serving the remainder of a suspension or denial of the issuance of a license or permit, a person may enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension or denial of the issuance of a license or permit, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle equal to the length of time remaining on the person's suspension or denial of the issuance of a license or permit. If the length of time remaining is less than three months, the ignition interlock device is required to be affixed to the motor vehicle for three months. Once a person has enrolled in the Ignition Interlock Device Program and obtained an ignition interlock restricted license, the person is subject to Section 56-5-2941 and cannot subsequently choose to serve the suspension.
(J) A person's driver's license, permit, or nonresident operating privilege must be restored when the person's period of suspension or ignition interlock restricted license requirement under pursuant to subsection (I) has concluded, even if the person has not yet completed the Alcohol and Drug Safety Action Program in which he is enrolled. After the person's driving privilege is restored, he must the person shall continue the services of the Alcohol and Drug Safety Action Program in which he is enrolled. If the person withdraws from or in any way stops making satisfactory progress toward the completion of the Alcohol and Drug Safety Action Program, the person's license must be suspended until the completion of the Alcohol and Drug Safety Action Program. A person must shall be attending or have completed an Alcohol and Drug Safety Action Program pursuant to Section 56-5-2990 before his the person's driving privilege can be restored at the conclusion of the suspension period or ignition interlock restricted license requirement.
(K) When a nonresident's privilege to drive a motor vehicle in this State has been suspended under pursuant to the provisions of this section, the department must shall give written notice of the action taken to the motor vehicle administrator of the state of the person's residence and of any state in which he the person has a license or permit.
(L) The department must shall not suspend the privilege to drive of a person under the age of twenty-one pursuant to Section 56-1-286, if the person's privilege to drive has been suspended under pursuant to this section arising from the same incident.
(M) A person whose driver's license or permit is suspended pursuant to this section is not required to file proof of financial responsibility.
(N) An insurer may shall not increase premiums on, add surcharges to, or cancel the automobile insurance of a person charged with a violation of Section 56-1-286, 56-5-2930, 56-5-2933, or 56-5-2945, or another a law of this State another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or another drug other drugs based solely on the violation unless he the person is convicted of the violation.
(O) The department must shall administer the provisions of this section and must promulgate regulations necessary to carry out its provisions.
(P) If a person does not request a contested case hearing within the thirty-day period as authorized pursuant to this section, the person may file with the department a form after enrolling in a certified Alcohol and Drug Safety Action Program to apply for a restricted license. The restricted license permits him to drive only to and from work and his place of education and in the course of his employment or education during the period of suspension. The restricted license also permits him to drive to and from Alcohol and Drug Safety Action Program classes or a court-ordered drug program. The department may issue the restricted license at any time following the suspension upon a showing by the individual that he is employed or enrolled in a college or university, that he lives further than one mile from his place of employment, place of education, the location of his Alcohol and Drug Safety Action Program classes, or the location of his court-ordered drug program, and that there is no adequate public transportation between his residence and his place of employment, his place of education, the location of his Alcohol and Drug Safety Action Program classes, or the location of his court-ordered drug program. The department must designate reasonable restrictions on the times during which and routes on which the individual may drive a motor vehicle. A change in the employment hours, place of employment, status as a student, status of attendance of Alcohol and Drug Safety Action Program classes, status of his court-ordered drug program, or residence must be reported immediately to the department by the licensee. The route restrictions, requirements, and fees imposed by the department for the issuance of the restricted license issued pursuant to this item are the same as those provided in this section had the person requested a contested case hearing. A restricted license is valid until the person successfully completes a certified Alcohol and Drug Safety Action Program, unless the person fails to complete or make satisfactory progress to complete the program."
SECTION 14. Section 56-5-2990 of the 1976 Code is amended to read:
"Section 56-5-2990. (A)(1) The Department of Motor Vehicles shall suspend the driver's license of a person who is convicted, receives sentence upon a plea of guilty or of nolo contendere, or forfeits bail posted for a violation of Section 56-5-2930, 56-5-2933, or for the violation of another law or ordinance of this State or of a municipality of this State a law of another state that prohibits a person from driving a motor vehicle while under the influence of intoxicating liquor, drugs, or narcotics for six months for the first conviction, plea of guilty or nolo contendre, or forfeiture of bail; one year for the a second conviction, plea of guilty or of nolo contendere, or forfeiture of bail; two years for the a third conviction, plea of guilty or of nolo contendere, or forfeiture of bail; and a permanent revocation of the driver's license for the a fourth or subsequent conviction, plea of guilty or of nolo contendere, or forfeiture of bail. Only those violations which occurred within ten years including and immediately preceding the date of the last violation shall constitute prior violations within the meaning of this section. However, if the third conviction occurs within five years from the date of the first offense, then the department shall suspend the driver's license for four years. A person whose license is revoked following conviction for a fourth offense as provided in this section is forever barred from being issued any license by the Department of Motor Vehicles to operate a motor vehicle except as provided in Section 56-1-385 alcohol or other drugs.
(2) For a first offense:
(a) If a person refused to submit to a breath test pursuant to Section 56-5-2950, the person's driver's license must be suspended six months. The person is not eligible for a provisional license pursuant to Article 7, Chapter 1, Title 56. In lieu of serving the remainder of the suspension, the person may enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle equal to the length of time remaining on the person's suspension. If the length of time remaining is less than three months, the ignition interlock device is required to be affixed to the motor vehicle for three months. Once a person has enrolled in the Ignition Interlock Device Program and obtained an ignition interlock restricted license, the person is subject to Section 56-5-2941 and cannot subsequently choose to serve the suspension.
(b) If a person submitted to a breath test pursuant to Section 56-5-2950 and had an alcohol concentration of less than twelve one hundredths of one percent, the person's driver's license must be suspended six months. The person is eligible for a provisional license pursuant to Article 7, Chapter 1, Title 56. In lieu of serving the remainder of the suspension, the person may enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle equal to the length of time remaining on the person's suspension. If the length of time remaining is less than three months, the ignition interlock device is required to be affixed to the motor vehicle for three months. Once a person has enrolled in the Ignition Interlock Device Program and obtained an ignition interlock restricted license, the person is subject to Section 56-5-2941 and cannot subsequently choose to serve the suspension.
(c) If a person submitted to a breath test pursuant to Section 56-5-2950 and had an alcohol concentration of twelve one hundredths of one percent or more, the person shall enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle for six months. The person is not eligible for a provisional license pursuant to Article 7, Chapter 1, Title 56.
(3) For a second offense, a person shall enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle for two years.
(4) For a third offense, a person shall enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle for three years. If the third offense occurs within five years from the date of the first offense, the ignition interlock device is required to be affixed to the motor vehicle for four years.
(5) For a fourth or subsequent offense, a person shall enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle for life.
(6) Except as provided in subsection (A)(4), only those offenses which occurred within ten years, including and immediately preceding the date of the last offense, shall constitute prior offenses within the meaning of this section.
(B) A person whose license is suspended under the provisions pursuant to this section, Section 56-1-286, Section 56-5-2945, or Section 56-5-2951 must be notified by the department of the suspension and of the requirement to enroll in and successfully complete an Alcohol and Drug Safety Action Program certified by the Department of Alcohol and Other Drug Abuse Services. A person who must complete an Alcohol and Drug Safety Action Program as a condition of reinstatement of his driving privileges or a court-ordered drug program may use the route restricted or special restricted driver's license to attend the Alcohol and Drug Safety Action Program classes or court-ordered drug program in addition to the other permitted uses of a route restricted driver's license or a special restricted driver's license. An assessment of the extent and nature of the alcohol and drug abuse problem, if any, of the applicant person must be prepared and a plan of education or treatment, or both, must be developed for the applicant person. Entry into and successful completion of the services, if the services are necessary, recommended in the plan of education or treatment, or both, developed for the applicant person is a mandatory requirement of the issuance of an ignition interlock restricted license and restoration of driving privileges to the applicant person whose license is suspended pursuant to this section. The Alcohol and Drug Safety Action Program shall determine if the applicant person has successfully completed the services. Alcohol and Drug Safety Action Programs shall meet at least once a month. The person whose license is suspended must shall attend the first Alcohol and Drug Safety Action Program available after the date of enrollment.
(C) The Department of Alcohol and Other Drug Abuse Services shall determine the cost of services provided by each certified Alcohol and Drug Safety Action Program. Each applicant person shall bear the cost of services recommended in the applicant's person's plan of education or treatment. The cost may not exceed five hundred dollars for education services, two thousand dollars for treatment services, and two thousand five hundred dollars in total for all services. No applicant person may be denied services due to an inability to pay. Inability to pay for services may not be used as a factor in determining if the applicant person has successfully completed services. An applicant A person who is unable to pay for services shall perform fifty hours of community service as arranged by the Alcohol and Drug Safety Action Program, which may use the completion of this community service as a factor in determining if the applicant person has successfully completed services. The Department of Alcohol and Other Drug Abuse Services will shall report annually to the House Ways and Means Committee and Senate Finance Committee on the number of first and multiple offenders completing the Alcohol and Drug Safety Action Program, the amount of fees collected and expenses incurred by each Alcohol and Drug Safety Action Program, and the number of community service hours performed in lieu of payment.
(D) If the applicant person has not successfully completed the services as directed by the Alcohol and Drug Safety Action Program within one year of enrollment, a hearing must be provided by the Alcohol and Drug Safety Action Program whose decision is appealable to the Department of Alcohol and Other Drug Abuse Services. If the applicant person is unsuccessful in the Alcohol and Drug Safety Action Program, the Department of Motor Vehicles may restore the privilege to drive a motor vehicle waive the successful completion of the program as a mandatory requirement of the issuance of an ignition interlock restricted license upon the recommendation of the Medical Advisory Board as utilized by the department Department of Motor Vehicles, if it the Medical Advisory Board determines public safety and welfare of the petitioner person may not be endangered.
(E) The Department of Motor Vehicles and the Department of Alcohol and Other Drug Abuse Services shall develop procedures necessary for the communication of information pertaining to relicensing, or otherwise. These procedures must be consistent with the confidentiality laws of the State and the United States. If the drivers a person's driver's license of any a person is suspended by authority of pursuant to this section, no an insurance company may shall not refuse to issue insurance to cover the remaining members of his the person's family, but the insurance company is not liable for any actions of the person whose license has been suspended or who has voluntarily turned his the person's license in to the Department of Motor Vehicles.
(F) Except as provided for in Section 56-1-365(D) and (E), the driver's license suspension periods under this section begin on the date the person is convicted, receives sentence upon a plea of guilty or of nolo contendere, or forfeits bail posted for the a violation of Section 56-5-2930, 56-5-2933, or for the violation of any other a law of this State or ordinance of a county or municipality of this State that prohibits a person from operating a motor vehicle while under the influence of intoxicating liquor, or narcotics; however, a person is not prohibited from filing a notice of appeal and receiving a certificate which entitles him to operate a motor vehicle for a period of sixty days after the conviction, plea of guilty or nolo contendere, or bail forfeiture pursuant to Section 56-1-365(F)."
SECTION 15. The repeal or amendment by this act of any law, whether temporary or permanent or civil or criminal, does not affect pending actions, rights, duties, or liabilities founded thereon, or alter, discharge, release or extinguish any penalty, forfeiture, or liability incurred under the repealed or amended law, unless the repealed or amended provision shall so expressly provide. After the effective date of this act, all laws repealed or amended by this act must be taken and treated as remaining in full force and effect for the purpose of sustaining any pending or vested right, civil action, special proceeding, criminal prosecution, or appeal existing as of the effective date of this act, and for the enforcement of rights, duties, penalties, forfeitures, and liabilities as they stood under the repealed or amended laws.
SECTION 16. This act takes effect on October 1, 2014. /
Renumber sections to conform.
Amend title to conform.
Senator MALLOY was recognized to speak on the committee amendment.
Senator HUTTO spoke on the committee amendment.
Amendment No. 1
Senator MALLOY proposed the following Amendment No. 1 (JUD0137.014), which was tabled:
Amend the bill, as and if amended, page [137-26], by striking lines 30-36, and inserting:
/ (2) After the person is released from prison, the person shall enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle for three years when 'great bodily injury' results and for life when a death occurs. /
Renumber sections to conform.
Amend title to conform.
Senator MALLOY explained the amendment.
Senator HUTTO spoke on the amendment.
Senator HUTTO moved to lay the amendment on the table.
The "ayes" and "nays" were demanded and taken, resulting as follows:
Ayes 30; Nays 9; Abstain 1
AYES
Alexander Allen Bennett
Bright Campbell Campsen
Cleary Coleman Corbin
Courson Cromer Fair
Hayes Hembree Hutto
Leatherman Lourie Martin, Larry
Martin, Shane Massey Nicholson
O'Dell Peeler Rankin
Reese Setzler Shealy
Thurmond Turner Young
Total--30
NAYS
Ford Jackson Johnson
Malloy Matthews McElveen
McGill Scott Williams
Total--9
ABSTAIN
Bryant
Total--1
The amendment was laid on the table.
Amendment No. 2
Senator HUTTO proposed the following Amendment No. 2 (JUD0137.016), which was adopted:
Amend the bill, as and if amended, by striking, beginning on page [137-15], SECTION 8 in its entirety, and inserting:
/ SECTION 8. Section 56-5-2941 of the 1976 Code is amended to read:
"Section 56-5-2941. (A) Except as otherwise provided in this section, in addition to the penalties required and authorized to be imposed against a person violating the provisions of Section 56-5-2930, 56-5-2933, or 56-5-2945, or violating the provisions of another law of any other another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or other drugs the The Department of Motor Vehicles must shall require the a person, if he is a subsequent offender and who is a resident of this State, and who has violated the provisions of Section 56-5-2930, 56-5-2933, 56-5-2945, 56-5-2947, or a law of another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or other drugs, to have installed on any motor vehicle the person drives an ignition interlock device designed to prevent driving of the motor vehicle if the person has consumed alcoholic beverages. This section does not apply to a person convicted of a first offense violation of Section 56-5-2930 or 56-5-2933, unless the person submitted to a breath test pursuant to Section 56-5-2950 and had an alcohol concentration of twelve one hundredths of one percent or more. The Department of Motor Vehicles department may waive the requirements of this section if it finds the department determines that the offender person has a medical condition that makes him the person incapable of properly operating the installed device. If the department grants a medical waiver, the department shall suspend the person's driver's license for the length of time that the person would have been required to hold an ignition interlock restricted license. The department may withdraw the waiver at any time that the department becomes aware that the person's medical condition has improved to the extent that the person has become capable of properly operating an installed device. The department also shall require a person who has enrolled in the Ignition Interlock Device Program in lieu of the remainder of a driver's license suspension or denial of the issuance of a driver's license or permit to have an ignition interlock device installed on any motor vehicle the person drives.
The length of time that an interlock a device is required to be affixed to a motor vehicle following the completion of a period of license suspension imposed on the offender person is two years for a second offense, three years for a third offense, and the remainder of the offender's person's life for a fourth or subsequent offense is set forth in Sections 56-1-286, 56-5-2945, 56-5-2947, 56-5-2951, and 56-5-2990.
(B) Notwithstanding the pleadings, for purposes of a second or a subsequent offense, the specified length of time that an interlock a device is required to be affixed to a motor vehicle is based on the Department of Motor Vehicle's records for offenses pursuant to Section 56-1-286, 56-5-2930, 56-5-2933, or 56-5-2945, 56-5-2947, 56-5-2950, or 56-5-2951.
(B)(C) If a person who is a subsequent offender and a resident of this State is convicted of violating the provisions of a law of any other another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or other drugs, and, as a result of the conviction, the person is subject to an ignition interlock device requirement in the other state, the person is subject to the requirements of this section for the length of time that would have been required for an offense committed in South Carolina, or for the length of time that is required by the other state, whichever is longer.
(C)(D) If a person from another state becomes a resident of South Carolina while subject to an ignition interlock device requirement in another state, the person may only obtain a South Carolina driver's license if the person enrolls in the South Carolina ignition interlock device program Ignition Interlock Device Program pursuant to this section. The person is subject to the requirements of this section for the length of time that would have been required for an offense committed in South Carolina, or for the length of time that is required by the other state, whichever is longer.
(D)(E) The offender shall person must be subject to an Ignition Interlock Device Point System managed by the Department of Probation, Parole and Pardon Services. An offender receiving A person accumulating a total of:
(1) two points or more, but less than three points, will must have their the length of time that the interlock device is required extended by two months.;
(2) An offender receiving a total of three points or more, but less than four points, will must have their the length of time that the interlock device is required extended by four months, and must shall submit to a substance abuse assessment pursuant to Section 56-5-2990, and shall successfully complete the plan of education and treatment, or both, as recommended by the certified substance abuse program. Should the individual person not complete the recommended plan, or not make progress toward completing the plan, the Department of Motor Vehicles must shall suspend the individual's driver's person's ignition interlock restricted license until the plan is completed or progress is being made toward completing the plan.;
(3) An offender receiving a total of four points or more shall must have their the person's ignition interlock restricted license suspended for a period of one year six months, and shall submit to a substance abuse assessment pursuant to Section 56-5-2990, and shall successfully complete the plan of education and treatment, or both, as recommended by the certified substance abuse program. Completion of the plan is mandatory as a condition of reinstatement of the person's driving privileges Should the person not complete the recommended plan or not make progress toward completing the plan, the Department of Motor Vehicles shall leave the person's ignition interlock restricted license in suspended status, or, if the license has already been reinstated following the six-month suspension, shall resuspend the person's ignition interlock restricted license until the plan is completed or progress is being made toward completing the plan. The Department of Alcohol and Other Drug Abuse Services is responsible for notifying the Department of Motor Vehicles of an individual's a person's completion and compliance with education and treatment programs. Upon reinstatement of driving privileges following the six-month suspension, the Department of Probation, Parole and Pardon Services shall reset the person's point total to zero points, and the person shall complete the remaining period of time on the ignition interlock device.
(E)(F) The cost of the interlock device must be borne by the offender person. However, if the offender believes he person is indigent and cannot afford the cost of the ignition interlock device, the offender person may submit an affidavit of indigency to the Department of Probation, Parole and Pardon Services for a determination of indigency as it pertains to the cost of the ignition interlock device. The affidavit of indigency form must be made publicly accessible on the Department of Probation, Parole and Pardon Services' Internet web site. If the Department of Probation, Parole and Pardon Services determines that the offender person is indigent as it pertains to the ignition interlock device, it the Department of Probation, Parole and Pardon Services may authorize an interlock a device to be affixed to the motor vehicle and the cost of the initial installation and standard use of the ignition interlock device to be paid for by the Ignition Interlock Device Fund managed by the Department of Probation, Parole and Pardon Services. Funds remitted to the Department of Probation, Parole and Pardon Services for the Ignition Interlock Device Fund also may be used by the Department of Probation, Parole and Pardon Services to support the Ignition Interlock Device Program. For purposes of this section, a person is indigent if the person is financially unable to afford the cost of the ignition interlock device. In making a determination whether a person is indigent, all factors concerning the person's financial conditions should be considered including, but not limited to, income, debts, assets, number of dependants dependents claimed for tax purposes, living expenses, and family situation. A presumption that the person is indigent is created if the person's net family income is less than or equal to the poverty guidelines established and revised annually by the United States Department of Health and Human Services published in the Federal Register. 'Net income' means gross income minus deductions required by law. The determination of indigency is subject to periodic review at the discretion of the Department of Probation, Parole and Pardon Services.
(F)(G) The ignition interlock service provider must shall collect and remit monthly to the Ignition Interlock Device Fund a fee as determined by the Department of Probation, Parole and Pardon Services not to exceed three hundred sixty thirty dollars per year month for each year month the person is required to drive a vehicle with an ignition interlock a device. Any A ignition service provider failing who fails to properly remit funds to the Ignition Interlock Device Fund may be decertified as an ignition interlock a service provider by the Department of Probation, Parole and Pardon Services. If a service provider is decertified for failing to remit funds to the Ignition Interlock Device Fund, the cost for removal and replacement of an ignition interlock a device must be borne by the service provider.
(G)(H)(1) The offender must person shall have the interlock device inspected every sixty days to verify that the device is affixed to the motor vehicle and properly operating, and to allow for the preparation of an ignition interlock device inspection report by the service provider indicating the offender's person's alcohol content at each attempt to start and running re-test retest during each sixty-day period. Failure of the person to have the interlock device inspected every sixty days must result in one ignition interlock device point.
(2) Only a service provider authorized by the Department of Probation, Parole and Pardon Services to perform inspections on ignition interlock devices may conduct inspections. The service provider immediately must shall report any devices that fail inspection to the Department of Probation, Parole and Pardon Services. The report must contain the person's name of the offender, identify the vehicle upon which the failed device is installed, and the reason for the failed inspection, and.
(3) If the inspection report reflects that the person has failed to complete a running retest, the person must be assessed one ignition interlock device point.
(4) The inspection report must indicate the offender's person's alcohol content at each attempt to start and running re-test retest during each sixty-day period. Failure of the offender to have the interlock device inspected every sixty days will result in one ignition interlock device point. Upon review of the ignition interlock device inspection report, if the report reflects that the offender attempted to start the motor vehicle with an alcohol concentration of two one-hundredths of one percent or more, the offender is assessed one-half interlock device point. Upon review of the interlock device inspection report, if If the report reflects that the offender person violated a running re-test retest by having an alcohol concentration of:
(a) between two one-hundredths of one percent or more and but less than four one-hundredths of one percent, the offender is person must be assessed one-half ignition interlock device point.;
(b) Upon review of the interlock device inspection report, if the report reflects that the offender person violated a running re-test retest by having an alcohol concentration between four one-hundredths of one percent or more and but less than fifteen one-hundredths of one percent, the offender is person must be assessed one ignition interlock device point.; or
(c) Upon review of the interlock device inspection report, if the report reflects that the offender person violated a running re-test retest by having an alcohol concentration above fifteen one-hundredths of one percent or more, the offender is person must be assessed two ignition interlock device points.
(5) An individual A person may appeal any interlock device points received to an administrative hearing officer with the Department of Probation, Parole and Pardon Services through a process established by the Department of Probation, Parole and Pardon Services. The administrative hearing officer's decision on appeal shall be is final and no appeal from such decision shall be is allowed.
(H)(I) Ten Five years from the date of the person's last conviction driver's license reinstatement and every five years thereafter a fourth or subsequent offender whose license has been reinstated pursuant to Section 56-1-385 may apply to the Department of Probation, Parole and Pardon Services for removal of the ignition interlock device and the removal of the restriction from his the person's driver's license. The Department of Probation, Parole and Pardon Services may, for good cause shown, remove the device and remove the restriction notify the Department of Motor Vehicles that the person is eligible to have the restriction removed from the offender's person's license.
(I)(J)(1) Except as otherwise provided in this section, it is unlawful for a person issued a driver's license with an ignition interlock restriction who is subject to the provisions of this section to drive a motor vehicle that is not equipped with a properly operating, certified ignition interlock device. A person who violates this section must be punished in the manner provided by law subsection:
(a) for a first offense, is guilty of a misdemeanor, and, upon conviction, must be fined not less than five hundred dollars, or be imprisoned not more than ninety days, or be confined to the person's place of residence pursuant to the Home Detention Act for not more than ninety days. The person must have the length of time that the ignition interlock device is required extended by six months;
(b) for a second offense, is guilty of a misdemeanor, and, upon conviction, must be fined not less than one thousand dollars, or be imprisoned not more than three years, or be confined to the person's place of residence pursuant to the Home Detention Act for one year. The person must have the length of time that the ignition interlock device is required extended by one year; and
(c) for a third or subsequent offense, is guilty of a felony, and, upon conviction, must be fined not less than five thousand dollars, or be imprisoned not more than ten years, or be confined to the person's place of residence pursuant to the Home Detention Act for three years. The person must have the length of time that the ignition interlock device is required extended by three years.
(2) No portion of the minimum sentence imposed pursuant to this subsection may be suspended.
(3) Notwithstanding any other provision of law, a first or second offense punishable pursuant to this subsection may be tried in summary court.
(J)(K)(1) An offender that A person who is required in the course and scope of his the person's employment to drive a motor vehicle owned by the offender's person's employer may drive his the employer's motor vehicle without installation of an ignition interlock device, provided that the offender's person's use of the employer's motor vehicle is solely for the employer's business purposes. This subsection does not apply to an offender a person who is self-employed or to an offender a person who is employed by a business owned in whole or in part by the offender person or a member of the offender's person's household or immediate family unless during the defense of a criminal charge, the court finds that the vehicle's ownership by the business serves a legitimate business purpose and that titling and registration of the vehicle by the business was not done to circumvent the intent of this section.
(2) Whenever the person operates the employer's vehicle pursuant to this subsection, the person shall have with the person a copy of the Department of Motor Vehicle's form specified by Section 56-1-400(B).
(3) This subsection will be construed in parallel with the requirements of subsection 56-1-400(B). A waiver issued pursuant to this subsection will be subject to the same review and revocation as described in subsection 56-1-400(B).
(K)(L) It is unlawful for a person to tamper with or disable, or attempt to tamper with or disable, an ignition interlock device installed on a motor vehicle pursuant to this section. Obstructing or obscuring the camera lens of an ignition interlock device constitutes tampering. A person who violates this subsection is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days, or both.
(L)(M) It is unlawful for a person to knowingly rent, lease, or otherwise provide an offender a person who is subject to the provisions of this section with a motor vehicle without a properly operating, certified ignition interlock device. A person who violates this subsection is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days, or both.
(M)(N) It is unlawful for an offender a person who is subject to the provisions of this section to solicit or request another person, or for a person to solicit or request another person on behalf of an offender a person who is subject to the provisions of this section, to engage an ignition interlock device to start a motor vehicle with a device installed pursuant to this section. A person who violates this subsection is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days, or both.
(N)(O) It is unlawful for another person to engage an ignition interlock device to start a motor vehicle with a device installed pursuant to this section. A person who violates this subsection is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days, or both.
(O)(P) Only ignition interlock devices certified by the Department of Probation, Parole and Pardon Services may be used to fulfill the requirements of this section.
(1) The Department of Probation, Parole and Pardon Services must shall certify whether a device meets the accuracy requirements and specifications provided in guidelines or regulations adopted by the National Highway Traffic Safety Administration, as amended from time to time. All devices certified to be used in South Carolina must be set to prohibit the starting of a motor vehicle when an alcohol concentration of two one-hundredths of one percent or more is measured and all running re-tests retests must record violations of an alcohol concentration of two one-hundredths of one percent or more, and must capture a photographic image of the driver as the driver is operating the ignition interlock device. The photographic images recorded by the ignition interlock device may be used by the Department of Probation, Parole and Pardon Services to aid in the Department of Probation, Parole and Pardon Services' management of the Ignition Interlock Device Program; however, neither the Department of Probation, Parole and Pardon Services, the Department of Probation, Parole and Pardon Services' employees, nor any other political subdivision of this State may be held liable for any injury caused by a driver or other person who operates a motor vehicle after the use or attempted use of an ignition interlock device.
(2) The Department of Probation, Parole and Pardon Services shall maintain a current list of certified ignition interlock devices and their manufacturers. The list must be updated at least quarterly. If a particular certified device fails to continue to meet federal requirements, the device must be decertified, may not be used until it is compliant with federal requirements, and must be replaced with a device that meets federal requirements. The cost for removal and replacement must be borne by the manufacturer of the noncertified device.
(3) Only ignition interlock installers certified by the Department of Probation, Parole and Pardon Services may install and service ignition interlock devices required pursuant to this section. The Department of Probation, Parole and Pardon Services shall maintain a current list of vendors that are certified to install the devices.
(P)(Q) In addition to availability under the Freedom of Information Act, any Department of Probation, Parole and Pardon Services policy concerning ignition interlock devices must be made publicly accessible on the Department of Probation, Parole and Pardon Service's Services' Internet web site. Information obtained by the Department of Probation, Parole and Pardon Services and ignition interlock service providers regarding a person's participation in the Ignition Interlock Device Program is to be used for internal purposes only and is not subject to the Freedom of Information Act. A person participating in the Ignition Interlock Device Program or the person's family member may request that the Department of Probation, Parole and Pardon Services provide the person or family member with information obtained by the department and ignition interlock service providers. The Department of Probation, Parole and Pardon Services may release the information to the person or family member at the department's discretion. The Department of Probation, Parole and Pardon Services and ignition interlock service providers may retain information regarding a person's participation in the Ignition Interlock Device Program for a period not to exceed eighteen months from the date of the person's completion of the Ignition Interlock Device Program.
(Q)(R) The Department of Probation, Parole and Pardon Services shall develop policies including, but not limited to, the certification, use, maintenance, and operation of ignition interlock devices and the Ignition Interlock Device Fund." /
Renumber sections to conform.
Amend title to conform.
Senator HUTTO explained the amendment.
Senator MALLOY spoke on the amendment.
The "ayes" and "nays" were demanded and taken, resulting as follows:
Ayes 42; Nays 0; Abstain 1
AYES
Alexander Allen Bennett
Bright Campbell Campsen
Cleary Coleman Corbin
Courson Cromer Davis
Fair Ford Grooms
Hayes Hembree Hutto
Jackson Johnson Leatherman
Lourie Malloy Martin, Larry
Martin, Shane Massey Matthews
McElveen McGill Nicholson
O'Dell Peeler Rankin
Reese Scott Setzler
Shealy Sheheen Thurmond
Turner Williams Young
Total--42
NAYS
Total--0
ABSTAIN
Bryant
Total--1
Amendment No. 3
Senator MASSEY proposed the following Amendment No. 3 (JUD0137.006), which was adopted:
Amend the bill, as and if amended, page [137-21], by striking lines 1-23.
/ (a) for a first offense, is guilty of a misdemeanor, and, upon conviction, must be fined not less than one thousand dollars or imprisoned not more than one year. The person must have the length of time that the ignition interlock device is required extended by six months;
(b) for a second offense, is guilty of a misdemeanor, and, upon conviction, must be fined not less than five thousand dollars or imprisoned not more than three years. The person must have the length of time that the ignition interlock device is required extended by one year; and
(c) for a third or subsequent offense, is guilty of a felony, and, upon conviction, must be fined not less than ten thousand dollars or imprisoned not more than ten years. The person must have the length of time that the ignition interlock device is required extended by three years.
(2) No portion of the minimum sentence imposed pursuant to this subsection may be suspended.
(3) Notwithstanding any other provision of law, a first or second offense punishable pursuant to this subsection may be tried in summary court. /
Renumber sections to conform.
Amend title to conform.
Senator MASSEY explained the amendment.
Amendment No. 4
Senators CROMER, SHEALY, MASSEY, LOURIE, SETZLER, LARRY MARTIN and FAIR proposed the following Amendment No. 4 (JUD0137.018), which was adopted:
Amend the bill, as and if amended, by adding an appropriately numbered SECTION to read:
/ SECTION __. This act may be cited as "Emma's Law". /
Renumber sections to conform.
Amend title to conform.
Senator MASSEY explained the amendment.
Senator LOURIE spoke on the amendment.
Amendment No. 5
Senator MALLOY proposed the following Amendment No. 5 (JUD0137.020), which was adopted:
Amend the bill, as and if amended, page [137-22], by striking lines 11-17 and inserting:
/ (L)(M) It is unlawful for a person to knowingly rent, lease, or otherwise provide an offender a person who is subject to this section with a motor vehicle without a properly operating, certified ignition interlock device. This subsection does not apply if the person began the lease contract period for the motor vehicle prior to the person's arrest for a first offense violation of Section 56-5-2930 or Section 56-5-2933. A person who violates this subsection is guilty of a misdemeanor, and, upon conviction, must be fined not more than five hundred dollars or imprisoned not more than thirty days, or both. /
Renumber sections to conform.
Amend title to conform.
Senator MALLOY explained the amendment.
Amendment No. 6
Senator MALLOY proposed the following Amendment No. 6 (JUD0137.021), which was tabled:
Amend the bill, as and if amended, page [137-15], by striking lines 1-4.
Amend the bill further, as and if amended, page [137-15], by striking lines 40-43, and page [137-16], by striking lines 1-2, and inserting:
/ beverages. This section does not apply to a person convicted of a first offense violation of Section 56-5-2930 or 56-5-2933. The Department of Motor Vehicles /
Amend the bill further, as and if amended, page [137-39], by striking lines 16-43, and page [137-40], by striking lines 1-15, and inserting:
/ (2) For a first offense, a person's driver's license must be suspended six months. /
Renumber sections to conform.
Amend title to conform.
Senator MALLOY explained the amendment.
Senator HUTTO spoke on the amendment.
Senator HUTTO moved to lay the amendment on the table.
The "ayes" and "nays" were demanded and taken, resulting as follows:
Ayes 36; Nays 5; Abstain 1
AYES
Alexander Bennett Bright
Campbell Campsen Cleary
Coleman Corbin Courson
Cromer Davis Fair
Grooms Hayes Hembree
Hutto Jackson Leatherman
Lourie Martin, Larry Martin, Shane
Massey Matthews McElveen
McGill Nicholson O'Dell
Peeler Rankin Setzler
Shealy Sheheen Thurmond
Turner Williams Young
Total--36
NAYS
Allen Johnson Malloy
Reese Scott
Total--5
ABSTAIN
Bryant
Total--1
The amendment was laid on the table.
Amendment No. 7
Senator MALLOY proposed the following Amendment No. 7 (JUD0137.022), which was tabled:
Amend the bill, as and if amended, page [137-14], by striking lines 32-43, and page [137-15], by striking lines 1-15, and inserting:
Amend the bill further, as and if amended, page [137-15], by striking lines 25-43, and page [137-16], by striking lines 1-19, and inserting:
/ "Section 56-5-2941.(A) Except as otherwise provided in this section, in addition to the penalties required and authorized to be imposed against a person violating the provisions of Section 56-5-2930, 56-5-2933, or 56-5-2945, or violating the provisions of another law of any other another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or other drugs Pursuant to Sections 56-5-2945 and 56-5-2990, the Department of Motor Vehicles must shall require the a person, if he is a subsequent offender and who is a resident of this State, and who has violated the provisions of Section 56-5-2930, 56-5-2933, 56-5-2945, 56-5-2947, or a law of another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or other drugs, to have installed on any motor vehicle the person drives an ignition interlock device designed to prevent driving of the motor vehicle if the person has consumed alcoholic beverages. This section does not apply to a person convicted of a first offense violation of Section 56-5-2930 or 56-5-2933, unless the person submitted to a breath test pursuant to Section 56-5-2950 and had an alcohol concentration of fifteen one hundredths of one percent or more. The Department of Motor Vehicles department may waive the requirements of this section if it finds the department determines that the offender person has a medical condition that makes him the person incapable of properly operating the installed device. If the department grants a medical waiver, the department shall suspend the person's driver's license for the length of time that the person would have been required to hold an ignition interlock restricted license pursuant to Sections 56-5-2945 and 56-5-2990. The department may withdraw the waiver at any time that the department becomes aware that the person's medical condition has improved to the extent that the person has become capable of properly operating an installed device. The department also shall require a person who has enrolled in the Ignition Interlock Device Program in lieu of the remainder of a driver's license suspension or denial of the issuance of a driver's license or permit pursuant to Section 56-1-286 or 56-5-2951 to have an ignition interlock device installed on any motor vehicle the person drives.
The length of time that an interlock a device is required to be affixed to a motor vehicle following the completion of a period of license suspension imposed on the offender person is two years for a second offense, three years for a third offense, and the remainder of the offender's person's life for a fourth or subsequent offense is set forth in Sections 56-1-286, 56-5-2945, 56-5-2947, 56-5-2951, and 56-5-2990. /
Amend the bill further, as and if amended, page [137-39], by striking lines 16-43, and page [137-40], by striking lines 1-15, and inserting:
/ (2) For a first offense:
(a) If a person refused to submit to a breath test pursuant to Section 56-5-2950, the person's driver's license must be suspended six months. The person is not eligible for a provisional license pursuant to Article 7, Chapter 1, Title 56. In lieu of serving the remainder of the suspension, the person may enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle equal to the length of time remaining on the person's suspension. If the length of time remaining is less than three months, the ignition interlock device is required to be affixed to the motor vehicle for three months. Once a person has enrolled in the Ignition Interlock Device Program and obtained an ignition interlock restricted license, the person is subject to Section 56-5-2941 and cannot subsequently choose to serve the suspension.
(b) If a person submitted to a breath test pursuant to Section 56-5-2950 and had an alcohol concentration of less than fifteen one hundredths of one percent, the person's driver's license must be suspended six months. The person is eligible for a provisional license pursuant to Article 7, Chapter 1, Title 56. In lieu of serving the remainder of the suspension, the person may enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle equal to the length of time remaining on the person's suspension. If the length of time remaining is less than three months, the ignition interlock device is required to be affixed to the motor vehicle for three months. Once a person has enrolled in the Ignition Interlock Device Program and obtained an ignition interlock restricted license, the person is subject to Section 56-5-2941 and cannot subsequently choose to serve the suspension.
(c) If a person submitted to a breath test pursuant to Section 56-5-2950 and had an alcohol concentration of fifteen one hundredths of one percent or more, the person shall enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle for six months. The person is not eligible for a provisional license pursuant to Article 7, Chapter 1, Title 56. /
Renumber sections to conform.
Amend title to conform.
Senator MALLOY explained the amendment.
Senator HUTTO spoke on the amendment.
Senator HUTTO moved to lay the amendment on the table.
The "ayes" and "nays" were demanded and taken, resulting as follows:
Ayes 39; Nays 3; Abstain 1
AYES
Alexander Bennett Bright
Campbell Campsen Cleary
Coleman Corbin Courson
Cromer Davis Fair
Grooms Hayes Hembree
Hutto Jackson Johnson
Leatherman Lourie Martin, Larry
Martin, Shane Massey Matthews
McElveen McGill Nicholson
O'Dell Peeler Rankin
Reese Scott Setzler
Shealy Sheheen Thurmond
Turner Williams Young
Total--39
NAYS
Allen Ford Malloy
Total--3
ABSTAIN
Bryant
Total--1
The amendment was laid on the table.
Senator MALLOY asked unanimous consent to make a motion to take up Amendment No. 9 for immediate consideration.
There was no objection.
Amendment No. 9
Senator MALLOY proposed the following Amendment No. 9 (JUD0137.023), which was adopted:
Amend the bill, as and if amended, page [137-3], by striking lines 30-42, and page [137-4], by striking lines 1-17, and inserting:
/ (F) If Except as provided in subsection (H), if a person refuses upon the request of the primary investigating officer officer's request to submit to chemical tests as provided in subsection (C), the department must shall suspend his the person's license, permit, or any nonresident operating privilege, or deny the issuance of a license or permit to him the person for:
(1) six months; or
(2) one year, if the person, within the five three years preceding the violation of this section, has been previously convicted of violating Section 56-5-2930, 56-5-2933, or 56-5-2945, or any other a law of this State or another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or another drug other drugs, or the person has had a previous suspension imposed pursuant to Section 56-1-286, 56-5-2950, or 56-5-2951, or 56-5-2990.
(G) If Except as provided in subsection (H), if a person submits to a chemical test and the test result indicates an alcohol concentration of two one-hundredths of one percent or more, the department must shall suspend his the person's license, permit, or any nonresident operating privilege, or deny the issuance of a license or permit to him the person for:
(1) three months; or
(2) six months, if the person, within the five three years preceding the violation of this section, has been previously convicted of violating Section 56-5-2930, 56-5-2933, or 56-5-2945, or any other a law of this State or another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or another drug other drugs, or the person has had a previous suspension imposed pursuant to Section 56-1-286, 56-5-2950, or 56-5-2951, or 56-5-2990. /
Renumber sections to conform.
Amend title to conform.
Senator MALLOY explained the amendment.
Amendment No. 8
Senator MALLOY proposed the following Amendment No. 8 (JUD0137.015), which was tabled:
Amend the bill, as and if amended, by adding an appropriately numbered section to read:
/ SECTION __. Article 7, Chapter 1, Title 56 of the 1976 Code is repealed. /
Amend the bill further, as and if amended, page [137-15], by striking lines 25-43, and page [137-16], by striking lines 1-19, and inserting:
/ "Section 56-5-2941.(A) Except as otherwise provided in this section, in addition to the penalties required and authorized to be imposed against a person violating the provisions of Section 56-5-2930, 56-5-2933, or 56-5-2945, or violating the provisions of another law of any other another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or other drugs Pursuant to Sections 56-5-2945 and 56-5-2990, the Department of Motor Vehicles must shall require the a person, if he is a subsequent offender and who is a resident of this State, and who has violated the provisions of Section 56-5-2930, 56-5-2933, 56-5-2945, 56-5-2947, or a law of another state that prohibits a person from driving a motor vehicle while under the influence of alcohol or other drugs, to have installed on any motor vehicle the person drives an ignition interlock device designed to prevent driving of the motor vehicle if the person has consumed alcoholic beverages. The Department of Motor Vehicles department may waive the requirements of this section if it finds the department determines that the offender person has a medical condition that makes him the person incapable of properly operating the installed device. If the department grants a medical waiver, the department shall suspend the person's driver's license for the length of time that the person would have been required to hold an ignition interlock restricted license pursuant to Sections 56-5-2945 and 56-5-2990. The department may withdraw the waiver at any time that the department becomes aware that the person's medical condition has improved to the extent that the person has become capable of properly operating an installed device. The department also shall require a person who has enrolled in the Ignition Interlock Device Program in lieu of the remainder of a driver's license suspension or denial of the issuance of a driver's license or permit pursuant to Section 56-1-286 or 56-5-2951 to have an ignition interlock device installed on any motor vehicle the person drives.
The length of time that an interlock a device is required to be affixed to a motor vehicle following the completion of a period of license suspension imposed on the offender person is two years for a second offense, three years for a third offense, and the remainder of the offender's person's life for a fourth or subsequent offense is set forth in Sections 56-1-286, 56-5-2945, 56-5-2947, 56-5-2951, and 56-5-2990. /
Amend the bill further, as and if amended, page [137-39], by striking lines 16-43, and page [137-40], by striking lines 1-15, and inserting:
/ (2) For a first offense, a person shall enroll in the Ignition Interlock Device Program pursuant to Section 56-5-2941, end the suspension, and obtain an ignition interlock restricted license pursuant to Section 56-1-400. The ignition interlock device is required to be affixed to the motor vehicle for six months. /
Renumber sections to conform.
Amend title to conform.
Senator MALLOY explained the amendment.
Senator HUTTO moved to lay the amendment on the table.
The "ayes" and "nays" were demanded and taken, resulting as follows:
Ayes 34; Nays 8; Abstain 1
AYES
Alexander Allen Bennett
Bright Campbell Campsen
Cleary Coleman Corbin
Courson Cromer Davis
Fair Grooms Hayes
Hembree Hutto Jackson
Leatherman Lourie Martin, Larry
Martin, Shane Massey Matthews
McGill Nicholson O'Dell
Peeler Rankin Setzler
Shealy Thurmond Turner
Young
Total--34
NAYS
Ford Johnson Malloy
McElveen Reese Scott
Sheheen Williams
Total--8
ABSTAIN
Bryant
Total--1
The amendment was laid on the table.
Amendment No. 11
Senator HUTTO proposed the following Amendment No. 11 (JUD0137.024), which was adopted:
Amend the bill, as and if amended, page [137-12], by striking lines 3-42, page [137-13], by striking lines 1-43, and page [137-14], by striking lines 1-11, and inserting:
/ SECTION 3. Section 56-1-460 of the 1976 Code is amended to read:
"Section 56-1-460. (A)(1) Except as provided in item (2), a person who drives a motor vehicle on any a public highway of this State when his the person's license to drive is canceled, suspended, or revoked must, upon conviction, be punished as follows:
(a) for a first offense, fined three hundred dollars or imprisoned for up to thirty days, or both;
(b) for a second offense, fined six hundred dollars or imprisoned for up to sixty consecutive days, or both; and
(c) for a third and or subsequent offense, fined one thousand dollars, and imprisoned for up to ninety days or confined to a person's place of residence pursuant to the Home Detention Act for not less than up to ninety days nor more than six months. No portion of a term of imprisonment or confinement under home detention may be suspended by the trial judge except when the court is suspending a term of imprisonment upon successful completion of the terms and conditions of confinement under home detention. For purposes of this item, a person sentenced to confinement pursuant to the Home Detention Act is required to pay for the cost of such confinement.
(d) Notwithstanding the provisions of Sections 22-3-540, 22-3-545, 22-3-550, and 14-25-65, an offense punishable under this item may be tried in magistrates or municipal court.
(e)(i) A person convicted of a first or second offense of this item, as determined by the records of the department, and who is employed or enrolled in a college or university at any time while his the person's driver's license is suspended pursuant to this item, may apply for a route restricted driver's license permitting him the person to drive only to and from work or his the person's place of education and in the course of his the person's employment or education during the period of suspension. The department may issue the route restricted driver's license only upon a showing by the person that he the person is employed or enrolled in a college or university and that he the person lives further than one mile from his the person's place of employment or place of education.
(ii) When the department issues a route restricted driver's license, it shall designate reasonable restrictions on the times during which and routes on which the person may operate a motor vehicle. A person holding a route restricted driver's license pursuant to this item must shall report to the department immediately any change in his the person's employment hours, place of employment, status as a student, or residence.
(iii) The fee for a route restricted driver's license issued pursuant to this item is one hundred dollars, but no additional fee is due when changes occur in the place and hours of employment, education, or residence. Of this fee, eighty dollars must be placed by the Comptroller General into a special restricted account to be used by the Department of Motor Vehicles to defray its the Department of Motor Vehicle's expenses. The remainder of the fees collected pursuant to this item must be credited to the Department of Transportation State Non-Federal Aid Highway Fund.
(iv) The operation of a motor vehicle outside the time limits and route imposed by a route restricted license by the person issued that license is a violation of subsection (A)(1).
(2) A person who drives a motor vehicle on any a public highway of this State when his the person's license has been suspended or revoked pursuant to the provisions of Section 56-5-2990 or 56-5-2945 must, upon conviction, be punished as follows:
(a) for a first offense, fined three hundred dollars or imprisoned for not less than ten nor more than thirty days;
(b) for a second offense, fined six hundred dollars or imprisoned for not less than sixty days nor more than six months;
(c) for a third and or subsequent offense, fined one thousand dollars and imprisoned for not less than six months nor more than three years;
(d) noNo portion of the minimum sentence imposed under pursuant to this item may be suspended.
(C) One hundred dollars of each fine imposed pursuant to this section must be placed by the Comptroller General into a special restricted account to be used by the Department of Public Safety for the Highway Patrol." /
Renumber sections to conform.
Amend title to conform.
Senator HUTTO explained the amendment.
There being no further amendments, the question then was the second reading of the Bill.
Senator MALLOY spoke on the Bill.
Senator LOURIE spoke on the Bill.
The "ayes" and "nays" were demanded and taken, resulting as follows:
Ayes 41; Nays 0; Abstain 1
AYES
Alexander Allen Bennett
Bright Campbell Campsen
Cleary Coleman Corbin
Courson Cromer Davis
Fair Ford Grooms
Hayes Hembree Hutto
Jackson Johnson Leatherman
Lourie Malloy Martin, Larry
Martin, Shane Massey McElveen
McGill Nicholson O'Dell
Peeler Rankin Reese
Scott Setzler Shealy
Sheheen Thurmond Turner
Williams Young
Total--41
NAYS
Total--0
ABSTAIN
Bryant
Total--1
The Bill was read the second time, passed and ordered to a third reading.
The Bill was returned to the status of Special Order on the Calendar.
Statement by Senator BRYANT
Our business is researching the possibility of installing interlocking devices. Therefore, I have recused myself from voting on S. 137 and all amendments to this Bill.
| 2015-08-31T13:19:05 |
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|
https://www.anl.gov/topic/advanced-photon-source
|
# Argonne National Laboratory
## Filter Results
• ### Argonne’s Velociprobe takes rapid steps forward
Recent studies have taken advantage of the Velociprobe’s blazing fast scanning speed to achieve high-resolution views of large sections of important devices.
• ### How sweet: Researchers find what makes chocolate melt in your mouth
Scientists use X-rays to see the true nature of chocolate.
• ### Scientists discover “electron equivalents” in colloidal systems
Scientists find unusual behaviors in colloidal crystals.
• ### Argonne takes the guesswork out of electrospinning
Capturing real-time data as nanofibers form makes the technique more affordable and effective.
• ### New X-ray imaging approach could boost nanoscale resolution for Advanced Photon Source Upgrade
A long-standing problem in optics holds that an improved resolution in imaging is offset by a loss in the depth of focus. Now, scientists are joining computation with X-ray imaging as they develop a new and exciting technique to bypass this limitation.
| 2020-01-28T11:11:01 |
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|
https://bison.inl.gov/Documentation/source/auxkernels/tensor_mechanics/UO2IsotropicDislocationDensity.aspx
|
# UOvar element = document.getElementById("moose-equation-89954227-ca13-4d37-b330-87c13e2b250b");katex.render("_2", element, {displayMode:false,throwOnError:false}); Isotropic Dislocation Density AuxKernel
Calculates an effective isotropic dislocation density for UO2 fuel by smearing the sum of the dislocations across all of the slip planes; uses a Kocks-type dislocation density model.
## Description
This auxkernel is used to calculate the dislocation density in UO fuel as a function of burnup. The calculated dislocation density is intended to be used in conjunction with a simplified cluster dynamics model that describes the evolution of intra-grannular bubbles in the fuel. The dislocation density measure calculated in this auxkernel does not contribute to the strain.
This auxkernel model was developed by simplifying the Continuum Dislocation Dynamics (CDD) model developed by Li et.al. to calculate a smeared-out effective total dislocation density (Li et al., 2014). The effective total dislocation density is treated as the sum of the dislocation densities on each of the slip planes in the crystal. The prominent simplifying assumption is that the density of immobile dislocation is comparable to the density of mobile dislocations. Applying this assumption, the evolution of dislocation density equations reduces to the form of the classical Kocks' dislocation density model while retaining the physical basis of the parameters (Kocks, 1976). (1)
The analytical solution of Eq. 1 is reformulated as a function of burnup, , by taking the dislocation driving force, , to be proportional to burnup. The dislocation density expression is defined as (2) where the coefficients relate to physical lattice parameters from the CDD model, as shown in the table below, and the initial dislocation density is taken as = 6.0e13 from Noirot (2006). The coefficient includes a conversion factor from time (sec) to burnup in (GWd/tU) which is on the order of 10. The values of the coefficients in Eq. 2 were determined by fitting the model to experimental data for dislocation density under increasing burnup (Nogita and Une, 1994).
Table 1: Values for coefficients in the isotropic dislocation density expression ( Eq. 2)
ParameterFitted ValuePhysical Interpretation
$\alpha_1 / \vec{b}$
$R_c / \vec{b}$
Figure 1: Comparison between the experimental results and the present model predictions of dislocation density as a function of burnup.
In Table 1 represents the initial shear slip rate, is the dislocation multiplication coefficient, is the burger's vector of the lattice, and is the capture radius for dislocation mutual annihilation.
The parameters in Table 1 were selected by emphasizing the fit for the first five experimental data points, taken below 45 GWd/tU. The Ham experimental approach applied in Nogita and Une (1994) is known to underestimate dislocation densities in extremely tangled dislocation networks; therefore, we allowed the fit of the parameters to deviate above the experimentally measured 83 GWd/tU dislocation densities where tangled networks were observed. The present model does, however, capture the saturation of the dislocation density at higher burnup, as shown in Figure 1.
The alignment of the current model parameters with the expected physically based values demonstrates the connection of the present model to the fuel microstructure.
## Example Input Syntax
[./dislocation_density]
type = UO2IsotropicDislocationDensity
variable = dislocation_density
burnup = burnup
execute_on = 'initial linear'
[../]
(test/tests/dislocation_density/isotropic_dislocation_density_burnup_aux.i)
## Input Parameters
• variableThe name of the variable that this object applies to
C++ Type:AuxVariableName
Description:The name of the variable that this object applies to
### Required Parameters
• initial_dislocation_density6e+13Dislocation density of as-recieved fuel (1/m^2)
Default:6e+13
C++ Type:double
Description:Dislocation density of as-recieved fuel (1/m^2)
• effective_dislocation_velocity0.00028Smeared isotropic parameter representing dislocation velocity as a function of burnup
Default:0.00028
C++ Type:double
Description:Smeared isotropic parameter representing dislocation velocity as a function of burnup
• blockThe list of block ids (SubdomainID) that this object will be applied
C++ Type:std::vector
Description:The list of block ids (SubdomainID) that this object will be applied
• execute_onLINEARThe list of flag(s) indicating when this object should be executed, the available options include NONE, INITIAL, LINEAR, NONLINEAR, TIMESTEP_END, TIMESTEP_BEGIN, FINAL, CUSTOM.
Default:LINEAR
C++ Type:ExecFlagEnum
Description:The list of flag(s) indicating when this object should be executed, the available options include NONE, INITIAL, LINEAR, NONLINEAR, TIMESTEP_END, TIMESTEP_BEGIN, FINAL, CUSTOM.
• boundaryThe list of boundary IDs from the mesh where this boundary condition applies
C++ Type:std::vector
Description:The list of boundary IDs from the mesh where this boundary condition applies
• burnup_functionBurnup function
C++ Type:BurnupFunctionName
Description:Burnup function
• dislocation_multiplication_factor2.5e+09Smeared isotropic parameter used to determine the multiplication of dislocations to create new dislocations
Default:2.5e+09
C++ Type:double
Description:Smeared isotropic parameter used to determine the multiplication of dislocations to create new dislocations
• burnupCoupled Burnup, in units of fissions/atoms-U
C++ Type:std::vector
Description:Coupled Burnup, in units of fissions/atoms-U
• dislocation_annhiliation_interaction_radius10Number of burgers' vectors in the radius of interaction between two annhiliating dislocations
Default:10
C++ Type:double
Description:Number of burgers' vectors in the radius of interaction between two annhiliating dislocations
### Optional Parameters
• control_tagsAdds user-defined labels for accessing object parameters via control logic.
C++ Type:std::vector
Description:Adds user-defined labels for accessing object parameters via control logic.
• enableTrueSet the enabled status of the MooseObject.
Default:True
C++ Type:bool
Description:Set the enabled status of the MooseObject.
• seed0The seed for the master random number generator
Default:0
C++ Type:unsigned int
Description:The seed for the master random number generator
• use_displaced_meshFalseWhether or not this object should use the displaced mesh for computation. Note that in the case this is true but no displacements are provided in the Mesh block the undisplaced mesh will still be used.
Default:False
C++ Type:bool
Description:Whether or not this object should use the displaced mesh for computation. Note that in the case this is true but no displacements are provided in the Mesh block the undisplaced mesh will still be used.
| 2020-12-04T05:53:46 |
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|
https://zims-en.kiwix.campusafrica.gos.orange.com/wikipedia_en_all_nopic/A/Virial_stress
|
# Virial stress
Virial stress is a measure of mechanical stress on an atomic scale for homogeneous systems. The expression of the (local) virial stress can be derived as the functional derivative of the free energy of a molecular system with respect to the deformation tensor[1].
## Volume averaged Definition
The instantaneous volume averaged virial stress is given by
${\displaystyle \tau _{ij}={\frac {1}{\Omega }}\sum _{k\in \Omega }\left(-m^{(k)}(u_{i}^{(k)}-{\bar {u}}_{i})(u_{j}^{(k)}-{\bar {u}}_{j})+{\frac {1}{2}}\sum _{\ell \in \Omega }(x_{i}^{(\ell )}-x_{i}^{(k)})f_{j}^{(k\ell )}\right)}$
where
• ${\displaystyle k}$ and ${\displaystyle \ell }$ are atoms in the domain,
• ${\displaystyle \Omega }$ is the volume of the domain,
• ${\displaystyle m^{(k)}}$ is the mass of atom k,
• ${\displaystyle u_{i}^{(k)}}$ is the ith component of the velocity of atom k,
• ${\displaystyle {\bar {u}}_{j}}$ is the jth component of the average velocity of atoms in the volume,
• ${\displaystyle x_{i}^{(k)}}$ is the ith component of the position of atom k, and
• ${\displaystyle f_{i}^{(k\ell )}}$ is the ith component of the force applied on atom ${\displaystyle k}$ by atom ${\displaystyle \ell }$.
At zero kelvin, all velocities are zero so we have
${\displaystyle \tau _{ij}={\frac {1}{2\Omega }}\sum _{k,\ell \in \Omega }(x_{i}^{(\ell )}-x_{i}^{(k)})f_{j}^{(k\ell )}}$.
This can be thought of as follows. The τ11 component of stress is the force in the x1-direction divided by the area of a plane perpendicular to that direction. Consider two adjacent volumes separated by such a plane. The 11-component of stress on that interface is the sum of all pairwise forces between atoms on the two sides.
The volume averaged virial stress is then the ensemble average of the instantaneous volume averaged virial stress.
In a three dimensional, isotropic system, at equilibrium the "instantaneous" atomic pressure is usually defined as the average over the diagonals of the negative stress tensor:
${\displaystyle {\mathcal {P}}_{at}=-{\frac {1}{3}}Tr(\tau ).}$
The pressure then is the ensemble average of the instantaneous pressure[2]
${\displaystyle P_{at}=\langle {\mathcal {P}}_{at}\rangle .}$
This pressure is the average pressure in the volume ${\displaystyle \Omega }$.
### Equivalent Definition
It's worth noting that some articles and textbook[2] use a slightly different but equivalent version of the equation
${\displaystyle \tau _{ij}={\frac {1}{\Omega }}\sum _{k\in \Omega }\left(-m^{(k)}(u_{i}^{(k)}-{\bar {u}}_{i})(u_{j}^{(k)}-{\bar {u}}_{j})-{\frac {1}{2}}\sum _{\ell \in \Omega }x_{i}^{(k\ell )}f_{j}^{(k\ell )}\right)}$
where ${\displaystyle x_{i}^{(k\ell )}}$ is the ith component of the vector oriented from the ${\displaystyle \ell }$th atoms to the kth calculated via the difference
${\displaystyle x_{i}^{k\ell }=x_{i}^{(k)}-x_{i}^{(\ell )}}$
Both equation being strictly equivalent, the definition of the vector can still lead to confusion.
### Derivation
The virial pressure can be derived, using the virial theorem and splitting forces between particles and the container[3] or, alternatively, via direct application of the defining equation ${\displaystyle P=-{\frac {\partial F(N,V,T)}{\partial V}}}$ and using scaled coordinates in the calculation.
## Inhomogeneous Systems
If the system is not homogeneous in a given volume the above (volume averaged) pressure is not a good measure for the pressure. In inhomogeneous systems the pressure depends on the position and orientation of the surface on which the pressure acts. Therefore in inhomogeneous systems a definition of a local pressure is needed[4]. As a general example for a system with inhomogeneous pressure you can think of the pressure in the atmosphere of the earth which varies with height.
## Instantaneous local virial stress
The (local) instantaneous virial stress is given by[1]:
${\displaystyle \tau _{ab}({\vec {r}})=-\sum _{i=1}^{N}\delta ({\vec {r}}-{\vec {r}}^{(i)})\left(m^{(i)}u_{a}^{(i)}u_{b}^{(i)}+{\frac {1}{2}}\sum _{j=1,j\neq i}^{N}({\vec {r}}^{(i)}-{\vec {r}}^{(j)})_{a}{\vec {f}}_{b}^{(ij)}\right),}$
## Measuring the virial pressure in molecular simulations
The virial pressure can be measured via the formulas above or using volume rescaling trial moves.[5]
## References
1. Morante, S., G. C. Rossi, and M. Testa. "The stress tensor of a molecular system: An exercise in statistical mechanics." The Journal of chemical physics 125.3 (2006): 034101, http://aip.scitation.org/doi/abs/10.1063/1.2214719.
2. Allen, MP; Tildesley, DJ (1991). Clarendon Press (ed.). Computer Simulations of Liquids. Oxford. pp. 46–50.
3. Navet, M.; Jamin, E.; Feix, M. R. (1980-02-01). "« Virial » pressure of the classical one-component plasma". Journal de Physique Lettres. 41 (3): 69–73. doi:10.1051/jphyslet:0198000410306900. ISSN 0302-072X.
4. Numerical Simulations of a Smectic Lamellar Phase of Amphiphilic Molecules, p. 40, https://books.google.de/books?id=rPpegGthzO4C&lpg=PA40&dq=local%20pressure%20tensor&hl=de&pg=PA40#v=onepage&q=local%20pressure%20tensor&f=false
5. Miguel, Enrique de; Jackson, George (2006-10-30). "The nature of the calculation of the pressure in molecular simulations of continuous models from volume perturbations". The Journal of Chemical Physics. 125 (16): 164109. doi:10.1063/1.2363381. ISSN 0021-9606.
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| 2020-10-22T02:41:14 |
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https://www.zbmath.org/authors/?q=ai%3Aschoof.rene
|
# zbMATH — the first resource for mathematics
## Schoof, René
Compute Distance To:
Author ID: schoof.rene Published as: Schoof, R.; Schoof, R. J.; Schoof, René External Links: MGP · Wikidata
Documents Indexed: 52 Publications since 1980, including 2 Books Reviewing Activity: 69 Reviews
all top 5
#### Co-Authors
31 single-authored 3 Van der Geer, Gerard 3 Washington, Lawrence C. 2 Kraft, James Stuart 2 van der Vlugt, Marcel 1 Bayer-Fluckiger, Eva 1 Corrales-Rodrigáñez, Capi 1 de Smit, Bart 1 Dose, Valerio 1 Fernandez, Julio 1 González, Josep R. 1 Lario, Joan-Carles 1 Larsen, Michael Jeffrey 1 Lenstra, Hendrik W. jun. 1 Mercuri, Pietro 1 Mestre, Jean-François 1 Monsurrò, Marina 1 Moonen, Ben 1 Parimala, Raman 1 Rubin, Karl Cooper 1 Schappacher, Norbert 1 Talamanca, Valerio 1 Tzanakis, Nikos 1 Van de Craats, Jan 1 Zagier, Don Bernard
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#### Serials
8 Mathematics of Computation 5 Journal of Number Theory 4 Compositio Mathematica 2 Journal of Combinatorial Theory. Series A 2 Experimental Mathematics 2 Journal de Théorie des Nombres de Bordeaux 1 The Mathematical Intelligencer 1 Acta Arithmetica 1 Gazette des Mathématiciens 1 Journal of Algebra 1 Journal of Pure and Applied Algebra 1 Journal für die Reine und Angewandte Mathematik 1 Manuscripta Mathematica 1 Mathematische Annalen 1 Pacific Journal of Mathematics 1 Bulletin of the American Mathematical Society. New Series 1 Nieuw Archief voor Wiskunde. Vierde Serie 1 Selecta Mathematica. New Series 1 Nieuw Archief voor Wiskunde. Vijfde Serie 1 Progress in Mathematics 1 Universitext
all top 5
#### Fields
44 Number theory (11-XX) 23 Algebraic geometry (14-XX) 5 Information and communication theory, circuits (94-XX) 3 General and overarching topics; collections (00-XX) 3 Field theory and polynomials (12-XX) 3 Group theory and generalizations (20-XX) 2 Commutative algebra (13-XX) 2 Computer science (68-XX) 1 History and biography (01-XX) 1 Associative rings and algebras (16-XX) 1 Category theory; homological algebra (18-XX)
#### Citations contained in zbMATH
38 Publications have been cited 652 times in 582 Documents Cited by Year
Elliptic curves over finite fields and the computation of square roots mod p. Zbl 0579.14025
Schoof, René
1985
Nonsingular plane cubic curves over finite fields. Zbl 0632.14021
Schoof, René
1987
Counting points on elliptic curves over finite fields. Zbl 0852.11073
Schoof, René
1995
Primitive normal bases for finite fields. Zbl 0615.12023
Lenstra, H. W. jun.; Schoof, R. J.
1987
Quintic polynomials and real cyclotomic fields with large class numbers. Zbl 0649.12007
Schoof, René; Washington, Lawrence C.
1988
Computing Iwasawa modules of real quadratic number fields. Zbl 0840.11043
Kraft, James S.; Schoof, René
1995
Hecke operators and the weight distributions of certain codes. Zbl 0729.11065
Schoof, René; van der Vlugt, Marcel
1991
The support problem and its elliptic analogue. Zbl 0922.11086
Corrales-Rodrigáñez, Capi; Schoof, René
1997
Families of curves and weight distributions of codes. Zbl 0854.11072
Schoof, René
1995
Class numbers of real cyclotomic fields of prime conductor. Zbl 1052.11071
Schoof, René
2003
Infinite class field towers of quadratic fields. Zbl 0589.12011
Schoof, René
1986
Effectivity of Arakelov divisors and the theta divisor of a number field. Zbl 1030.11063
van der Geer, Gerard; Schoof, René
2000
Computing Arakelov class groups. Zbl 1188.11076
Schoof, René
2008
Minus class groups of the fields of the $$l$$-th roots of unity. Zbl 0902.11043
Schoof, René
1998
Algebraic curves over $${\mathbb{F}}_ 2$$ with many rational points. Zbl 0762.11026
Schoof, René
1992
Abelian varieties over $$\mathbb Q$$ with bad reduction in one prime only. Zbl 1173.11333
Schoof, René
2005
Abelian varieties over cyclotomic fields with good reduction everywhere. Zbl 1058.11038
Schoof, René
2003
Beppo Levi and the arithmetic of elliptic curves. Zbl 0849.01036
Schappacher, Norbert; Schoof, René
1996
Weight formulas for ternary Melas codes. Zbl 0768.94017
van der Geer, Gerard; Schoof, René; van der Vlugt, Marcel
1992
The exponents of the groups of points on the reductions of an elliptic curve. Zbl 0726.14023
Schoof, René
1991
Criteria for complete intersections. Zbl 0903.13003
De Smit, Bart; Rubin, Karl; Schoof, René
1997
The automorphism group of the non-split Cartan modular curve of level 11. Zbl 1330.14049
Dose, Valerio; Fernández, Julio; González, Josep; Schoof, René
2014
Semistable abelian varieties with good reduction outside 15. Zbl 1323.11040
Schoof, René
2012
Visibility of ideal classes. Zbl 1226.11123
Schoof, René; Washington, Lawrence C.
2010
Catalan’s conjecture. Zbl 1186.11018
Schoof, René
2008
Class groups of complex quadratic fields. Zbl 0516.12002
Schoof, R. J.
1983
Integral points of a modular curve of level 11. Zbl 1292.11057
Schoof, René; Tzanakis, Nikos
2012
Four primality testing algorithms. Zbl 1196.11169
Schoof, René
2008
Trace forms of $$G$$-Galois algebras in virtual cohomological dimension 1 and 2. Zbl 1069.12004
Bayer-Fluckiger, Eva; Monsurrò, Marina; Parimala, R.; Schoof, René
2004
Some computations with Hecke rings and deformation rings. With an appendix by Amod Agashe and William Stein. Zbl 1116.11310
Lario, Joan-C.; Schoof, René
2002
The structure of the minus class groups of abelian number fields. Zbl 0719.11074
Schoof, René
1990
Quadratic fields and factorization. Zbl 0527.12003
Schoof, R. J.
1982
On the modular curve $$X_0(23)$$. Zbl 1317.14098
Schoof, René
2012
A refined counter-example to the support conjecture for abelian varieties. Zbl 1097.14036
Larsen, Michael; Schoof, René
2006
Number fields and function fields – two parallel worlds. Zbl 1078.11002
van der Geer, Gerard (ed.); Moonen, Ben (ed.); Schoof, René (ed.)
2005
Homophonic quotients of free groups. Zbl 0818.20033
Mestre, Jean-François; Schoof, René; Washington, Lawrence; Zagier, Don
1993
Cohomology of class groups of cyclotomic fields; an application to Morse- Smale diffeomorphisms. Zbl 0651.12004
Schoof, René
1988
Papers from the conference 21st Journées Arithmétiques held at the Università Lateranense, Rome, July 12–16, 2001. Zbl 1041.11500
Schoof, René (ed.); Talamanca, Valerio (ed.)
2001
The automorphism group of the non-split Cartan modular curve of level 11. Zbl 1330.14049
Dose, Valerio; Fernández, Julio; González, Josep; Schoof, René
2014
Semistable abelian varieties with good reduction outside 15. Zbl 1323.11040
Schoof, René
2012
Integral points of a modular curve of level 11. Zbl 1292.11057
Schoof, René; Tzanakis, Nikos
2012
On the modular curve $$X_0(23)$$. Zbl 1317.14098
Schoof, René
2012
Visibility of ideal classes. Zbl 1226.11123
Schoof, René; Washington, Lawrence C.
2010
Computing Arakelov class groups. Zbl 1188.11076
Schoof, René
2008
Catalan’s conjecture. Zbl 1186.11018
Schoof, René
2008
Four primality testing algorithms. Zbl 1196.11169
Schoof, René
2008
A refined counter-example to the support conjecture for abelian varieties. Zbl 1097.14036
Larsen, Michael; Schoof, René
2006
Abelian varieties over $$\mathbb Q$$ with bad reduction in one prime only. Zbl 1173.11333
Schoof, René
2005
Number fields and function fields – two parallel worlds. Zbl 1078.11002
van der Geer, Gerard (ed.); Moonen, Ben (ed.); Schoof, René (ed.)
2005
Trace forms of $$G$$-Galois algebras in virtual cohomological dimension 1 and 2. Zbl 1069.12004
Bayer-Fluckiger, Eva; Monsurrò, Marina; Parimala, R.; Schoof, René
2004
Class numbers of real cyclotomic fields of prime conductor. Zbl 1052.11071
Schoof, René
2003
Abelian varieties over cyclotomic fields with good reduction everywhere. Zbl 1058.11038
Schoof, René
2003
Some computations with Hecke rings and deformation rings. With an appendix by Amod Agashe and William Stein. Zbl 1116.11310
Lario, Joan-C.; Schoof, René
2002
Papers from the conference 21st Journées Arithmétiques held at the Università Lateranense, Rome, July 12–16, 2001. Zbl 1041.11500
Schoof, René (ed.); Talamanca, Valerio (ed.)
2001
Effectivity of Arakelov divisors and the theta divisor of a number field. Zbl 1030.11063
van der Geer, Gerard; Schoof, René
2000
Minus class groups of the fields of the $$l$$-th roots of unity. Zbl 0902.11043
Schoof, René
1998
The support problem and its elliptic analogue. Zbl 0922.11086
Corrales-Rodrigáñez, Capi; Schoof, René
1997
Criteria for complete intersections. Zbl 0903.13003
De Smit, Bart; Rubin, Karl; Schoof, René
1997
Beppo Levi and the arithmetic of elliptic curves. Zbl 0849.01036
Schappacher, Norbert; Schoof, René
1996
Counting points on elliptic curves over finite fields. Zbl 0852.11073
Schoof, René
1995
Computing Iwasawa modules of real quadratic number fields. Zbl 0840.11043
Kraft, James S.; Schoof, René
1995
Families of curves and weight distributions of codes. Zbl 0854.11072
Schoof, René
1995
Homophonic quotients of free groups. Zbl 0818.20033
Mestre, Jean-François; Schoof, René; Washington, Lawrence; Zagier, Don
1993
Algebraic curves over $${\mathbb{F}}_ 2$$ with many rational points. Zbl 0762.11026
Schoof, René
1992
Weight formulas for ternary Melas codes. Zbl 0768.94017
van der Geer, Gerard; Schoof, René; van der Vlugt, Marcel
1992
Hecke operators and the weight distributions of certain codes. Zbl 0729.11065
Schoof, René; van der Vlugt, Marcel
1991
The exponents of the groups of points on the reductions of an elliptic curve. Zbl 0726.14023
Schoof, René
1991
The structure of the minus class groups of abelian number fields. Zbl 0719.11074
Schoof, René
1990
Quintic polynomials and real cyclotomic fields with large class numbers. Zbl 0649.12007
Schoof, René; Washington, Lawrence C.
1988
Cohomology of class groups of cyclotomic fields; an application to Morse- Smale diffeomorphisms. Zbl 0651.12004
Schoof, René
1988
Nonsingular plane cubic curves over finite fields. Zbl 0632.14021
Schoof, René
1987
Primitive normal bases for finite fields. Zbl 0615.12023
Lenstra, H. W. jun.; Schoof, R. J.
1987
Infinite class field towers of quadratic fields. Zbl 0589.12011
Schoof, René
1986
Elliptic curves over finite fields and the computation of square roots mod p. Zbl 0579.14025
Schoof, René
1985
Class groups of complex quadratic fields. Zbl 0516.12002
Schoof, R. J.
1983
Quadratic fields and factorization. Zbl 0527.12003
Schoof, R. J.
1982
all top 5
#### Cited by 671 Authors
12 Sutherland, Andrew V. 11 Schoof, René 10 Ichimura, Humio 9 Maire, Christian 9 Miret, Josep M. 8 Shparlinski, Igor E. 7 Schost, Éric 6 Fan, Shuqin 6 Gras, Georges 6 Morain, François 6 Sumida-Takahashi, Hiroki 5 Banaszak, Grzegorz 5 Bröker, Reinier 5 Hachenberger, Dirk 5 Han, Wenbao 5 Kapetanakis, Giorgos 5 Lercier, Reynald 5 Tran, Ha Thanh Nguyen 5 Vanstone, Scott Alexander 5 von zur Gathen, Joachim 4 Brumer, Armand 4 Cohen, Stephen D. 4 Cornacchia, Pietro 4 Couveignes, Jean-Marc 4 Ezome, Tony 4 Gaudry, Pierrick 4 Huang, Ming-Deh A. 4 Koblitz, Neal I. 4 Kramer, Kenneth B. 4 Krasoń, Piotr 4 Lauder, Alan G. B. 4 Lauter, Kristin Estella 4 Menezes, Alfred J. 4 Moreno, Ramiro 4 Pujolàs, Jordi 4 Robert, Damien 4 Top, Jaap 4 Valls, Magda 4 van der Vlugt, Marcel 4 Vlǎduţ, Sergei Georgievich 4 Xing, Chaoping 3 Barańczuk, Stefan 3 Bayer-Fluckiger, Eva 3 Bisson, Gaetan 3 De Feo, Luca 3 Dieulefait, Luis Victor 3 Doliskani, Javad 3 Farashahi, Reza Rezaeian 3 Feng, Rongquan 3 Fieker, Claus 3 Fukuda, Takashi 3 Gaál, István 3 Gajda, Wojciech 3 Güneri, Cem 3 Hajir, Farshid 3 James, Kevin 3 Kontogeorgis, Aristides I. 3 Lachaud, Gilles 3 Lubicz, David 3 McGuire, Gary 3 Miller, John C. 3 Moisio, Marko J. 3 Nguyen Quang Do, Thong 3 Pomerance, Carl Bernard 3 Reis, Lucas 3 Satoh, Takakazu 3 Scholl, Travis 3 Silverman, Joseph Hillel 3 Smith, Ethan 3 Taya, Hisao 3 Tena Ayuso, Juan Gabriel 3 Thaine, Francisco 3 Valera, Javier 3 Van der Geer, Gerard 3 Voloch, José Felipe 3 Wake, Preston 3 Wan, Daqing 3 Wu, Hongfeng 3 Xiong, Maosheng 3 Zarkhin, Yuriĭ Gennad’evich 2 Abelard, Simon 2 Achter, Jeffrey D. 2 Agathocleous, Eleni 2 Agnew, Gordon B. 2 Anju 2 Bach, Eric 2 Bartoli, Daniele 2 Bekker, Boris Mikhaĭlovich 2 Belabas, Karim 2 Blake, Ian F. 2 Bostan, Alin 2 Bruen, Aiden A. 2 Cao, Xiwang 2 Deng, Yingpu 2 Dose, Valerio 2 Elia, Michele 2 Elkies, Noam David 2 Feng, Keqin 2 Ferri, Stefania 2 Flori, Jean-Pierre ...and 571 more Authors
all top 5
#### Cited in 134 Serials
68 Mathematics of Computation 68 Journal of Number Theory 50 Finite Fields and their Applications 23 Journal de Théorie des Nombres de Bordeaux 21 LMS Journal of Computation and Mathematics 17 Designs, Codes and Cryptography 11 Journal of Symbolic Computation 11 Journal of Cryptology 11 Applicable Algebra in Engineering, Communication and Computing 10 Proceedings of the American Mathematical Society 9 International Journal of Number Theory 8 Journal of Algebra 8 Transactions of the American Mathematical Society 8 The Ramanujan Journal 7 Rocky Mountain Journal of Mathematics 7 Manuscripta Mathematica 6 Discrete Mathematics 6 Acta Arithmetica 6 Duke Mathematical Journal 6 Journal of Pure and Applied Algebra 6 Experimental Mathematics 5 Annales de l’Institut Fourier 5 Mathematische Annalen 5 Proceedings of the Japan Academy. Series A 5 Comptes Rendus. Mathématique. Académie des Sciences, Paris 4 Bulletin of the Australian Mathematical Society 4 Compositio Mathematica 4 Journal of Complexity 4 Computational Complexity 4 Foundations of Computational Mathematics 3 Communications in Algebra 3 Mathematical Proceedings of the Cambridge Philosophical Society 3 Abhandlungen aus dem Mathematischen Seminar der Universität Hamburg 3 Archiv der Mathematik 3 Functiones et Approximatio. Commentarii Mathematici 3 Mathematische Zeitschrift 3 Nagoya Mathematical Journal 3 Osaka Journal of Mathematics 3 Rendiconti del Circolo Matemàtico di Palermo. Serie II 3 European Journal of Combinatorics 3 Bulletin of the American Mathematical Society. New Series 3 Journal of Discrete Mathematical Sciences & Cryptography 3 Journal of Algebra and its Applications 3 Advances in Mathematics of Communications 3 Cryptography and Communications 3 Science China. Mathematics 2 Discrete Applied Mathematics 2 Mathematical Notes 2 Advances in Mathematics 2 Applied Mathematics and Computation 2 Inventiones Mathematicae 2 Journal of Combinatorial Theory. Series A 2 Mathematika 2 Results in Mathematics 2 Theoretical Computer Science 2 Tohoku Mathematical Journal. Second Series 2 Acta Applicandae Mathematicae 2 Revista Matemática Iberoamericana 2 Applied Mathematics Letters 2 Journal of the American Mathematical Society 2 Linear Algebra and its Applications 2 Proceedings of the Indian Academy of Sciences. Mathematical Sciences 2 St. Petersburg Mathematical Journal 2 Annales Mathématiques Blaise Pascal 2 Journal of Applied Mathematics and Computing 2 Journal of Mathematical Cryptology 2 Asian-European Journal of Mathematics 2 JSIAM Letters 2 Research in Number Theory 1 American Mathematical Monthly 1 Archive for History of Exact Sciences 1 Computers & Mathematics with Applications 1 Information Processing Letters 1 Lithuanian Mathematical Journal 1 Moscow University Mathematics Bulletin 1 Reviews of Modern Physics 1 Russian Mathematical Surveys 1 The Mathematical Intelligencer 1 Annali di Matematica Pura ed Applicata. Serie Quarta 1 Illinois Journal of Mathematics 1 Information Sciences 1 Publications Mathématiques 1 Journal of Computational and Applied Mathematics 1 Journal of Computer and System Sciences 1 Journal of the Mathematical Society of Japan 1 Journal für die Reine und Angewandte Mathematik 1 Mathematics and Computers in Simulation 1 Mathematische Nachrichten 1 Pacific Journal of Mathematics 1 Proceedings of the London Mathematical Society. Third Series 1 Publications of the Research Institute for Mathematical Sciences, Kyoto University 1 Tokyo Journal of Mathematics 1 Advances in Applied Mathematics 1 Combinatorica 1 Chinese Annals of Mathematics. Series B 1 Algorithmica 1 Information and Computation 1 Mathematical and Computer Modelling 1 Journal of the Ramanujan Mathematical Society 1 Séminaire de Théorie des Nombres de Bordeaux. Deuxième Série ...and 34 more Serials
all top 5
#### Cited in 33 Fields
510 Number theory (11-XX) 216 Algebraic geometry (14-XX) 103 Information and communication theory, circuits (94-XX) 36 Field theory and polynomials (12-XX) 33 Computer science (68-XX) 19 Group theory and generalizations (20-XX) 13 Combinatorics (05-XX) 12 Geometry (51-XX) 7 Commutative algebra (13-XX) 6 $$K$$-theory (19-XX) 6 Special functions (33-XX) 5 Numerical analysis (65-XX) 4 History and biography (01-XX) 3 Mathematical logic and foundations (03-XX) 3 Order, lattices, ordered algebraic structures (06-XX) 3 Associative rings and algebras (16-XX) 3 Quantum theory (81-XX) 2 Linear and multilinear algebra; matrix theory (15-XX) 2 Topological groups, Lie groups (22-XX) 2 Several complex variables and analytic spaces (32-XX) 2 Probability theory and stochastic processes (60-XX) 2 Game theory, economics, finance, and other social and behavioral sciences (91-XX) 1 General and overarching topics; collections (00-XX) 1 Partial differential equations (35-XX) 1 Approximations and expansions (41-XX) 1 Harmonic analysis on Euclidean spaces (42-XX) 1 Convex and discrete geometry (52-XX) 1 Manifolds and cell complexes (57-XX) 1 Statistics (62-XX) 1 Fluid mechanics (76-XX) 1 Relativity and gravitational theory (83-XX) 1 Geophysics (86-XX) 1 Biology and other natural sciences (92-XX)
#### Wikidata Timeline
The data are displayed as stored in Wikidata under a Creative Commons CC0 License. Updates and corrections should be made in Wikidata.
| 2021-04-16T02:53:48 |
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|
https://atlaswww.hep.anl.gov/asc/wikidoc/doku.php?id=community:hepsim
|
# ATLAS Support Center
### Sidebar
community:hepsim
This manual is outdated. Please use http://atlaswww.hep.anl.gov/hepsim/doc/doku.php
# HepSim manual
HepSim is a public repository with Monte Carlo simulated events for high-energy physics (HEP) experiments. The HepSim repository was started at ANL during the US long-term planning study of the American Physical Society’s Division of Particles and Fields (Snowmass 2013) with the goal to create references to truth-level MC records for current and future experiments. Event data samples are created using:
• BlueGene/Q supercomputer of the Argonne Leadership Computing Facility ([email protected] library)
• OSG (Open Science Grid) Connect (“FutureColliders” project).
• ATLAS Connect virtual cluster service (“ATLAS CI” project)
• Argonne’s Laboratory Computing Resource Center (LCRC) (“HepSim” project)
• ATLAS Analysis support (ASC) cluster at HEP/ANL
The file storage is provided by:
• STASH2 storage at OSG CI Connect
• FAXBOX storage at ATLAS Connect
• MC.HEP server at ASC ANL
This repository was created following the guidelines and principles of the DOE Public Access Plan for unclassified and otherwise unrestricted scientific data in digital formats.
# For HepSim users
If you are a HepSim user, start from here.
# Physics and detector studies
Here are several links to extending this Wiki for particular detector-performance topics:
# For developers
If you plan to contribute to HepSim (Monte Carlo events, data storage etc), start from here:
# How to cite
If you use HepSim event samples, Python/Jython analysis scripts and output XML files in your research, talks or publications, please cite this project as:
S.V. Chekanov. HepSim: a repository with predictions for high-energy physics experiments. Advances in High Energy Physics, vol. 2015, ID136093, 2015. arXiv:1403.1886 and link.
@article{Chekanov:2014fga,
author = "Chekanov, S.V.",
title = "{HepSim: a repository with predictions for high-energy physics experiments}",
year = "2015",
eprint = "1403.1886",
journal = "Advances in High Energy Physics",
volume = "2015",
pages = "136093",
archivePrefix = "arXiv",
primaryClass = "hep-ph",
note = {Available as \url{http://atlaswww.hep.anl.gov/hepsim/}}
}
# Acknowledgement
The current work is supported UChicago Argonne, LLC, Operator of Argonne National Laboratory (Argonne''). Argonne, a U.S. Department of Energy Office of Science laboratory, is operated under Contract No. DE-AC02-06CH11357. This research used resources of the Argonne Leadership Computing Facility at Argonne National Laboratory, which is supported by the Office of Science of the U.S. Department of Energy under contract DE-AC02-06CH11357.
Sergei Chekanov 2016/04/29 16:24
| 2023-01-30T21:06:08 |
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https://indico.fnal.gov/event/11999/timetable/?view=standard_numbered
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Indico will be rebooted on Tuesday, June 21st, at 5:30 pm Central Time. The downtime will be just few minutes. Thank you.
# 2017 Meeting of the APS Division of Particles and Fields (DPF 2017)
US/Central
Ramsey Auditorium (Fermi National Accelerator Laboratory)
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
Kirk Road & Pine Street Batavia, IL 60510-5011
Description
The conference will take place July 31 - August 4, 2017 in Batavia, IL, hosted by the Fermi National Accelerator Laboratory.
DPF Conference Homepage
Participants
• Aakaash Narayanan
• Aaron Bercellie
• Aaron Webb
• Aaron White
• Abhishek Mohapatra
• Abid Patwa
• Adam Lister
• Adam Lyon
• Adam Moren
• Adrian Lee
• Aida El-Khadra
• Ajeeta Khatiwada
• Akash Dixit
• Al Goshaw
• Alberto Marchionni
• Aleena Rafique
• Alejandro Diaz
• Alejandro Gomez Espinosa
• Alessandra Lucà
• Alex Drlica-Wagner
• Alex Tapia
• Alexander Himmel
• Alexander Khanov
• Alexander Radovic
• Alexander Tuna
• Alexey Petrov
• Alexis Mulski
• Alfredo Aranda
• Ali Ashtari Esfahani
• Amit Bashyal
• Amy Bender
• Amy Cottle
• Anadi Canepa
• Anatoly Ronzhin
• Andreas Jung
• Andrei Gaponenko
• Andrew Askew
• Andrew Fiedler
• Andrew Lankford
• Andrew Lopez
• Andrew Ludwig
• Andrew Norman
• Andrew Whitbeck
• Andrés Abreu
• Andy Beretvas
• ANIMESH CHATTERJEE
• Anna Mazzacane
• Anne Schukraft
• Anthony Barker
• Antonella Palmese
• Aristeidis Tsaris
• Aron Soha
• Arthur Kreymer
• Artur Apresyan
• Ayesh Gunawardana
• Bahareh Roozbahani
• Bai-Cian Ke
• Barbara Yaeggy
• Bashayr Bashaa
• Basil Schneider
• Ben Jones
• Benedetto Gianluca Siddi
• Benjamin Kreis
• Benjamin Nachman
• Benjamin Tannenwald
• Bertrand Echenard
• Bhaskar Dutta
• Biao Wang
• Bilas Pal
• Bin Gui
• Biswaranjan Behera
• Bjoern Penning
• Blair Ratcliff
• Blake Burghgrave
• Boaz Klima
• Bob Hirosky
• Bob Tschirhart
• Bodhitha Jayatilaka
• Bogdan Dobrescu
• Bonnie Fleming
• Boqun Wang
• Boris Kayser
• Brad Cox
• Brandon Becker
• Breese Quinn
• Brendan Casey
• Brendan Kiburg
• Brenna Flaugher
• Brett Cornell
• Brian Beckford
• Brian Kirby
• Brian Nord
• Brian Pollack
• Brian Rebel
• Brian Welch
• Brooke Russell
• Bruce Baller
• Bruce Brown
• Bryan FULSOM
• Bryce Littlejohn
• Bryce Littlejohn
• Burt Holzman
• Cameron Marshall
• Can Kilic
• Carl Akerlof
• Carl Albright
• Carlos Escobar
• Carrie McGivern
• Cary Yoshikawa
• Caterina Vernieri
• Catrin Bernius
• Cecilia Gerber
• Chandrashekhara Bhat
• Chang Kee Jung
• Charles Burton
• Charles Glaser
• Charles Mueller
• Chen Zhou
• Ching Li
• Chris Polly
• Chris Quigg
• Christian Herwig
• Christian Schnaible
• Christopher Grant
• Christopher Hilgenberg
• Christopher Hill
• Christopher Lee
• Christopher Martin
• Christopher Murphy
• Christopher Neu
• Christopher Tunnell
• Christos Tzounis
• Cindy Joe
• Colton Hill
• Corrado Gatto
• corrinne mills
• Cory Crowley
• Cory Rude
• Craig Group
• Cristiana Principato
• Cristina Ana Mantilla Suarez
• Cristovao Vilela
• Daisy Kalra
• Dan Amidei
• Dan Bauer
• Daniel Bowring
• Daniel Hackett
• Daniel Noonan
• Daniel Smith
• Darcy Barron
• David Asner
• David Bartlett
• David Brown
• David LISSAUER
• David London
• David Martinez Caicedo
• David Morrison
• David Neuffer
• David Rivera
• David Saltzberg
• de graft akouku
• Debtosh Chowdhury
• Deepak Sathyan
• DEEPIKA JENA
• Derek Hazard
• Diana Patricia Mendez
• Diego Tonelli
• Dmitri Denisov
• Dominic Brailsford
• Donatella Torretta
• Doug McKay
• Douglas Glenzinski
• Dylan Frizzell
• E. Craig Dukes
• Eak Raj Paudel
• Eckhard ELSEN
• Ed Kearns
• Edmond Berger
• Efe Yigitbasi
• Elena Gramellini
• Elizabeth Buckley-Geer
• Elizabeth Simmons
• Elodie Resseguie
• Emrah Tiras
• Enectali Figueroa-Feliciano
• Enhao Song
• Enrique Jimenez Ramos
• Eran Moore Rea
• Eric Amador
• eric bosompem
• Eric Braaten
• Eric Linder
• Eric Prebys
• Erica Smith
• Erich Schmitz
• Erik Gustafson
• Erik Ramberg
• Erika Catano Mur
• Evan Johnson
• Evan Wolfe
• Eve Vavagiakis
• Evelyn Thomson
• Everardo Granados
• Federico Sforza
• Fedor Ratnikov
• Felix Kling
• Felix Ringer
• Fernanda Psihas
• Francesco Rubbo
• Francisco Javier Rosas-Torres
• Frank Chlebana
• Frank Jensen
• Fredrick Olness
• Gabriel Perdue
• Gabriel Santucci
• Gabriele Benelli
• Gail Hanson
• Gary Goldstein
• Gavin S. Davies
• George Redlinger
• George W.S. Hou
• Georgia Karagiorgi
• Gerald Eigen
• Giacinto Piacquadio
• Gil Paz
• Giordon Stark
• Giulio Stancari
• Giuseppe Cerati
• Glen Crawford
• Glenn Simon
• Gonzalo Díaz Bautista
• Gordon Watts
• Greg Bock
• Gregorio Bernardi
• Gregory Pulliam
• Gregory Snow
• Guang Yang
• Gunn Quznetsov
• HAICHEN WANG
• Hajime Muramatsu
• Hanyu Wei
• Harish Potti
• Harry Cheung
• Heather Russell
• Hector Mendez
• Helmut Marsiske
• Henry Schreiner
• Herbert Greenlee
• Herman B. White
• Hitoshi Yamamoto
• Hong Liu
• Hongbo Zhu
• Hongtao Yang
• Hongxi Xing
• Hongyue Duyang
• Howard Baer
• Huan Lin
• Huijing Li
• Ian Lewis
• Ian Snyder
• INA SARCEVIC
• Ines Ochoa
• IRVING DANIEL SANDOVAL
• Irwin Gaines
• Ivan Polyakov
• J. Michael Roney
• Jack Dolde
• Jae-Kwang Hwang
• Jaehoon Yu
• James Dunlop
• James Miller
• James Mueller
• James Patrick
• james simone
• Jan Strube
• Jane Nachtman
• Jangbae LEE
• Jared Sturdy
• Jason Gallicchio
• Jason Kumar
• Jason Stock
• Javier Duarte
• Javier Tiffenberg
• Jay Lawhorn
• Jeff McMahon
• Jeffrey Dandoy
• Jeffrey Kleykamp
• Jelena Maricic
• Jennifer Raaf
• Jennifer Roloff
• Jeremy Marshall
• Jhovanny Mejia
• Jianming Bian
• Jianwei Qiu
• Jie Gao
• Jim Annis
• Jim Hylen
• Jingyu Zhang
• Joakim Olsson
• JoAnne Hewett
• Joao Pedro Athayde Marcondes de André
• Jodi Cooley
• Joel Butler
• John Brandenburg
• John Butler
• John Campbell
• John Conway
• JOHN FINLEY
• John Peoples
• John Quirk
• John Stupak
• Jon Eliason
• Jonathan Echevers
• Jonathan Lewis
• Jonathan Miller
• Jonathan Paley
• Jonathan Rosner
• Jonathon Sensenig
• Jorge G. Morfin
• Jose Ignacio Crespo Anadon
• Joseph Angelo
• Joseph Haley
• Joseph Lykken
• Joseph Reichert
• Joseph Zennamo
• Joshua Barrow
• Joshua Berger
• Joshua Sayre
• Joshua Spitz
• Joydeep Roy
• Juan Maldacena
• Julia Gonski
• Julie Whitmore
• Junjie Zhu
• Justin Cammarota
• Justin Pilot
• Justin Vasel
• JYOTI JOSHI
• Jyoti Tripathi
• K.K. Gan
• K.S. Babu
• Kaixuan Ni
• kaori maeshima
• Karie Badgley
• Karla Natalia Herrera Guzman
• Karla Prosperi
• Katarzyna Frankiewicz
• Kate Scholberg
• Kate Whalen
• Katherine Woodruff
• Katie Yurkewicz
• Kaushik De
• Keisuke Yoshihara
• Keith Pedersen
• Ken Bloom
• Kenneth Cecire
• Kenneth Herner
• Kevin Burkett
• Kevin Pedro
• Kevin Pitts
• Kevin Siehl
• Kiel Howe
• Kimmy Wu
• Kirsten Tollefson
• Kurt Francis
• Kurt Riesselmann
• kwame appiah
• Larry Sulak
• Laser Kaplan
• Laura Fields
• Laura Reina
• Lauren Biron
• Lauren Yates
• Leah Broussard
• lei feng
• Leigh Schaefer
• Leo Bellantoni
• Leo Michelotti
• Leo Piilonen
• Leonard Spiegel
• Leonidas Aliaga Soplin
• Leslie Rogers
• Liang Guan
• Lige Zhang
• Liming Zhang
• linda amaniampong
• Lindsey Bleem
• Lindsey Gray
• Lothar Bauerdick
• Lous Antonelli
• Lousie Suter
• Lu Ren
• Madhuranga Thilakasiri Madugoda Ralalage Don
• Mandy Rominsky
• Manolis Kargiantoulakis
• Manqi RUAN
• Manuel Silva
• Maral Alyari
• Marc Sher
• Marc-Andre Pleier
• Marcel Demarteau
• Marcela Carena
• Marcelle Soares-Santos
• Marco Del Tutto
• Marco Verzocchi
• Marguerite Tonjes
• Maria Elena Monzani
• Maria Elidaiana da Silva Pereira
• Maria Vieites Diaz
• marina artuso
• Marina Guzzo
• Mario Balcazar
• Marjon Moulai
• Marjorie Bardeen
• Mark Devlin
• Mark Messier
• Mark Neubauer
• Mark Palmer
• Mark Thomson
• Mary Anne Cummings
• Mary Hall Reno
• Masao Sako
• Mathew Madhavacheril
• Matt Kramer
• Matt Toups
• Matt Zhang
• Matteo Cremonesi
• Matthew Coon
• Matthew Fritts
• Matthew Judah
• Matthew Rudolph
• Matthew Szydagis
• Maximilian Heindl
• Mazin Khader
• Meenakshi Narain
• Melissa Hutcheson
• Melody Saperston
• Michael Baird
• Michael Begel
• Michael Cooke
• Michael Eads
• Michael Hedges
• Michael Kirby
• Michael Levi
• Michael Schmitt
• Michael Schubnell
• Michael Sokoloff
• Michael Syphers
• Michelle Dolinski
• Michelle Stancari
• Mihai Horoi
• Mike Tuts
• Moein Mirza Amraji
• Mohammad Alhusseini
• Monica Soares Nunes
• Murray Moinester
• Myron Campbell
• Nadeesha Wickramage
• Nafisa Tasneem
• Nam Tran
• Nathaniel Craig
• Nathaniel Pastika
• Nausheen Shah
• Neelima Sehgal
• Neha Dokania
• Nhan Tran
• Nicholas Hadley
• Nicholas Lira
• Nicole Larsen
• Nigel Lockyer
• Nigel Sharp
• Nikolaos Kidonakis
• Norbert Neumeister
• olga mena
• Or Hen
• Orgho Neogi
• Orin Harris
• Oscar Eduardo Moreno Palacios
• P James Norris
• P.Q. Hung
• Pat Harding
• Patricia McBride
• Patrick Barry
• Patrick Fox
• Patrick Skubic
• Paul Karchin
• Paul L. G. Lebrun
• Paul Moch
• Pavel Murat
• Pavel Snopok
• Pawel Kryczynski
• Pedro Machado
• Pedrom Zadeh
• Pengfei Ding
• Peter Farris
• Peter Garbincius
• Peter Onyisi
• Peter Shanahan
• Peter Wilson
• Philip Ilten
• Philip Weigel
• Phillip Barbeau
• Phuong Dang
• Pilar Coloma
• Pinfold James
• Polina Abratenko
• Prabhjot Singh Singh
• Prajwal Mohan Murthy
• Pranava Teja Surukuchi
• Preet Sharma
• Priscilla Cushman
• Prudhvi Chintalapati
• Pushpalatha Bhat
• Qing QIN
• Qizhong Li
• Rachael Creager
• Rachel A Rosen
• Rachitha Mendis
• Radja Boughezal
• Radovan Dermisek
• Rafael Coelho Lopes de Sa
• Rafael Lang
• Raffaella Donghia
• Ralf Ehrlich
• Raul Alejandro Gutierrez Sanchez
• ray burnstein
• Ray Culbertson
• Ray Neely
• Raymond Brock
• Rebecca Linck
• Reddy Pratap Gandrajula
• regina demina
• Reinhard Schwienhorst
• Riccardo Cenci
• RICHARD BENAVIDES
• Richard Hill
• Richard Holmes
• Richard Kriske
• Richard Soluk
• Richard Talaga
• richmond apreku toprah
• Rijeesh Keloth
• Rizki Syarif
• Robert Abrams
• Robert Bernstein
• Robert Carey
• Robert Harr
• Robert Harris
• Robert Kehoe Kehoe
• Robert Kephart
• Robert Kutschke
• Robert Plunket
• Robert Svoboda
• Robin Erbacher
• Ron Ray
• Rowan Zaki
• Roxanne Guenette
• Ruth Van de Water
• Ryan Murphy
• Sachio Komamiya
• Sadia Khalil
• Salman Habib
• Sam Childress
• Sam Cunliffe
• Sam Zeller
• Sarah Demers
• Satyanarayan Nandi
• Sau Lan Wu
• Saul Gonzalez
• Saurabh Sandilya
• Scott Locke
• Seodong Shin
• Sergei Gleyzer
• Sergei Nagaitsev
• Sergey Uzunyan
• Seyda Ipek
• Shaikh Saad
• Shaokai Yang
• Shawn Zaleski
• Shekhar Mishra
• Sheldon Stone
• Shiqi Yu
• Shohreh Abdolrahimi
• Shreyashi Chakdar
• SIJITH EDAYATH
• Simona Rolli
• Sonaina Undleeb
• Sowjanya Gollapinni
• Spencer Axani
• Stefano Roberto Soleti
• Stephanie Su
• Stephen Holmes
• Stephen Kuhlmann
• Stephen Parke
• Stephen Wimpenny
• Steve Giddings
• Steve Nahn
• Steven Blusk
• Steven Dye
• Stoyan Stoynev
• Stuart Fuess
• Sudarshan Gutam
• Sudhir Malik
• SUDIP JANA
• Suman Baral
• Supratik Sarkar
• Swagato Banerjee
• Tammy Walton
• Tanaz Angelina Mohayai
• Tao Ren
• Taritree Wongjirad
• Tasneem Zehra Husain
• Theodore Lach
• Thomas Clayton
• Thomas Diehl
• Thomas Junk
• Thomas LeCompte
• Thomas Mehen
• Thomas Strauss
• Tim Andeen
• Tim Bolton
• Ting Li
• Tingjun Yang
• Todd Adams
• Tomonari Miyashita
• Tony Tong
• Tulika Bose
• Tyler Mitchell
• Ulrich Heintz
• Ulrich Schubert
• usha mallik
• V. Daniel Elvira
• Vadim Rusu
• Vallary Bhopatkar
• varun vaidya
• Varuna Crishan Meddage
• Vassili Papavassiliou
• Venkitesh Ayyar
• Verena Martinez Outschoorn
• Vikas Bansal
• Vincent Theeuwes
• Vinu Vikraman
• Vitaly Yakimenko
• Vitor Barroso Silveira
• Vivian O'Dell
• Vlad Past
• Volodymyr Aushev
• Wade Fisher
• Walter Hopkins
• Wei Tang
• Weinan Si
• Wesley Gohn
• Wesley Ketchum
• Wesley Smith
• Will DiClemente
• William Foreman
• William Kilgore
• William Marsh
• William Shepherd
• Wlliam Bardeen
• Wolfgang Altmannshofer
• Xiangting Meng
• Xiangyang Ju
• Xiaoyue Li
• Xinchou LOU
• Xing Wang
• Yagmur Torun
• Yanchu Wang
• Yang Bai
• Yangyang Cheng
• Yannick Meurice
• Yaqian Wang
• Yi Yin
• Yicheng Guo
• yu liang
• Yuanyuan Zhang
• Yuhan Wang
• YUNLONG CHI
• Yuri Gershtein
• Yuri Oksuzian
• Zack Sullivan
• Zalak Shah
• Zechariah Gelzer
• Zeeshan Ahmed
• Zhenbin Wu
• Ziqing Hong
• Zirui Wang
• Zoltan Gecse
• Monday, July 31
• Registration Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
Kirk Road & Pine Street Batavia, IL 60510-5011
Convener: Joy Pomillo (Fermilab)
• Plenary: Monday morning Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
Kirk Road & Pine Street Batavia, IL 60510-5011
Convener: Dmitri Denisov (Fermilab)
• 1
Introduction
Speaker: Dmitri Denisov (Fermilab)
• 2
Welocme from DPF
Speaker: Dr Marcela Carena (Fermilab)
• 3
Welcome from Fermilab
Speaker: Nigel Lockyer (Fermilab)
• 4
Properties of the Higgs boson
Speaker: Prof. Giacinto Piacquadio (Stony Brook University)
• 5
Searches for new physics at the energy frontier
Speaker: Dr Sadia Khalil (Kansas State)
• 6
Physics at the future colliders
Speaker: Prof. Liantao Wang (University of Chicago)
• 10:15 AM
Break
• Beyond Standard Model: Monday morning 1 West
### 1 West
#### Fermi National Accelerator Laboratory
Kirk Road & Pine Street Batavia, IL 60510-5011
Convener: Prof. Christopher Hill (The Ohio State University)
• 7
Search for 3rd generation superpartners with the ATLAS experiment
Two of the most important parameters in supersymmetry are the masses of the stop and sbottom, the supersymmetric partners of the third generation quarks. A stop mass lighter than 1 TeV is favored in theory, however experimental evidence for a light stop has not been indicated from the various searches at the LHC so far. Therefore, it is very important to extend the searches to various pMSSM models with different mass splittings between the stop, neutralino(s), and chargino(s). Recent ATLAS results from searches for direct stop (sbottom) pair production are presented in final states with jets, missing transverse momentum, and leptons. The analyses are based on 36 fb$^{−1}$ of $\sqrt{s}=$13 TeV proton-proton collision data recorded with ATLAS detector at the LHC in 2015 and 2016.
Speaker: Dr Keisuke Yoshihara (University of Pennsylvania)
• 8
SUSY searches using top quark tagging at CMS
Results for searches for supersymmetry targeting top squarks and gluions will be presented in this talk. The analysis is optimized to specifically target top squark pair production and more generic supersymmetry signals with tops in the final state, including gluino pair production. These searches employ methods of tagging top quarks in the final state to reject standard model background in addition to traditional selection requirements such as missing transverse momentum. Due to the wide range of top quark transverse momentum and multiplicity produced in supersymmetric models, custom algorithms which combine traditional boosted top tagging techniques with algorithms designed to reconstruct tops combining individual reconstructed jets were developed. The results, using 35.9 ifb of data collected by the CMS experiment, are interpreted using simplified models of supersymmetry to place limits on top squark and gluino production.
Speaker: Nathaniel Pastika (Baylor University)
• 9
Search for supersymmetry in multijet events with missing transverse momentum in proton-proton collisions at 13 TeV
A search for supersymmetry is presented based on multijet events with large missing transverse momentum produced in proton-proton collisions at center-of-mass energy sqrt(s) = 13 TeV. The data, corresponding to an integrated luminosity of 35.9 fb-1, were collected with the CMS detector at the CERN LHC in 2016. The analysis utilizes four-dimensional exclusive search regions defined in terms of the number of jets, the number of tagged bottom quark jets, the scalar sum of jet transverse momenta, and the magnitude of the vector sum of jet transverse momenta. No evidence for a significant excess of events is observed relative to the expectation from the standard model. Limits on the pair production of gluinos and squarks are derived in the context of simplified models. Assuming the lightest supersymmetric particle to be a weakly interacting neutralino, 95% confidence level lower limits on the gluino mass as large as 1800 to 1960 GeV are derived, and on the squark mass as large as 960 to 1390 GeV, depending on the production and decay scenario.
Speaker: Kevin Pedro (Fermilab)
• 10
Search for production of supersymmetric particles in final states with missing transverse momentum and multiple b-jets at s√=13~TeV proton-proton collisions with the ATLAS experiment
A search for supersymmetry involving the pair production of gluinos decaying via third-generation squarks to the lightest neutralino (χ̃ 10) is reported. It uses LHC proton-proton collision data at a center-of-mass energy s√=13 TeV, corresponding to an integrated luminosity of 36 ifb collected with the ATLAS detector in 2015 and 2016. The search is performed in events containing large missing transverse momentum and several energetic jets, at least three of which must be identified as originating from b-quarks, and are also used to form large-R jets using jet reclustering. To increase sensitivity, the sample is further divided depending on the presence or absence of electrons or muons. No excess is found above the predicted background. For χ̃10 masses below approximately 200 GeV, gluino masses of less than 2.0 (1.9) TeV are excluded at the 95% CL in simplified models of the pair-production of gluinos decaying via top (bottom) squarks. An interpretation of the limits in terms of the branching ratios of the gluinos in third generation squarks is also provided. These results significantly extend the exclusion limits obtained with the 3.2 fb−1 of data collected in 2015, with the exclusion limit on the gluino mass extended by up to 250 GeV for the case of massless neutralinos.
Speaker: Giordon Stark (University of Chicago)
• 11
Revisiting Dyons in Particle Physics
Revisiting Dyons in Particle Physics Schwinger’s dyon is a bound system of a magnetic monopole and an electric charge. Suppose a monopole (B=g/r2) is a distance zo above an electric charge (E= q/r2). Then (in gaussian units) this system stores an angular momentum about the z-axis of L = qg/8πc regardless of the magnitude of zo. Schwinger proposed that all hadronic matter is composed of dyons: the mesons are a dyon and an anti-dyon, the baryons are three dyons. Dyons can lead to all three of the familiar forces in the Standard Model (Science Magazine , 1969). As proposed by Schwinger, the dyon complemented quarks: the smallest charge |qo|=(1/3)e. The smallest magnetic charge go is the Dirac monopole go=(137/2)qo. Quantized magnetic charge g substitutes for the now usual color. All hadrons are colorless. In a subsequent publication, Schwinger explicitly excluded the integrally-charged Han-Nambu quarks and, rightfully, claimed credit for the prediction of the mass of the J/ψ (Science, 1975). Two Colorado professors, Kalyana Mahanthappa and Asim Barut were keen participants in the discussion of dyons. Barut believed that all hadronic matter is made of integrally charged dyons. Thus “dyonium”. Mahanthappa worried about the axis implicit in the dyon. This axis makes the topology of the dyon two-dimensional. He argued that at least one dyon must disobey the usual connection between spin and statistics. We believe that both may have been right. Han-Nambu quarks are not caught by the very sensitive oil-drop experiment of Perl, Lee, and Loomba (2004). The parity of the b-“quark” is still not determined except in the context of the Standard Model (PDG-2016). It may not be a pseudoscalar. Schwinger had a novel treatment of the Cabibbo angle and predicted the mass of the W to be 53 GeV in an era when the only leptons were the muon and the electron. Perl’s discovery of the third lepton, the tau, came too late for physicists to appreciate that 80 GeV is 3/2 of 53 GeV. Recent data from LHCb hints that, in distinction to the KL, the B decays to an electron and an anti electron more often than it decays to a muon and an antimuon. Lifetime vs Mass data from the summary tables of PDG-2016 suggest regularities which Schwinger anticipated long ago. It might be useful to review whether the dyon model can really be excluded
Speaker: Mr David Bartlett (University of Colorado at Boulder)
• 12
Search for supersymmetry using boosted Higgs bosons and missing transverse momentum in proton-proton collisions at 13 TeV
CMS results at 8 and 13 TeV have placed bounds on gluino, squark, and electroweakino production in supersymmetric extensions to the Standard Model. The current sensitivity in some regions of phase space motivates more targeted searches. Depending on the mass spectra of the new particles, these models predict boosted objects, such as high pT vector bosons, in association with missing energy from sparticles escaping detection. A new analysis strategy using jet substructure techniques is applied in hopes of enhancing sensitivity to models where a boosted object can be contained in a single large jet. We will describe an analysis looking for evidence of supersymmetry in events with missing energy and boosted Higgs bosons (decaying to b-quarks) in the final state. We will compare our sensitivity to other analyses and describe the current limits on these production scenarios.
Speaker: Frank Jensen (University of Colorado)
• Cosmology and Astrophysics: Monday morning Comitium
### Comitium
#### Fermi National Accelerator Laboratory
Convener: Dr James Annis (Fermilab)
• 13
TeV Particle Astrophysics with the High Altitude Water Cherenkov (HAWC) Detector
The High Altitude Water Cherenkov (HAWC) Gamma-ray Observatory was completed in March 2015 and is now giving us a new view of the sky. HAWC is a continuously operating, wide field-of-view observatory situated near Puebla, Mexico that observes 0.5–100 TeV gamma rays. It is 15 times more sensitive than previous generation Extensive Air Shower gamma-ray instruments and is able to detect the Crab nebula at >5σ a day. HAWC operates 24 hrs/day with >95% on-time and observes the entire overhead sky (~2 sr) serving as a TeV “finder” telescope for Imaging Atmospheric Cherenkov Telescopes (IACTs). It monitors the same sky as gamma-ray satellites (Fermi), gravity-wave (LIGO) detectors and neutrino observatories (IceCube) allowing for multi-wavelength and multi-messenger observations. I will present highlights from HAWC’s first year and half of operations.
Speaker: Kirsten Tollefson (Michigan State University)
• 14
Constraints on the astrophysical flux and the dark matter decay with IceCube HESE data
The IceCube detection of High Energy Starting Events (HESE) and the upward muon track events (6 year data) are presently hard to explain with the single power-law astophysical flux for energies above 30TeV. We investigate the possibility that a significant component of the additional neutrino flux originates due to the decay of a very heavy dark matter particle via several possible channels into standard model particles. We perform a full 4 parameter fit to IceCube data in which we vary astrophysical flux normalization, power-law index, dark matter mass, dark matter lifetime and dark matter decay mode. We show that that dark matter with mass in the PeV range and the lifetime around 10^27s provides much better fit to IC data than the best-fit astrophysical flux alone. We also find dark matter lifetime limits which are much stronger that those obtained from gamma-ray data for all channels except $b \bar{b}$, which is also disfavored by the IceCube HESE data.
Speaker: Prof. INA SARCEVIC (UNIVERSITY OF ARIZONA)
• 15
Searching for Dwarf Galaxies with DECam
Milky Way satellite dwarf galaxies are some of the oldest, smallest, and most dark matter dominated galaxies in the known universe. The study of these tiny dwarf galaxies can help shed light on the nature of dark matter and the mysteries of galaxy formation. Over the last two years, efforts using the Dark Energy Camera (DECam) have nearly doubled the known population of Milky Way satellite galaxies. However, to date, only a fraction of the southern sky has been uniformly imaged by DECam. I will present results from two new surveys, the Magellanic Satellites Survey (MagLiteS) and the Blanco Imaging of the Southern Sky (BLISS) survey, which are using DECam to image the southern sky at unprecedented depths.
Speaker: Alex Drlica-Wagner (Fermilab)
• 16
Constraining the Nature of Dark Matter with the Milky Way Satellite Galaxies
The census of Milky Way satellite galaxies provides crucial tests of both galaxy formation models and the broader Cold Dark Matter paradigm. A total of 27 new Milky Way satellite candidates have been discovered in the last two years, primarily in data from the Dark Energy Survey. These discoveries may represent a 100% increase in the number of known Milky Way satellite galaxies, leading a huge advance in solving the missing satellite problem, if spectroscopic follow-up observations confirm the majority of these systems are dark matter dominated dwarf galaxies. Furthermore, many of these newly discovered dwarf galaxies are excellent targets for providing constraints on WIMP dark matter cross section and MACHO dark matter abundance with the spectroscopic follow-up analysis. In this talk, I will present the initial results from a spectroscopic campaign on the newly discovered dwarf galaxy candidates using 4-8 meter class telescopes in the southern hemisphere.
Speaker: Ting Li (Fermilab)
• 17
Study of Galaxy Evolution in DES Clusters
Clusters of galaxies represent a powerful probe for cosmology in the era of large photometric surveys such as the Dark Energy Survey. At the same time, understanding the astrophysical processes that drive their evolution is needed for a correct cosmology: cluster galaxies show particular properties with respect to field galaxies, processes like cluster membership selection often require knowledge of clusters and galaxy evolution. In particular, the efficiency with which halos convert the matter they contain into stars is still matter of debate and it is crucial for understanding galaxy formation and evolution. We present a measurement of the stellar-to-halo mass relation for the DES Year 1 redmapper clusters, showing the results for centrals, satellites and total content. We also explore the evolution of the fraction of blue galaxies and the star formation rate. We show that stellar mass is also a powerful mass proxy for clusters by comparing our results to X-ray temperature measurements that overlap with the DES Y1 footprint.
Speaker: Antonella Palmese (Fermilab/UCL)
• Dark Matter: Monday morning Hornets Nest
### Hornets Nest
#### Fermi National Accelerator Laboratory
Convener: Prof. Rafael Lang (Purdue University)
• 18
Dark matter collider at DUNE: relativistic scattering of boosted dark matter
I will talk about a novel dark matter (DM) detection strategy for the models with non-minimal dark sector such as "inelastic boosted DM", which expects a secondary cascade signature after an inelastic and relativistic scattering of a light dark matter component. I will discuss the detection prospects at DUNE. The boosted DM can be produced both in the current universe and in the fixed target.
Speaker: Dr Seodong Shin (Yonsei University)
• 19
The SuperCDMS Soudan High Mass Analysis
The SuperCDMS Soudan experiment searches for direct interactions of WIMP dark matter particles with germanium nuclei. The experiment uses detectors (iZIPs) with sophisticated ionization and phonon sensors to distinguish nuclear-recoils from electron-recoil backgrounds or surface contaminants. We report the result of an analysis, based on a ∼1700 kg-day exposure, that seeks to maximize our experimental sensitivity to spin-independent WIMP-nucleon interaction in the high mass regime (M > 10 GeV/c^2).
Speaker: Mr Brett Cornell (Caltech)
• 20
Dark Matter Search Results from the PICO-60 C3F8 Bubble Chamber
The PICO-60 dark matter detector has recently concluded its first run with a C3F8 target, producing a new world-leading limit on WIMP-proton spin-dependent interactions, a factor of 17 stronger than PICO’s previous leading result. This result is obtained from a blind 30 live-day run that contained zero WIMP candidate events and re-affirms the dominance of the bubble chamber technology in searching for this type of interaction. The absence of events confirms that the bubble chamber technology is background-free and ready for future ton-scale dark matter detectors.
Speaker: Dr Orin Harris (NEIU)
• 21
The SENSEI project
We present the status and prospects of the Sub-Electron Noise Skipper Experimental Instrument (SENSEI) currently operating in the MINOS cavern at Fermilab. SENSEI uses a non-destructive readout technique to achieve stable readout for a thick fully depleted silicon CCD in the far sub-electron regime (∼ 0.05 e- rms/pix). This is the first instrument to achieve discrete sub-electron counting reproducibly over millions of pixels on a stable, large-area detector. This innovative technology has nearly immediate implications for a wide range of scientific disciplines including Dark Matter Direct detection experiments, astronomy and fundamental particle physics.
Speaker: Dr Javier Tiffenberg (Fermilab)
• 22
The DAMIC Experiment at SNOLAB
Millimeter-thick charge-coupled devices (CCDs) are outstanding particle detectors. Although initially developed for near-infrared astronomy, the low pixel noise also makes them the most sensitive detectors to signals from ionizing radiation. By virtue of their very low energy threshold (<100 eV of ionizing energy) and their unique capabilities for background characterization based on their high spatial resolution, CCDs are poised to become the leading technology in the search for a wide variety of dark matter candidates with masses in the range 1 eV/c/c – 10 GeV/c/c. I will present the status of the DAMIC100 experiment, an ongoing direct dark matter search consisting of an array of 16-Mpixel CCDs hosted in the low-radioactivity environment of the SNOLAB underground laboratory. I will also discuss the recent progress toward DAMIC-1K, a lower-background 1-kg CCD dark matter detector with an ionization threshold of 2 electrons.
Speaker: Dr Juan Estrada (FNAL)
• 23
Light Dark matter eXperiment
The Light Dark Matter eXperiment (LDMX) proposes a high-statistics search for dark matter in fixed-target electron-nucleus collisions, ultimately exploring thermal relic dark matter over most of the viable sub-GeV mass range to a decisive level of sensitivity. To achieve this goal, LDMX employs the missing momentum technique, where electrons scattering in a thin target can produce dark matter via “dark bremsstrahlung” giving rise to significant missing momentum and energy in the detector. To identify these rare signal events, LDMX individually tags incoming beam-energy electrons, unambiguously associates them with low energy, moderate transverse-momentum recoils of the incoming electron, and establishes the absence of any additional forward-recoiling charged particles or neutral hadrons. LDMX will employ low mass tracking to tag incoming beam-energy electrons with high purity and cleanly reconstruct recoils. A high-speed, granular calorimeter with MIP sensitivity is used to reject the high rate of bremsstrahlung background at trigger level while working in tandem with a hadronic calorimeter to veto rare photo nuclear reactions. This talk will summarize the small-scale detector concept for LDMX, ongoing performance studies, and near future prospects.
Speakers: Andrew Whitbeck (Fermilab), Dr Philip Schuster (SLAC)
• Higgs and EWSB: Monday morning Sunrise
### Sunrise
#### Fermi National Accelerator Laboratory
Convener: Prof. Tulika Bose (Boston University)
• 24
Higgs-boson physics at the LHC: from discovery to precision physics.
The LHC Higgs-boson physics programme is broad and challenging. The progress of experimental analyses has been matched by an unprecedented theoretical effort to describe both production and decay properties of the Standard-Model Higgs boson. In most cases the measurement of Higgs production and properties is not limited these days by theoretical systematic, but cases still exist where this is the case. In these cases, further effort to reach a more satisfactory theoretical accuracy will have to be matched by a dedicated program of experimental measurements. In this talk I will review the interplay between theory and experiments in defining a Higgs precision-physics program, and I will discuss how, when combined with global electroweak precision fits, this can be used to constrain extensions of the Standard Model.
Speaker: Laura Reina (Florida State University)
• 25
Measurement of Higgs boson production in the diphoton decay channel with the ATLAS experiment
The measurement of the production cross section of the Higgs boson in the diphoton decay channel is presented, using proton-proton collision data collected at √s=13 GeV by the ATLAS experiment 2015 and 2016. Diphoton candidate events from different production modes are analyzed by a simultaneous fit to the invariant mass spectrum.
Speaker: Zirui Wang (Shanghai Jiao Tong Univ. / U.Michigan)
• 26
Inclusive search for boosted SM Higgs bosons using H to bb decays with the CMS detector at 13 TeV
We present an inclusive search for the standard model Higgs boson produced with high transverse momentum decaying to a bottom-antibottom quark pair using a data set of pp collisions at 13 TeV collected with the CMS experiment at the LHC in 2016. The data sample corresponds to an integrated luminosity of 35.9 inverse femotbarns. High-transverse-momentum Higgs bosons are reconstructed in a single jet with opening angle corresponding to R = 0.8. Jet substructure and dedicated b-tagging techniques are used to identify boosted H to bb.
Speaker: Javier Duarte (Fermilab)
• 27
Search for SM Higgs Boson in the H->tautau->mumu decay mode with the CMS experiment at 13TeV
A search for standard model (SM) Higgs bosons decaying into pairs of tau leptons and then to two muons plus (anti)-neutrinos are presented. The analysis is performed using data collected by the CMS detector in 2016 with 35.9 $fb^{-1}$ of integrated luminosity. This channel has been studied in three event categories with different jet multiplicities focusing on Higgs boson signal events produced via gluon-gluon fusion and vector boson fusion. A multivariate analysis with boosted decision trees (BDT) is used to suppress the large Drell-Yan background. The di-tau mass is reconstructed using a secondary-vertex fit (SVFit) algorithm using a maximum likelihood approach. Experimental limits are presented in all three categories extracted from two-dimensional maximum likelihood fit in the plane of reconstructed di-tau mass and BDT response.
Speaker: Ms Vallary Bhopatkar (Florida institute of Technology)
• Neutrino Physics: Monday morning Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
Kirk Road & Pine Street Batavia, IL 60510-5011
Convener: Dr JYOTI JOSHI (Brookhaven National Laboratory)
• 28
Sterile Neutrino Searches with NOvA
The existence of light sterile neutrinos would have profound implications for both particle physics and cosmology. The NOvA (NuMI Off-Axis ve Appearance) experiment is sensitive to new neutrino flavors through searches for the disappearance of the known active neutrinos from the NuMI beam over a baseline of 810 km. We describe the method used by NOvA to look for oscillations into sterile neutrinos, with a focus on the disappearance of neutral-current (NC) neutrino events. We present the results from the first NC Disappearance analysis using 6.05E20 POT of neutrino data, and discuss the status and outlook for ongoing and future sterile neutrino searches with NOvA, at both long and short baselines.
Speaker: Dr Gavin S. Davies (Indiana University)
• 29
The Short Baseline Near Detector at Fermilab
SBND (Short-Baseline Near Detector) is a 112 ton liquid argon TPC neutrino detector under construction on the Fermilab Booster Neutrino Beam. Together with MicroBooNE and ICARUS-T600, SBND will search for shortbaseline neutrino oscillations in the 1 eV^2 mass range. SBND will also perform detailed studies of the physics of neutrino-argon interactions, thanks to a data sample of millions of electron and muon neutrino interactions. Finally SBND plays an important role in the on-going R&D effort to develop the LArTPC technology, testing several technologies that can be used in a future kiloton-scale neutrino detectors for a long-baseline experiment. We will discuss the detector design, its current status, and the physics program.
Speaker: Dr José Ignacio Crespo-Anadón (Columbia University Nevis Laboratories)
• 30
Improved Search for a Light Sterile Neutrino at Daya Bay, and Combined Analysis with MINOS and Bugey-3
Reactor neutrino experiments are well-suited for probing the existence of a light sterile neutrino in the region of a sub-eV$^2$ mass splitting (largely unexplored until recently). Using eight functionally identical antineutrino detectors (ADs), the Daya Bay experiment measures the electron antineutrinos produced by six 2.9 GW commercial nuclear reactors located near Shenzhen, China. By combining 404 days of 8-AD data with 217 days of 6-AD data (previously reported), a sample of 1.2 million antineutrino candidates was used to test for oscillations to a sterile fourth neutrino in the mass range of $2\times 10^{-4}\, \lesssim \Dm241 \lesssim 0.3$ eV$^2$. Joint fits were performed for $\theta_{13}$, $\theta_{14}$, and $\Dm241$, dominated either by the ratio of the two near-hall spectra (for $\Dm241 \gtrsim 0.01$ eV$^2$) or the ratio of far to near-hall spectra (for smaller splittings). Independent fits were performed using two techniques, a covariance matrix approach and one using nuisance parameters, and limits were set using the Feldman-Cousins and CL$_s$ methods, respectively. The two methods were mutually consistent within expectation, and found no evidence for a sterile neutrino in the mass range considered. For $\Dm241 \lesssim$ 0.2 eV$^2$, 95\% C.L. limits of $\sin^22\theta_{14}\,\lesssim 0.01$ were set, forming the most stringent constraints to date in this region. Going further, sensitivity was extended for $0.2 \lesssim \Dm241 \lesssim 2$ eV$^2$ by including the results of the Bugey-3 short-baseline reactor experiment in a combined reanalysis. Finally, the addition of MINOS acclerator neutrino data enabled strong constraints to be set on $\sin^2 2\theta_{\mu e} = 4|U_{e4}|^2|U_{\mu4}|^2$, which governs the strength of the anomalous short-baseline signals claimed by the LSND and MiniBooNE experiments. This three-experiment joint analysis excludes the LSND/MiniBooNE allowed regions for $\Dm241 \lesssim 1$~eV$^2$ at 90\% C.L., significantly constraining the allowed parameter space for a four-flavor explanation of the anomaly.''
Speaker: Mr Matt Kramer (UC Berkeley)
• 31
Evolution of the Reactor Antineutrino Flux and Spectrum at Daya Bay
The Daya Bay experiment has utilized eight functionally identical underground detectors to sample reactor antineutrino fluxes from three pairs of nuclear reactors in South China, accruing the largest reactor antineutrino sample to date. This talk will summarize Daya Bay’s most recent result, which presents observations of correlations between reactor core fuel evolution and changes in the detected reactor antineutrino flux and energy spectrum. Four antineutrino detectors in two experimental halls were used to identify 2.2 million inverse beta decays (IBDs) over 1230 days spanning multiple fuel cycles for each of Daya Bay’s six 2.9 GW reactor cores. A 10σ variation in IBD yield was found to be energy-dependent, rejecting the hypothesis of a constant antineutrino energy spectrum at 5.1 standard deviations. While measurements of the energy-dependence of this variation show general agreement with predictions from recent reactor models, the variation in integrated IBD yield disagrees with recent predictions at 3.1σ. This discrepancy indicates that an overall deficit in measured flux with respect to predictions does not result from equal fractional deficits from the primary fission isotopes 235U, 239Pu, 238U, and 241Pu. A 7.8% discrepancy between the observed and predicted 235U yield suggests that this isotope may be the primary contributor to the reactor antineutrino anomaly.
Speaker: Dr David Martinez Caicedo (Illinois Institute of Technology)
• Particle Detectors: Monday morning IARC Building
### IARC Building
#### Fermi National Accelerator Laboratory
Convener: Mr Diego Tonelli (INFN Trieste)
• 32
Microhexcavity Plasma Panel Detectors
Plasma panel detectors are a variant of micropattern detectors that are sensitive to ionizing radiation. They are motivated by the design and operation of plasma display panels. The detectors consist of arrays of electrically and optically isolated pixels defined by metallized cavities embedded in a dielectric substrate. These are hermetically sealed gaseous detectors that use exclusively non-hydrocarbon gas mixtures. The newest variant of these “closed-architecture” detectors is known as the Microhexcavity plasma panel detector (µH-PPS), consisting of 2 mm wide, regular close-packed hexagonal pixels each with a circular thin-film anode. The fabrication, staging, and operation of these detectors is described. Initial tests with the µH-PPS detectors operated in Geiger mode yield Volt-level signals in the presence of ionizing radiation. The spontaneous discharge rate in the absence of a source is roughly 2-3 orders of magnitude lower compared to the rates measured using low energy betas.
Speaker: Alexis Mulski (University of Michigan)
• 33
Ultra long-lived particles searches with MATHUSLA
Many extensions of the Standard Model (SM) include particles that are neutral, weakly coupled, and long-lived that can decay to final states containing several hadronic jets. Long-lived particles (LLPs) can be detected as displaced decays from the interaction point, or missing energy if they escape. ATLAS and CMS have performed searches at the LHC and significant limits have been set in recent years. However, the current searches performed at colliders have limitations. A LLP does not interact with the detector and it is only visible once it decays. Unfortunately, no existing or proposed search strategy will be able to observe the decay of non-hadronic electrically neutral LLPs with masses above ~ GeV and lifetimes near the limit set by Big Bang Nucleosynthesis (cτ ~ 107-108 m). Therefore, ultra-long-lived particles (ULLPs) produced at the LHC will escape the main detector with extremely high probability. In this talk we describe the concept of the MATHUSLA surface detector (MAssive Timing Hodoscope for Ultra Stable neutraL pArticles), which can be implemented with existing technology and in time for the high luminosity LHC upgrade to find such ultra-long-lived particles, whether produced in exotic Higgs decays or more general production modes. The MATHUSLA detector will consist of resistive plate chambers (RPC) and scintillators with a total sensitive area of 200x200 m square. It will be installed on the surface, close to the ATLAS or CMS detectors. A small-scale test detector (~ 6 m square) is going to be installed on the surface above ATLAS in June 2017. It will consist of three layers of RPCs used for tracking and two layers of scintillators for timing measurements. It will be placed above the ATLAS interaction point to estimate cosmic backgrounds and proton-proton backgrounds coming from ATLAS during nominal LHC operations. We will report on the status of the test detector, on the on-going background studies, and plans for the main detector.
Speaker: Prof. Gordon Watts (University of Washington)
• 34
Overview of the CEPC Vertex Detector
he Circular Electron Positron Collider (CEPC) has been proposed to measure with unprecedented precision the Higgs properties as well as the electroweak parameters. Its vertex detector that will be located as close as possible to the interaction point, must be built with state-of-the-art pixel detector technologies. In the presentation, performance requirements including single point resolution, readout time, and radiation hardness against total ionization dose (TID) and non-ionization energy loss (NIEL) will be explained. Potential candidate technologies and their R&D progress will be discussed together with the detector layout optimization. In addition, a preliminary design of the complicated interaction, which has dramatical impacts on the vertex detector will be also presented
Speaker: Dr Hongbo Zhu (Institute of High Energy Physics)
• 35
Optical Ring Resonators for HEP and Cosmology Applications
Optical ring resonators have been used in telecommunications and other fields, but so far not in HEP. Used as wavelength notch filters, they could have a major impact in reducing infrared sky background for future cosmology surveys. Ring resonators also are a potential low mass, low power, fast, and compact technology for readout of pixel tracking detectors and/or implementing pattern triggering. We describe a current R&D effort in fabrication and testing prototype optical ring resonators for multiple HEP applications.
Speaker: Stephen Kuhlmann (Argonne National Laboratory)
• 36
The Construction and Commissioning of the Belle II iTOP Counter
The barrel-region particle identification detector is crucial for extending the physics reach of the Belle II experiment operating at the SuperKEKB accelerator. For this purpose, an imaging-Time-of-Propagation (iTOP) counter was developed, which is a new type of ring-imaging Cherenkov detector. The iTOP consists of 16 separate modules arranged azimuthally around the beam line. Each module consists of optical components fabricated from quartz (one mirror, one prism, and two bars), an array of micro-channel-plate photo-multiplier tubes (MCP-PMTs), and front-end electronics. The waveforms read out are processed by firmware, and the resulting pulse-heights and hit times are sent to the Belle II data acquisition system. The detector construction was completed and the detector installed by the summer of 2016, and since then the detector has undergone commissioning. This talk describes the construction and commissioning of the Belle II iTOP counter.
Speaker: Dr Boqun Wang (University of Cincinnati)
• QCD: Monday morning Racetrack
### Racetrack
#### Fermi National Accelerator Laboratory
Convener: Radja Boughezal (Argonne National Laboratory)
• 37
PDF Flavor Determination with LHC W/Z production
We use nCTEQ15 nPDFs with uncertainties to identify measurements which have a potential impact on nuclear corrections and flavor differentiation. In particular, recent LHC W/Z vector boson production data in proton-lead and lead-lead collisions are quite sensitive to heavier flavors (especially the strange PDF). This complements the information from neutrino-DIS data. As the proton flavor determination is dependent on nuclear corrections (from heavy target DIS, for example), this information can also help improve proton PDFs.
Speaker: Prof. Fredrick Olness (SMU)
• 38
Update on CTEQ-TEA PDFs
We present recent progress on the parton distribution functions (PDFs) of the proton from the CTEQ-TEA collaboration.
Speaker: Carl Schmidt (Michigan State University)
• 39
Refinement of the Pion PDF implementing Drell-Yan Experimental Data
The proton is more complex than a collection of three valence quarks. We realize that an abundance of “sea” quarks and gluons is crucial to understanding the mass and internal structure of the proton. The pion is intimately related with the proton as analyses indicate an effective pion cloud exists around the core valence structure. In the Drell-Yan (DY) process, two hadrons (such as protons or pions) collide, one donating a quark and the other donating an antiquark. The quark-antiquark pair annihilate, forming a virtual photon, which creates a lepton-antilepton pair. By measuring the cross-section of the dilepton pair, we obtain rich information about the parton distribution function (PDF) of the hadrons. The PDF is the probability of finding a parton (quark, antiquark, or gluon) at a momentum fraction of the hadron, x, between 0 and 1. Experiments performed at Fermilab such as E866 and SeaQuest collect data in the DY process. Determining the pion PDFs from the DY process stems from understanding the abundance of sea quarks. Complementary to the DY process is deep inelastic scattering (DIS). Here, a target nucleon is probed by a lepton, and we investigate the pion cloud of the nucleon. The experiments H1 and ZEUS done at HERA at DESY collect DIS data. Both DY and DIS processes can measure small and large x depending on kinematics. Numerically, we have implemented the DY cross-section and have obtained the result consistent with (Becher, et al. 2008). Now, we perform a double-Mellin transform on the hard-scattering kernel to easily evolve the PDFs over energy scales as in (Stratmann and Vogelsang, 2001). We present some preliminary fits of pion PDFs to DY datasets from Fermilab-E615 and CERN-NA10. We aim to perform a full NLO QCD global analysis and a state-of-the-art fitting technique to all available data for DY and DIS as in (McKenney, et al. 2016) to determine pion PDFs more accurately in all x regions.
Speaker: Mr Patrick Barry (North Carolina State University)
• 40
Are PDFs still consistent with Tevatron data?
As active data taking has moved to the LHC at CERN, more and more LHC data have been included into fits of parton distribution functions. An anomaly has arisen where formerly excellent agreement between theoretical predictions and experiment in single-top-quark production at the Tevatron is no longer very good. Is this indicative of a deeper issue?
Speaker: Prof. Zack Sullivan (Illinois Institute of Technology)
• Quark and Lepton Flavor: Monday morning Curia II
### Curia II
#### Fermi National Accelerator Laboratory
Convener: Prof. Alexey Petrov (Wayne State University / MCTP)
• 41
The Mu2e Experiment at Fermilab
Searching for Muon to electron conversion : The Mu2e experiment at Fermilab The Mu2e experiment will measure the charged-lepton flavor violating (CLFV) neutrino-less conversion of a negative muon into an electron in the field of a nucleus. The conversion process results in a monochromatic electron with an energy slightly below the muon rest mass (104.97 MeV). Mu2e will improve the previous measurement by four orders of magnitude using a new technique, reaching a SES (single event sensitivity) of 2.5 x 10^{-17} on the conversion rate. The experiment will reach mass scales of nearly 10^4 TeV, far beyond the direct reach of colliders. The experiment is sensitive to a wide range of new physics, complementing and extending other CLFV searches. Mu2e is under design and construction at the Muon Campus of Fermilab; we expect to start in 2020 with 3 years of running from 2021 to 2023.
Speaker: Dr Yuri Oksuzian (Univeristy of Virginia)
• 42
Lepton-flavour violation in a Pati-Salam model with gauged flavour symmetry
Combining Pati-Salam (PS) and flavour symmetries in a renormalisable setup, we devise a scenario which produces realistic masses for the charged leptons. Flavour-symmetry breaking scalar fields in the adjoint representations of the PS gauge group are responsible for generating different flavour structures for up- and down-type quarks as well as for leptons. The model is characterised by new heavy fermions which mix with the Standard Model quarks and leptons. In particular, the partners for the third fermion generation induce sizeable sources of flavour violation. Focusing on the charged-lepton sector, we scrutinise the model with respect to its implications for lepton-flavour violating processes such as $\mu \rightarrow e\gamma$, $\mu\rightarrow 3e$ and muon conversion in nuclei.
Speaker: Paul Moch (Theoretische Physik 1, University of Siegen)
• 43
Lepton flavor violating meson decays
We argue that lepton flavor violating (LFV) decays $M \to \ell_1 \overline \ell_2$ of quarkonium and heavy quark meson states $M$ with different quantum numbers could be used to put constraints on the Wilson coefficients of effective operators describing LFV interactions at low energy scales. We note that the restricted kinematics of the two-body decay of quarkonium or a heavy quark meson allows us to select operators with particular quantum numbers, significantly reducing the reliance on the single operator dominance assumption that is prevalent in constraining parameters of the effective LFV Lagrangian. We shall also argue that studies of radiative lepton flavor violating $M \to \gamma \ell_1 \overline \ell_2$ decays could provide important complementary access to those effective operators.
Speaker: Mr Derek Hazard (Wayne State University)
• 44
Flavor gauge models below the Fermi scale
In this talk I will construct a flavor model with a gauge boson below the weak scale. The model is viable and shows the synergy between low energy observables, meson decays, neutrino oscillations, and LHC physics. The role of neutrinos will be highlighted.
Speaker: Pedro Machado (Fermilab)
• 45
Gauge Model for Minimal Flavor Violation
We present a flavor gauge model based on $O(3)_L \times O(3)_R$ gauge symmetry, a maximal anomaly-free subgroup of the standard model flavor symmetry. In this model the fermion mass hierarchy has a dynamical origin. The model provides a UV complete realization of the Minimal Flavor Violation Hypothesis. Implications for quark sector and lepton sector flavor violation arising through higher dimensional effective operators involving the Higgs field are outlined. CP violation arising from these operators is also studied. Vector-like fermions responsible for the generation of the top quark, bottom quark, and the tau lepton masses are in the TeV range, and potentially within reach of the LHC.
Speakers: K.S. Babu (Oklahoma State University), Shaikh Saad (Oklahoma State University)
• Top Quark Physics: Monday morning 1 East
### 1 East
#### Fermi National Accelerator Laboratory
Convener: Prof. Stephen Wimpenny (University of California - Riverside)
• 46
Top-pair and tW production at approximate N^3LO
I present approximate N^3LO theoretical results for top-antitop pair production and for single-top production in association with a W boson. The higher-order corrections are from soft-gluon radiation which is dominant near partonic threshold. I present results for total cross sections as well as transverse-momentum and rapidity distributions of the top quark and compare with data at LHC energies.
Speaker: Prof. Nikolaos Kidonakis (Kennesaw State University)
• 47
Measurement of quantum interference between doubly and singly resonant top quark production with the ATLAS experiment
Physics processes involving top quarks compose a major background for many searches for new physics. Both doubly-resonant "ttbar" and singly-resonant "single top" processes can contribute at similar levels where sophisticated tools are used to effectively reduce ttbar backgrounds. However, because both ttbar and Wt single top with an additional b-quark in the final state can yield an identical final state (WWbb) the processes quantum-mechanically interfere. The ambiguity in how this interference is modeled can lead to large theoretical uncertainties on the Wt prediction. A measurement is presented that is designed to probe the WWbb final state in a region of large interference, selecting final states with two isolated leptons and b-tagged jets. The result uses data from pp collisions delivered by the Large Hadron Collider in 2015 and 2016 at a center-of-mass energy of 13 TeV recorded by the ATLAS detector, corresponding to an integrated luminosity of 36/fb. Differential distributions of interference-sensitive variables are measured and subsequently unfolded to truth level. The analysis is sensitive to differences in the modeling of the interference term provided by state-of-the-art WWbb generators
Speaker: Theodor Christian Herwig (University of Pennsylvania)
• 48
Measurement of the cross section of the production of a top quark pair in association with a photon in pp collisions at 8 TeV
A measurement of the cross section of top quark pairs produced in association with a photon is presented. The data were collected by the CMS experiment in proton-proton collisions at a center of mass energy of 8 TeV. The measurement is performed in the electron+jets and muon+jets final state. The fiducial cross section for top quark pair plus photon production is measured in the phase space corresponding to the semileptonic decay of the top quark pair with a 25 GeV photon, and is measured relative to the cross section of inclusive top quark pair production.
Speaker: Daniel Noonan (Florida Institute of Technology)
• 49
Measurement of the $t\bar{t}$ spin correlations and top quark polarization in dileptonic channel
The degree of top polarization and strength of $t\bar{t}$ correlation are dependent on production dynamics, decay mechanism, and choice of the observables. At the LHC, measurement of the top polarization and spin correlations in $t\bar{t}$ production is possible through various observables related to the angular distribution of decay leptons. A measurement of differential distribution provides a precision test of the standard model of particle physics and probes for deviations, which could be a sign of new physics. In particular, the phase space for the super-symmetric partner of the top quark can be constrained. We present updates to the recent top quark polarization and spin correlation studies in dileptonic channel at the Compact Muon Solenoid experiment.
Speaker: Dr Ajeeta Khatiwada (Purdue University)
• 50
Measuring Polarized Gluon Distributions by Heavy Quark Spin Correlations and Polarizations
The production of heavy flavor quark pairs, including top-anti-top, at the LHC proceeds primarily through gluon fusion. The correlation between the gluon spins affects various spin correlations between the produced quark and anti-quark. Both single spin asymmetries and double correlations of the quark pair spins will be manifest in the subsequent hadronization and decay distributions. For top pairs this is most pronounced. Dilepton, single lepton, and purely hadronic top pair decay channels allow for the extraction of gluon spin information as well as providing a window into possible interactions Beyond the Standard Model. The derivations of many spin related asymmetries and polarizations will be presented. The implications for experimental determination will be discussed.
Speaker: Prof. Gary Goldstein (Tufts University)
• 51
Forward-backward asymmetry in pp̄ → tt̄ events at the Tevatron
We discuss the complete overview of the forward-backward asymmetry measurements in the angular distributions of pp̄ → tt̄ events at the Tevatron collider. These measurements use the full Run II data set in lepton plus jets and dilepton channels, recorded in the D0 and CDF detectors, corresponding to an integrated luminosity of ≈ 2 × 10 fb −1 . The combinations of inclusive and differential asymmetries are presented and compared with the NNLO QCD predictions.
Speakers: Collaboration CDF (Fermilab), Collaboration D0 (Fermiab), Ziqing Hong (Northwestern University)
• Lunch
• 52
DOE PIs Meeting: HEP Civics
Speaker: Dr Michael Cooke (U.S. Department of Energy)
• Meetings with DOE Representatives: HEP Civics 1 West
### 1 West
#### Fermi National Accelerator Laboratory
Kirk Road & Pine Street Batavia, IL 60510-5011
Convener: Dr Michael Cooke (U.S. Department of Energy)
• 53
HEP Civics
Speaker: Dr Michael Cooke (U.S. Department of Energy)
• Beyond Standard Model: Monday afternoon 1 West
### 1 West
#### Fermi National Accelerator Laboratory
Convener: Dr Bjoern Penning (Fermilab/UChicago)
• 54
Searches for electroweakly produced supersymmetry with CMS
In supersymmetry, most solutions to the hierarchy problem feature light higgsinos, since it is the most important ingredient to stabilize the Standard Model higgs mass. Light higgsinos, however, are notoriously difficult to detect. This talk will outline the challenges of finding higgsinos and present various search results and techniques, that focus on supersymmetric models where colored sparticles are out of reach at the LHC and electroweakino production is the dominant process beyond the Standard Model. The searches are performed on data corresponding to an integrated luminosity of 36 fb-1 and a center of mass energy of 13 TeV, recorded with the CMS detector at the CERN LHC in 2016.
Speaker: Mr Basil Schneider (FNAL)
• 55
Search for compressed supersymmetry using low pT leptons and missing transverse energy with the ATLAS detector
A search is presented for the electroweak production of gauginos, the supersymmetric partners of the Standard Model gauge bosons, in a scenario where the mass difference between the lightest supersymmetric particle (LSP) and other light gauginos is small, resulting in decays to virtual W/Z bosons and the LSP. The search is based on 36 fb^-1 of sqrt(s) = 13 TeV data collected by the ATLAS detector at the LHC in 2015 and 2016. The signature is two or three low transverse momentum (pT) charged leptons (e, mu) and large missing transverse energy, which is enhanced by requiring a high pT initial state radiation jet. The use of very low pT leptons poses challenges for triggering, particle identification, and background estimation.
Speaker: Joseph Reichert (University of Pennsylvania)
• 56
Search for electroweak production of supersymmetric particles in the two and three lepton final state at $\sqrt s = 13$ TeV with the ATLAS detector
Supersymmetry gives a solution to naturalness as well as a candidate for dark matter by predicting a new bosonic (fermionic) partner for each Standard Model fermion (boson). Searches for electroweak production of supersymmetric particles decaying via sleptons and gauge bosons, $W$ and $Z$, to final states with two or three leptons and missing transverse momentum were performed with the ATLAS detector. The search uses proton-proton collisions at $\sqrt s = 13$ TeV recorded with the ATLAS detector at the LHC during 2015 and 2016 corresponding to $36fb^{-1}$. No significant excesses over the Standard Model were observed so exclusion limits are set on masses of the gauginos, the supersymmetric partners of $W^{\pm}$, $Z^{0}$, and $h$, in simplified models.
Speaker: Elodie Resseguie (University of Pennsylvania)
• 57
One-loop effects on Z boson decays in the SM EFT
I will present partial one-loop corrections to SM EFT parameterizations of new physics effects on Z boson decays, and discuss the impact of LEP I data on SM EFT fits. The findings indicate that any measurement which reaches percent-level sensitivity to new physics effects in Z decays, like the precise LEP data, cannot be consistently used at higher precision to reach fixed conclusions on Wilson coefficients, as too many operators contribute at loop level which are currently not constrained in a consistent EFT treatment. This work motivates further effort in understanding the correct treatment of high energy, non-resonant data in an EFT context.
Speaker: Dr William Shepherd (JGU Mainz)
• 58
Little hierarchy in the minimally specified MSSM
We study constrained versions of the minimal supersymmetric model and investigate the hierarchy between the electroweak scale and the scale of superpartners that can be achieved without relying on specifying model parameters by more than one digit. This approach automatically avoids scenarios in which a large hierarchy is obtained by special choices of parameters and yet keeps scenarios that would be otherwise disfavored by various sensitivity measures. We consider models with universal gaugino and scalar masses, models with non-universal Higgs masses or non-universal gaugino masses and focus on scenarios in which all the model parameters are either of the same order or zero at the grand unification scale. We find that the maximal hierarchy between the electroweak scale and stop masses, requiring that model parameters are not specified beyond one digit, ranges from a factor of 30 for the CMSSM up to 300 for models with non-universal Higgs or gaugino masses.
Speaker: Prof. Radovan Dermisek (Indiana University)
• 59
Imposing LHC constraints on the combined Anomaly and Z'-Mediation mechanism of Supersymmetry Breaking
Combining anomaly with Z' mediation of SUSY breaking allows us to solve the tachyonic problem of the former and avoid fine tuning in the latter. This scenario includes an extra U(1)' gauge symmetry and extra singlet scalar S which provides a solution to the ‘µ problem’ of the MSSM. The low-energy particle spectrum is calculated from the UV inputs using the Renormalization Group Equations. The benchmark points considered in the original model, suggested before the Higgs discovery, predicted a Higgs mass close to the current measured value of 125 GeV. We use the current LHC data to update the predictions of the model, its particle spectrum and in particular the mass of the Z' gauge boson.
Speaker: Mr Joydeep Roy (Wayne state University)
• 60
Critical behavior of SU(3) lattice gauge theory with 12 light flavors
It is expected that when the number of light flavors of QCD-like theories is increased beyond some critical value, a transition having some Kosterlitz-Thouless features occurs. We report numerical results for a four-dimensional SU(3) lattice gauge theory with 12 flavors of unimproved staggered fermions. We show that the scaling of the imaginary part of the zeros of the partition function in the complex coupling plane is consistent with a first order phase transition for small values of the mass. We report searches for the endpoint of the line of first order phase transition in the mass-coupling plane. A light and weakly interacting scalar is expected near this endpoint. We present recent calculations of the second-order Renyi entanglement entropy for the two-dimensional O(2) model and show that it allows to delimit the Kosterlitz-Thouless phase in the chemical potential-coupling plane. We discuss the possibility of calculating this quantity for gauge theories with fermions.
Speaker: Yannick Meurice (U. of Iowa)
• Computing, Analysis Tools, and Data Handling: Joint session with Particle Detectors, Monday afternoon 1 East
### 1 East
#### Fermi National Accelerator Laboratory
Convener: Matthew Judah (Colorado State University)
• 61
The Calorimeter Global Feature Extractor (gFEX) for the Phase-I Upgrade of the ATLAS experiment
The ATLAS Level-1 calorimeter trigger is planning a series of upgrades in order to face the challenges posed by the upcoming increase of the LHC luminosity. The upgrade will benefit from the new front end electronics for parts of the calorimeter which provide the trigger system with digital data with a tenfold increase in granularity. The Global Feature Extractor (gFEX) module is one of the updates of the Level-1 calorimeter trigger project. This unique single ATCA board will use 3 processor Xilinx Ultra-scale FPGAs for data processing and one Xilinx Ultra-scale+, multi-processor system-on-chip, ZYNQ, for configuring all of the processor FPGAs and monitoring the board status and environment. It will allow the identification in real time of large radius jets for capturing Lorentz-boosted objects such as top quarks, Higgs, Z and W bosons, as well as the calculation of global event variables such as missing transverse energy, centrality for heavy ion collisions and event-by-event pile-up subtraction which are fundamental for the LHC physics studies. Extensive simulation studies are carried out to understand and optimise the characteristics of gFEX. Prototypes have been built and extensively tested to prepare for the final steps and the production of the modules. The design of the final gFEX module as well as the performance of the prototypes will be presented.
Speaker: Giordon Stark (University of Chicago)
• 62
The ATLAS New Small Wheel Trigger
The New Small Wheel (NSW) is a major upgrade to the muon spectrometer of the ATLAS experiment, which will be installed in 2019-2020. The NSW will comprise both sTGC and Micromegas detectors. One of the major goals on the upgrade is fast, precise muon reconstruction in hardware to allow triggering on single muon events in high pileup environments. This talk presents the status of the NSW trigger and integration into the NSW electronics readout path, with emphasis on the test stand at Harvard taking cosmic ray muon data with an octuplet of prototype Micromegas chambers.
Speaker: Alexander Tuna (Harvard University)
• 63
Instantaneous luminosity calibration of the ATLAS experiment with $Z\to \mu ^{-} \mu ^ {+}$
In this talk, a new method of calibrating the instantaneous luminosity of the ATLAS experiment with $Z\to \mu \mu$ process is presented. At the designed center-of-mass energy of the LHC, cross-section of $Z\to \mu \mu$ process is known to a very high precision and has a very good production rate (~1000 events/minute), which makes it suitable for luminosity measurement. Leading systematic uncertainties in this method come from the Standard Model theory, which are totally different compared to the leading systematic uncertainties on the current ATLAS luminosity measurement based on the Van der Meer method. A comparison of results with the official ATLAS luminosity measurements is presented for the entire data collected in 2015 and 2016.
Speaker: Mr Harish Potti (University of Texas at Austin)
• 64
Mu2e Trigger & DAQ Design and Challenges
The Mu2e experiment at Fermilab aims to measure the charged-lepton flavor violating neutrinoless conversion of a negative muon into an electron, producing a monochromatic electron with an energy slightly below the rest mass of the muon (104.97 MeV). We expect to set a limit on the ratio between the muon conversion and capture rate of 6.7 × 10^−17 at 90% CL in three years of running using a pulsed μ- beam that should provide ~10^18 stopped muons on an aluminum target. A critical component of the experiment is the Trigger and Data Acquisition (TDAQ) subsystem. The TDAQ is responsible for collecting data from the detector subsystems, as well as generating and distributing timing information to synchronize the subsystems. The TDAQ also controls the operating modes for each event window, and provides monitoring and operator interfaces. Before delivering data to be processed offline, the TDAQ system must also provide online processing and filtering to achieve a rejection factor of 100 or more, resulting in approximately 7 Petabytes of data per year. We present an overview of the TDAQ design and the progress of our development work as we seek to facilitate the accomplishment our physics goals.
Speaker: Dr Tomonari Miyashita (California Institute of Technology)
• 65
The ATLAS Trigger algorithms upgrade and performance in Run 2 (TDAQ)
The ATLAS trigger has been used very successfully for the online event selection during the first part of the second LHC run (Run-2) in 2015/16 at a center-of-mass energy of 13 TeV. The trigger system is composed of a hardware Level-1 trigger and a software-based high-level trigger; it reduces the event rate from the bunch-crossing rate of 40 MHz to an average recording rate of about 1 kHz. The excellent performance of the ATLAS trigger has been vital for the ATLAS physics program of Run-2, selecting interesting collision events for wide variety of physics signatures with high efficiency. The trigger selection capabilities of ATLAS during Run-2 have been significantly improved compared to Run-1, in order to cope with the higher event rates and pile-up which are the result of the almost doubling of the center-of-mass collision energy and the increase in the instantaneous luminosity of the LHC. At the Level-1 trigger the undertaken improvements resulted in more pile-up robust selection efficiencies and event rates and in a reduction of fake candidate particles. A new hardware system, designed to analyze event-topologies, supports a more refined event selection at the Level-1. A hardware-based high-rate track reconstruction, currently being commissioned, enables the software trigger to make use of tracking information at the full input rate. Together with a re-design of the high-level trigger to deploy more offline-like reconstruction techniques, these changes improve the performance of the trigger selection turn-on and efficiency to nearly that of the offline reconstruction. In order to prepare for the anticipated further luminosity increase of the LHC in 2017/18, improving the trigger performance remains an ongoing endeavor. Thereby coping with the large number of pile-up events is one of the most prominent challenges. This presentation gives a short review the ATLAS trigger system and its performance in 2015/16 before describing the significant improvements in selection sensitivity and pile-up robustness, which we implemented in preparation for the expected highest ever luminosities of the 2017/18 LHC.
Speaker: Catrin Bernius (SLAC)
• 66
The ATLAS Trigger Menu design for higher luminosities in Run 2 (TDAQ)
The ATLAS experiment aims at recording about 1 kHz of physics collisions, starting with an LHC design bunch crossing rate of 40 MHz. To reduce the large background rate while maintaining a high selection efficiency for rare physics events (such as beyond the Standard Model physics), a two-level trigger system is used. Events are selected based on physics signatures such as the presence of energetic leptons, photons, jets or large missing energy. The trigger system exploits topological information, as well as multivariate methods to carry out the necessary physics filtering for the many analyses that are pursued by the ATLAS community. In total, the ATLAS online selection consists of nearly two thousand individual triggers. A Trigger Menu is the compilation of these triggers, it specifies the physics selection algorithms to be used during data taking and the rate and bandwidth a given trigger is allocated. Trigger menus must reflect the physics goals of the collaboration for a given run, but also take into consideration the instantaneous luminosity of the LHC and limitations from the ATLAS detector readout and offline processing farm. For the 2017 run, the ATLAS trigger has been enhanced to be able to handle higher instantaneous luminosities (up to 2.0x10^{34}cm^{-2}s^{-1}) and to ensure the selection robustness against higher average multiple interactions per bunch crossing. In this presentation we describe the design criteria for the trigger menu for Run 2. We discuss several aspects of the process of planning the trigger menu, starting from how ATLAS physics goals and the need for detector performance measurements enter the menu design, and how rate, bandwidth, and CPU constraints are folded in during the compilation of the menu. We present the tools that allow us to predict and optimize the trigger rates and CPU consumption for the anticipated LHC luminosities. We outline the online system that we implemented to monitor deviations from the individual trigger target rates and to quickly react to changing LHC conditions and data taking scenarios. Finally we give a glimpse of the 2017 Trigger Menu, allowing the listener to get a taste of the vast physics program that the trigger is supporting.
Speaker: Heather Russell (McGill University)
• Dark Matter: Monday afternoon Hornets Nest
### Hornets Nest
#### Fermi National Accelerator Laboratory
Convener: Prof. Enectali Figueroa-Feliciano (Northwestern University)
• 67
LUX, and the Combating of the Lamppost Effect
New results from the Large Underground Xenon (LUX) detector, a 100-kg-scale, 2-phase xenon direct dark matter search experiment, will be shared. Dark matter, the missing ~25% of the mass-energy content of the universe, is sought in new ways, using effective field theory operators to extend the search to higher-mass Weakly Interacting Massive Particles (WIMPs), spin-dependent interaction operators, and electron instead of nuclear recoil, to seek axions. In addition, 2-neutrino double electron capture of 124Xe will be explored. Lastly, both old and new calibrations and position and energy reconstruction techniques will be reviewed, in the context of the new background and signal models being developed by LUX.
Speaker: Prof. Matthew Szydagis (University at Albany, SUNY)
• 68
First Dark Matter Search Results from the XENON1T Experiment
XENON1T is the current experiment of the XENON dark matter search program based on dual-phase (liquid-gas) xenon time projection chambers (TPCs) of increasing target mass and decreasing background. The experiment was constructed and assembled over the past 3 years at the INFN Laboratori Nazionali del Gran Sasso (LNGS). The XENON1T detector is the first multi-ton scale liquid xenon (LXe) TPC containing a total of 3200 kg of ultra-pure LXe of which 2000 kg are active. Commissioning of the LXe TPC and the surrounding muon veto water Cherenkov detector, as well as associated cryogenics and purification plants was completed during the fall of 2016. A blind analysis of 1042 kg fiducial mass and 34.2 live days of data acquired between November 2016 and January 2017 was performed. XENON1T continues to take data following a short break caused by the January 18, 2017 earthquake. The results from this first dark matter search and outlook for the science program with XENON1T will be presented.
Speaker: Chris Tunnell (University of Oxford)
• 69
The XENONnT Dark Matter Experiment
With XENON1T leading the search for dark matter, the XENON collaboration has started to plan an upgrade of the detector for the next phase, referred to as XENONnT. The XENONnT experiment will utilize the already built and functioning XENON1T infrastructures, such as the cryogenic system, Kr distillation system, and Xe storage and recovery system, with the time projection chamber (TPC) as the main upgrade. The upgraded XENONnT detector will be filled with 7.5 tons of ultra-pure liquid xenon, tripling the active liquid xenon target mass of XENON1T. About 500 low-radioactive three-inch R11410 PMTs will be used. Background from internal sources such as radon will be reduced. It will enable another order of magnitude improvement in dark matter search sensitivity compared to that of XENON1T, or accumulate statistics if a positive dark matter signal is observed by XENON1T. The detailed TPC upgrade plan, background control and reduction techniques, and predicted sensitivity reach will be presented.
Speaker: Prof. Kaixuan Ni (UC San Diego)
• 70
The LUX-Zeplin Dark Matter Search: detector design and sensitivity
The nature and origin of Dark Matter are among the most compelling mysteries of contemporary science. For over three decades, physicists have been trying to detect Dark Matter particles via collisions on target nuclei, with little success. The LZ collaboration is designing a massive Dark Matter detector, to be installed at the 4850 level of the Sanford Underground Research Facility in Lead, South Dakota. This detector will feature 7 active tons of target nuclei and use the established liquid xenon TPC technology to achieve unprecedented sensitivity to a wide range of Dark Matter candidates. In this talk, I will discuss the design and sensitivity of the experiment, together with its status.
Speaker: Maria Elena Monzani (SLAC National Accelerator Laboratory)
• 71
Background Simulations for the LUX-ZEPLIN Experiment
The LUX-ZEPLIN experiment will use a seven tonne dual-phase xenon TPC for the direct detection of dark matter. Understanding and mitigating background signals are crucial in its aim to push to an unprecedented sensitivity for WIMPs. I will describe the methods used to assess these, including simulations that characterise the electron and nuclear recoil responses in the detector from both internal and external background sources. Combined with the results of ongoing radioactive assays, these give an estimate of the expected background rates. Suppression of these backgrounds is achieved through fiducialisation and a veto strategy involving anti-coincidence between the main TPC and outer detectors (an instrumented xenon ‘skin’ and liquid scintillator detector). Under the present background model, LZ is projected to have a baseline sensitivity, with 1000 live days, of 2.3 x 10-48 cm2 for a 40 GeV/c2 WIMP mass.
Speaker: Dr Amy Cottle (Fermi National Accelerator Laboratory)
• 72
ADMX - axion dark matter experiment
The ADMX experiment is now taking data that is sensitive for the first time to a possible QCD axion with couplings to photons that can provide a solution to the strong-CP problem and account for a sizable amount of the dark matter of the universe.
Speaker: Daniel Bowring (Fermilab)
• 73
Emission of Photons and Relativistic Axions from Axion Stars
The number of nonrelativistic axions can be changed by inelastic reactions that produce relativistic axions or photons. Any even number of nonrelativistic axions can scatter inelastically into two relativistic axions. Any odd number of axions can annihilate into two photons. This reaction produces a monochromatic radio-frequency signal at an odd-integer harmonic of the fundamental frequency set by the axion mass.The loss rates of axions from axion stars through these inelastic relations are calculated using the framework of a nonrelativistic effective field theory. Odd-integer harmonics of a fundamental radio-frequency signal provide a unique signature for collapsing axion stars or any dense configuration of axions.
Speaker: Mr Abhishek Mohapatra (The Ohio State University)
• Higgs and EWSB: Monday afternoon Sunrise
### Sunrise
#### Fermi National Accelerator Laboratory
Convener: Laura Reina (Florida State University)
• 74
Search for the dimuon decay of the Higgs boson with the ATLAS experiment
The Standard Model Higgs boson Yukawa coupling to dimuons offers an opportunity to study the Higgs interaction with second generation fermions. The Standard Model branching fraction of the Higgs decay to $\mu^+\mu^-$ is $2.2\times10^{−4}$, much smaller compared to the decays to the third generation lepton/quark pairs $\tau^+\tau^-$ and $b\bar{b}$, and the second generation quark pair $c\bar{c}$. Despite the low branching fraction, this channel has the highest trigger and particle identification efficiencies of the other listed decays as well as a comparatively small background. This makes this channel an attractive way to study the Higgs Yukawa coupling. The background to this channel is a dominant irreducible dimuon production from the Drell-Yan process, $Z/\gamma *\to\mu^+\mu^-$, which is $\approx1700$ times the signal rate. To increase our detection sensitivity we use three categories to tag events by the Higgs production mechanism: gluon-gluon fusion (ggF), vector boson fusion (VBF), and vector boson associated production (VH). This talk presents the strategies of the analysis and summarizes the results from Run 1 and Run 2 data (2015-2016). The new developments in event categorization and the detection sensitivity for the expected 150 $fb^{-1}$ data in Run 2 are also reported.
Speaker: Aaron White (University of Michigan)
• 75
Search for the Higgs Boson Decays into Dimuons at CMS
A search for the standard model Higgs boson decaying into a muon pair is presented. The analysis is conducted with pp collisions data collected at 13 TeV with CMS at the LHC. Observed and expected limits of are placed on the standard model Higgs cross section times branching ratio at the 95% confidence level.
Speaker: Sergei Gleyzer (University of Florida)
• 76
Combined measurements of the Higgs boson production and decay rates using pp collisions at √s = 13 TeV with the ATLAS Experiment
After the Higgs boson was discovered at the LHC in 2012, it is of great importance to study how the Higgs boson interacts with Standard Model particles. In this presentation, I will report on the combined measurements of Higgs boson production and decay rates using LHC Run 2 proton-proton collision data collected at the center-of-mass energy of 13 TeV by the ATLAS detector in 2015 and 2016. The combination is based on the analysis of five production processes, namely gluon fusion, vector boson fusion, and associated production with a W or a Z boson or a pair of top quarks, and of multiple decay modes. I will also discuss how the measurements constrain the Higgs boson’s couplings to Standard Model particles as well as the existence of new physics.
Speaker: Hongtao Yang (University of Wisconsin-Madison)
• 77
Mass Dependence of Higgs Production at Large Transverse Momentum
The transverse momentum distribution of the Higgs at large $P_T$ is complicated by its dependence on three important energy scales: $P_T$, the top quark mass $m_t$, and the Higgs mass $m_H$. A strategy for simplifying the calculation of the cross section at large $P_T$ is to calculate only the leading terms in its expansion in $m_t^2/P_T^2$ and/or $m_H^2/P_T^2$. The expansion of the cross section in inverse powers of $P_T$ is complicated by logarithms of $P_T$ and by mass singularities. In this work, we consider the top-quark-loop contribution to the subprocess $q\bar{q}\to H+g$ at leading order in $\alpha_s$, which proceeds through a top quark loop. We show that the leading power of $1/P_T^2$ can be expressed in the form of a factorization formula that separates the large scale $P_T$ from the scale of the masses. All the dependence on $m_t$ and $m_H$ can be factorized into fragmentation amplitudes for $t \bar t \to H$ and for $t \bar t \to g$ and an endpoint contribution. This factorization approach will be useful for calculating the $P_T$ distribution at large $P_T$ to next-to-leading order in $\alpha_s$.
Speaker: Eric Braaten (Ohio State University)
• 78
Radiative Decays of the Higgs Boson to a Pair of Fermions
We revisit the radiative decays of the Higgs boson to a fermion pair $h\rightarrow f\bar{f}\gamma$ where $f$ denotes a fermion in the Standard Model (SM). We include the chirality-flipping diagrams via the Yukawa couplings at the order $\mathcal{O}(y_f^2 \alpha)$, the chirality-conserving contributions via the top-quark loops of the order $\mathcal{O}(y_t^2 \alpha^3)$, and the electroweak loops at the order $\mathcal{O}(\alpha^4)$. The QED correction is about $Q_f^2\times {\cal O}(1\%)$ and contributes to the running of fermion masses at a similar level, which should be taken into account for future precision Higgs physics. The chirality-conserving electroweak-loop processes are interesting from the observational point of view. First, the branching fraction of the radiative decay $h \to \mu^+\mu^- \gamma$ is about a half of that of $h \to \mu^+\mu^-$, and that of $h \to e^+ e^- \gamma$ is more than four orders of magnitude larger than that of $h \to e^+ e^-$, both of which reach about $10^{-4}$. The branching fraction of $h \to \tau^+\tau^- \gamma$ is of the order $10^{-3}$. All the leptonic radiative decays are potentially observable at the LHC Run 2 or the HL-LHC. The kinematic distributions for the photon energy or the fermion pair invariant mass provide non-ambiguous discrimination for the underlying mechanisms of the Higgs radiative decay. We also study the process $h \to c\bar c \gamma$ and evaluate the observability at the LHC. We find it potentially comparable to the other related studies and better than the $h \to J/\psi\ \gamma$ channel in constraining the charm-Yukawa coupling.
Speaker: Xing Wang (University of Pittsburgh)
• Neutrino II: Monday afternoon Racetrack
### Racetrack
#### Fermi National Accelerator Laboratory
Kirk Road & Pine Street Batavia, IL 60510-5011
Convener: Prof. Sowjanya Gollapinni (University of Tennessee, Knoxville)
• 79
Signal Simulation and Processing in the MicroBooNE LArTPC
MicroBooNE is an 85-ton Liquid Argon Time Projection Chamber (LArTPC) and the first of a trio of LArTPCs in the Short Baseline Neutrino (SBN) program which will search for a light sterile neutrino and measure neutrino-argon interaction cross sections. Located in the Booster neutrino beam at Fermi National Accelerator Laboratory, MicroBooNE has been taking neutrino data since October 2015. In this talk, we will describe the reconstruction of the distribution of ionization electrons given the induced current in all wire planes. Owing to the ultra-low noise cold electronics inside the LAr, the first successful extraction of the ionization charge from the induction wire planes in single-phase LArTPCs has been achieved. This development opens up new possibilities for using charge information to assist the event reconstruction. Latest results of a quantitative evaluation of the signal processing using full TPC signal simulation and a comparison of data and Monte Carlo will be shown.
Speaker: Brian Kirby (Brookhaven National Lab)
• 80
Design and Fabrication of the ProtoDUNE Dual Phase LArTPC
The WA105 protoDUNE Dual Phase Liquid-argon Time Projection Chamber (LArTPC) is a large demonstrator based on the GLACIER design, with a 6x6x6 m3 (a Dual-phase LArTPCs are one of the far detector technology options foreseen for the Deep Underground Neutrino Experiment (DUNE) at Fermilab. Dual Phase (DP) refers to the extraction of ionization electrons at the interface between liquid and gaseous argon and their amplification and collection in the gas phase. ProtoDUNE will be operating at the CERN neutrino platform test beam facility. It not only serves as the engineering prototype of the FD, but will also demonstrate the concept of a very large dual-phase LAr TPC and calibrate it with charged particle test beam. We will briefly discuss the actual dimension of the design, fabrication, testing, installation and commissioning of the detector components at CERN.
Speaker: Dr ANIMESH CHATTERJEE (The University of Texas at Arlington)
• 81
Recent progress on wire-cell tomographic reconstruction for LArTPC
The Deep Underground Neutrino Experiment (DUNE) will use the state-of-the-art massive Liquid Argon Time Projection Chambers (LArTPCs) to search for CP violation in the neutrino sector, proton decay, and supernova neutrinos. The 3D reconstruction of the particle trajectories in LArTPCs relies on multiple wire planes, which can be challenging due to the intrinsic ambiguity of identifying where along the wire the charge is deposited. In this talk, we present a novel 3D reconstruction method “Wire-Cell” inspired by the concept of tomography. Based on the independent measurements of the same charge from the three planes of wires, the 3D images of ionization charge can be efficiently reconstructed following the principle of compressed sensing utilizing mathematical techniques such as the L1 regularization. Current status and future prospects of the development will be reported.
Speaker: Dr Hanyu Wei (brookhaven national laboratory)
• 82
Cold electronics preparation for the protoDUNE experiment
The main purpose of the DUNE experiment is to measure the CP-violation phase in long-baseline neutrino oscillations with a liquid-argon detector of unprecedented size. The DUNE detector will consist of a liquid-argon Time Projection Chamber. The protoDUNE detectors at CERN are prototypes of the full-scale DUNE experiment; their operation will provide important input for the success of DUNE. Cold electronics is one of the most challenging topics for DUNE and protoDUNE. The functionality of the front-end motherboard and warm interface board needs to be understood at a detailed level. In this talk, the integration test plan, as well as results of tests of the protoDUNE cold electronics will be presented.
Speaker: Dr Guang Yang (Stony brook university)
• 83
Measurement of Electron Attenuation using Cosmic Ray Muons in the MicroBooNE Detector
The MicroBooNE experiment at Fermilab uses liquid argon time projection chamber (LArTPC) technology to study neutrino interactions in argon. A fundamental requirement for LArTPCs is to achieve and maintain a low level of electronegative contaminants in the liquid to minimize the capture of drifting ionization electrons. The attenuation time for the drifting electrons should be long compared to the maximum drift time, so that the signals from particle tracks that generate ionization electrons with long drift paths can be detected efficiently. In this talk, we present MicroBooNE’s measurement of electron attenuation using cosmic ray muons. The result yields a minimum electron 1/e lifetime of 18 ms under typical operating conditions, which is long compared to the maximum drift time of 2.3 ms.
Speaker: Mr Varuna Meddage (Kansas State University)
• Neutrino Physics: Monday afternoon Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
Convener: Georgia Karagiorgi (Columbia University)
• 84
Summary of the Second Numu Disappearance Results from the NOvA Experiment Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
In light of the Nobel Prize awarded for neutrino oscillations in 2015, it is an exciting time to be a part of a long-baseline neutrino oscillation experiment. NOvA is one such experiment based out of Fermilab National Accelerator Laboratory, which uses two liquid scintillator detectors, one at Fermilab (the near" detector) and a second 14 kton detector in northern Minnesota (the far" detector.) The numu disappearance analysis is sensitive to the mixing parameters $\theta_{23}$ and $\Delta m^{2}_{32}$ and is capable of shedding light on the open question of whether or not $\theta_{23}$ is maximal. This talk will present the results from the second $\nu_{\mu}$ disappearance analysis using a full detector equivalent of $6.05 \times 10^{20}$ POT, which rejects the maximal mixing solution at 2.6$\sigma$.
Speaker: Dr Michael Baird (University of Virginia)
• 85
Muon Neutrino Dissapearance in the NOvA experiment Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
NOvA is a long-baseline neutrino oscillation experiment looking for muon neutrino disappearance and electron neutrino appearance. Having the longest baseline of any past or present accelerator experiment, NOvA uses the upgraded Neutrino Main Injector (NuMI) beam at Fermilab. The experiment measures oscillations within a muon neutrino beam using a 300 ton Near Detector and a 14 kiloton Far Detector placed 810 km away from each other, both located 14 milliradians off-axis. The energy spectra observed in this neutrino beam peaks at 2 GeV close to the oscillation maximum. NOvA being an oscillation experiment uses the Near Detector (ND) at Fermilab to measure the initial beam spectra and flavour composition. Then the spectra is extrapolated to the Far Detector (FD) at Ash River to search for oscillations. The NOvA Collaboration has updated its first analysis and has recently released a new $\nu_{\mu}$ disappearance result using an exposure of $6\times10^{20}$ protons-on-traget (POT). Our just-published result disfavours the symmetric mixing scenario ($\theta_{23}=\pi/4$) at 2.6 sigma significance, well beyond that of past results. By the end of February 2017, NOvA had been exposed to $9\times10^{20}$ POT for a $\nu_{\mu}$ beam which will allow us to better constrain the allowed regions for the oscillation parameters $\Delta m^2_{32}$ and sin$^2\theta_{23}$. Furthermore, the Disappearance Analysis Group has been pushing to increase its sensitivity, coming from a finner energy binning and hadronic energy fractions. These improvements are underway and waiting to be tested with real data once the reconstruction is done and ready by the beginning of Summer 2017. This talk will discuss the improvements to the muon neutrino disappearance analysis and how our sensitivity to non-maximal mixing can be improved.
Speaker: Ms Diana Patricia Mendez (University of Sussex)
• 86
Recent Developments in T2K Oscillation Analysis Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
The T2K experiment is a long base-line neutrino experiment located in Japan. Having successfully discovered $\nu_{e}$ appearance from a $\nu_{\mu}$ beam, T2K is now aimed at probing CP violation in the lepton sector, the mass hierarchy, and the precision measurement of $\sin^2{\theta_{23}}$. Since data taking started in 2010, T2K has accumulated $14.7\times10^{20}$ protons on target (POT) in neutrino beam mode, and $7.6\times10^{20}$ POT in antineutrino beam mode. A new reconstruction algorithm for Super-Kamiokande (SK) -- the far detector of T2K -- is being used for event selection for the first time. The SK fiducial volume has been expanded,increasing the statistics by $\sim20\%$ from the previous selection with the same beam exposure. The latest developments in the T2K oscillation analysis within the PMNS framework, especially the measurement of $\delta_{CP}$, will be presented, and details of the analysis will be discussed.
Speaker: Ms Xiaoyue Li (Stony Brook University)
• 87
Using the PPFX package for the DUNE Experiment
PPFX for the Deep Underground Neutrino Experiment (DUNE) is a project that aims to improve the prediction of DUNE's flux and the estimation of hadron production uncertainties using hadron production data. Currently, the DUNE flux relies on GEANT4 based physics model which large uncertainties from hadronic interactions in the beamline. We used PPFX, a package developed by the MINERvA experiment at Fermilab to add improved hadronic interaction data to the GEANT4 based flux prediction. We use PPFX to study the predicted flux uncertainties for several candidate beamline designs. In this talk, I will discuss the process of applying the PPFX package to DUNE's flux and the resulting flux uncertainties.
Speaker: Amit Bashyal (Oregon State University)
• 88
Design of the LBNF Beamline Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
The Long Baseline Neutrino Facility (LBNF) will utilize a beamline located at Fermilab to provide and aim a neutrino beam of sufficient intensity and appropriate energy range toward DUNE detectors, placed deep underground at the Sanford Underground Research Facility (SURF) in South Dakota. The primary proton beam (60-120 GeV) will be extracted from the MI-10 section of Fermilab’s Main Injector. Neutrinos are produced after the protons hit a solid target and produce mesons which are subsequently focused by magnetic horns into a 194m long decay pipe where they decay into muons and neutrinos. The parameters of the facility were determined taking into account the physics goals, spacial and radiological constraints and the experience gained by operating the NuMI facility at Fermilab. The Beamline facility is designed for initial operation at a proton-beam power of 1.2 MW, with the capability to support an upgrade to about 2.4 MW. LBNF/DUNE obtained CD-1 approval in November 2015. We discuss here the design status and the associated challenges as well as the R&D and plans for improvements before baselining the facility.
Speaker: Jim Hylen (Fermi National Accelerator Laboratory)
• 89
Analytic Neutrino Oscillation Probabilities in Matter Revisited. Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
As we enter the precision measurement era for neutrino oscillation physics, it is imperative that our understanding of three flavor neutrino oscillations is also at comparable precision. Even in vacuum, three flavor oscillations is highly none trivial at a precision of 5% or better. Matter effects further complicate three flavor oscillation physics. Here, I will revisit the analytic description of three flavor neutrino oscillation physics as given in recent papers, and discuss their implications for the current generation of neutrino oscillation experiments, in particular T2K and NOvA, and follow up with the next generation of experiments DUNE, T2HKK, and JUNO.
Speaker: Dr Stephen Parke (Fermilab)
• Particle Detectors: Monday afternoon IARC Building
### IARC Building
#### Fermi National Accelerator Laboratory
Convener: Ms Angela Fava (Fermilab)
• 90
Upgrade of the ATLAS Monitored Drift Tube Electronics for the HL-LHC
To cope with large amount of data and high event rate expected from the planned High-Luminosity LHC (HL-LHC) upgrade, the ATLAS monitored drift tube (MDT) readout electronics will be replaced. In addition, the MDT detector will be used at the first-level trigger to improve the muon transverse momentum resolution and reduce the trigger rate. A new trigger and readout system has been proposed. Prototypes for two frontend ASICs and a data transmission board have been designed and tested, detailed simulation of the trigger latency has been performed, and segment-finding and track fitting algorithms have been developed. We will present the overall design of the trigger and readout system and show latest results from various prototype studies
Speaker: Mr yu liang (University of Michigan)
• 91
Near-Infrared Scintillation of Liquid Argon
After briefly reviewing past attempts to observe and measure the scintillation of condensed noble gases in the near-infrared (NIR), we outline the prospects and advantages of using the NIR scintillation as the light signal in liquid argon time projection chambers. We conclude with preliminary results obtained at Fermilab's Proton Assembly Building cryogenic facilities.
Speaker: Carlos Escobar (Fermilab and UNICAMP)
• 92
Studies with the LArIAT Light Collection System
The detection of scintillation from particles in liquid argon time projection chambers (LArTPCs) serves a crucial role in triggering and interaction timing for liquid argon neutrino experiments, with potential to enhance calorimetry and particle identification efficiency as well. The LArIAT experiment provides an opportunity to explore new ideas for light collection in LArTPCs in a controlled test beam environment. Two cryogenic photomultiplier tubes (PMTs) and several varieties of silicon photomultipliers (SiPMs) mounted to custom preamplifier boards are suspended behind the LArIAT TPC's wireplanes. Reflective foils coated in tetraphenyl butadiene (TPB) line the field cage walls to down-shift scintillation vacuum-ultraviolet (VUV) photons into detectable visible light. In the most recent run, this configuration was changed to having a transparent cathode with TPB coated reflector foils mounted behind to more closely mimic proposed upcoming neutrino experiments. Additionally, a new light detection device (the ARAPUCA) was deployed for R&D studies. Analyses are underway which use this light to identify and study Michel electrons, improve particle identification, and enhance calorimetry of beam particles by combining light with total charge collected on the wireplanes.
Speaker: Ms Monica Nunes (UNICAMP)
• 93
Characterizing LArTPC detector performance with MicroBooNE
With many current and future neutrino experiments relying on Liquid Argon Time Projection Chamber (LArTPC) technology, characterizing the performance of these detectors is critical. The MicroBooNE LArTPC experiment is capable of performing numerous measurements to better understand the technology. These include identification and filtering of excess TPC noise, signal calibration and measurements of diffusion and recombination. MicroBooNE, residing on the surface, can also provide useful information about cosmic ray rate and the build up of space charge in the TPC volume. A laser calibration system has been designed and employed to investigate these important effects.
Speaker: Dr JYOTI JOSHI (Brookhaven National Laboratory)
• 94
Detector performance and cosmic-ray reconstruction efficiency in MicroBooNE
The MicroBooNE detector is a liquid argon time projection chamber at Fermilab designed for short-baseline neutrino oscillation physics and neutrino-argon interaction cross-section measurements. Due to its location near the surface, a good understanding of cosmic muons as a source of backgrounds is of fundamental importance for the experiment. This talk will show recent results on MicroBooNE detector performance from our first 18 months of running and a method to determine the cosmic-ray reconstruction efficiency using an external cosmic-ray counter, installed above the main detector. The analysis represents a small-scale demonstration of the method that can be used with future data coming from a recently installed cosmic-ray tagger system, which is able to tag ≈ 80% of the cosmic rays passing through the MicroBooNE detector.
Speaker: Mr Stefano Roberto Soleti (University of Oxford)
• 95
protoDUNE-SP Cold Electronics Quality Control
The protoDUNE-SP detectors are large-scale prototypes of the single-phase Liquid Argon Time Projection Chamber (LArTPC) and cold electronics designs proposed for the Deep Underground Neutrino Experiment (DUNE). TPC wires will be instrumented by 15360 readout channels implemented with low noise shaping-amplifier and digitization ASICs integrated into Front End Motherboards (FEMBs) operating at cryogenic temperature within the cryostat. The large number of electronics channels and high performance specifications require a large-scale production electronics quality control effort including highly automated test methods under realistic cryogenic operating conditions. This talk will summarize the protoDUNE-SP cold electronics quality control plan, details of its implementation and preliminary results.
Speaker: Brian Kirby (Brookhaven National Lab)
• 96
Development of fast timing detectors at Fermilab
Results of development of fast timing detectors at Fermilab presented. The detectors are based on different type of radiators (scintillators, quartz, crystals) and photodetectors (PMT, MCP-PMT, SiPMs) detecting the light converted in charge. Part of detectors based on silicon registration the charge produced by particle. Detectors are tested at FTBF. The obtained time resolution (TR) for some of detectors is less of 10 picoseconds. The results show the detectors could be used for CMS upgrade, HEP experiments and medical research.
Speaker: Dr Anatoly Ronzhin (Fermi National Accelerator Laboratory)
• QCD: Monday afternoon Curia II
### Curia II
#### Fermi National Accelerator Laboratory
Convener: Radja Boughezal (Argonne National Laboratory)
• 97
NNLO QCD Predictions
In this talk, I will review the current status of NNLO QCD predictions at the LHC
Speaker: Dr Xiaohui Liu (Beijing Normal University)
• 98
The spin-dependent quark beam function at NNLO
The question of how the nucleon’s spin is distributed among the partons is one of the important unsolved problems in physics and has recently received substantial attention from experimental measurements. In order to fully exploit these measurements an accurate theoretical description of the observables is required. The N-jettiness subtraction scheme provides a framework in which the desired accuracy can be achieved. In this talk I present the calculation of the beam function for longitudinally polarized quarks through next-to-next-to-leading order (NNLO) in QCD perturbation theory. This is the last missing ingredient needed to apply the factorization theorem for the N-jettiness event-shape variable in polarized collisions through the NNLO level. A special emphasis is given to the computational techniques, used to perform this computation and the treatment of the fifth gamma matrix in dimensional regularization. The NNLO polarized quark beam function is an essential ingredient for describing polarized collisions at NNLO precision. Therefore its knowledge is a big step towards extending the global fit of the polarized proton structure to the NNLO level.
Speaker: Ulrich Schubert (Argonne National Laboratory)
• 99
Analytic resummation of TMD distributions in momentum space in SCET_II.
We study the transverse momentum spectra of gauge bosons ( Z, $\gamma^*$, Higgs) in PP collisions in the regime of low transverse momentum. We also develop a scheme of resummation allowing us to choose the factorization scale for virtuality in momentum space which is then applied to obtain the transverse momentum spectra for the Drell-Yan and Higgs at NNLL accuracy. Using this scheme, we show, for the first time, how an analytic formula for these cross sections can be obtained at each order of resummation. Finally, a comparison with other resummation schemes is presented along with a discussion of possible non-perturbative effects.
Speaker: Dr Varun vaidya (lanl)
• 100
Pion Polarizability at CERN COMPASS
The pion polarizability is of fundamental interest in the low-energy sector of quantum chromodynamics. It is directly linked to the quark-gluon substructure and dynamics of the pion, the lightest bound system of the strong interaction. COMPASS measured the electromagnetic polarizability of the charged pion, which describes the stiffness of the pion against deformation in strong electromagnetic fields. Previous low statistics experiments in Serpukhov (Russia), where the Primakoff method for realizing interactions of charged pions with quasi-real photons was first employed. Later, other measurements based on photon-nucleon and photon-photon collisions were also carried out at different laboratories. The COMPASS measurement demonstrates that the charged-pion polarizability is significantly smaller than previous results, roughly by a factor two, with the smallest uncertainties realized so far. The results are consistent with chiral perturbation theory predictions, and strength the identification of the pion with the Goldstone boson of the strong interaction. Strong interaction theory makes a precise prediction on the polarisability of pions – the degree to which their shape can be stretched. This polarizability has baffled scientists since the 1980s, when the first measurements appeared to be at odds with the theory. Today’s result is in close agreement with theory. The electric απ and magnetic βπ charged pion Compton polarizabilities provide stringent tests of Chiral Perturbation Theory. The combination (απ-βπ) was measured at CERN COMPASS via radiative pion Primakoff scattering (Bremsstrahlung of 190 GeV/c π-s) in the nuclear Coulomb field: π + Z → π + γ + Z. This reaction is identified experimentally by virtue of the very small momentum transfer to the target nucleus; and is equivalent to γ + π → γ + π Compton scattering for laboratory γ's of order 1 GeV/c incident on a target pion at rest. COMPASS data analysis (assuming απ+βπ=0 based on theory) gives a value απ = -βπ = 2.0 ± 0.6(stat) ± 0.7(syst) × 10-4 fm3. This is the most precise measurement of this fundamental low-energy parameter of strong interaction that has been addressed since long by various methods with conflicting outcomes.This new measurement strengthens the identification of the pion with the Goldstone boson of strong interactions.
Speaker: Prof. Murray Moinester (Tel Aviv University)
• 3:15 PM
Break
• Plenary: Monday afternoon Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
Kirk Road & Pine Street Batavia, IL 60510-5011
Convener: Prof. Priscilla Cushman (University of Minnesota)
• 101
WIMP dark matter searches progress and plans
Speaker: Prof. Rafael Lang (Purdue University)
• 102
Progress and new ideas in non-WIPM dark matter searches
Speaker: Kathryn Zurek (Berkeley Lab)
• 103
APS Fellows award ceremony
Speaker: Dr Marcela Carena (Fermilab)
• Meeting Photo In front of the Wilson Hall
### In front of the Wilson Hall
#### Fermi National Accelerator Laboratory
Kirk Road & Pine Street Batavia, IL 60510-5011
Convener: Mr Reidar Hahn Hahn (Fermilab - Office of Communications - Visual Media Services)
• Poster Session and Reception Reception Area
### Reception Area
#### Fermi National Accelerator Laboratory
• 104
Gamow penetration factor for nuclear fusion reaction in quantum plasmas
The quantum shielding effects on the nuclear fusion reaction process are investigated in quantum plasmas. The closed expression of the classical turning point for the Gamow penetration factor in quantum plasmas is obtained by the Lambert W-function. The closed expressions of the Gamow penetration factor and the cross section for the nuclear fusion reaction in quantum plasmas are obtained as functions of the plasmon energy and the relative kinetic energy by using the effective interaction potential with the WKB analysis. It is shown that the influence of quantum screening suppresses the Sommerfeld reaction factor. It is also shown that the Gamow penetration factor increases with an increase of the plasmon energy. It is also shown that the quantum shielding effect enhances the deuterium formation by the proton-proton reaction in quantum plasmas. In addition, it is found that the energy dependences on the reaction cross section and the Gamow penetration factor are more significant in high plasmon-energy domains.
Speaker: Prof. Young-Dae Jung (Hanyang University)
• 105
Investigation of Beam Emittance and Beam Transport Line Optics on Polarization
Effects of beam emittance, energy spread, optical parameters and magnet misalignment on beam polarization through particle transport systems are investigated. Particular emphasis will be placed on the beam lines being used at Fermilab for the development of the muon beam for the Muon g-2 experiment, including comparisons with the natural polarization resulting from pion decay, and comments on the development of systematic correlations among phase space variables. This work was supported by the National Science Foundation Grant 1623691.
Speaker: Mr Andrew Fiedler (Northern Illinois University)
• 106
Probing MeV Scale Physics in LArTPCs with Radioactive Calibration Sources
The Liquid Argon Time Projection chamber (LArTPC) is a unique technology well suited for large scale neutrino detectors. They allow for millimeter scale 3D precision particle tracking and calorimetry with good $\frac{dE}{dx}$ resolution, which provides excellent efficiency of particle identification and background rejection. While studies of detector response to high energy events have begun, there has been little to no direct demonstration of LArTPCs’ capabilities in producing ground breaking physics with solar and supernovae low-energy neutrinos. We aim to facilitate the development of low-energy LArTPC capabilities by developing the first 1-10 MeV calibration subsystems for large LArTPCs. In this talk, I will introduce the properties of supernova neutrinos, discuss how they can be detected in LArTPCs, and overview the low-energy LArTPC calibration source conceptual designs we are developing.
Speaker: Jonathan Echevers (University of Illinois at Urbana-Champaign)
• 107
Testing data connections for use with the HL-LHC CMS forward pixel electronics
For the CMS HL-LHC upgrade, a new Inner Tracker will be installed consisting of silicon pixel detector layers in the central region and disks placed in the forward region. A new readout chip will be used along with gigabit optical data links. Proposed designs for the readout chain electronics include a mix of high bandwidth electronic transmission cables and optical links. Until the new custom readout chips are available, a Xilinx Virtex-7 FPGA chip and prototype card will provide functional emulation for studies of the readout chain presented here.
Speaker: Mario D. Balcazar (University of Kansas)
• 108
Real time trigger rate monitoring at CMS
Throughout Run II, the trigger rate monitoring tool used by CMS has helped identify problems throughout the detector, leading to faster diagnosis and correction thanks to real time monitoring and alarms. This tool also incorporates trigger rates into CMS data certification. An overview of this tool is presented.
Speaker: Charles Mueller (University of Notre Dame)
• 109
Shower reconstruction performance studies for DUNE far detector
Two of the flagship analyses at the DUNE far detector are to determine the neutrino mass hierarchy and to measure the CP violating phase, using the appearance of electron-neutrino signal events in the far detector. To efficiently select signal events, we require robust shower reconstruction tools to achieve the maximal electron/photon separation. We present a summary of existing shower reconstruction algorithms, and their efficiency and performance by calculating the shower purity and completeness, as well as the dE/dX distributions for electron and photon showers. We also explore possible areas of improvements for the electron shower reconstruction for better electron-neutrino signal reconstruction.
Speaker: Dr Reddy Pratap Gandrajula (Michigan State University)
• 110
The Cosmological Principle Breaks Down as Superstructures Grow in the Universe
Humanity's cosmic physics relies on the assumption that, "the Universe looks the same for all observers, regardless of location." This assumption is called the Cosmological Principle, which is defined by the properties of homogeneity and isotropy. Homogeneity states that, the Universe looks the same at each point, while isotropy states that the Universe looks the same in all directions. While it is known that the cosmological principle breaks down at smaller cosmic scales (e.g., clusters of galaxies and solar systems), most research suggests that it holds at larger scales where clusters of galaxies are simply dots on the cosmic landscape. However, we now know that galaxies are not randomly distributed throughout the Universe. Greater than 90% of galaxies are located in dense areas of dark matter, where dark matter has condensed to form a cosmic web across the Universe. This cosmic, dark matter web is not static, but is continuing to condense, with "branches" in the web merging to become thicker "superstructures" over time. These findings suggest that the Cosmological Principle will eventually break down at all scales. The questions, then, are (1) at what scale does the Cosmological Principle fail now and (2) when will the largest scales of the Universe look like this current, "failed" scale? Using a database from The Max Planck Institute for Astrophysics, the distribution of dark matter hot spots was tested for significant deviations from random at different scales. Then, the database was used to estimate the growth rate of dark matter superstructures. These data were then combined to find that the Cosmological Principle will fail, at all scales, in another 54.7 billion years (a 68.4 billion-year-old Universe). Given that life could exist in the Universe for another 120 trillion years, the Cosmological Principle appears to be a fleeting characteristic of the infant Universe.
Speaker: Mr Cameron Marshall (Manhattan High School & Kansas State University)
• 111
New fermionic dark matters, extended standard model and cosmic rays
Three generations of leptons and quarks correspond to the lepton charges (LC) in the present work. Then, the leptons have the electric charges (EC) and lepton charges (LC). The quarks have the EC, LC and color charges (CC). Three heavy leptons and three heavy quarks are introduced to make the missing third flavor of EC. Then the three new particles which have the electric charges (EC) are proposed as the bastons (dark matters) with the rest masses of 26.121 eV/c2, 42.7 GeV/c2 and 1.9 1015 eV/c2. The RK anomaly is discussed here. And these new particles are applied to explain the origins of the astrophysical observations like the ultra-high energy cosmic rays and super-nova 1987A anti neutrino data. It is concluded that the 3.5 keV x ray peak observed from the cosmic x-ray background spectra is originated not from the pair annihilations of the dark matters but from the x-ray emission of the Q1 baryon atoms which are similar in the atomic structure to the hydrogen atom. New particles can be indirectly seen from the astrophysical observations like the cosmic ray and cosmic gamma ray [1,2]. [1] https://www.researchgate.net/publication/314877019 . [2] https://www.researchgate.net/publication/314246000 .
Speaker: Dr Jae-Kwang Hwang (JJJ Physics Laboratory)
• 112
CMS Pixel Detector Upgrade for HL-HLC
To meet the experimental challenges and reach the physics potential of the High Luminosity LHC (HL-LHC), the CMS experiment will be replacing its current pixel detector with new technology and designs. The upgrade plan includes extending the inner pixel detector in the forward region from the current coverage of |\eta|<2.4 to 4, and adopting small-pitch pixel sensors and next-generation electronic read-out. This talk reviews the objective and status of the pixel detector upgrade. Studies in simulation, from design optimization, detector modeling, and performance estimation, will be the focus of this talk. Finally, potential physics benefits from the upgrade are discussed.
Speaker: Yangyang Cheng (Cornell University)
• 113
Reaching Out for Particle Physics
The International Particle Physics Outreach Group (IPPOG) is a global network of physicists and educators committed to promote the particle physics research in the community through informal education and outreach. Following the model of experimental particle physics collaborations, IPPOG itself has become a scientific collaboration based on a memorandum of understanding. We describe the collaboration and its work to share ideas and best practices for reaching both scientist enthusiasts and audiences new to science.
Speaker: Marjorie Bardeen (FNAL)
• 114
A Flux Spectrometer for LBNF/DUNE
The Long-Baseline Neutrino Facility (LBNF) will include a conventional neutrino beam made by colliding a high energy proton beam with a fixed target, focusing the resulting hadron using a set of magnetic horns and allowing them to decay to neutrinos. As with most conventional neutrino beams, uncertainties on the number of neutrinos in the beam as a function of energy are of order 10%. The Flux Spectrometer is a proposal to measure the LBNF hadron flux after the focusing horns and before the decay volume, substantially reducing uncertainties in the neutrino flux. Recent work on the Spectrometer, including potential locations, possible designs and preliminary simulations, will be presented.
Speaker: Laura Fields (Fermilab)
• 115
Performance Studies of Capacitively Coupled HVCMOS Pixel Sensors Before and After Gamma Irradiation
High voltage CMOS pixel sensors are a promising technology that is being considered for particle physics detectors such as the ATLAS Inner Tracker due to their potential to realize a fully monolithic design at considerable cost savings while not compromising on high track reconstruction efficiency, charge collection, and radiation hardness. HVCMOS sensors have circuitry built into each pixel cell that amplifies the signal from the collected charge increasing it enough where it can be read-out via capacitive coupling by a traditional front-end read-out chip. In the case of a fully monolithic sensor, the on-pixel circuitry includes discrimination and digitization. The H35DEMO is a prototype pixel sensor built using 350 nm technology that demonstrates multiple examples of HVCMOS technology including several amplification and digitization matrices. The radiation tolerance of the analog matrices was assessed using test beam data to measure the impact on track reconstruction performance after gamma irradiation.
Speaker: Dylan Frizzell (University of Oklahoma)
• 116
The Low Background Laboratory at Idaho State University
The Deep Underground Neutrino Experiment (DUNE) hopes to study in great detail atmospheric, solar and supernova neutrino events. In order to do so, the background radiation at both the near detector (at Fermilab) and the far detector (at the Sanford research facility in South Dakota) must be understood in great detail. The Low Background Laboratory (LBL) is to be built at Idaho State University (ISU) to understand this background radiation and will be used to control the radio-purity of materials used in the construction of both of the DUNE detectors. The goal of the proposed LBL is to provide a tool to identify the most practical and radiologically clean materials to be used by DUNE and to model the background radiation to be expected in the DUNE detectors over the next 20 years. The cosmic ray background at 4850 feet depth will be relatively small. The background from naturally occurring radioactive isotopes however, is expected to be substantial. Just one of the radioactive isotopes in the detector, i.e. 39Ar, is expected to produce a 20KHz background signal, which will severely degrade the detector performance at low energy. Other natural radioactive isotopes, e.g. 40K, 220Rn and 222Rn and the other isotopes from the Uranium and Thorium decay chains, are expected to produce comparable, or higher backgrounds. The LBL will allow us to substantially reduce those radiological backgrounds which we can control by allowing us to select construction materials not only for their performance, but also for their radiological purity. In order to measure as accurately as possible the radiological purity of construction materials, the LBL will reduce the Radon related background by an expected 90% by placing the entire detector system in a class 10000 clean room with autonomous HVAC system, HEPA filters, and the ability to maintain overpressure. The combination of passive and active shielding will substantially reduce the background. We will estimate the background reduction factor with Monte Carlo simulations and in situ measurements. Finally, the LBL will model the background radiation to be expected at both the near and far detectors using GEANT4 on the College of Science and Engineering’s Minerve cluster.
Speaker: Mr P James Norris (Idaho State University)
• 117
Search for Dark Interactions with the ATLAS experiment
Hidden sector or dark sector states appear in many extensions to the Standard Model, to provide a candidate for the dark matter in the universe or to explain astrophysical observations of positron excesses. A hidden or dark sector can be introduced with an additional U(1)d dark gauge symmetry. The presence of the dark sector could be inferred either from deviations from the SM-predicted rates of Drell-Yan (DY) events or from Higgs boson decays through exotic intermediate states. The discovery of the Higgs boson during Run 1 of the Large Hadron Collider opens a new and rich experimental program that includes the search for exotic decays H —> Z Zdark —> 4l and. H —> Zdark Zdark ->4l, where Zdark is a dark vector boson. In this talk, we will review the status of current searches for dark sector states with the ATLAS detector and the prospects for LHC Run 2.
Speaker: Dr Ketevi Adikle Assamagan (Brookhaven National Laboratory)
• 118
Measurement of PTFE Reflectance for Xenon Scintillation Light
The LUX-ZEPLIN (LZ) experiment is a next-generation direct detection experiment under construction to search for dark matter. The detector contains a dual-phase liquid xenon (LXe) time projection chamber with a total active mass of 7 tons and is located at the Sanford Underground Research Facility (SURF) in South Dakota. LZ takes advantage of the high VUV reflectivity of PTFE to achieve high light collection efficiency. Previous work has shown that thinner PTFE layers may reduce radiological backgrounds, and thus these are preferred so long as no significant loss in reflectance results. In this presentation, experimental results of the reflectance near wavelengths of 178 nm of thin PTFE, Kapton, and PEEK sheets immersed in LXe, conducted with the Michigan Xenon Detector (MiX), will be discussed. It is further planned to compare those measurements with light propagation simulations to estimate the absolute reflectance of these materials.
Speaker: Yuhan Wang (University of Michigan)
• 119
Muon Intensity Increase by Wedge Absorbers
Low energy muon experiments such as mu2e and g-2 have a limited energy spread acceptance. Following techniques developed in muon cooling studies and the MICE experiment, the number of muons within the desired energy spread can be increased by the matched use of wedge absorbers. More generally, the phase space of muon beams can be manipulated by absorbers in beam transport lines. Applications with simulation results are presented.
Speaker: Dr David Neuffer (Fermilab)
• 120
Testing, Installation, Integration and Performance Studies of a Cosmic Ray Tagging System for the Short Baseline Neutrino Program Far Detector (ICARUS)
The ICARUS T600 liquid argon time-projection chamber will be the far detector for the Short Baseline Neutrino Program. The detector will operate at shallow depth and therefore be exposed to the full surface flux of cosmic rays. Application of overburden attenuates most of this background expected for muons. However, the remaining background is problematic since a photon produced by a muon passing in close proximity to the T600 active volume can be mistaken for a neutrino event. In principle, a large fraction of these events can be removed from the data through application of selection cuts as suggested by Monte Carlo studies. However, this method of background rejection reduces fiducial target mass and renders analysis of the systematics difficult. A straightforward way to remove the cosmic muon background more thoroughly is to utilize a detector external to the liquid argon active volume capable of tagging thoroughgoing cosmic muons with high efficiency (e.g. > 95%). Ideally, this external cosmic ray tagger (CRT) would provide full geometric coverage of the T600. During the past 18 months at Colorado State University (CSU), we performed Monte Carlo studies of the tagging efficiencies of the system and conducted an extensive research and development program of such a system based on extruded organic scintillator, wavelength-shifting fibers, and silicon photomultipliers. Subsequently, it was decided that our European colleagues would design and construct the top portion of the CRT while the US groups would provide the side (~400 m^2) and bottom (~215 m^2) portions using salvaged MINOS veto shield modules on the sides and Double Chooz veto modules on the bottom. These two systems will need to be tested for basic functionality and to have their detailed response characterized in order to optimize the system configuration as well as prepare for future analysis tasks and integration with the other detector sub-systems.
Speaker: Mr Christopher Hilgenberg (Colorado State University)
• 121
LBNF Optimized Horn Design & Target Integration
Optimization efforts for the Long Baseline Neutrino Facility (LBNF) have been pursued as an opportunity to further expand the reach of the experiment in the energy spectrum, and to significantly increase neutrino flux to the detectors. Major improvements and subsequent reconfigurations have been completed to the horn focusing system, in addition to the target, achieving the goals set forth. The optimized design is proposed as a three-horn system, with the graphite target now integrally supported within the primary horn, Horn A. Secondary and tertiary horns have been enlarged to increase pion gathering and maximize the potential of the near site facilities. Preliminary thermal and structural analysis for critical components will be presented, in conjunction with conceptual target layout and overall system operation.
Speaker: Mr Cory Crowley (Fermi National Accelerator Lab)
• 122
A Minimal non-universal EW extension of the Standard Model: A chiral family of models
We report the most general expression for the chiral charges of a non-universal U(1)' with identical charges for the first two families but different charges for the third one. The model is minimal in the sense that only standard model fermions plus right-handed neutrinos are required. By imposing anomaly cancellation and constraints coming from Yukawa couplings we obtain two different solutions. In one of these solutions, the anomalies cancel between fermions in different families. These solutions depend on four independent parameters which result very useful for model building. We build different benchmark models in order to show the flexibility of the parameterization. We also report LHC and low energy constraints for these benchmark models.
Speaker: Dr Richard Benavides (Instituto Tecnológico Metropolitano)
• 123
The Mu2e Solenoid Cold Mass Position Monitor System
The Mu2e experiment at Fermilab is designed to search for charged-lepton flavor violation by looking for muon to electron conversions in the field of the nucleus. The concept of the experiment is to generate a low momentum muon beam, stopping the muons in a target and measuring the momentum of the conversion electrons. The implementation of this approach utilizes a complex magnetic field composed of graded solenoidal and toroidal fields. The location of the solenoid cold mass relative to external fiducials are needed for alignment as well as monitoring coil movements during cool down and magnet excitation. This paper describes a novel design of a Cold Mass Position Monitor System that will be implemented for the Mu2e experiment.
Speaker: Dr Thomas Strauss (FNAL)
• 124
A Study of Mass Matrices with Permutational Symmetry for Quark Families
A set of 3x3 mass matrices are identified that have eigenstates that are mathematically equivalent to conventional QCD color states, and which have mass eigenvalues equal to the three quark flavor masses, for each of the two quark families. When integrated into the Dirac equations for each family, one obtains a theory that satisfies, TCP, Lorentz, U(1), and SU(2)L transformations, as well as parity and charge conjugation. With this approach, one obtains 3 degenerate mass eigenstates per color and flavor, which permits a unique and accurate fit of the CKM matrix, and a physical rationale is provided. SU(3) is not automatically satisfied for the mass terms in this theory. This is addressed by using an SU(3) Higgs mechanism, which is complementary with SU(2)L in creating mass in this theory for quarks.
Speaker: Richard Holmes (Boeing Company)
• 125
Search for vector-like quarks in fully hadronic final states with the ATLAS detector
This poster is presenting a search for pair produced vector-like quarks decaying in to a fully hadronic final state using 36.1 fb−1 of pp collisions with a center of mass energy of 13 TeV collected by the ATLAS experiment. We consider the decays of pair produced T and B vector-like quarks in to third generation standard model quarks with Higgs boson and gauge bosons W and Z. The analysis uses the variable radius re-clustering algorithm to reconstruct the large-radius jets and a multi-class deep neural network is used to tag the jets as hadronically-decaying top quarks, Higgs bosons, W bosons or Z bosons.
Speaker: Mr Madhuranga Thilakasiri Madugoda Ralalage Don (Oklahoma State University)
• 126
CosmicWatch: the Desktop Muon Detector
The CosmicWatch Desktop Muon Detectors were designed as an outreach tool to promote particle physics to undergraduates and high-school students. The detectors are pocket-sized, self-contained, light-weight (~100g), and require a very small amount of power (sub-Watt). The data can be read-out through a USB serial connection or saved locally to an SD-card. We've been working with students at various universities and high-schools through-out the world and have found that a single detector can be built by a new student in under a few hours for approximately $100. Speaker: Spencer Axani (MIT) • 127 The formalization of the relation between wave and particle and the unifying of three kinds of wave-particle duality After Jihua Gan’s solution for contradiction of separation and continence between classical physics and quantum theory, the contradiction of particle and wave consequentially has new solution. Based on the advance of Dirac's work in 1927, from "mode decomposition of classical electromagnetic field" to "photon decomposition of classical electromagnetic field”, a corresponding relation of basic units between classical electromagnetic field and quantum electromagnetic field is established, and a new wave-particle duality which is the third kind of wave-particle duality is revealed. It indicates that classical electromagnetic field has particle features in structure, which can be formed by superposition of a series of electromagnetic element-waves. Further more, energy and momentum of each electromagnetic element-wave can be equal to the energy and momentum of a photon in the same frequency. Later, three kinds of wave-particle duality, Einstein’s Wave-particle duality of light in 1905, de Broglie’s Wave-particle duality of particle in 1923, and Gan’s Wave-particle duality of wave in 1994, are compared. A relation of π-type structure among them is presented, and the π-type triple wave-particle duality of micro-object is revealed. Finally, after mathematical abstraction and physical generalization of π-type triple wave-particle duality, not only formulation of relation between wave and particle is accomplished but also the deep arcanum behind electromagnetic waves and photons is betrayed. It is just Tai Chi photon-wave and electromagnetic wave and photon are but two different showing forms of Tai Chi photon-wave under proper condition. Speaker: Mr Yongchao Gan (Faculty of Physics & Electronic Science, Hubei University) • 128 Background estimation for the electron neutrino appearance analysis in NOvA The NOvA experiment is an off-axis, two-detector experiment designed to study electron neutrino ($\nu_e$) appearance in the NuMI beam from Fermilab. The 300-ton Near Detector is 1 km from the target, and allows the study of the neutrino beam spectrum and composition before oscillations, while the larger (14,000 ton) Far Detector, situated on the surface 810 km away, observes the oscillated beam. The main backgrounds to$\nu_e$appearance in the Far Detector arise from the intrinsic beam-$\nu_e$contamination, and mis-classified neutral current and muon neutrino charged current interactions. This poster describes the techniques we use to predict such beam-induced backgrounds in the NOvA Far Detector based on the observed Near Detector data. Speaker: Erika Catano Mur (Iowa State University) • 129 Design of a Nitrogen Cooled Target Shield Pile for the LBNF Beamline The Long Baseline Neutrino Facility (LBNF) will utilize a beamline at Fermilab to produce a neutrino beam aimed at the Sanford Underground Research Facility in South Dakota. A primary proton beam will interact with a target to produce mesons, which will be focused by magnetic horns before decaying into neutrinos. The target and horns are contained in a chamber, which is surrounded by a shield pile made of steel, concrete, marble, and borated high-density polyethylene to protect workers and surrounding groundwater from irradiation. The shielding is cooled by nitrogen gas which is pumped through the entirety of the chamber. The nitrogen also prevents corrosion and the production of unwanted radioactive isotopes. The chamber is kept at a positive pressure to prevent the infiltration of air into the chamber. The sealing system of the chamber is composed of a leak-tight stainless steel barrier around the target chamber, a modular hatch cover system to allow access to the chamber for maintenance, sealed feedthroughs which allow cooling water, power, and instrumentation to reach the target and horns inside, and a fill/purge system. The shielding closest to the beamline components is also cooled using water-cooled panels. We discuss here the current design of the shield pile, and the cooling and sealing systems which support it, as well as the expected challenges and plans for improvement. Speaker: Joseph Angelo (Fermi National Accelerator Laboratory) • 130 Looking at BNB Neutrinos in the NOvA Near Detector The NOvA Near Detector (ND) is a 300-ton, fine-grained, nearly fully active low-Z tracking calorimeter located at Fermilab, located 1 km from the NuMI beam target. The unique positioning of the ND also results in an exposure to Booster Neutrino Beam (BNB) neutrinos at 162 mrad off-axis, 780 m away from the target with a kaon-induced neutrino energy peak around 1.4 GeV and a pion-induced energy peak around 400 MeV. With an estimated 2500 νμ true charged-current interactions from the BNB per year, there are enough data to perform a pion/kaon production ratio measurement, with an opportunity to augment the NOvA ND energy scale and add to the understanding of neutrino cross-sections in the 1-2 GeV region in the future. This analysis implements new algorithms to identify and reconstruct low energy events by using visual deep learning tools such as convolutional neural networks. This poster discusses the current status of the analysis. Speaker: Ryan Murphy (Indiana University) • 131 Tracking Detector Performance and Data Quality in the NOvA Experiment NOvA is a long-baseline neutrino oscillation experiment. It uses the NuMI beam from Fermilab and two sampling calorimeter detectors located off-axis from the beam. The NOvA experiment measures the rate of electron-neutrino appearance in the almost pure muon-neutrino NuMI beam, with the data measured at the Near Detector being used to accurately determine the expected rate at the Far Detector. It is very important to have automated and accurate monitoring of the data recorded by the detectors so any hardware, DAQ or beam issues arising in the 344k (20k) channels of the Far (Near) detector which could effect quality of the data taking are determined. This poster will cover the techniques and detector monitoring systems in various stages of data taking. Speaker: Mr Biswaranjan Behera (IIT Hyderabad/Fermilab) • 132 Prospects for Neutron-Antineutron Oscillation Searches with Convolutional Neural Networks in Liquid Argon Time Projection Chambers Future, large-scale liquid argon time projection chamber (LArTPC) detectors provide a unique opportunity to search for neutron-antineutron oscillation. This is a rare, baryon-number-violating signature predicted only by theories beyond the Standard Model. This talk will present a convolutional neural network approach that can be used to search for neutron-antineutron oscillation events in the future Deep Underground Neutrino Experiment (DUNE). The network performance will be presented, along with preliminary sensitivity results. Speaker: Georgia Karagiorgi (Columbia University) • 133 Particle Identification and Kaon Physics in LArIAT Kaon physics in liquid argon time projection chambers (LArTPCs) is important for future proton decay searches in large-scale LArTPCs, such as DUNE. Using LArIAT, a LArTPC test beam experiment at Fermilab, we have selected—with traditional beam line instrumentation—around 3E3 kaon candidate events, creating the first kaon data sample in a LArTPC. This sample allows us to perform the first studies of kaons in this detector, including the kaon total cross section on argon, automatic reconstruction performance of kaon topologies, and LArTPC-based kaon identification efficiencies. Further, we explore ways to improve this LArTPC-based particle identification through the use of data-driven machine learning techniques, work beneficial to all future automatic LArTPC reconstruction. Speaker: Mr Daniel Smith (Boston University) • 134 Measuring the$t\bar{t}$Forward-Backward Asymmetry using semi-leptonic final states at 8 TeV with the CMS detector We presents a measurement of Forward-Backward Asymmetry($\displaystyle{A_{FB}}$) in$t\bar{t}$production. The data sample corresponds to$19.7\,\textrm{fb}^{-1}$of integrated luminosity in proton-proton collisions at$\sqrt{s} = 8\,\textrm{TeV}$collected by the CMS experiment at the LHC. Events selected contain a single isolated muon or electron, with four or five jets of which two are b-tagged. A template technique is used to extract the asymmetry from the top quark kinematic distributions. This technique is based upon an extension of the tree-level cross section for$q\bar{q}$initial states that sensitively isolates$q\bar{q}$from$gg/qg$initial states. The measured$A_{FB}$and relative aboundance of$q\bar{q}$initiated$t\bar{t}$will be reported and compared to both theoretical calculation and results from D0 and CDF experiments of Tevatron. Speaker: lei feng (Johns Hopkins University) • 135 Search for a large muon neutrino magnetic moment in the NOvA Near Detector Various scenarios of beyond the Standard Model physics predict Majorana neutrinos with large magnetic moments. NOvA is well suited for such searches since its detectors are optimized for efficient electron detection and its Near Detector (ND) is exposed to an intense neutrino flux from the NuMI neutrino beam at Fermilab. This facilitates the accumulation of significant statistics for studying muon-neutrino-electron elastic scattering in the ND. A deep learning neural network for particle identification training is used to distinguish scattered electrons from neutral pion induced electromagnetic showers and the charged current background. We present an overview of this technique and the sensitivity on the search for a muon neutrino magnetic moment. Speaker: Mr Biao Wang (Southern Methodist University) • 136 Probing new physics scale through dimension-6 operator and enhanced$t\bar{t}h$and$hh$production at the LHC No matter what the scale new physics is, deviations from the Standard Model for the Higgs observables will indicate the existence of such a scale. We consider effective six dimensional operators, and their effects on the Higgs productions and decays to estimate this new scale. Large uncertainties with the SM predictions still remains in some of the observables of these measurements. This encourages us to venture if there is a new physics scale that might be estimated from the uncertainty in these measurements, as well as if we can make make predictions which can be tested in the LHC. With this aim in mind, we consider the effect of a selected set of dimension six operators along with the SM. The dimension six operators related to Higgs physics can be introduced both in the strong sector, as well as in the electroweak sector. Such operators will make extra contributions for the Higgs productions, as well as for its various decay modes. In the most general case, for the effective dimension six operators, there are many operators, and involve large number of parameters. In order to reduce the number of parameters, we only consider a selected set of such operators in the gauge sector (both strong and electroweak (EW), as well as the Yukawa sector, which are responsible for larger effects, and do not affect the constraints from the EW precision tests in a significant way. Given the large uncertainties in the Higgs Productions and decays, we find that this scale can be as low as 500 GeV. We then calculate the$t\bar{t}h$̄productions , as well as double Higgs using the effective couplings at the Large Hadron Collider, and show these can be much different than those predicted by the Standard Model, for an wide region of these parameters space. These predictions can be tested in the current or the future runs of the LHC. Speaker: SUDIP JANA (OKLAHOMA STATE UNIVERSITY) • 137 An overview of the ANNIE experiment at Fermilab The Accelerator Neutrino Neutron Interaction Experiment (ANNIE) is located at SciBooNE Hall along the Booster Neutrino Beam at Fermilab. It consists of a 23-ton water Cherenkov detector loaded with gadolinium, muon range detector and a veto wall. The main goal of the experiment is to measure the final state neutron multiplicity from charged current neutrino-nucleus interactions within the gadolinium-loaded water. Currently, ANNIE is running in Phase-I and it will be upgraded to Phase-II in the summer, by installing Large Area Picosecond Photodetectors (LAPPDs) in the detector. LAPPDs are a novel photodetector technology with single photoelectron time resolutions less than 100 picoseconds, and spatial imaging capabilities to within a single centimeter. They will play a crucial role to separate events of charged-current quasi-elastic (CCQE) interactions and inelastic multi-track charged current interactions. In this talk, we discuss the current status and future plans of the experiment. Speaker: Dr Emrah Tiras (Iowa State University) • 138 The NOvA Data Driven Trigger The NOvA experiment is a long-baseline neutrino experiment utilizing an intense off-axis neutrino beam and two segmented liquid-scintillator-based detectors, a 300t near detector and a 14kt far detector located 810 km from the beam source. The NOvA experiment employs a data-driven trigger system to fully exploit the detectors during non-beam operation. We will present an overview of the NOvA trigger design and implementation, as well as data-driven trigger algorithms currently being used for calibration and a non-beam physics program. Speaker: Matthew Judah (Colorado State University) • 139 A Panel Prototype for the Mu2e Straw Tube Tracker at Fermilab The Mu2e experiment will search for coherent, neutrino-less conversion of muons into electrons in the Coulomb field of an aluminum nucleus with a sensitivity of four orders of magnitude better than previous experiments. The signature of this process is an electron with energy nearly equal to the muon mass. Mu2e relies on a precision (~0.1%) measurement of the outgoing electron momentum to separate signal from background. In order to achieve this goal, Mu2e has chosen a very low-mass straw tracker, made of about 20,000 5 mm diameter thin-walled (15 μm) Mylar® straws, held under tension to avoid the need for supports within the active volume, and arranged in an approximately 3 m long by 0.7 m radius cylinder, operated in vacuum and a 1 T magnetic field. Groups of 96 straws are assembled into modules, called panels. We present the prototype and the assembly procedure for a Mu2e tracker panel built at Fermilab. Speaker: Alessandra Lucà (FERMILAB) • 140 LAr Scintillation Light Detection, Simulation and Analysis in LArIAT LArIAT is a Liquid Argon Time Projection Chamber (LArTPC) installed in a charged particle beam at the Fermilab Test Beam Facility. This experiment, currently in its third run of data taking, is exploring the response of LAr at particle energies relevant for neutrino experiments. It also serves as a platform to prepare and benchmark the simulation, analysis and reconstruction software, used in LAr neutrino experiments. One of LArIAT's R&D goals is to develop readout methods for scintillation light in LArTPCs. The scintillation light detection system consists of Photomultipliers and Silicon Photomultipliers combined with wavelength-shifter covered reflector foils to enhance the detection efficiency and increase uniformity. This poster will present the methods of using scintillation light in LArTPCs to evaluate detector performance, PID and calorimetry and their results in LArIAT. Speaker: Pawel Kryczynski (IFJ PAN, Krakow) • 141 NNLO QCD Predictions of W and Z Bosons in proton-proton collisions at 7, 8, 13, 14 and 100 TeV Center of Mass Energies Large Hadron Collider has run at 7, 8, 13 TeV but it is expected and planned to collect data at 14 TeV center of mass energy in 2019. Meanwhile, a 100 TeV hadron collider, called Future Circular Collider (FCC), is proposed to be built as a post-LHC particle accelerator. Therefore, we estimated W and Z boson cross sections and their uncertainties at LO, NLO and NNLO QCD using different most modern PDF models to understand the effect of the energy increase from 7 to 100 TeV. The predictions are computed using publicly available parton level Monte Carlo program DYnnlo1.5 and FEWZ 3.1. PDF, strong coupling constant, scale, model and parameterization uncertainties are considered and their size changes by energy increase are investigated. Speaker: Dr Emrah Tiras (Iowa State University) • 142 NOvA Short-Baseline Tau Neutrino Appearance Search Standard three-flavor neutrino oscillations have well explained by a wide range of neutrino experiments. However the anomalous results, such as electron-antineutrino excess seen by LSND and MiniBooNE do not fit the three-flavor paradigm. This can be explained by an additional fourth flavor sterile neutrino at a larger scale than the existing three flavor neutrinos. The NOvA experiment consists of two finely segmented, liquid scintillator detectors operating 14 .6 mrad off-axis from the NuMI muon-neutrino beam. The Near Detector is located on the Fermilab campus, 1 km from the NuMI target, while the Far Detector is located at Ash River, MN, 810 km from the NuMI target. The NOvA experiment is primarily designed to measure electron-neutrino appearance at the Far Detector using the Near Detector to control systematic uncertainties; however, the Near Detector is well suited for searching for anomalous short-baseline oscillations. This poster will present a novel method for selecting tau neutrino interactions with high purity at the Near Detector using a convolutional neural network. Using this method, the sensitivity to anomalous short-baseline tau-neutrino appearance due to sterile neutrino oscillations will be presented. Speaker: Mr Rijeesh Keloth (Cochin University of Science and Technology) • 143 Calibration of gBlocks using Offline Jets for the gFEX Subsystem of the ATLAS Level 1 Calorimeter Trigger The Global Feature Extractor (gFEX) subsystem of the ATLAS Level 1 calorimeter trigger will identify large-radius jets, which are typical of Lorentz-boosted objects. Here I present results from calibrating gBlocks, groups of towers, using offline R=0.4 jets. Dijet Monte Carlo simulation samples at a center of mass energy of 13 TeV are used to find calibration factors. Effects on energy resolution are studied as well. Speaker: Ian Snyder (University of Oregon) • 144 Cross Section Predictions of W/Z + Jets at LHC Cross section predictions of W and Z bosons in association with jets (up to 6 jets) are presented using Alpgen MC generator with CTEQ6L1, a leading order parton distribution function (PDF). This study has been performed at center of mass energies of √s= 7, 8, 13, 14 TeV. To validate the results, a detailed comparison of cross section predictions is performed with the measured results by CMS and ATLAS collaborations. In addition, NLO QCD predictions are performed up to 2 jets using MCFM-8.0 MC generator. Speaker: Dr Emrah Tiras (Iowa State University) • 145 Skimming tau neutrinos and tau showers in the atmosphere A technique to detect an astrophysical or cosmic high energy tau neutrino flux involves using the Earth as a neutrino converter. Taus produced near enough to the surface of the Earth can emerge and decay to produce atmospheric showers. The neutrino cross section, energy transfer to the tau, and tau energy loss via electromagnetic interactions will be discussed with applications to surface- and satellite-based detectors. The sensitivity of event rates to calculational approaches to the electromagnetic structure functions will be emphasized. Speaker: Prof. Mary Hall Reno (University of Iowa) • 146 Design, construction and characterization of a three channel of cosmic ray detector Cosmic rays are particles generated by astrophysical sources, which currently are studied for their physical properties. Cosmic rays research can be used to improve technology, for instance, spectroscopy for material identification. A three-channel detector was built using three photo-multipliers, two scintillation plastic and several common materials, water, air, oil, aluminum, and others, to scan. They were allocated in vertical position, where material to scan channel is between scintillation plastics channels in order to validate the signal and study the interaction of cosmic rays with the different materials. Details of characterization, operation and some preliminary physical results are reported. Speaker: Mr Oscar Eduardo Moreno Palacios (Universidad de Guanajuato) • 147 Towards a new approach to cosmology with the Dark Energy Survey and Gravitational Waves Motivated by the exciting prospect of new wealth of information that will arise from observations of gravitational and electromagnetic radiation from the same astrophysical phenomena, we have established a program to search for optical counterparts to LIGO/Virgo events using the the Dark Energy Camera (DECam). The project is performed in a broad collaboration including members of the Dark Energy Survey (DES) Collaboration, the LIGO/Virgo Collaboration, and the community at large. Its success has motivated us to pursue a new survey with DECam: the Blanco Images of the Southern Sky (BLISS) survey. BLISS expands the DECam sky coverage beyond the areas covered by DES and will increase the efficiency of our searches. In this talk, I present an overview of this effort, including results of searches for signatures of the first two binary black hole mergers detected by LIGO in the 2015-2016 observing campaign and status of the ongoing 2016-2017 campaign. I will also discuss plans for upcoming seasons and long term prospects for this exciting emerging field: multi-messenger cosmology with gravitational waves and optical data. Speaker: Dr Marcelle Soares-Santos (Fermilab) • 148 DES & Planck survey: Galaxy group-tSZ cross correlation Stacking Sunyaev-Zeldovich map of groups and clusters is powerful tool to find average distribution of hot gas in these systems. The goals of this work are to estimate the redshift evolution of SZ signal and average bias weighted electron pressure of the universe. We stack SZ signal from Planck at all the detected redmapper groups from year 1 Dark Energy Survey data. We use groups at different redshift and mass to find the average pressure profile of these systems. We show that the detected signal can be modeled by a halo model using Battaglia pressure profile. After the modeling we show that there is an evolution in the pressure profile in the groups and we estimate the average thermal energy of the universe. Speaker: Vinu Vikraman (Argonne National Lab) • 149 Photometric Properties and Stellar Masses in Dark Energy Survey Galaxy Clusters We present the results of a study of the properties of clusters, selected using the RedMaPPer technique, from the Dark Energy Survey Year 1 data, which cover an area of nearly 2000 square degrees on the sky. We calculate cluster membership probabilities and use a Gaussian mixture model method to characterize the red sequence and blue cloud components of our clusters, and we will present our results on properties such as red sequence peak color, slope, and width, and cluster blue fraction, in particular as functions of redshift. Moreover, we introduce a new cluster stellar mass observable, mu*, and will show that it works as a reliable mass proxy for cosmology by comparing our predictions to X-ray measurements. Finally, we will show our results for the redshift evolution of the stellar masses and star formation rates in our cluster member galaxies. Speaker: Brian Welch (University of Chicago/Fermilab) • 150 A search for BH dark matter using microlensing in the Dark Energy Survey Massive Primordial Black Holes (MPBH) generated from large inflation-era curvature fluctuations that reenter during the radiation era could constitute the majority of the dark matter, an idea revived by the LIGO observations of merging 30 solar mass black holes. In this model, the mass distribution of MPBH ranges from 0.01 to 100 solar masses, peaking perhaps at 50 solar masses. There is, remarkably, a window in the constraints at these masses; furthermore the MPBH could be clustered, breaking one of the assumptions of microlensing limits. We describe a project that uses the Dark Energy Survey data to perform a microlensing measurement of massive compact objects at 10-100 solar masses. The key idea is that a microlensing event has a duration of t = 2.5 years (M/10M_solar)^{1/2} and thus masses in the range expected for MPBH are observable in the DES. The DES observes its entire footprint twice per year per bandpass, so there are 8 usable visits per year as microlensing is achromatic. The primary difference between this project and the MACHO/OGLE/EROS surveys is that we will use the 10^7 field stars in the DES south galactic cap and not the LMC or Galactic Center. We will describe our expected limits on MPBH mass distributions assuming they make up all of the dark matter. Speaker: James Annis (Fermilab) • 151 Charged Lepton Flavor Violation in Electron-Positron Scattering: Calculations of Cross Section and Asymmetry Using an Effective Field Theory We performed theoretical calculations of charged lepton flavor violation (CLFV) cross sections and asymmetries in electron-positron scattering. Examples of CLFV include electron antitau final states and electron antimuon final states. We used an effective field theory that incorporated three types of Beyond Standard Model operators: leptonic operators and radiative operators leading to tree-level diagrams and quark-lepton operators leading to a one-loop diagram. The one-loop diagram was treated in two ways: perturbatively using Standard Model Feynman Rules and non-perturbatively using dispersion relations to account for possible resonance effects. We calculated constraints on the effective coupling constants from current experimental upper bounds. Future colliders such as Belle II and BES III can use our calculations in searches for charged lepton flavor violation. Speaker: Mr Ching Li (Haverford College) • 152 Zero-Range Effective Field Theory for Resonant Wino Dark Matter The most dramatic "Sommerfeld enhancements" of neutral-wino-pair annihilation occur when the wino mass is tuned to near critical values where there is a zero-energy S-wave resonance at the neutral-wino-pair threshold. If the wino mass is larger than the critical value, the resonance is a wino-pair bound state. If the wino mass is near a critical value, low-energy winos can be described by a zero-range effective field theory in which the winos interact nonperturbatively through a contact interaction. The effective field theory is controlled by a renormalization group fixed point at which the neutral and charged winos are degenerate in mass and their scattering length is infinite. The parameters of the zero-range effective field theory can be determined by matching wino scattering amplitudes calculated by solving the Schrödinger equation for winos interacting through a potential due to the exchange of weak gauge bosons. The power of the zero-range effective field theory is illustrated by calculating the rate for formation of the bound state in the collision of two neutral winos through the emission of two soft photons. Speaker: Evan Johnson (Ohio State University) • 153 Impact of Neutrino Decay on Sterile Neutrino Search in IceCube Anomalies in short-baseline neutrino experiments have suggested the existence of a ~1 eV sterile neutrino. IceCube, an ice-Cherenkov neutrino detector at the South Pole is an ideal testing ground for such neutrinos, but recent searches have found no evidence for them. In a 3+1 sterile neutrino model, decay of the heaviest mass eigenstate to lighter eigenstates is largely unconstrained and could modify the results of the searches in IceCube. We present the results of a phenomenological study where neutrino decay is included as a sub-leading effect to oscillation in a 3+1 model in IceCube. Speaker: Marjon Moulai (MIT) • 154 Full TPC Signal and Noise Simulation MicroBooNE is an 89-ton Liquid Argon Time Projection Chamber (LArTPC) and the first of a trio of LArTPCs in the Short Baseline Neutrino (SBN) program which will search for a light sterile neutrino and measure neutrino-argon interaction cross sections. Located in the Booster neutrino beam at Fermi National Accelerator Laboratory, MicroBooNE has taken neutrino data since October 2015. This poster outlines the intricacies of a full TPC noise and signal simulation. More specifically, this poster will detail the noise simulation based on measurement in the data and summarize the ramifications of induced current from nearest neighboring wires and other effects unique to LArTPC technology. The implementation of the full TPC signal and noise simulation is crucial to understanding the detector response for this technology. Speaker: Ms Brooke Russell (Yale University) • 155 Studies of Radiation Damage to Silicon Photomultipliers We present results of radiation tests of 1.3×1.3 mm^2 and 2.0×2.0 mm^2 for Hamamatsu silicon photo-multiplier (SiPM) sensors. These studies were performed to evaluate the suitability of the Hamamatsu devices for use in the Mu2e Cosmic Ray Veto. Distinct sets of eight SiPMs were exposed to four different 1 MeV neutron equivalent doses of 200 MeV protons. Measurements of the breakdown voltage, gain and noise rates at different bias overvoltages, photoelectron thresholds, and LED illumination levels were taken before and after irradiation. Speaker: Dr Sergey Uzunyan (Northern Illinois University, for the Mu2e Cosmic Ray Veto Group) • 156 Drifted Charge Extraction in Single Phase LArTPCs The MicroBooNE detector is the first to be built in the short-baseline neutrino program. It is a single-phase LArTPC built to observe interactions of neutrinos from the on-axis Booster and off-axis NuMI beams at the Fermi National Accelerator Laboratory in Batavia, IL. We describe the concept and procedure of LArTPC drifted-charge extraction which converts the raw digitized TPC waveform to the number of ionized electrons passing through the wire plane at a given time. The proper recovery of the number of ionized electrons from both induction and collection anode wire planes is important to the success of the subsequent reconstruction algorithms. In this poster, we will show the details of the procedure including the key steps of 2D deconvolution and region-of-interest finding. Speaker: Dr JYOTI JOSHI (Brookhaven National Laboratory) • 157 Liquid argon test of the ARAPUCA device at the National Laboratory of Synchrotron Light in Campinas (São Paulo) The ARAPUCA is a new concept for liquid argon scintillation detection, particularly suited for large liquid argon time projection chambers. It is constituted by a combination of a passive light collector and photo-sensitive silicon devices, which will allow to improve the detection efficiency of actual devices by an order of magnitude. The basic idea is to trap photons inside a box whose internal surface has an extremely high reflectivity and which is observed by silicon devices (SiPM), so that the detection efficiency is high even with a small active coverage of the internal surfaces. The photon trapping is obtained with a smart combination of a short-pass dichroic filter and two different wavelength shifters, one of each side of the filter, which represents the acceptance window of the ARAPUCA. We will report of the first liquid argon test of the device in Brazil - at the National Laboratory of Synchrotron Light in Campinas (Sao Paulo) - which, to our knowledge, is the first liquid argon experiment in Latin America ever done up to now. The device was exposed to an alpha source of known energy so that it was possible to estimate its detection efficiency. The results were excellent and in perfect agreement with Monte Carlo predictions. Speaker: Mrs Marina Guzzo (UNICAMP) • 158 Pion Production Measurements at MINERvA The MINERvA collaboration has performed important measurements on pion reactions off a scintillator (CH) target, using the NuMI beam at Fermilab in both neutrino and anti-neutrino configurations. These reactions, used by generators to improve nuclear models, are essential for a better understanding of neutrino oscillation experiment results. An important fraction of the signal and background systematic uncertainties in this experiments come from the misidentification of these reactions. The current NOvA era, with a more energetic and intense NuMI beam, allows MINERvA to perform a more extensive exploration of these neutrino reactions, with more exciting results coming. Speaker: Prof. Gonzalo Diaz (Rochester University) • 159 MuSim, a Graphical User Interface for Multiple Simulation Codes MuSim is a user-friendly program designed to interface to many different particle simulation codes, regardless of their data formats or geometry descriptions. It presents the user with a compelling graphical user interface that includes a flexible 3-D view of the simulated world plus powerful editing and drag-and-drop capabilities. All aspects of the design can be parameterized so that parameter scans and optimizations are easy. It is simple to create plots and display events in the 3-D viewer, allowing for an effortless comparison of different simulation codes. Simulation codes: G4beamline 3.02, MCNP 6.1, and MAD-X; more are coming. Many accelerator design tools and beam optics codes were written long ago, with primitive user interfaces by today's standards. MuSim is specifically designed to make it easy to interface to such codes, providing a common user experience for all, and permitting the construction and exploration of models with very little overhead. For today's technology-driven students, graphical interfaces meet their expectations far better than text-based tools, and education in accelerator physics is one of our primary goals. Speaker: Dr Mary Anne Cummings (Muons, Inc.) • 160 Pre-production and quality assurance of the Mu2e Silicon Photomultipliers The Mu2e calorimeter is composed by two disks of 1348 un-doped parallelepiped CsI crystals of 34x34x200 mm^3 dimension, each one readout by two large area SiPM arrays. We translated the calorimeter requirements in a series of technical specifications for the SiPMs that are summarized by the following list: - high gain, above 10^6, for each monolithic (6x6) mm^2 SiPM cell; - good photon detection efficiency, PDE, of above 20% at 310 nm to well match the light emitted by the un-doped CsI crystals; - large active area that, in combination with the PDE, could provide a light yield of above 20 p.e./MeV; - fast rise time and a narrow signal width to improve time resolution and pileup rejection; - Mean to Time Failure (MTTF) of O(10$^6$) hours; - good resilience to neutrons for a total fluency up to 10^12 n(1 MeV-eq)/cm^2. A modular and custom SiPM layout has been chosen to satisfy these requirements. A pre-production of 150 Mu2e SiPMs has been procured by three international firms (Hamamatsu, Sensl and Advansid). A detailed quality assurance, QA, has been carried out on each SiPM. A summary of the techniques used and of the QA characterization of the sensors will be shown. Speaker: Mrs Raffaella Donghia (LNF - INFN) • 161 NuMI Target and Horn Studies for NOvA The NuMI Off-axis νe Appearance (NOvA) experiment is a long baseline neutrino oscillation experiment designed to measure both νe appearance and νµ disappearance. The Neutrinos at the Main Injector (NuMI) facility produces an intense muon neutrino beam by directing 120 GeV protons onto a 2.5 interaction length graphite target segmented into 48 fins. The secondary particles produced at the target are focused by two magnetic horns and followed by a long decay pipe where most of the short-lived particles (pions and kaons) decay to neutrinos.The NOvA detectors are placed 14.6 mad off-axis to the NuMI beam. In this poster we present an update on the target and horn set configuration study for an optimized NOvA neutrino flux. We found that a new target design with 24 fins upstream and 24 fins extended inside of the first horn produces more off-axis neutrino flux than the existing NOvA target that has 48 fins upstream of the first horn. We show also our progress on optimizing the position of the second horn and the prospect to include a third horn (identical to the existing second horn) into the focusing system. Additional studies of material in the beam downstream of the horns are also under study. Speaker: Ms Jyoti Tripathi (Panjab University) • 162 Data Acquisition and Triggering for the KOTO Experiment The KOTO experiment at the J-PARC research facility in Tokai-mura, Japan aims to observe and measure the rare decay of the neutral kaon, KL → π0νν¯, in which a neutral kaon decays to a neutral pion and a neutrino antineutrino pair. This decay has a Standard Model predicted branching ratio of (3.00 ± 0.30) x 10^−11. While this decay is extremely rare, it is one of the best decays for studying charge-parity (CP) violation in the quark sector. Because the signal decay has such a low branching ratio, the data acquisition (DAQ) system for the KOTO experiment uses three levels of trigger cuts to selectively record events of interest and discard background events. The KOTO DAQ system is designed to have a highly optimized signal acceptance and background rejection due to the high trigger rate. This poster will focus on these details and how the triggers and DAQ system address the physics requirements of the detectors. Speaker: Ms Melissa Hutcheson (University of Michigan) • 163 Large Neutrino Mixing Angles in Minimal SO(10) Unification The possibility of generating small neutrino mass and large neutrino mixing angles, in the context of the most economic Yukawa sector of non-supersymmetric SO(10) unification is studied. In SO(10) grand unification, the mass matrices of the quarks and leptons are related and given in terms of the same fundamental Yukawa coupling matrices. This is why, it is highly challenging to reproduce the small quark mixings and large neutrino mixings simultaneously. In this work, the minimal SO(10) grand unified theory consistent with these phenomenological requirements is constructed. Our study shows that, if SO(10) gauge symmetry is the only symmetry of the theory, then the Yukawa sector consists of a real 10, a real 120 and a complex 126 dimensional representations. This minimal setup demands the neutrino mass hierarchy to be normal ordering and predicts the two experimentally yet unmeasured quantities, the leptonic Dirac CP-violating phase and the lightest neutrino mass. Gauge coupling unification and proton decay are also analysed. Speaker: Shaikh Saad (Oklahoma State University) • 164 Cosmic Ray Backgrounds in the Mu2e Experiment at Fermilab The Mu2e experiment will study charged lepton flavor violation by searching for the neutrinoless, coherent conversion of a 𝜇− to an 𝑒−. Such a process will result in an electron of 105 MeV energy. A major background source comes from cosmic-ray muons which can either be misidentified as signal electrons or produce 105 MeV electrons. Such events will occur at a rate of approximately one per day. An active veto detector surrounding the apparatus will be used to detect incoming cosmic-ray muons. Results will be shown from one of the most extensive simulation campaigns ever undertaken in which the cosmic-ray background from several times the entire running period was simulated: over 1012 generated cosmic-ray muons. Speaker: Dr Ralf Ehrlich (University of Virginia) • 165 Muon Tomography of Galeras Volcano: first results leaded by young scientists in Colombia Muon radiography is based on the observation of the absorption of muons in matter, as the ordinary radiography does by using X-rays.The interaction of cosmic rays with the atmosphere produce Extensive Air Showers (EAS), which provide abundant source of muons. These particles can be used for various applications of muon radiography, in particular to study the internal structure of different volcanoes edifice. In this talk we will present results leaded by young scientists in Colombia, and the relevance to provide guidance to future young undergraduate and high school students in software as ROOT, GEANT4 and C++ and their applications in fields as high energy physics. As part of the results to be presented, we will show the first study of the muon lateral distribution at Pasto City altitude (4276 m a.s.l.) using CORSIKA to model the interaction of the cosmic rays with the atmosphere. Furthermore the first simulation in GEANT4 of an active volcano in Pasto city (Colombia) and a particle detector located near the volcano cone will be presented. Speakers: Dr Alex Tapia (University of Medellin), Dr David Martinez Caicedo (Illinois Institute of Technology) • 166 Radiopurity Screening and Radiological Simulation for DUNE The design of the far detector of the Deep Underground Neutrino Experiment (DUNE) consists of four 10 kton supermodules, each filled with liquid Argon and to be located underground at SURF/SD. Radiological backgrounds are mostly relevant for the low-energy physics of DUNE, such as supernova neutrinos. Radiopurity requirements are driven by the intrinsic Ar-39 contamination of about 1 Bq/kg for undepleted liquid argon. The long electron drift length of about 3.5 m inside each time projection chamber, as well as the one sided light collection, complicate further the impact of radiological backgrounds from detector materials. The radiopurity screening of detector materials will be discussed and how the results enter a comprehensive radiological simulation using LArSoft. Additionally, LArSoft improvements to the usability of the photon simulation are presented. Speaker: Jason Stock (South Dakota School of Mines and Technology) • 167 Sterile neutrino search in the NOvA Far Detector. The majority of neutrino oscillation experiments have obtained evidence for neutrino oscillations that are compatible with the three-flavor model. Explaining anomalous results from short-baseline experiments, such as LSND and MiniBooNE, in terms of neutrino oscillations requires the existence of sterile neutrinos. The search for sterile neutrino mixing conducted in NOvA uses a long baseline of 810 km between Near Detector (ND) at Fermilab and Far Detector (FD) in Minnesota. The signal for sterile neutrino oscillations is a deficit of neutral-current neutrino interactions at the FD with respect to the ND prediction. In this poster, I will present the analysis improvements that we are implementing for future NC sterile neutrino searches with NOvA. These include: improved modelling of our detector response; the inclusion of NC 2p2h interaction modelling; implementing a better energy reconstruction technique; and including possible oscillation due to sterile neutrinos in the ND. This improvements will enable us to do a simultaneous ND-FD shape fit of the NC energy spectrum covering a wider sterile mass range than previous analyses. Speaker: Mr SIJITH EDAYATH (COCHIN UNIVERSITY OF SCIENCE AND TECHNOLOGY, INDIA) • 168 Exploring end-to-end image-based deep learning for particle & event classification An essential part of new physics searches at the Large Hadron Collider at CERN involves event classification, or distinguishing signal decays from one of its many background look-alikes. Traditional techniques have relied on reconstructed particle candidates and their physical attributes. However, such reconstructed data are the result of a long, potentially lossy process of forcing the raw sensor data into progressively more physically intuitive quantities. Meanwhile, powerful image-based machine learning algorithms have emerged that are able to directly digest raw sensory data and output a prediction---so called end-to-end deep learning classifiers. We explore the use of such algorithms to perform physics classification using raw sensory data from the CMS detector. As proof of concept, we classify photon- versus electron-induced ECAL showers and compare the performance of using raw sensor data versus shower shape data. Speaker: Michael Andrews (Carnegie Mellon University) • 169 Observing Neutrinos from the Next Galactic Supernova with the NOvA Detectors The next galactic core-collapse supernova will deliver a wealth of neutrinos which for the first time we are well-situated to measure. These explosions produce neutrinos with energies between 10 and 100 MeV over a period of tens of seconds. Galactic supernovae are relatively rare events, occurring with a frequency of just a few per century. It is therefore essential that all neutrino detectors capable of detecting these neutrinos are ready to trigger on this signal when it occurs. This poster describes a data-driven trigger which is designed to detect the neutrino signal from a galactic core-collapse supernova with the NOvA detectors. The trigger analyzes 5ms blocks of detector activity and applies background rejection algorithms to detect the signal time structure over the background. This background reduction is an essential part of the process, as the NOvA detectors are designed to detect neutrinos from Fermilab's NuMI beam which have an average energy of 2 GeV--well above the average energy of supernova neutrinos. Speaker: Justin Vasel (Indiana University) • 170 Design and Simulation of the IsoDAR RFQ Direct Injection System and Spiral Inflector The IsoDAR (Isotope Decay-At-Rest) experiment aims to explore physics beyond the standard model by searching for anomalous neutrino oscillations indicative of sterile neutrinos. The experiment requires a primary beam of H2+ ions to be accelerated to an energy of 60 MeV/amu at a current of 5 mA, which will be accomplished by using a high-power compact cyclotron. One of the challenges in this scheme is the injection into the cyclotron, where space-charge forces are strong and acceptance into a small RF phase window is desired. We aim to achieve this by using a Radio-Frequency Quadrupole (RFQ) injector, brought very close to the center of the cyclotron, which is capable of efficiently transporting and bunching the beam before an electrostatic deflector - called a spiral inflector - turns the beam onto the mid-plane of the cyclotron for acceleration. Careful design and simulation of this process is necessary. To this end, electric and magnetic field maps are generated in OPERA and loaded into the accelerator simulation code OPAL to run start-to-end simulations of the injection system and first few turns in the cyclotron. Several iterations between RFQ design and spiral inflector simulations will be necessary to optimize the geometry of the spiral inflector, i.e. to minimize the number of ions lost during injection and maximize beam current. I will present the development and latest results of the particle simulations and design optimizations for the IsoDAR RFQ direct injection project, particularly the spiral inflector. Speaker: Philip Weigel (Drexel University) • 171 Seasonal Variations of multiple-muons in NOvA Seasonal variations of cosmic ray muons have been well-measured by a number of underground experiments at a variety of overburdens and it has been found that the rate of muons increases in the summer and decreases in the winter. This is understood from the properties of the atmosphere as the temperature varies. But with large statistics the seasonal variation of multiple muons was measured in the MINOS ND (225 mwe) and the MINOS FD (2100 mwe). The rates increase in the winter and decrease in the summer, opposite to the result for single muons. Several hypotheses for this unexpected result were considered, but the effect is not currently explained. New data from the NOvA ND (225 mwe) will be used to study the situation further. Speaker: Prof. Philip Schreiner (Benedictine University) • 172 ProtoDUNE Trigger Study DUNE is an experiment aimed at determining the mass hierarchy of neutrinos and measuring parity violation in the neutrino sector. The ProtoDUNE detector is a prototype Liquid Argon (LAr) TPC for the DUNE far detector and will be operated at CERN to primarily study hadronic interactions in LAr at the few GeV energy scale. Due to the operation of ProtoDUNE in a beamline near the surface, the detector will need to be able to discern between the intended beam particles and background events arising primarily from cosmics and beam byproducts such as halo muons and other contaminants. Thus, in order to reduce the data rates to manageable levels, ProtoDUNE will employ the use of triggers. The Central Trigger Board (CTB) was designed to make use of the the available information from the Cosmic Ray Tagger, Beam Instrumentation, and Photon Detection System to generate triggers for ProtoDUNE. The CTB itself is a custom Printed Circuit Board which houses an FPGA (Xilinx Zynq 7Z020), where the trigger logic is implemented in firmware, and an embedded processor running a Linux distribution. In this poster we discuss possible trigger schemes and their viability based on timing simulations. Speakers: David Rivera (University of Pennsylvania), Jonathon Sensenig (University of Pennsylvania) • 173 Ongoing Community Efforts in Machine Learning in Particle Physics In this poster we will highlight the different community efforts in machine learning in high-energy physics and their positive impact on the community. These efforts include the Inter-Experimental (IML) LHC Machine Learning working group, the Machine Learning group at Fermilab, aMVA4NewPhysics, INSIGHTS, Data Science at HEP workshops. Additional opportunities in the areas of education, training and outreach, as well as involvement of the broader ML community would further enable the progress of machine learning in HEP. Speakers: Ms Fernanda Psihas (Indiana University), Sergei Gleyzer (University of Florida) • 174 Silicon and Germanium Ionization Yield Measurements with Neutron Beams SuperCDMS SNOLab is using low energy threshold Si/Ge detectors for dark matter direct searches. One mode of operation for the experiment runs detectors in a high-voltage-biased mode, to use Neganov-Luke Amplification. Understanding the ionization yield of low-energy nuclear recoils is essential for interpreting dark matter search data taken in this mode. We present two calibration experiments designed to measure the ionization yield with the CDMS-style detectors in monoenergetic neutron beams. One experiment is performed with an Adiabatic-Demagnetization Refrigerator at the TUNL facility, and the other one with a Dilution Refrigerator in the NEXUS@FNAL facility with a DD neutron generator. In this poster, we show the experimental setups and simulation results of this calibration program. Speaker: Ziqing Hong (Northwestern University) • 175 A uniform magnetic field generator system and a Cu hybrid cosmic ray detector of 4 channels In the universe, there are several sources that produce very energetic cosmic rays that interact with the Earth’s atmosphere and create new low energy particles. These particles can be electrically charged and neutral. There are different methods to detect them, according to its interaction with a medium such as the ionization of a material and Cerenkov radiation, among others. An obtained signal can be validated with another detection method, as in a Cu hybrid detector, or with a specific array of detectors. Knowing some points where a particle has passed through, inside a magnetic field, its trajectory and electric charge can be determined. This work presents the design, construction and characterization of a uniform magnetic field generator system and a Cu hybrid cosmic ray detector of 4 channels. Details and some preliminary results will be presented. Speakers: Mr Francisco Rosas-Torres (Universidad de Guanajuato), Prof. Julian Felix (Universidad de Guanajuato), Ms Karla Natalia Herrera Guzman (Universidad de Guanajuato), Mr Raul Alejandro Gutierrez Sanchez (Universidad de Guanajuato) • 176 Effects of Magnetic Horn Geometry Uncertainty on Neutrino Flux at DUNE The goals of the Deep Underground Neutrino Experiment (DUNE) at Fermi Lab, is to precisely measure neutrino and antineutrino oscillation properties to determine if charge-parity (CP) symmetry is violated in the lepton sector, thus providing a possible explanation for the matter-antimatter asymmetry in the universe, and to measure the neutrino mass ordering. To maximize the neutrino flux in the desired energy range, the secondary charged mesons produced in the interactions of an intense proton beam with a target are focused using the magnetic field created by a set of horns. To ensure an accurate understanding of the beam line and the neutrino flux, it is essential o study uncertainties stemming from the geometry to these horns. In this study, two geometric parameters are considered, (i) the eccentricity and (ii) the ellipticity of the inner conductors. The effects of eccentricity and ellipticity of the inner conductor to the resulting neutrino flux are presented. Speaker: Amador Eric (University of Texas Arlington) • 177 A particle hypothesis based approach for energy estimation in muon neutrino charged current events at NOvA NOvA is a neutrino oscillation experiment which probes the neutrino CP-violating phase and mass ordering, as well as improve limits on current neutrino oscillation parameters, by measuring oscillations of muon neutrinos and muon anti-neutrinos produced in the NuMI beam at Fermilab. The muon neutrino disappearance analysis specifically focuses on the measurements of$\Delta m_{32}^2$and$\sin^2(\theta_{23})$. Choosing the right energy estimator is key to oscillation analyses; the estimator currently used by the muon neutrino disappearance analysis identifies the muon in an event, and labels all other energy depositions as hadronic energy. However, it is possible to use a version of NOvA's convolutional visual network (CVN) to separate the hadronic energy into its individual components. Once the particle is identified using CVN, we measure the energy of these tracks with a method called "Break Point Fitting" developed to track a scattering particle passing through a detector that takes measurements at discrete intervals. The track is fit under three assumptions: muons, protons, and pions, and the energy is calculated for each. The combination of tagging particles with CVN and more accurate energy calculation with BPF will allow for a more robust energy estimator, with a possibility for an improved energy resolution. Speaker: Dr Erica Smith (Indiana University) • 178 Studies of effect of aging and studies to optimize scintillation counter response for the Mu2e Cosmic Ray Veto System The Mu2e experiment will conduct a search for charged lepton flavor violation through observation of a neutrino-less muon-to-electron conversion. In order to reduce backgrounds from cosmic ray muons, a cosmic ray veto consisting of counters made from scintillating plastic will be read out by wavelength-shifting fibers. The cosmic ray veto must have an overall detection efficiency of 99.99%. In order to meet this requirement, the light yield must be optimized and well understood. The counters are designed to meet photoelectron yield requirements over a working lifetime of 10 years. Aging studies are measuring the temporal response of the light yield of the scintillator and transmission of light through optical fibers. An oven has been used to heat samples to simulate an advanced aging process. Tests include measuring the attenuation of light through the aged optical fiber using an LED flasher with a photodiode or spectrometer and measuring the response of aged counters to radioactive sources and cosmic rays. We will describe the affect from aging on the counter and fiber response as well as several measurements aimed at improving the light yield, including the investigation of different reflectors at the far end of counters with single-ended readout. Speakers: Mr Pedrom Zadeh (University of Virginia), Peter Farris (University of Virginia) • 179 R&D Toward Ton-Scale HPGXe Neutrinoless Double Beta Decay Experiments The NEXT collaboration is developing a sequence of high pressure xenon gas time projection chambers with the aim of creating a ton-scale, very low background neutrinoless double beta decay search. While most aspects of this technology are easily scalable, some detector elements require R&D in order to be realized on a large scale. This poster will describe a new, large-scale test facility under development at the University of Texas at Arlington, which will be used to test electroluminescent gain regions, high voltage feed-throughs and field cage elements for 100kg- and ton-scale xenon gas experiments. Speaker: Leslie Rogers (University of Texas in Arlington) • 180 Site characterization for ground-based CMB observations with a 183GHz radiometer The cosmic microwave background (CMB) is a rich source of information about the cosmos. Over the past ten years, gains in experimental sensitivity have enabled ground-based instruments to begin the search for B-mode polarization in the CMB as a test of the inflationary paradigm. However, the atmosphere is not fully transparent in the 35-270GHz region targeted by these observations. Poorly-mixed and rapidly-varying water vapor in the atmosphere presents a challenging source of sky noise for CMB telescopes. Ground-based experiments minimize atmospheric perturbations by selecting dry, high-altitude sites where the amount of precipitable water vapor (PWV) in the atmosphere is as low and as stable as possible. The leading sites in use for present experiments are the South Pole and Chajnantor Plateau, Chile. The next-generation CMB-S4 experiment will make use of these two locations but is also turning an eye to potential sites in the northern hemisphere with the goal of increasing the observed sky fraction. To better understand the effects of PWV on current and future CMB experiments, we have undertaken the first coordinated measurement of atmospheric water vapor fluctuations with high time resolution over long time scales at sites around the world. We use the Dicke-switched 183GHz water vapor radiometer (WVR) initially commissioned for the Atacama Large Millimeter/submillimeter Array (ALMA) and built by Omnisys Instruments AB, with the addition of custom azimuth/elevation scanning optics and a temperature-controlled environmental enclosure. Two identical units are currently deployed at the South Pole and Summit Station, Greenland. We report here on the performance and measurements from these WVRs, and we discuss how these atmospheric measurements might drive site selection and design choices for future telescopes. Speaker: Nicole Larsen (U. Chicago, KICP) • Tuesday, August 1 • Plenary: Tuesday morning Ramsey Auditorium ### Ramsey Auditorium #### Fermi National Accelerator Laboratory Kirk Road & Pine Street Batavia, IL 60510-5011 Convener: Mr Myron Campbell (University of Michigan) • 181 CERN program and plans for the European Strategy Speaker: Prof. Eckhard Elsen (CERN) • 182 Next European strategy process Speaker: Prof. Sijbrand de Jong (Roadbed University Nijmegen and Nikhef) • 183 Asia particle physics program Speaker: Sachio Komamiya (The University of Tokyo) • 184 US Particle Physics Program Speaker: Prof. JoAnne Hewett (SLAC) • 10:15 AM Break • Beyond Standard Model: Tuesday morning 1 West ### 1 West #### Fermi National Accelerator Laboratory Convener: Prof. Howard Baer (University of Oklahoma) • 185 Spectroscopy of lattice SU4 gauge theory with fermions in multiple representations We study the spectroscopy of an SU(4) gauge theory with dynamical fermions in both the fundamental and the two-index antisymmetric representations. Such theories are of interest in the study of Physics Beyond the Standard Model, specifically in the context of partial compositeness. We discuss the spectrum of this theory and its implications. Speaker: Dr Venkitesh Ayyar (University of Colorado, Boulder) • 186 Thermodynamics of SU(4) gauge theory with fermions in multiple representations We study the phase structure of SU(4) gauge theory with dynamical quarks in both the fundamental and two-index antisymmetric representations. Such "multi-representation" theories have been speculated to exhibit separated phase transitions, but our lattice calculations suggest the existence of only a single thermal phase transition: both species of fermion appear to confine and break chiral symmetry simultaneously. We investigate the order of the combined phase transition in various limits of the theory, and compare to theoretical expectations based on chiral symmetry. Speaker: Daniel Hackett (University of Colorado, Boulder) • 187 Search for Vector-like Top Quarks in di-Leptons We present a search for the pair-production of a vector-like top quark partner T of charge + 2/3, using proton-proton collision data at √s=13 TeV collected by the CMS Experiment in 2016 at the CERN LHC. Our search targets T quarks decays to final states with two light charged leptons, b-jets, and multiple light flavored jets. Both same-sign and opposite sign di-lepton channels are considered. Speaker: Dr Anthony Barker (Purdue University) • 188 Search for vector-like quarks with oppositely-charged dilepton pairs, jets, and missing transverse energy in proton-proton collisions at centre-of-mass energy of 13 TeV We Present results of the search for pair produced Vector-like T quark using the proton-proton Collison data collected by the CMS experiment in 2016 with integrated luminosity of 35.9 /fb at a centre-of-mass energy of 13 TeV . Vector-like quarks appear in several extensions of the standard model, and can cancel the diverging loop corrections to the Higgs mass, and thus stabilize it at the electroweak scale.The T quark can decay in to either of three states, bW, tZ of tH. The pair produced T final state consists of two oppositely charged electrons or muons consistent with decay products from Z boson, jets and MET. We set limits on mass of the T quark for various branching ratios. Speaker: Mr Rachitha Mendis (Kansas State University) • 189 Inclusive search for vector-like T quark pairs in leptonic final states in proton-proton collisions at √s = 13 TeV A search is presented for pair production of heavy vector-like T quarks using proton- proton collisions were collected by the CMS experiment at the CERN LHC in 2016 with an integrated luminosity of 35.9 fb−1. A vector-like T quark of charge 2e/3 is predicted to decay to bW, tZ, and tH, so pair production of T quarks yields a wide array of final states. This inclusive search is performed in three channels: a single lepton channel that identifies boosted hadronic W and Higgs boson decays, same-sign dilepton channel and a trilepton channel that is enriched in Z boson decays. Production of vector-like B quarks that decay to tW, bZ, and bH are also considered. Results remain blinded at this time, but if no excess of data is observed this search will exclude T quark masses in the range of 1090 – 1210 GeV for many branching ratio combinations. Speaker: Mr Rizki Syarif (Brown University) • 190 Search for vector-like B quarks with oppositely-charged dilepton pairs in proton-proton collisions at 13 TeV We present the results of searches for pair-produced vector-like B quarks using proton-proton collision data collected with the CMS detector at the CERN LHC at a center-of-mass energy of 13 TeV. The searches are performed using opposite sign dileptons from a Z boson decay. Vector-like quarks, having symmetric interactions in the weak sector of the Standard Model (SM), are postulated as an alternate mechanism to solve the Hierarchy problem of the SM, compared to SUSY models. The search focuses on a vector-like quark doublet, meaning the vector-like B quark can decay to two potential channels: bZ or bH. Using a chi-squared minimization technique, we are able to reconstruct the potential vector-like B invariant mass. This mass is used to distinguish signal from background. This search allows us to probe for B quark masses up to 1.1 GeV assuming a 100% branching ratio of the B quark decay. Speaker: Tyler Mitchell (Kansas State University) • Cosmology and Astrophysics: Tuesday morning Comitium ### Comitium #### Fermi National Accelerator Laboratory Convener: Prof. Neelima Sehgal (Stony Brook University) • 191 Galaxy Cluster Science Results with the Dark Energy Survey Constraining LambdaCDM cosmology with galaxy cluster abundance is one of the fundamental goals for the Dark energy survey (DES). Based on observations collected in the first year, DES has identified many thousands of clusters out to redshift 1.0. Weak lensing and multi-wavelength studies with X-ray data and cosmic microwave background are performed to provide inputs to the cosmology constraint analysis. Astrophysical studies to understand cluster evolution over time is yielding fruitful results. This presentation will present DES science results from galaxy cluster cosmology and astrophysics studies. Speaker: Dr Yuanyuan Zhang (Fermilab) • 192 Cluster Cosmology with the South Pole Telescope The South Pole Telescope (SPT) is a 10-meter millimeter-wavelength telescope optimized for high resolution observations of the Cosmic Microwave Background (CMB). The SPT has been used to conduct several wide-area surveys: the 2500-square-degree SPT-SZ survey (completed in 2011) as well as two recently completed surveys conducted using the SPTpol receiver: the 500-square-degree SPTpol Survey and the SPTpol Extended Cluster Survey (the former surveyed ~20% of the SPT-SZ footprint to a level 3x deeper than the SPT-SZ survey, the latter covered an additional 2500-square-degrees to somewhat shallower depths than SPT-SZ). One of the primary objectives of the wide-area SPT surveys was the construction of a mass-limited sample of galaxy clusters identified via the thermal Sunyaev- Zel’dovich (SZ) effect, through which massive clusters imprint subtle temperature distortions on the CMB sky. The abundance of such clusters is a powerful cosmological probe as it depends sensitively upon both the expansion history of the universe and the growth of density fluctuations. In this talk I will discuss progress analyzing these three datasets including updated cosmological constraints from the initial SPT-SZ cluster sample using new weak lensing data as well as ongoing work characterizing the strong lensing properties of these systems using the new PISCO imager on Magellan. The results presented in this talk will be significantly improved with data from the SPT-3G survey---deployed in Jan 2017---that will identify an order of magnitude more clusters than past generation SZ surveys. Speaker: Dr Lindsey Bleem (Argonne National Laboratory) • 193 Fundamental Physics from SZ Cluster Surveys with CMB and Optical Lensing Mass Calibration Future high resolution CMB experiments will detect tens of thousands of galaxy clusters. The abundance of clusters as a function of mass and redshift allows us to map the growth of structure and consequently measure the sum of neutrino masses and constrain the nature of dark energy. Such measurements are currently limited by our ability to calibrate the masses of galaxy clusters. Planned CMB experiments will be sensitive enough to offer competent mass calibration from CMB lensing that is complementary to optical weak lensing of galaxies. I will review and compare the prospects of CMB and optical mass calibration, discussing this in the context of methods applied to ongoing CMB experiments like Advanced ACT, and focusing on systematics such as contamination from astrophysical foregrounds. Speaker: Dr Mathew Madhavacheril (Princeton University) • 194 Measuring the pairwise kinematic Sunyaev-Zel'dovich effect with the Atacama Cosmology Telescope We have made improved measurements of the kinematic Sunyaev-Zel’dovich (kSZ) effect using data from the Atacama Cosmology Telescope (ACT) and the Baryon Oscillation Spectroscopic Survey (BOSS). A map of the Cosmic Microwave Background (CMB) composed from two seasons of observations each by ACT and the Atacama Cosmology Telescope Polarimeter (ACTPol) receiver was used. The mean pairwise baryon momentum associated with the positions of 50,000 bright galaxies in the BOSS DR11 Large Scale Structure catalog was evaluated over the 600 square degrees of overlapping sky area. The kSZ signal arising from the large-scale motions of clusters was measured by fitting data to an analytical model, with the free parameter of the fit determining the optical depth to microwave photon scattering for the cluster sample. Our most conservative simulation-based uncertainty estimates for the mean pairwise momenta as a function of galaxy separation gave signal-to-noise values between 3.6 and 4.1 for various luminosity cuts. A novel approach to estimating cluster optical depths from the average thermal Sunyaev-Zel’dovich (tSZ) signal at the cluster positions was explored, and our results are broadly consistent with those obtained from the kSZ signal. In the future, the tSZ signal may provide a valuable source of cluster optical depths, enabling the extraction of velocities from the kSZ sourced mean pairwise momenta. The mean pairwise velocity of clusters is sensitive to the growth of structure and the Universe’s expansion history, making it an excellent probe for gravity on large scales and a means for neutrino mass sum constraints. New CMB maps from multi-frequency ACTPol observations promise to improve statistics and systematics for SZ measurements. With these and other upcoming data, such as measurements from DESI, CCAT-prime, and Simons Observatory, the pairwise kSZ signal is poised to become a powerful new cosmological tool, able to test models of modified gravity and dark energy and constrain neutrino physics. Speaker: Ms Eve Vavagiakis (Cornell University) • 195 Delensing CMB B-modes: results from SPT. A promising signature of cosmic inflation is the presence of a "B-mode" component in the polarization of the Cosmic Microwave Background (CMB) induced by primordial gravitational waves. For many inflation models, this B-mode signal is predicted to be at a level detectable in the near future. However, current searches are limited by a "lensing B-mode" component that is produced by gravitationally lensed primordial E modes. In order to potentially detect the inflationary signal from B-mode measurements, lensing B modes must be characterized and removed in a process referred to as "delensing." This process has been studied extensively theoretically and with simulations, but has not been performed on polarization data. In this talk, we present the results of CMB B-mode delensing using polarization data from the South Pole Telescope polarimeter, SPTpol. Furthermore, using realistic simulations that include filtering and realistic CMB noise, we will show what is currently limiting the delensing efficiency and how it will rapidly improve in the near future. Speaker: Dr Kimmy Wu (UC Berkeley) • Dark Matter: Tuesday morning Hornets Nest ### Hornets Nest #### Fermi National Accelerator Laboratory Convener: Prof. Rafael Lang (Purdue University) • 196 Flavored Dark Matter and a Secret Asymmetry I will present a mechanism where the dark matter abundance arises from asymmetries generated in the early universe, even though the distribution of dark matter may appear symmetric today. This mechanism can be realized in the framework of of flavored dark matter, among others. I will discuss the experimental signatures of this setup, as well as generic phenomenological features of the flavored dark matter scenario that set it apart from single-flavor dark matter. Speaker: Prof. Can Kilic (University of Texas at Austin) • 197 Sommerfeld-Enhanced J-Factors For Dwarf Spheroidal Galaxies For models in which dark matter annihilation is Sommerfeld-enhanced, the annihilation cross section increases at low relative velocities. Dwarf spheroidal galaxies (dSphs) have low characteristic dark matter particle velocities and are thus ideal candidates to study such models. In this paper we model the dark matter phase space of dSphs as isotropic and spherically-symmetric, and determine the J-factors for several of the most important targets for indirect dark matter searches. For Navarro-Frenk-White density profiles, we quantify the scatter in the J-factor arising from the astrophysical uncertainty in the dark matter potential. We show that, in Sommerfeld-enhanced models, the ordering of the most promising dSphs may be different relative to the standard case of velocity-independent cross sections. This result can have important implications for derived upper limits on the annihilation cross section, or on possible signals, from dSphs. Speaker: Jason Kumar (University of Hawaii) • 198 Searches for dark matter with the Super-Kamiokande detector Indirect searches for dark matter using data collected with the Super-Kamiokande detector in years 1996-2016 were performed. The excess of neutrinos from possible dark matter sources such as Sun, Earth and Galactic Center, compared to the expected atmospheric neutrino background was searched. Event samples including both electron and muon neutrinos covering a wide range of energies were used, with sensitivity to dark matter masses down to tens of GeV. Allowed number of dark matter induced neutrinos which can be contained in SK data so far was estimated. Obtained limits on DM induced neutrino flux were related to limit on spin-dependent (for the Sun) and spin-independent (for the Sun and the Earth's core) WIMP-nucleon cross section. In case of Galactic Center analysis, the upper limit on the self-annihilation cross-section was derived. Speaker: Ms Katarzyna Frankiewicz (National Centre for Nuclear Research) • 199 Dark Matter Searches with HAWC The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is a wide field-of-view observatory sensitive to 0.5 TeV - 100 TeV gamma-rays and cosmic-rays. The HAWC observatory performed an indirect search for dark matter via GeV-TeV photons resulting from dark matter annihilation and decay considering various sources, including dwarf spheroidal galaxies (dSphs), the M31 galaxy, and the Virgo cluster. HAWC has not seen statistically significant excess from these sources. We searched for dark matter annihilation and decay at dark matter masses above 1 TeV, including masses higher than 70 TeV that are currently unconstrained. We will present the annihilation cross-section and decay lifetime limits. Speaker: Dr J. Patrick Harding (Los Alamos National Laboratory) • 200 Supersymmetric Resonant Dark Matter: an Explanation to AMS-02 Positron Excess We construct a thermal dark matter model with the dark matter annihilations mediated by a resonance to explain the positron excess observed by PAMELA, Fermi-LAT and AMS-02 and to satisfy other experimental constraints. Based on a spontaneous breaking global symmetry of SU(3)/SU(2)xU(1), we provide a natural explanation for why the resonance mass is very close to twice of the dark matter mass. The pseudo Nambu Goldstone Bosons in the coset space, with a mass below one GeV, mainly decay into two muons and provide a good fit to the positron excess spectrum. I will also discuss other dark matter phenomenology of our model. Speaker: Joshua Berger (University of Wisconsin-Madison) • 201 Explaining Diverse Rotation Curves of Spiral Galaxies with Self-Interacting Dark Matter Self-interacting dark matter (SIDM) is a simple and well motivated scenario that demonstrates great potential to solve small scale issues. One recent example is the diversity problem due to the failure of the lambda cold dark matter (LambdaCDM) paradigm to explain the diverse behavior in observed rotation curves, especially for dwarf galaxies. To address this issue in SIDM paradigm, we follow our previous work and fit 120 galaxy velocity rotation curves from SPARC dataset using SIDM model with a fixed value of self-interaction cross section and only assuming the halo concentration-mass relation predicted by the LambdaCDM model. Our result shows SIDM dramatically improves the ability to fit the rotation curve comparing to CDM. Discrepancy in halo masses corresponding to the same disk mass between result from fitting and expectation from abundance matching may indicate the "too-big-to-fail" problem still exist with current SIDM. Radial acceleration relation and baryonic Tully-Fisher relation are closely reproduced though with a bit large reasonable scatter. In addition, SIDM direct detection will be briefly discussed. Speaker: Tao Ren (UC Riverside) • Neutrino Physics: Tuesday morning Ramsey Auditorium ### Ramsey Auditorium #### Fermi National Accelerator Laboratory Kirk Road & Pine Street Batavia, IL 60510-5011 Convener: Prof. Sowjanya Gollapinni (University of Tennessee, Knoxville) • 202 Current Analysis Status for the Inclusive Neutral Current π0 Production Cross section Measurement with the NOvA Near Detector NOvA (NuMI Off-axis νe Appearance) experiment is designed to study long-baseline neutrino oscillations using two detectors, the Near Detector (ND) at Fermilab and the Far Detector (FD) at a distance 810 km in Northern Minnesota. NOvA looks for the νe appearance at the FD using a narrow band νμ beam peaked at 2 GeV in energy. Neutral Current (NC) interactions with a π0 in the final state represents the main background in the νe appearance measurement. The π0 decay into two photons can fake the νe appearance signal either due to merging of two photon showers or one of the two photons escaping the detection. Therefore, a complete understanding of νμ induced NC interactions with π0 in the final state is very important. It will also help in reducing the background uncertainties for current and future long-baseline neutrino oscillation experiments. We will present the current status of the analysis related to the inclusive NC π0 production cross section measurement with the NOvA ND. Speaker: Ms Daisy Kalra (Student) • 203 Measurement of Neutral Current Coherent Pi0 Production In The NOvA Near Detector The NOvA experiment is a long-baseline neutrino oscillation experiment designed to measure electron neutrino appearance in a muon neutrino beam. It consists of two finely segmented, liquid scintillator detectors at 14 mrad off-axis in the NuMI beam.The NOvA Near Detector, located at Fermilab, provides an excellent opportunity to study neutrino-nucleus interactions which are important for the neutrino oscillation measurements. This talk will present one of the first such measurements from the NOvA Near Detector: neutral current coherent-Pi0 production. Neutrinos can coherently interact with the target nucleus via neutral current exchange and produce a single, forward Pi0, which is a background to the NuE appearance measurement. This analysis measures the coherent-Pi0 kinematics and cross-section and compares it to the model predictions. A data-driven method is developed to constrain the neutral current resonance and deep-inelastic pi0 productions which are background to this analysis. Speaker: Hongyue Duyang (university of south carolina) • 204 Measurement of Reconstructed Charged Particle Multiplicities of Neutrino Interactions in MicroBooNE MicroBooNE is a liquid argon Time Projection Chamber experiment situated on the Booster Neutrino Beam at Fermilab that is designed to probe neutrino interactions, investigate non-standard neutrino oscillations, and further develop the LArTPC detector technology. In this talk, we compare the observed charged particle multiplicity distribution, which is produced via neutrino charged current interactions in the visible phase-space to predictions of this distribution from current generator models. The data used in this analysis were collected in 2015-2016 by MicroBooNE detector. The analysis employs a fully automatic event selection and charged particle track reconstruction and uses a novel data-driven technique to separate neutrino interactions from cosmic-induced backgrounds. Speaker: Ms Aleena Rafique (Kansas State University) • 205 Neutrino-Nucleus Deep Inelastic Scattering (DIS) results from MINERvA Neutrino-Nucleus Deep Inelastic Scattering (DIS) events provide a probe into the structure of nucleons within a nucleus that cannot be accessed via charged lepton-nucleus interactions. The MINERvA experiment is stationed in the Neutrinos from the Main Injector (NuMI) beam line at Fermi National Accelerator Laboratory. With the recent increase in average neutrino energy and the greatly increased intensity of the NuMI beam line, projected sensitivities for DIS cross section ratio analyses using MINERvA's suite of nuclear targets (C, CH, Fe and Pb) will be greatly increased. The current state of the field and the projected reach and impacts of these measurements will be discussed. Speaker: Mr Dipak Rimal (University of Florida) • 206 Antineutrino to neutrino charged-current interaction cross section ratio in MINERvA The neutrino and anti-neutrino charged-current inclusive cross sections are important ingredients for current and future neutrino oscillation experiments. MINERvA recently measured these cross sections on carbon, and their ratio, using data from the forward and reversed horn focusing modes of the Fermilab low-energy NuMI beamline. The flux prediction was obtained from a sample of charged-current events at low nuclear recoil energy ($\nu$) along with precise higher energy external neutrino cross section data overlapping our energy regime. Common systematic uncertainties cancel in the extracted antineutrino-neutrino cross section ratio and reaches a precision of 5$\%$at low energy since we benefit from the fact that the cross-sections are obtained within the same experiment using the same technique. This talk will discuss these results. Speaker: Dr Lu Ren (University of pittsburgh) • Particle Detectors: Tuesday morning IARC Building ### IARC Building #### Fermi National Accelerator Laboratory Convener: corrinne mills (University of Illinois at Chicago) • 207 The LUCID-2 detector The LUCID-2 detector is the main online and offline luminosity provider of the ATLAS experiment. It provides over 100 different luminosity measurements from different algorithms for each of the 2808 LHC bunches. LUCID was entirely redesigned in preparation for LHC Run 2: both the detector and the electronics were upgraded in order to cope with the challenging conditions expected at the LHC center of mass energy of 13 TeV with only 25 ns bunch-spacing. While LUCID-1 used gas as a Cherenkov medium, the LUCID-2 detector is in a new unique way using the quartz windows of small photomultipliers as the Cherenkov medium. The main challenge for a luminometer is to keep the efficiency constant during years of data-taking. LUCID-2 is using an innovative calibration system based on radioactive 207 Bi sources deposited on the quartz window of the readout photomultipliers. This makes it possible to accurately monitor and control the gain of the photomultipliers so that the detector efficiency can be kept stable at a percent level. A description of the detector and its readout electronics will be given, as well as preliminary results on the ATLAS luminosity measurement and related systematic uncertainties. Speaker: Prof. Pinfold James (University of ALberta) • 208 Performance of the ATLAS Tile Calorimeter in Run 2 and Electronics Upgrade for High Luminosity LHC The Tile Calorimeter (TileCal) is the hadronic calorimeter covering the central region of the ATLAS experiment at the Large Hadron Collider (LHC). This talk is divided into two parts. The first part will present studies of the TileCal energy scale using in-situ E/p measurements conducted during Run 2 of the LHC. The second part will discuss the plans and current results of the program to upgrade the TileCal front-end electronics for the High Luminosity LHC (HL-LHC) Phase-II upgrade, scheduled for the mid-2020s. Specifically, the performance of prototype electronics currently being tested in an extensive program of test beam studies will be presented. Speaker: Mr Joakim Olsson (University of Chicago) • 209 Commissioning and operation of the new CMS Phase 1 pixel detector The Phase I upgrade of the CMS pixel detector is built out of four barrel layers (BPIX) and three forward disks in each endcap (FPIX). It comprises a total of 124M pixel channels, in 1,856 modules and it is designed to withstand instantaneous luminosities of up to 2 x 10^34 cm-2 s-1. Different parts of the detector have been assembled over the last year and later brought to CERN for installation inside the CMS tracker. At various stages during the assembly tests have been performed to ensure that the readout and power electronics, and the cooling system meet the design specifications. After tests of the individual components, system tests have been performed before the installation inside CMS. In addition to reviewing these tests, we also present results from the final commissioning of the detector in-situ using the central CMS DAQ system. Finally we review results from the initial operation of the detector first with cosmic rays and then with pp collisions. Speaker: Weinan Si (UC Riverside) • 210 Construction of the Phase 1 upgrade of the CMS pixel detector The innermost layers of the CMS tracker are built out of pixel detectors arranged in three barrel layers (BPIX) and two forward disks in each endcap (FPIX). The original CMS detector was designed for the nominal instantaneous LHC luminosity of 1 x 10^34 cm^-2 s^-1. Under the conditions expected in the coming years, which will see an increase of a factor two of the instantaneous luminosity, the CMS pixel detector will see a dynamic inefficiency caused by data losses due to buffer overflows. For this reason the CMS Collaboration has installed during the recent extended end of year shutdown a replacement pixel detector. The Phase I upgrade of the CMS pixel detector will operate at full efficiency at an instantaneous luminosity of 2 x 10^34 cm^-2 s^-1 with increased detector acceptance and additional redundancy for the tracking, while at the same time reducing the material budget. These goals are achieved using a new readout chip and modified powering and readout schemes, one additional tracking layer both in the barrel and in the disks, and new detector supports including a CO2 based evaporative cooling system, that contribute to the reduction of the material in the tracking volume. This contribution will review the design and technological choices of the Phase I detector, with a focus on the challenges and difficulties encountered, as well as the lessons learned for future upgrades. Speaker: Maral Alyari (Fermilab) • 211 The LHCb Upgrades During the LHC Run-1 the LHCb experiment has successfully performed a large number of world’s class precision measurements in heavy flavour physics, and is now further increasing the datasets in Run-2. However, most of the LHCb measurements will remain limited by statistics. LHCb will therefore undergo a major upgrade in the Long Shutdown 2 (LS2) of LHC aimed at collecting an order of magnitude more data during Run-3 and Run-4. The upgrade consists of a new full readout at the LHC bunch crossing rate (40 MHz) with the ultimate flexibility of a pure software trigger. In order to increase the instantaneous luminosity up to 2x10ˆ33 cm-2s-1, several sub-detector upgrades are also underway, in order to cope with the expected higher occupancies and radiation dose. The architecture of the upgraded detector will be presented along with physics goals. Furthermore, the LHCb collaboration is planning a further upgrade to be installed during LS4 that aims at raising the instantaneous luminosity by another factor 10, in order to collect order of 300 fb-1 by the end of the Run-5. Conceptual design and physics reach will be also discussed. Speaker: Matthew Rudolph (Syracuse University) • Precision Electroweak Physics: Tuesday morning Sunrise ### Sunrise #### Fermi National Accelerator Laboratory Convener: Prof. Richard Hill (Perimeter Institute) • 212 Monte Carlo Simulations of the PEN experiment: A Precision Measurement of$\pi\rightarrow$e$\nu(\gamma)$Branching Ratio The PEN collaboration performed a precision measurement of the$\pi^+\rightarrow e^+\nu_e(\gamma)$branching ratio with the goal of obtaining a relative uncertainty of$5\times10^{-4}$or better at the Paul Scherrer Institute. A precision measurement of the branching ratio$\Gamma(\pi\rightarrow e\bar{\nu}(\gamma))/\Gamma(\pi\rightarrow \mu \bar{\nu}(\gamma))$can be used to give mass bounds on new'', or non V$-$A, particles and interactions. This ratio also proves to be one of the most sensitive tests for lepton universality. The PEN detector consists of beam counters, an active target, a mini-time projection chamber, cylindrical multi-wire proportional chambers, a plastic scintillating hodoscope, and a spherical 240-module pure CsI electromagnetic calorimeter. The Geant4 Monte Carlo simulation is used to construct ultra-realistic events by digitizing energies and times, creating synthetic target waveforms, and fully accounting for photo-electron statistics. We focus on the detailed detector response to signal and background processes in order to sharpen the discrimination between them in the data analysis. Speaker: Mr Charles Glaser (University of Virginia) • 213 Measurement of same-sign WW diboson production with the ATLAS experiment We present a study of same-sign W±W± boson pairs produced in association with two or more jets in pp collisions at √s = 13 TeV. Same-sign W±W± production is sensitive to the mechanism of electroweak symmetry breaking and physics beyond the standard model, particularly through vector boson scattering (VBS) production. Unlike opposite-sign WW production, in same-sign W±W± production the electroweak mediated diagrams are comparable in size to the QCD mediated diagrams, making it well suited for VBS studies. An inclusive cross section measurement of both the electroweak and QCD same sign W±W± processes is performed using leptonically decaying W± bosons with electrons and/or muons in the final state. The first evidence of of same sign W±W± production was seen by the ATLAS collaboration in 20.3 fb^-1 of 8 TeV data, seeing an excess in data of 3.6σ over backgrounds. We expect greater sensitivity with the 36 fb^-1 of 13 TeV data collected by ATLAS in 2015 and 2016. Speaker: Will DiClemente (University of Pennsylvania) • 214 Single W/Z boson production cross sections with the CMS detector Measurements of single W and Z boson inclusive and differential production cross sections with the CMS detector are presented. Measurements of Drell-Yan cross sections in the mass range of 15 to 3000 GeV are also reported. The results are compared to predictions from different Monte Carlo generators. Speaker: Jay Lawhorn (Caltech) • QCD: Tuesday morning Racetrack ### Racetrack #### Fermi National Accelerator Laboratory Convener: Radja Boughezal (Argonne National Laboratory) • 215 The proton radius puzzle In 2010 the proton charge radius was extracted for the first time from muonic hydrogen, a bound state of a muon and a proton. The value obtained was five standard deviations away from the regular hydrogen extraction. Taken at face value, this might be an indication of a new force in nature coupling to muons, but not to electrons. It also forces to reexamine our understanding of the structure of the proton. In this talk I will describe an ongoing theoretical research effort that seeks to address and resolve this "proton radius puzzle". In particular, I will present a reevaluation of the proton structure effects, correcting 40 years of such calculations, and the development of new effective field theoretical tools that would allow to directly connect muonic hydrogen and muon-proton scattering. Speaker: Prof. Gil Paz (Wayne State University) • 216 On HQET and NRQCD Operators of Mass Dimension 8 and Above Effective field theories such as Heavy Quark Effective Theory (HQET) and Non Relativistic Quantum Chromo-(Electro-) dynamics NRQCD (NRQED) are indispensable tools for controlling the effects of the strong interaction. The increasing experimental precision requires the knowledge of higher dimensional operators. These operators are important to the evaluation of decay rates of the B-meson. We present a general method that allows for an easy construction of HQET (NRQED and NRQCD) operators that contain two heavy quark (non-relativistic) fields and any number of covariant derivatives. As an application of our method, we give for the first time all such terms in the 1/M^4 NRQCD Lagrangian, where M is the mass of the spin-half field. We analyze the general dimension-nine spin-independent HQET matrix element, which was not considered so far in the literature, and calculate moments of the leading power shape function up to and including dimension nine HQET operators. Speaker: Mr AYESH GUNAWARDANA (Wayne State University) • 217 Alternative Formulation of the z-Expansion in Semileptonic Decays We propose an alternative method to perform the z expansion in the B→π l ν decay by using a rational expression that automatically satisfies the constraint imposed by the conservation of angular momentum. This avoids having to impose a constraint on the truncated series. The accuracy of the formulation was checked by fitting the lattice data in conjunction with the experimental data from Belle and BaBar. We discuss the accuracy of extrapolations based on fits of subregions of the kinematic range. Speaker: Mr Erik Gustafson (University of Iowa) • 218 Recent measurements of exclusive hadronic cross sections at BABAR and the implication for the muon g-2 calculation The BABAR Collaboration has an intensive program studying hadronic cross sections in low-energy$e^+e^-$annihilations, which are accessible with data taken near the Upsilon(4S) via initial-state radiation. Our measurements allow significant improvements in the precision of the predicted value of the muon anomalous magnetic moment. These improvements are necessary for shedding light on the current ~3 sigma difference between the predicted and the experimental values. We have previously published results on a number of processes with two to six hadrons in the final state. We report here on several recent measurements of hadronic cross sections in$e^+e^-$annihilations. Speaker: Dr David Brown (University of Louisville) • 219 Regge Trajectories of triply heavy baryons$\Omega_{ccc}$,$\Omega_{bbb}$,$\Omega_{ccb}$and$\Omega_{bbc}$baryons are considerable theoretical interest in a baryonic analogue of heavy quarkonium because of the color-singlet bound state of three heavy quark (c,b) combination inside ({\it free from light quarks}) \cite{olive}. Regge trajectories are concerned with the mass spectrum of the particles so that the present study exhibits the regge trajectories obtained from excited states of four experimentally unknown triply heavy$\Omega$baryons. The trajectories are plotted in (n,$M^{2}$) and (J,$M^{2}$) planes which is helpful to determine the unknown quantum number and$J^P$values. The calculations have computed in Hypercentral Constituent Quark Model with hyper coulomb plus linear potential \cite{EPJC}. Many author have also study the mass spectra by different approaches\cite{brown, PAD2014, vijande2015, kwei2}. However, LHCb experiment possibly detect$\Omega_{bbb}$,$\Omega_{bbc}$and$\Omega_{bbc}^{*}$baryons at appropriate integrated luminosity and collision energy \cite{lhcb}. \begin{thebibliography}{90} \bibitem{olive}{C. Patrignani et. al., Chin. Phys. C \textbf{40}, 100001 (2016)}. \bibitem{kwei2}K-W Wei, B. Chen and X-H Guo, Phys. Rev. D \textbf{92}, 076008 (2015). \bibitem{EPJC}Z. Shah, K. Thakkar and A. K. Rai, Eur. Phys. J. C {\bf76}, 530 (2016); Eur. Phys. J. C {\bf77}, 129 (2017);Chin. Phys. C \textbf{40}, 123102 (2016). \bibitem{brown}Z. S. Brown, W. Detmold, S. Meinel, and K. Orginos, Phys. Rev. D \textbf{90}, 094507 (2014) \bibitem{PAD2014} M. Padmanath, R. G. Edwards, N. Mathur, and M. Peardon, Phys. Rev. D \textbf{90}, 074504 (2014) \bibitem{vijande2015} J. Vijande, A. Valcarce and H. Garcilazo, Phys. Rev. D \textbf{91}, 054011 (2015). \bibitem{lhcb}S.-Z. Wu, Y.-W. Li and R. Rashidin, Phys. Rev. D {\bf 86}, 114504 (2012) \end{thebibliography} Speakers: Dr Ajaykumar Rai (Assistant Professor), Mrs Zalak Shah (PhD student) • Quark and Lepton Flavor: Tuesday morning Curia II ### Curia II #### Fermi National Accelerator Laboratory Convener: Prof. Alexey Petrov (Wayne State University / MCTP) • 220 Exotic multiquark states in pp̄ collisions at D0 We use the full Run II dataset consisting of 10.4 fb −1 of pp̄ collisions recorded by the D0 detector at the Fermilab Tevatron collider at sqrt s = 1.96 TeV to search for new exotic multiquark states. We report the evidence of a new state X(5568) decaying to Bsπ seen in the Bs → J/ψφ decay channel and its independent confirmation in the semi-leptonic channel Bs → μ± Ds∓ X. We also report on the search for other exotic states. Speaker: Peter Garbincius (Fermilab) • 221 Heavy hadron spectroscopy at LHCb We report on the first observation of excited hadronic states in both the charm and beauty sector with special emphasis on the observation of five excited Omega_c states. Similar techniques are used to search the LHCb data for states observed in other datasets, such as the tetraquark state X(5568) whose evidence was reported by D0. Speaker: Dr Ivan Polyakov (CERN) • 222 Pentaquark & tetraquark states at LHCb The observation of two pentaquark resonances and the proof of the resonant nature of the Zc state opened to the search for the many isospin partner of these multi-quark states. We review the studies of these states and discuss the prospects for the analyses of the LHCb Run2 data. Speaker: Dr Liming Zhang (Tsinghua University) • 223 Beauty-full Tetraquarks Non-relativistic two-body heavy quark system has been proved to be very useful to understand the QCD dynamics. Extending it to many-body heavy quark system may not just provide a new and interesting tetraquark state, but also helps us to understand QCD more. In this talk, I will discuss a way to calculate the ground-state energy of a tetraquark of four beauty quarks, which can behave as a Y(1S)Y*(1S) resonance. Speaker: Dr Yang Bai (University of Wisconsin-Madison) • 224 Thomas-Fermi quark model for mesons The first results of a new application of the Thomas-Fermi statistical quark model to mesonic states will be presented. Interesting aspects of the theory will be discussed, distinguishing such states from baryonic matter. A major motivation of this study is the tetraquark states discovered at the LHC and the possibility that stable multi-quark families of such states exist. Similar to the previous baryonic study, we use a two-inequivalent wavefunction approach to investigate aspects of many-meson matter. We think of our model as a tool for quickly assessing the characteristics of new, possibly bound, particle states of higher quark number content, which cannot yet be examined by lattice methods. Speaker: Suman Baral (Baylor University) • Top Quark Physics: Tuesday morning 1 East ### 1 East #### Fermi National Accelerator Laboratory Convener: Reinhard Schwienhorst (Michigan State University) • 225 Direct measurement of the top quark mass in$p\bar p$collisions at D0 We report the most recent measurements of the mass of the the top quark, performed by the D0 experiment at the Fermilab Tevatron collider using the full Run II (2001--2011) data set corresponding to an integrated luminosity of$9.7\ $fb$^{-1}$. This includes measurements in the dilepton channels using the matrix element and neutrino weighting approaches, as well as measurements in the lepton+jets channel using the matrix element method. We also discuss the final D0 combination and the preliminary D0+CDF combination of the top quark mass using Run I (1992--1996) and Run II measurements. Speaker: Gregorio Bernardi (LPNHE Paris) • 226 Measurement of the pole mass of the top quark using pp̄ → tt̄ production cross sections at D0 We present an alternative approach to the direct measurements of the top quark mass using D0 data. We discuss extractions of the pole mass of the top quark based on measurements of the inclusive and unfolded differential pp̄ → tt̄ production cross section as a function of p T (t) and tt̄ mass.. We use the full Run II data set of pp̄ collisions collected by the D0 experiment, corresponding to an integrated luminosity of 9.7 fb −1 . Speaker: Andreas Jung (Fermilab) • 227 P5' anomaly for top: tZ' associated production at LHC The LHCb experiment uncovered the P5' anomaly, a deviation in data from Standard Model expectations in the said B -> K*mumu angular observable. This has motivated a possible Z' boson that couples to left-handed b to s transitions, where a model would be the gauged L_mu - L_tau symmetry, but direct search for such a Z' is not promising. Less constrained is a similar Z', but coupling to right-handed t to c transitions. Motivated by this, we study cg -> tZ' associated production at LHC, both for a generic model, and in the L_mu - L_tau with a vector-like U quark as its realization. We also study cc(bar) -> Z' production that would exist within the model. Both processes can be probed already by LHC Run 2 data, all the way up to the HL-LHC. Speaker: Prof. George W.S. Hou (National Taiwan University) • 228 A Boosted Event Shape Tagger for Heavy Object Classification We present a novel approach to the problem of discriminating jets produced from the hadronic decays of highly-boosted heavy particles (top, W, Z, H) from light jets. By hypothesizing different particle origins for the jets and boosting all jet constituents into the corresponding rest frames, angular and kinematic distributions of reconstructed particles can be used to discriminate 2- or 3-prong topologies from those of light jets produced in QCD processes. Machine learning techniques are utilized to build discriminants capable of simultaneously separating and classifying the particle species. This approach adds additional information relative to existing techniques, thereby improving sensitivities of analyses dependent on such heavy-object tagging tools. We demonstrate the performance of this tagging method and provide a proof-of-principle application to a simple analysis scenario. Speaker: Justin Pilot (University of California, Davis) • 229 Toward Precision Top Quark Measurements in e+e- collisions This talk will review new developments toward precision top quark measurements at e+e- colliders, including improvements in the experimental strategies for top quark pair production in the continuum, improvements in the precision theoretical understanding of this process, and sensitivity to new physics models. It will also update the study of the precision measurement of the t-tbar threshold. Speaker: Prof. Hitoshi Yamamoto (Tohoku University) • Lunch • Meetings with DOE Representatives: Intensity Frontier 1 West ### 1 West #### Fermi National Accelerator Laboratory Kirk Road & Pine Street Batavia, IL 60510-5011 Convener: Glen Crawford (US Dept of Energy) • 230 Intensity Frontier Speaker: Dr Michael Cooke (U.S. Department of Energy) • Beyond Standard Model: Tuesday afternoon 1 West ### 1 West #### Fermi National Accelerator Laboratory Convener: Prof. Robin Erbacher Erbacher (UC Davis) • 231 Search for pair production of vector-like quarks in final states with a boosted W boson and b-jet with the ATLAS experiment This talk will present a search for the pair production of heavy vector-like$T$and$B$quarks, primarily targeting$T$quark decays to a$W$boson and a$b$quark. The search is based on 36 fb$^{−1 }$of$pp$collisions at$\sqrt{s} = 13$TeV recorded in 2015 and 2016 with the ATLAS detector at the CERN Large Hadron Collider. Data are analyzed in the lepton plus jets final state, including at least one$b$-tagged jet and a large-radius jet identified as originating from the hadronic decay of a high-momentum$W$boson. Speaker: Prof. Joseph Haley (Oklahoma State University) • 232 Search for electroweak production of a vectorlike quark decaying to a top quark and a Higgs or Z boson using boosted topologies in an all-hadronic final state We present a search for the electroweak production of a vector-like top quark partner T of charge + 2/3 in association with a standard model top or bottom quark, using proton-proton collision data at √s=13 TeV collected by the CMS Experiment at the CERN LHC. Our search targets T quarks decaying to a top quark and a Higgs or Z boson in a fully hadronic final state. For a T quark with mass above 1 TeV the daughter top quark and Higgs/Z boson are highly Lorentz-boosted and can appear together as a single hadronic jet. The top quark and Higgs/Z boson are identified using b-tagging and jet substructure techniques, which also acts to suppress the standard model backgrounds. Speaker: Erich Schmitz (University of Kansas) • 233 Search for low mass dijet resonances in association with ISR at the ATLAS experiment A search for low mass resonances decaying to a jet pair in association with an ISR jet or photon in the context of a dark matter mediator. The ISR object acts as the event trigger, and the resonance jet pair is subsequently boosted and reconstructed as a large-radius jet. Novel jet substructure techniques allow for signal jets to be selected over the dominant QCD background. The search uses 36 fb of pp collision data at a center-of-mass energy of 13 TeV collected in 2015 and 2016 by the ATLAS detector at the LHC. Resonances are searched for in the mass range of 100-250 GeV, using a leptophobic Z' benchmark model. Speaker: Laser Kaplan (University of Wisconsin-Madison) • 234 Search for light vector resonances decaying to a quark pair produced in association with a jet with the CMS detector at 13 TeV We perform a search for light generic dijet resonances produced in association with a high transverse momentum jet to get above trigger thresholds. It uses novel jet substructure observables to identify the Z' signal. The signal is then extracted on top of a falling QCD soft drop mass distribution estimated with a novel data-driven technique. Results are presented in a mass-coupling phase space and are the most sensitive to date, extending previous limits below 100 GeV. Speaker: Cristina Ana Mantilla Suarez (Fermilab) • 235 Search for paired dijet resonances in the boosted and non-boosted regime with the CMS detector at 13 TeV We present a search for paired dijet resonances using data from proton-proton collisions at a center-of-mass energy of 13 TeV, recorded in 2016 by the CMS detector at the LHC. We exploit jet substructure techniques to reach low mass boosted paired dijet resonances, while for higher resonance masses we search for four jets in the final state. We consider the pair production of top squarks (stops) as the benchmark model, where each stop decays through the hadronic R-parity violating (RPV) coupling; in the case of the UDD312 coupling the stops decay into two light quarks and, for the UDD323 coupling the stops decay into a light quark and a b-quark. Speaker: Alejandro Gomez Espinosa (Rutgers, The State University of New Jersey) • 236 Searches for new heavy resonances in final states with leptons, photons, and jets in CMS Many new physics models beyond the Standard Model predict the existence of narrow or broad resonances decaying to a pair of quarks/gluons, leptons, or photons. At the LHC, the production of heavy resonances decaying into a pair of particles can be probed at unprecedented centre-of-mass energies. This talk presents CMS searches for new resonances in the diet, dilepton, diphoton, and other final states that include leptons and photons, focusing on the recent results obtained using data collected during the 2016 run. Speaker: Norbert Neumeister (Purdue University) • 237 Search for diphoton high-mass resonances with 36.7 fb−1 of data collected at √ s=13 TeV with the ATLAS experiment A search for heavy resonances decaying into two photons in the ATLAS experiment is presented. The analysis uses proton-proton collision data accumulated at the Large Hadron Collider during 2015 and 2016 with a corresponding luminosity of 36.7 fb^{-1} at 13 TeV. Two searches are shown, a search for spin-0 particles using a heavy Higgs-like particle as a benchmark model, and a search for spin-2 particles using a Randall-Sundrum graviton as a benchmark model. Limits on the production cross section times branching ratio to two photons for the two resonance types are reported. Speaker: Mr Manuel Silva (University of Wisconsin, Madison) • Computing, Analysis Tools, and Data Handling: Tuesday afternoon 1 East ### 1 East #### Fermi National Accelerator Laboratory Convener: Aristeidis Tsaris (Fermilab) • 238 Deep Neural Networks for HEP Images Deep neural networks (DNNs) have revolutionized many areas of science and technology. In this talk, we will discuss cutting edge developments in DNNs for high energy physics, using jet physics (including calorimeter showers) as an example that has attracted significant recent attention. Domain specific challenges require new techniques to make full use of the algorithms. A key focus is on understanding how and what the algorithms learn. DNN techniques are demonstrated for classification, regression, and generation. In addition to providing powerful baseline performance, we show how to train complex models directly on data and to generate sparse stacked images with non-uniform granularity. Speaker: Benjamin Nachman (LBNL) • 239 Applying Deep Learning in MicroBooNE Deep learning algorithms, which have emerged over the last decade, are opening up new ways to analyze data for many particle physics experiments. The MicroBooNE experiment, which is a neutrino experiment at Fermilab, has been exploring the use of such algorithms, in particular convolutional neural networks (CNNS). CNNs are the state-of-the-art method for a large class of problems requiring the analysis of image data. This makes CNNs an attractive approach as the MicroBooNE detector is a liquid argon time projection chamber, which produces high-resolution images of particle interactions. In this talk, I will discuss the ways CNNs can be applied to tasks like neutrino interaction detection and particle identification in MicroBooNE. Speaker: Taritree Wongjirad (MIT) • 240 Deep Learning and DUNE The observation of neutrino oscillations provides evidence of physics beyond the standard model, and the precise measurement of those oscillations remains an important goal for the field of particle physics. The planned DUNE experiment is set to become a leading experiment in the study of neutrino oscillations. Taking advantage of a two-detector technique, a tightly focused beam at Fermilab, and a far detector based on cutting edge Liquid Argon Time Projection chamber technology, DUNE will in a prime position to deliver precision measurements of the neutrino mass hierarchy, and CP violation. A key part of the delivery of those precision measurement will be the accurate identification and reconstruction of neutrino interactions in the DUNE far detector. Liquid Argon Time Projection chambers are rich sources of physical information, offering the equivalent of incredibly high resolution “images” of the particles produced in neutrino interactions. Conventional reconstruction tools have so far struggled to fully exploit the promise of that rich source of information, particularly compared to expert human event scanners. This talk will describe a variety of novel ways in which cutting edge deep learning tools are being explored to aid both event reconstruction and selection in DUNE detector simulations. Speaker: Dr Alexander Radovic (College of William and Mary) • 241 Advanced machine-learning solutions in LHCb operations and data analysis The LHCb detector is a forward spectrometer optimized for the reconstruction of charm- and bottom-hadron decays in LHC’s proton-proton collisions. The need to process large amounts of data within the constraints of the data-acquisition and offline-computing resources pushes steadily toward usage of advanced data-analysis techniques. Currently, LHCb takes data at rates significantly higher than the design values, thanks also to purpose-developed machine-learning (ML) solutions. Such soliutions are applied to an increasing class of essential online and offline tasks, including more precise and faster real-time classification of interesting events, smarter detector-performance calibrations, and more precise, efficient, and unbiased offline characterization of reconstructed events. This talk overviews recent original ML applications in the trigger, operations, and analysis of LHCb data in 2015-2016 and discusses ongoing and future developments. Speaker: Dr Fedor Ratnikov (YSDA) • Cosmology and Astrophysics: Tuesday afternoon Comitium ### Comitium #### Fermi National Accelerator Laboratory Convener: Dr Bradford Benson (Fermilab) • 242 News from BICEP/Keck Array CMB program The BICEP/Keck Array program comprises a series of telescopes at the South Pole designed to make deep measurements of cosmic microwave background polarization at degree angular scales on a 1% patch of sky. This talk will describe the latest science results from the program, including constraints on inflation, axion-like particles and primordial magnetic fields, as well as a high-significance detection of gravitational lensing. These results were derived using various combinations of 150GHz and 95GHz data collected by the BICEP/Keck receivers through 2014, and multi-frequency data from Planck and WMAP. The talk will also preview imminent science results that include one year of 220GHz data from BICEP/Keck. Finally, we will share plans for BICEP Array, the Stage 3 expansion of the BICEP/Keck program. Speaker: Zeeshan Ahmed (SLAC National Accelerator Laboratory) • 243 The ACTPol and Advanced ACTPol Experiments ACTPol and Advanced ACTPol are a series of cameras deployed on the Atacama Cosmology Telescope (ACT) and used to map the temperature and polarization of the cosmic microwave background (CMB) in multiple frequency bands and with arc minute resolution. Survey operations began in 2013 with a sky coverage of hundreds of square degrees in the 150 GHz band. Over the past five years we have upgraded the instrument and expanded the sky coverage. Beginning in 2016 we have been undertaking a wide survey covering 14,000 square degrees with sensitivity in the 90, 150, and 220 GHz bands. These data have been used to make measurements of CMB polarization, CMB lensing, and cross-correlations between these maps and observations at other wavelengths. In this presentation I given an overview of these experiments, our published results to date, and provide a preview of the science which will come out of the Advanced ACTPol data set for which analysis is ongoing. Speaker: Dr Jeff McMahon (University of Michigan) • 244 Recent progress from the SPT-3G experiment The South Pole Telescope is a millimeter-wavelength telescope dedicated to observations of the Cosmic Microwave Background (CMB). In late 2016, the telescope was upgraded with new receiver known as SPT-3G. The SPT-3G receiver contains a focal plane of approximately 16,000 polarization-sensitive superconducting detectors distributed between three frequency bands. SPT-3G will survey the sky for four years, resulting in extremely deep, high-resolution maps of the polarization of the CMB. With these data, SPT-3G has the potential to constrain inflationary gravitational waves as well as the effect of massive neutrinos on large-scale structure formation. I will describe some of the technological advances enabling the large-format SPT-3G focal plane as well as the current instrument status and cosmological forecasts. Speaker: Dr Amy Bender (Argonne National Laboratory) • 245 Cosmology from CMB Polarization with POLARBEAR and the Simons Array POLARBEAR is a cosmic microwave background (CMB) polarization experiment located in the Atacama desert in Chile. The science goals of the POLARBEAR project are to do a deep search for CMB B-mode polarization created by inflationary gravitational waves, as well as characterize the CMB B-mode signal from gravitational lensing. Gravitational lensing of large-scale structure creates B-mode polarization on arcminute scales, and surveys of this signal can be used to constrain the sum of the neutrino masses. POLARBEAR-1 started observations in 2012, and the POLARBEAR team has published a series of results from its first season of observations, including the first measurement of a non-zero B-mode polarization angular power spectrum. Recently, we released an improved measurement of the B-mode polarization power spectrum, reducing our uncertainties by a factor of two, by adding new data from our second observing season and re-analyzing the combined data set. To further improve on these measurements, POLARBEAR is expanding to include an additional two telescopes with dichroic receivers covering 95, 150, 220, and 270 GHz, known as POLARBEAR-2/Simons Array. With high sensitivity and large sky coverage, the Simons Array will create a detailed survey of B-mode polarization, and its spectral information will be used to extract the CMB signal from astrophysical foregrounds. We will present the latest POLARBEAR results, as well as the status of development of the Simons Array and its expected capabilities. Speaker: Dr Darcy Barron (UC Berkeley / LBNL) • 246 The Simons Observatory: Cosmology and Fundamental Physics from the Cosmic Microwave Background The Simons Observatory (SO) is a next generation observatory optimized to make precise measurements of the comic microwave background (CMB) over frequencies spanning 30-300 GHz. The observatory will be built with a combination of 6 meter class and 1 meter class telescopes and up to 40,000 detector focal-plane arrays to make high fidelity maps over degree to arc-minute angular scales. These data will be used to detect or place stringent limits on primordial gravitational waves, new light relativistic species, neutrino properties, and to make many other astrophysical and cosmological measurements. The SO instrument will be a stepping stone to CMB-S4 which will field hundreds of thousands of CMB detectors across multiple telescope platforms. We will present the status of the design development for the large- and small-aperture SO telescopes, the cryogenic receivers, cold optical elements, and our plan for fielding and reading out tens of thousands of multichroic, superconducting detectors. Speaker: Prof. Adrian Lee (University of California, Berkeley) • Dark Matter: Tuesday afternoon Hornets Nest ### Hornets Nest #### Fermi National Accelerator Laboratory Convener: Prof. Enectali Figueroa-Feliciano (Northwestern University) • 247 Search for new physics phenomena using events with missing transverse momentum and a Higgs boson decaying into two photons at sqrt(s) = 13 TeV with the ATLAS experiment A search for new physics phenomena is presented using events with missing transverse momentum and a Standard Model Higgs boson decaying into two photons. This search is based on 13 TeV proton-proton collision data collected by the ATLAS detector at the LHC in 2015 and 2016, corresponding to an integrated luminosity of 36.1$fb^{−1}$. No significant excess over the Standard Model expectation is observed. Upper limits at 95% confidence level on the production cross section times the branch ratio of the Higgs boson decaying into two photons are set for two Dark Matter models and a heavy scalar boson model. Additionally, the results are interpreted in terms of 90% confidence level limits on the dark matter-nucleon scattering cross section, as well as 95% confidence level limits on visible cross section. Speaker: Dr Chen Zhou (University of Wisconsin-Madison) • 248 Search for Dark Matter Produced in Association with a Higgs Boson Decaying to bb at sqrt(s) = 13 TeV with the ATLAS Experiment Several extensions of standard model predict dark matter production in association with a Higgs boson. In this talk the results of a search for such models in final states with large missing transverse momentum and a Higgs boson decaying to$b\bar{b}$will be presented. The search is performed with the ATLAS detector using 36 fb-1 of pp collisions at a center-of-mass energy of 13 TeV at the LHC. The results are interpreted in the context of a Dark Matter model and without extra model assumptions. Speaker: Mr Efe Yigitbasi (Boston University) • 249 Search for dark matter produced in association with a hadronically decaying vector boson at the ATLAS experiment A search for dark matter particles produced in association with a hadronically decaying W or Z boson with the ATLAS experiment at the LHC is reported. The search uses data corresponding to an integrated luminosity of 36.1/fb in proton-proton collisions at a centre-of-mass energy (√s) of 13 TeV. No significant excess over the Standard Model prediction is observed. The search results are interpreted in terms of an effective field theory and a simplified vetor-mediator model describing dark matter interactions with Standard Model particles. Speaker: Mr Yicheng Guo (University of Michigan; University of Science and Technology of China) • 250 Search for invisible decay of a dark photon produced in$e^+e^-$collisions at BaBar We report on a search for single-photon events in 53$fb^{-1} of $e^+e^-$ collision data collected with the BaBar detector at the PEP-II $B$-factory. We look for events with a single high-energy photon and a large missing momentum and energy, consistent with production of a spin-1 particle $A’$ through the process $e^+e^- \to \gamma A’$, $A’ \to invisible$. Such particles, referred to as “dark photons”, are motivated by theories applying a $U(1)$ gauge symmetry to dark matter. We find no evidence for such processes and set 90\% confidence level upper limits on the coupling strength of $A’ \to e^+e^-$ for a dark photon with a mass lower than 8 GeV. In particular, our limits exclude the values of the $A’$ coupling suggested by the dark-photon interpretation of the muon (g-2) anomaly, as well as a broad range of parameters.
Speaker: Dr Tomonari Miyashita (California Institute of Technology)
• 251
Search for muonic dark force at BABAR
Many models of New Physics postulate the existence new gauge bosons mediating interactions between “dark sectors” and the Standard Model. We present a search for a dark boson Z' coupling only to the second and third generation of leptons in the reaction e+e- -> mu+mu-Z', Z' -> mu+mu- with the full BABAR dataset. No significant signal is observed and limits improving upon bounds derived from neutrino experiments are set.
Speaker: Bertrand Echenard (Caltech)
• 252
An Indirect Search for Weakly Interacting Massive Particles in the Sun Using Upward-Going Muons in NOvA
We present the status of the a dark matter search using a dataset collected with an upward-going muon trigger at NOvA. Weakly Interactive Massive Particles are a theoretical potential non-baryonic form of Dark Matter. The nature of Dark Matter is one of the most interesting open questions in modern physics. Evidence for DM existence comes from cosmological observations but the discovery has not been made yet. If we assume that DM particles can produce Standard Model particles through their interactions, indirect searches can help shed light on this mystery. The NOvA collaboration has constructed a 14,000 ton, fine-grained, low-Z, total absorption tracking calorimeter. This detector, with its excellent granularity and energy resolution and relatively low-energy neutrino thresholds, is designed to observe electron neutrino appearance in a muon neutrino beam: but it also has unique capabilities suitable for more exotic measurements. In fact, with an efficient upward-going muon trigger and sufficient background suppression offline, NOvA will be capable of a competitive indirect dark matter search for low-mass WIMPs. To avoid the downward-going cosmic-ray muon background, we use only upward-going muons that point to the Sun. So, the search occurs at night when the Sun is on the other side of the Earth. This also allows us to use the time when the Sun is above the horizon as a control region to estimate the background. The goal is to select a sample of neutrino-induced upward-going muons and perform a competitive dark matter search.
Speaker: Cristiana Principato (University of Virginia)
• 253
The Potential of the ILC for Discovering New Particles
The LHC did not discover new particles beyond the Standard Model Higgs boson at 7 and 8 TeV, or in the first data samples at 13 TeV. However, the complementary nature of physics with e+e- collisions still offers many interesting scenarios in which new particles can be discovered at the ILC. These scenarios take advantage of the capability of e+e- collisions to observe particles with missing energy and small mass differences, to observe mono-photon events with precisely controlled backgrounds, and to observe the full range of exotic decay modes of the Higgs boson. The searches that an e+e- collider makes possible are particularly important for models of dark matter involving a dark sector with particles of 10--100 GeV mass. In this talk, we will review the opportunities that the ILC offers for new particle discovery.
Speaker: Prof. Howard Baer (University of Oklahoma)
• Higgs and EWSB: Tuesday afternoon Sunrise
### Sunrise
#### Fermi National Accelerator Laboratory
Convener: Laura Reina (Florida State University)
• 254
Soft Gluon Resummation at NNLL Accuracy for Associated $t\bar{t}H$ Production at the LHC
The $t\bar{t}H$ production process probes the top-Higgs Yukawa coupling directly which is especially sensitive to the underlying physics. The measurement of the $pp \to t\bar{t}H$ cross section is among the highest priorities of the current LHC physics program and improvement of the theoretical accuracy is of the central importance. In this talk the latest results for soft gluon resummation at fixed invariant mass for $pp \to t\bar{t}H$ will be presented. The resummation is extended to next-to-next-to-leading logarithmic accuracy. The invariant mass resummation results will be presented in the form of the inclusive cross section and the invariant mass distribution, including scale uncertainty.
Speaker: Vincent Theeuwes (SUNY, Buffalo)
• 255
Search for production of a Higgs boson and a single top quark
We present recent results from searches for the production of a Higgs boson in association with a single top quark (tHq), using data samples collected by the CMS detector in pp collisions at center-of-mass energy of 13 TeV, using data samples with integrated luminosity of up to 35.9 fb-1. The searches exploit a variety of top quark and Higgs boson decay modes resulting in final states with photons, bottom quarks, or multileptons, and employ a variety of multivariate techniques to maximize the sensitivity to the signal. Due to interference between the two main leading-order diagrams, the tHq process is sensitive to the relative sign of the couplings of the Higgs to the top quark and the vector bosons, and thus provides unique information on Higgs boson properties.
Speaker: Ken Bloom (University of Nebraska-Lincoln)
• 256
Search for the Higgs boson production in association with top quarks at \sqrt{s} = 13 TeV with the ATLAS detector
The observation of the Higgs boson production in association with top quarks (ttH) is of particular importance, as it will be a direct evidence of the top Higgs Yukawa coupling. Further measurements of this process may be sensitive to potential new physics beyond the Standard Model, due to the large value of the top Yukawa coupling. I present searches for this production mode using ATLAS data taken in 2015 and 2016 at a center-of-mass energy of 13 TeV, with a focus on the analyses of diphoton and bbbar final states.
• 257
Search for ttH production in multilepton final states using the ATLAS experiment at the LHC
The search for Higgs boson production in association with two top quarks allows the direct measurement of Higgs boson- top quark Yukawa coupling. In this talk, results from the measurement of $t\bar{t}H$ production decaying into multilepton final states are presented. This search uses 36 fb$^{-1}$ of proton-proton collision data collected by the ATLAS experiment at the center-of-mass energy of 13 TeV in 2015 and 2016. The analysis is most sensitive to $H\to WW$, $H\to ZZ$ and $H\to \tau \tau$ decay modes.
Speaker: Mr Harish Potti (University of Texas at Austin)
• 258
Search for production of a Higgs boson and a top quark pair at CMS
The discovery of a Higgs particle made by the CMS and ATLAS experiments at the Large Hadron Collider in 2012 was heralded as a significant advancement in our understanding of the fundamental world. In the post-discovery era, the task turned to characterizing this Higgs boson: to determine whether it is the particle predicted within the context of the standard model (SM) of particle physics – or is something altogether different. Essentially all measurements have thus far indicated that this Higgs boson is consistent with the predictions of the SM. However, one of the crucial characteristics that remains to be measured is the coupling strength between the Higgs boson and the top quark. The best opportunity for this measurement comes through the observation of production of a Higgs boson in association with a top quark pair (ttH production). In this talk, the status of the ttH campaign at CMS will be summarized covering results in all of the accessible decay channels.
Speaker: Mr Evan Wolfe (University of Virginia)
• Neutrino Physics: Tuesday afternoon Ramsey Auditorium
### Ramsey Auditorium
#### Fermi National Accelerator Laboratory
Convener: Dr Minerba Betancourt (Fermilab)
• 259
Nuclear Dependence of Quasi-Elastic Scattering at MINERvA
A precise understanding of quasi-elastic interactions is crucial to measure neutrino oscillations. Current neutrino oscillation experiments use different targets that range from carbon to argon. A sample of neutrino interactions on Fe, Pb, C and CH with one muon and at least one proton candidate is used to study quasielastic-like interactions and the role that the nuclear environment plays in modifying those interactions. Measurements of differential cross sections and ratios of Fe, Pb and C to scintillator are presented as a function of four-momentum transferred to the target nucleus, where the momentum transferred is reconstructed using proton kinematics. Comparisons of these measurements with the predictions from the GENIE and NuWro event generators will be shown.
Speaker: Prof. Aaron Bercellie (Rochester University)
• 260
Recent MINERvA Double Differential CCQE Cross Section Results Using Lepton Kinematics
MINERvA’s first CCQE results preferred models with 2p2h-like enhancements. Since then work using an inclusive sample measuring reconstructed available energy and three momentum transfer has demonstrated the effect of adding in RPA and 2p2h components to our base GENIE simulation. Further modification via a fit to the inclusive data results in an empirical model which well describes the full two dimensional cross sections in lepton variables, transverse and longitudinal momentum, for both the neutrino and anti-neutrino cases. These cross section results will be compared to this new model as well as other models.
Speaker: Prof. Jeffrey Kleykamp (Rochester University)
• 261
Status of an Alternative Measurement of the Inclusive Muon Neutrino Charged-current Cross Section in the NOvA Near Detector
NOvA is a long-baseline neutrino oscillation experiment. It uses the NuMI beam from Fermilab and two sampling calorimeter detectors off-axis from the beam. The 293 ton Near Detector measures the unoscillated neutrino energy spectrum, which can be used to predict the neutrino energy spectrum at the 14 kton Far Detector at Ash River, MN. The Near Detector also provides an excellent opportunity to measure cross sections with high statistics, which benefit current and future long-baseline neutrino oscillation experiments. This analysis implements new algorithms to identify $\nu_{\mu}$ charge-current events by using visual deep learning tools such as convolutional neural networks. In this talk we present the status of a measurement of the inclusive $\nu_{\mu}$ CC cross section in the NOvA Near Detector.
Speaker: Mr Biswaranjan Behera (IIT Hyderabad/Fermilab)
• 262
Status of the Charged Pion Semi-Inclusive Neutrino Charged-Current Cross Section in NOvA
The NOvA experiment is a long-baseline neutrino oscillation experiment designed to measure the rates of electron neutrino appearance and muon neutrino disappearance. The NOvA near detector is located at Fermilab, 800 m from the primary target and provides an excellent platform to measure and study neutrino-nucleus interactions.We present the status of the measurement of the double differential cross section with respect to muon kinematics for interactions involving charged pions in the final state, νμ+N → N +μ±π∓X.We have derived a convolutional neural network-based approach for the identification of neutrino interactions with the specific final state topology. We present event classification efficiency studies using this particle identification and classification methodology, along with systematic uncertainties, background estimates and prospects for the measurement.
Speaker: Mr Aristeidis Tsaris (Fermilab)
• 263
Status of the Electron-Neutrino Charged-Current Inclusive Cross-Section Measurement in NOvA
The electron-neutrino charged-current inclusive cross section on nuclei is an important input parameter for electron-neutrino appearance oscillation experiments. There are a small number of measurements, with limited statistics, in the few GeV region where current and future long base-line neutrinos experiments operate. The NOvA near detector is located at Fermilab, approximately 800 m from the NuMI beam production target and thus provides an excellent platform to measure and study neutrino interactions and cross sections with high statistics. We present our progress, including the use of a convolutional visual network (CVN) technique as event classifier, on this neutrino scattering measurement in the energy range of 1-3 GeV with data collected from November 2014 to February 2017 in the NOvA near detector.
Speaker: Mr Pengfei Ding
• 264
Measurement of Neutrino-Electron Elastic Scattering at NOvA Near Detector
NOvA is a long-baseline accelerator-based neutrino oscillation experiment that is optimized for electron-neutrino appearance measurements. It uses the upgraded NuMI beam from Fermilab and consists of a Far Detector in Ash River, Minnesota and a Near Detector at Fermilab. An accurate prediction of the neutrino flux is key to both oscillation and cross-section measurements. The precisely known neutrino-electron elastic scattering cross section provides an in situ constraint on the absolute flux. This talk discusses the status of the measurement of the rate of neutrino-electron elastic scattering in the NOvA Near Detector.
Speaker: Prof. Jianming Bian (University of California, Irvine)
• Particle Detectors: Tuesday afternoon IARC Building
### IARC Building
#### Fermi National Accelerator Laboratory
Convener: Georgia Karagiorgi (Columbia University)
• 265
Studies of GaInP based Geiger-mode APD arrays
Devices composed of wide band gap semiconductors such as GaInP have the theoretical potential to withstand many orders of magnitude larger radiation exposures compared to silicon. LightSpin Technologies has developed high density, large area SPAD arrays in GaInP with resolution for single photon peaks over the past several years. We report on measurements using a sample of the latest generation of prototype devices, demonstrating performance properties of new large GAPD arrays based on this compound semiconductor.
Speakers: Prof. Bob Hirosky (Virginia), Grace Cummings (Virginia Commonwealth University)
• 266
Detecting Axions with Superconducting Qubits
The Axion Dark Matter eXperiment (ADMX) aims to detect dark matter axions converting to single photons in a resonant cavity bathed in a uniform magnetic field. A qubit (two level system) operating as a single microwave photon detector is a viable readout system for ADMX and may offer advantages over the quantum limited amplifiers currently used ADMX. When weakly coupled to the detection cavity, the qubit transition frequency is shifted by an amount proportional to the cavity photon number. Through spectroscopy of the qubit, the frequency shift is measured and the cavity occupation number is extracted. At low enough temperatures, this system would allow sensitivities exceeding that of the standard quantum limit.
Speaker: Akash Dixit (University of Chicago)
• 267
Gain stabilization of Silicon Photomultipliers and Afterpulsing
The gain of silicon photomultipliers (SiPMs) increases with bias voltage and decreases with temperature. To operate SiPMs at stable gain, the bias voltage can be adjusted to compensate temperature changes. We have tested this concept with 30 SiPMs from three manufacturers (Hamamatsu, KETEK, CPTA) in a climate chamber at CERN varying the temperature from 1°C to 50°C. We built an adaptive power supply that used a linear temperature dependence of the bias voltage readjustment. With one selected bias voltage readjustment, we stabilized four SiPMs simultaneously. We fulfilled our goal of limiting the deviation from gain stability in the 20°C-30°C temperature range to less than ±0.5% for most of the tested SiPMs. We have studied afterpulsing of SiPMs for different temperatures and bias voltages.
Speaker: Prof. Gerald Eigen (University of Bergen)
• 268
Directional measurements of fast neutron backgrounds at SuperKEKB
During the commissioning of the SuperKEKB accelerator, the next-generation B factory located in Tsukuba, Japan, the BEAST II detector system was used to measure beam induced backgrounds. Fast neutrons have proven to be a notoriously pernicious background at collider experiments. Among the many measurements made by BEAST II, the Micro Time Projection Chambers (µTPCs) subsystem provided direction-sensitive measurements of fast neutrons by reconstructing the charge clouds from nuclear recoils in gas with high spatial resolution. We present measurements from the first SuperKEKB run, and compare the resulting data with beam-loss and detector simulations.
Speaker: Michael Hedges (BEAST II Collaboration)
• 269
Characterizing New Detectors for SuperCDMS SNOLAB
The Super Cryogenic Dark Matter Search (SuperCDMS) uses sub-Kelvin semiconductor detectors to search for dark matter WIMPs (Weakly Interacting Massive Particles), with excellent sensitivity to low mass WIMPs. The collaboration is currently building the next phase, SuperCDMS SNOLAB, with larger and more sensitive detectors. Two different detector designs have been developed: the iZIP design, which can discriminate between electron- and nuclear-recoil events, and the CDMS-HV design, which has extremely low energy thresholds allowing sensitivity to WIMPs with masses well below 1 GeV. Detectors of these designs are being fabricated with two different target materials, germanium and silicon, and all four detector types will be deployed at SNOLAB providing complementary sensitivities. I will report on early tests of prototypes of these new detectors and their performance parameters.
Speaker: Matthew Fritts (University of Minnesota)
• QCD: Tuesday afternoon Curia II
### Curia II
#### Fermi National Accelerator Laboratory
Convener: Christopher Lee (Los Alamos National Laboratory)
• 270
Quarkonium Production in Jets
This talk will describe new tests of quarkonium production using quarkonia that are produced within jets. We study the distribution in the fraction $z$ of a jet's longitudinal momentum carried by the quarkonium. The $z$ distribution is sensitive to the underlying NRQCD production mechanism. Analytic calculations the $z$ distributions in SCET that incorporate Next-to-Leading-Log (NLL) resummation disagree with default PYTHIA predictions. We describe a modified simulation method which agrees well with NLL analytic calculations. This method is then successfully applied to recent LHCb measurements of $J/\psi$ within jets. We discuss the implications of this measurement for extractions of NRQCD long-distance matrix elements. Finally, we discuss other observables involving quarkonium within jets which may be useful for discriminating between NRQCD production mechanisms.
Speaker: Dr Thomas Mehen (Duke University)
• 271
Studies of quarkonium at Belle and Belle II
Quarkonium is the bound state of a heavy quark and its anti-quark counterpart. The study of this system has experienced a renaissance thanks to results from the e+e- collider experiments, including discoveries of long-predicted conventional quarkonia, and unusual states consisting of four quarks. The Belle Experiment operated at KEK in Japan from 1999-2010. Analysis of the collected data continues to produce new findings. The Belle II experiment is a substantial upgrade of both the Belle detector and the KEKB accelerator, aiming to collect 50 times more data beginning in 2018. This talk will present recent Belle results related to hadronic and radiative decays in the bottomonium system. It will also describe the capabilities of Belle II to explore these topics, with a particular focus on the physics reach of the first data, where unique opportunities exist to make an immediate impact in this area.
Speaker: Dr Bryan Fulsom (Pacific Northwest National Laboratory)
• 272
Heavy flavour production at LHCb
Heavy flavour production measurements in proton-proton collisions are important tests of QCD. We report on updated production cross-section measurement of quarkonia, open-charm, and open-beauty states. Other aspects related to the quarkonium production mechanisms, such as the production of charmonium state in jets, will be discussed.
Speakers: Dr Marco Gersabeck (The University of Manchester), Philip Ilten (Massachusetts Institute of Technology)
• 273
Precise measurements of the mass differences between the $D^*(2010)^+$, and the $D^+$ and $D^0$ mesons with the BaBar detector
We present a high precision measurement of the mass difference between the $D^*(2010)^+$ and $D^+$ mesons using the decay chain $D^*(2010)^+ \to D^+ \pi^0$, with $D^+ \to K^- \pi^+ \pi^+$ . The analysis has been performed on a data sample corresponding to an integrated luminosity of about 477 ${\mathrm{fb}}^{-1}$, collected with the BaBar detector at the PEP-II e+e- collider. We additionally combine this result with a previous BaBar measurement of $m(D^*(2010)^+) - m(D^0)$ to extract the mass difference between the charged and neutral $D$ mesons. We obtain results that are approximately seven times more precise than the present world averages.
Speaker: Prof. Michael Sokoloff (University of Cincinnati)
• 274
| 2022-06-26T08:36:06 |
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|
https://lammps.sandia.gov/doc/improper_coeff.html
|
# improper_coeff command
## Syntax
improper_coeff N args
• N = improper type (see asterisk form below)
• args = coefficients for one or more improper types
## Examples
improper_coeff 1 300.0 0.0
improper_coeff * 80.2 -1 2
improper_coeff *4 80.2 -1 2
## Description
Specify the improper force field coefficients for one or more improper types. The number and meaning of the coefficients depends on the improper style. Improper coefficients can also be set in the data file read by the read_data command or in a restart file.
N can be specified in one of two ways. An explicit numeric value can be used, as in the 1st example above. Or a wild-card asterisk can be used to set the coefficients for multiple improper types. This takes the form “*” or “*n” or “n*” or “m*n”. If N = the number of improper types, then an asterisk with no numeric values means all types from 1 to N. A leading asterisk means all types from 1 to n (inclusive). A trailing asterisk means all types from n to N (inclusive). A middle asterisk means all types from m to n (inclusive).
Note that using an improper_coeff command can override a previous setting for the same improper type. For example, these commands set the coeffs for all improper types, then overwrite the coeffs for just improper type 2:
improper_coeff * 300.0 0.0
improper_coeff 2 50.0 0.0
A line in a data file that specifies improper coefficients uses the exact same format as the arguments of the improper_coeff command in an input script, except that wild-card asterisks should not be used since coefficients for all N types must be listed in the file. For example, under the “Improper Coeffs” section of a data file, the line that corresponds to the 1st example above would be listed as
1 300.0 0.0
The improper_style class2 is an exception to this rule, in that an additional argument is used in the input script to allow specification of the cross-term coefficients. See its doc page for details.
The list of all improper styles defined in LAMMPS is given on the improper_style doc page. They are also listed in more compact form on the Commands improper doc page.
On either of those pages, click on the style to display the formula it computes and its coefficients as specified by the associated improper_coeff command.
## Restrictions
This command must come after the simulation box is defined by a read_data, read_restart, or create_box command.
An improper style must be defined before any improper coefficients are set, either in the input script or in a data file.
| 2018-12-16T08:46:47 |
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|
http://legisquebec.gouv.qc.ca/en/showversion/cr/C-24.2,%20r.%2035?code=se:14&pointInTime=20190521
|
### C-24.2, r. 35 - Regulation respecting special permits
14. The driver of a vehicle for which a special permit has been issued shall comply with
(1) the provisions of subparagraph 5 of the first paragraph of section 5;
(2) the provisions of subparagraph 12 of the first paragraph of section 5, section 7, section 9 and the second and third paragraphs of section 13;
(3) the provisions of subparagraphs 2, 4, 8 and 9.1 of the first paragraph of section 5, sections 8, 10 to 12 and of the first paragraph of section 13.
O.C. 1444-90, s. 14; O.C. 1605-93, s. 15; O.C. 384-99, s. 2.
| 2019-08-23T00:32:25 |
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|
https://zbmath.org/authors/?q=ai%3Anash.john-f-jun
|
# zbMATH — the first resource for mathematics
## Nash, John Forbes jun.
Compute Distance To:
Author ID: nash.john-f-jun Published as: Nash, John Forbes jun.; Nash, John F. jun.; Nash, John F.; Nash, John; Nash, J. F.; Nash, John Forbes; Nash, J.; Nash, J. F. jun. External Links: IdRef · Google Scholar · MGP · theses.fr · Math-Net.Ru · Wikidata · dblp · GND · MacTutor Awards: Nobel Memorial Prize in Economic Sciences (1994) · Abel Prize (2015)
Documents Indexed: 29 Publications since 1950, including 3 Books Biographic References: 56 Publications
all top 5
#### Co-Authors
24 single-authored 1 Hammerstein, Peter 1 Harsanyi, John Charles 1 Kalisch, Gerhard K. 1 Kuhn, Harold William 1 Mayberry, John P. 1 Milnor, John Willard 1 Nering, Evar D. 1 Rassias, Michael Th. 1 Selten, Reinhard 1 Shapley, Lloyd S. 1 Shubik, Martin 1 van Damme, Eric 1 Weibull, Jörgen W.
all top 5
#### Serials
5 Annals of Mathematics. Second Series 3 Econometrica 3 Proceedings of the National Academy of Sciences of the United States of America 2 Uspekhi Matematicheskikh Nauk [N. S.] 1 American Journal of Mathematics 1 Bulletin de la Société Mathématique de France 1 Duke Mathematical Journal 1 Journal of Economic Theory 1 Games and Economic Behavior 1 International Journal of Mathematics, Game Theory and Algebra 1 International Game Theory Review
all top 5
#### Fields
17 Game theory, economics, finance, and other social and behavioral sciences (91-XX) 5 History and biography (01-XX) 1 General and overarching topics; collections (00-XX) 1 Number theory (11-XX) 1 Algebraic geometry (14-XX) 1 Partial differential equations (35-XX) 1 Convex and discrete geometry (52-XX) 1 Differential geometry (53-XX) 1 Global analysis, analysis on manifolds (58-XX) 1 Computer science (68-XX)
#### Citations contained in zbMATH Open
22 Publications have been cited 4,184 times in 3,567 Documents Cited by Year
Non-cooperative games. Zbl 0045.08202
Nash, John
1951
Equilibrium points in $$n$$-person games. Zbl 0036.01104
Nash, John F. jun.
1950
The bargaining problem. Zbl 1202.91122
Nash, John F. jun.
1950
Continuity of solutions of parabolic and elliptic equations. Zbl 0096.06902
Nash, John F.
1958
The imbedding problem for Riemannian manifolds. Zbl 0070.38603
Nash, John
1956
Two-person cooperative games. Zbl 0050.14102
Nash, John
1953
$$C^1$$ isometric imbeddings. Zbl 0058.37703
Nash, John
1954
The Cauchy problem for differential equations of a general fluid. (Le problème de Cauchy pour les équations différentielles d’un fluide général.) Zbl 0113.19405
Nash, John F.
1962
Real algebraic manifolds. Zbl 0048.38501
Nash, John
1952
Arc structure of singularities. Zbl 0880.14010
Nash, John F. jun.
1995
Parabolic equations. Zbl 0078.08704
Nash, John
1957
Analyticity of the solutions of implicit function problems with analytic data. Zbl 0173.09202
Nash, John F.
1966
A path space and the Stiefel-Whitney classes. Zbl 0064.17503
Nash, John
1955
Open problems in mathematics. Zbl 1351.00027
Nash, John Forbes jun. (ed.); Rassias, Michael Th. (ed.)
2016
Some experimental $$n$$-person games. Zbl 0058.13904
Kalisch, G. K.; Milnor, John W.; Nash, J. F.; Nering, E. D.
1954
A comparison of treatments of a duopoly situation. Zbl 0050.15104
Mayberry, J. P.; Nash, J. F.; Shubik, M.
1953
A simple three-person poker game. Zbl 0041.25602
Nash, J. F.; Shapley, L. S.
1950
The work of John Nash in game theory. Nobel seminar, December 8, 1994. Zbl 0853.90146
Kuhn, Harold W.; Harsanyi, John C.; Selten, Reinhard; Weibull, Jörgen W.; Van Damme, Eric; Nash, John F. jun.; Hammerstein, Peter
1996
The imbedding problem for Riemannian manifolds. Zbl 0217.47504
Nash, John F.
1971
The essential John Nash. Edited by Harold W. Kuhn and Sylvia Nasar. Zbl 1033.01024
Nash, John F. jun.
2002
The agencies method for modeling coalitions and cooperation in games. Zbl 1178.91019
Nash, John F. jun.
2008
The bargaining problem. Zbl 0267.90006
Nash, John F. jun.
1971
Open problems in mathematics. Zbl 1351.00027
Nash, John Forbes jun.; Rassias, Michael Th.
2016
The agencies method for modeling coalitions and cooperation in games. Zbl 1178.91019
Nash, John F. jun.
2008
The essential John Nash. Edited by Harold W. Kuhn and Sylvia Nasar. Zbl 1033.01024
Nash, John F. jun.
2002
The work of John Nash in game theory. Nobel seminar, December 8, 1994. Zbl 0853.90146
Kuhn, Harold W.; Harsanyi, John C.; Selten, Reinhard; Weibull, Jörgen W.; Van Damme, Eric; Nash, John F. jun.; Hammerstein, Peter
1996
Arc structure of singularities. Zbl 0880.14010
Nash, John F. jun.
1995
The imbedding problem for Riemannian manifolds. Zbl 0217.47504
Nash, John F.
1971
The bargaining problem. Zbl 0267.90006
Nash, John F. jun.
1971
Analyticity of the solutions of implicit function problems with analytic data. Zbl 0173.09202
Nash, John F.
1966
The Cauchy problem for differential equations of a general fluid. (Le problème de Cauchy pour les équations différentielles d’un fluide général.) Zbl 0113.19405
Nash, John F.
1962
Continuity of solutions of parabolic and elliptic equations. Zbl 0096.06902
Nash, John F.
1958
Parabolic equations. Zbl 0078.08704
Nash, John
1957
The imbedding problem for Riemannian manifolds. Zbl 0070.38603
Nash, John
1956
A path space and the Stiefel-Whitney classes. Zbl 0064.17503
Nash, John
1955
$$C^1$$ isometric imbeddings. Zbl 0058.37703
Nash, John
1954
Some experimental $$n$$-person games. Zbl 0058.13904
Kalisch, G. K.; Milnor, John W.; Nash, J. F.; Nering, E. D.
1954
Two-person cooperative games. Zbl 0050.14102
Nash, John
1953
A comparison of treatments of a duopoly situation. Zbl 0050.15104
Mayberry, J. P.; Nash, J. F.; Shubik, M.
1953
Real algebraic manifolds. Zbl 0048.38501
Nash, John
1952
Non-cooperative games. Zbl 0045.08202
Nash, John
1951
Equilibrium points in $$n$$-person games. Zbl 0036.01104
Nash, John F. jun.
1950
The bargaining problem. Zbl 1202.91122
Nash, John F. jun.
1950
A simple three-person poker game. Zbl 0041.25602
Nash, J. F.; Shapley, L. S.
1950
all top 5
#### Cited by 4,345 Authors
37 Nagurney, Anna 31 Smol’yakov, Èduard Rimovich 26 Hipel, Keith William 26 Thomson, William 24 Peters, Hans J. M. 21 Kilgour, D. Marc 21 Rachmilevitch, Shiran 20 Tijs, Stef H. 18 Mavronicolas, Marios 17 Borm, Peter E. M. 17 Petrosyan, Leon Aganesovich 16 Giannoni, Fabio 16 Kaneko, Mamoru 15 Bilò, Vittorio 14 Chun, Youngsub 14 Gushchin, Anatoliĭ Konstantinovich 14 Spirakis, Paul G. 12 Anbarci, Nejat 12 Monien, Burkhard 12 Morgan, Jacqueline 12 Székelyhidi, László jun. 12 Xin, Zhouping 12 Yeung, David Wing-Kay 11 Bossert, Walter 11 Flammini, Michele 11 Larbani, Moussa 11 Moscardelli, Luca 11 Nakai, Teruhisa 10 Huang, Xiangdi 10 Karagözoğlu, Emin 10 Kim, Won Kyu 10 Kucharz, Wojciech 10 Marchi, Ezio 10 Masiello, Antonio 10 Tian, Guoqiang 10 Zhukovskiĭ, Vladislav Iosifovich 9 Chen, Gui-Qiang G. 9 Cojocaru, Monica-Gabriela 9 Gurvich, Vladimir A. 9 Kalai, Ehud 9 Kıbrıs, Özgür 9 Lisser, Abdel 9 Pang, Jong-Shi 9 Park, Sehie 9 Serrano, Roberto 9 Szidarovszky, Ferenc P. 9 Xu, Haiyan 8 Barbagallo, Annamaria 8 Cruz, José M. T. S. 8 De Jesus, Isaías Pereira 8 Epstein, Leah 8 Fang, Liping 8 Hofmann, Steve 8 Ishii, Shihoko 8 Jansen, M. J. M. 8 Khan, Mohammed Ali 8 Li, Jing 8 Owen, Guillermo 8 Robinson, Derek W. 8 Savani, Rahul 8 Singh, Vikas Vikram 8 Tang, Zhili 8 Wang, Dehua 8 Yan, Weiping 7 Ansari, Qamrul Hasan 7 Carmona, Guilherme 7 Chen, Bang-Yen 7 Clempner, Julio B. 7 Driesen, Bram 7 Fearnley, John 7 García-Jurado, Ignacio 7 Güth, Werner 7 Harsanyi, John Charles 7 Laruelle, Annick 7 Liu, Zugang 7 Mármol, Amparo María 7 Mehta, Ruta 7 Nessah, Rabia 7 Perea, Andrés 7 Périaux, Jacques F. 7 Scalzo, Vincenzo 7 Selten, Reinhard 7 Sun, Yeneng 7 Yannelis, Nicholas C. 6 Aumann, Robert John 6 Boros, Endre 6 Brandt, Felix 6 Brihaye, Thomas 6 Bruyère, Véronique 6 Capistrano, Abraão J. S. 6 Corley, H. W. jun. 6 Cruz, José B. jun. 6 de Fernex, Tommaso 6 De Lellis, Camillo 6 De Marco, Giuseppe 6 Deligkas, Argyrios 6 Dolbeault, Jean 6 Geras’kin, M. I. 6 Huang, Zhimin 6 Kassmann, Moritz ...and 4,245 more Authors
all top 5
#### Cited in 556 Serials
145 Games and Economic Behavior 132 International Journal of Game Theory 107 European Journal of Operational Research 104 Journal of Economic Theory 100 Mathematical Social Sciences 74 Theory and Decision 70 Economics Letters 68 Journal of Optimization Theory and Applications 68 International Game Theory Review 60 Journal of Mathematical Analysis and Applications 53 Journal of Differential Equations 47 Archive for Rational Mechanics and Analysis 47 Journal of Mathematical Economics 42 Theoretical Computer Science 42 Social Choice and Welfare 39 Economic Theory 38 Applied Mathematics and Computation 36 Journal of Functional Analysis 31 Nonlinear Analysis. Theory, Methods & Applications. Series A: Theory and Methods 27 Transactions of the American Mathematical Society 27 Calculus of Variations and Partial Differential Equations 24 Artificial Intelligence 24 Mathematische Annalen 23 Annals of Operations Research 22 Automatica 22 Games 21 Communications in Mathematical Physics 21 Advances in Mathematics 21 Proceedings of the American Mathematical Society 20 Annales de l’Institut Fourier 20 Communications in Partial Differential Equations 19 Annali di Matematica Pura ed Applicata. Serie Quarta 19 Computers & Operations Research 19 Journal of Global Optimization 19 Bulletin of the American Mathematical Society. New Series 19 Bulletin of the American Mathematical Society 18 Duke Mathematical Journal 18 Algorithmica 18 Journal of Theoretical Biology 17 Discrete Applied Mathematics 17 Journal of Mathematical Physics 17 The Journal of Geometric Analysis 17 Differential Equations 16 Fuzzy Sets and Systems 16 Manuscripta Mathematica 16 Optimization 16 Mathematical Programming. Series A. Series B 15 Operations Research Letters 15 Annales de l’Institut Henri Poincaré. Analyse Non Linéaire 15 Journal of Mathematical Sciences (New York) 15 Theory of Computing Systems 14 Computers & Mathematics with Applications 14 Probability Theory and Related Fields 14 Information and Computation 14 Automation and Remote Control 14 Journal de Mathématiques Pures et Appliquées. Neuvième Série 14 Potential Analysis 13 Mathematical Notes 13 Mathematische Zeitschrift 13 Journal of Information & Optimization Sciences 13 Nonlinear Analysis. Real World Applications 13 Review of Economic Design 12 Mathematical Methods of Operations Research 12 CEJOR. Central European Journal of Operations Research 12 Annali della Scuola Normale Superiore di Pisa. Scienze Fisiche e Matematiche. III. Ser 12 Dynamic Games and Applications 11 Inventiones Mathematicae 11 Journal of Soviet Mathematics 11 Journal of Economics 11 Differential Geometry and its Applications 11 Journal of Mathematical Fluid Mechanics 11 Quantum Information Processing 10 Journal of the Franklin Institute 10 Journal of Geometry and Physics 10 Journal of Computational and Applied Mathematics 10 Journal of Mathematical Psychology 10 Proceedings of the National Academy of Sciences of the United States of America 10 Mathematical Problems in Engineering 10 Doklady Mathematics 10 Optimization Letters 10 Nonlinear Analysis. Theory, Methods & Applications 9 Geometriae Dedicata 9 Insurance Mathematics & Economics 9 Journal of Economic Dynamics & Control 9 Applied Mathematics Letters 9 Cybernetics and Systems Analysis 9 Top 9 Fixed Point Theory and Applications 8 Chaos, Solitons and Fractals 8 Operations Research 8 OR Spektrum 8 SIAM Journal on Mathematical Analysis 8 Computational Optimization and Applications 8 Discrete and Continuous Dynamical Systems 8 Science China. Mathematics 8 Journal of Dynamics and Games 7 Journal of Statistical Physics 7 Mathematical Methods in the Applied Sciences 7 Nonlinearity 7 The Annals of Probability ...and 456 more Serials
all top 5
#### Cited in 61 Fields
2,095 Game theory, economics, finance, and other social and behavioral sciences (91-XX) 593 Partial differential equations (35-XX) 467 Operations research, mathematical programming (90-XX) 244 Differential geometry (53-XX) 214 Computer science (68-XX) 211 Calculus of variations and optimal control; optimization (49-XX) 188 Fluid mechanics (76-XX) 173 Global analysis, analysis on manifolds (58-XX) 124 Probability theory and stochastic processes (60-XX) 117 Operator theory (47-XX) 103 Algebraic geometry (14-XX) 74 Numerical analysis (65-XX) 72 Functional analysis (46-XX) 67 Dynamical systems and ergodic theory (37-XX) 67 Biology and other natural sciences (92-XX) 66 Systems theory; control (93-XX) 64 Manifolds and cell complexes (57-XX) 48 General topology (54-XX) 46 Combinatorics (05-XX) 46 Statistical mechanics, structure of matter (82-XX) 43 Mathematical logic and foundations (03-XX) 43 Quantum theory (81-XX) 42 Several complex variables and analytic spaces (32-XX) 41 Ordinary differential equations (34-XX) 40 Mechanics of deformable solids (74-XX) 39 Statistics (62-XX) 36 Real functions (26-XX) 36 Relativity and gravitational theory (83-XX) 32 Potential theory (31-XX) 26 Algebraic topology (55-XX) 25 History and biography (01-XX) 23 Harmonic analysis on Euclidean spaces (42-XX) 21 Convex and discrete geometry (52-XX) 21 Information and communication theory, circuits (94-XX) 17 Classical thermodynamics, heat transfer (80-XX) 16 Integral equations (45-XX) 14 Functions of a complex variable (30-XX) 13 Measure and integration (28-XX) 13 Mechanics of particles and systems (70-XX) 12 Topological groups, Lie groups (22-XX) 10 General and overarching topics; collections (00-XX) 10 Geometry (51-XX) 9 Approximations and expansions (41-XX) 8 Commutative algebra (13-XX) 8 Optics, electromagnetic theory (78-XX) 8 Geophysics (86-XX) 7 Linear and multilinear algebra; matrix theory (15-XX) 7 Difference and functional equations (39-XX) 6 Abstract harmonic analysis (43-XX) 5 Field theory and polynomials (12-XX) 5 Group theory and generalizations (20-XX) 4 Order, lattices, ordered algebraic structures (06-XX) 4 Nonassociative rings and algebras (17-XX) 4 Special functions (33-XX) 4 Astronomy and astrophysics (85-XX) 3 Number theory (11-XX) 3 Category theory; homological algebra (18-XX) 3 Integral transforms, operational calculus (44-XX) 1 Associative rings and algebras (16-XX) 1 Sequences, series, summability (40-XX) 1 Mathematics education (97-XX)
#### Wikidata Timeline
The data are displayed as stored in Wikidata under a Creative Commons CC0 License. Updates and corrections should be made in Wikidata.
| 2021-09-17T09:32:45 |
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|
http://pdglive.lbl.gov/Particle.action?node=S054&init=0
|
Quark and Lepton Compositeness, Searches for INSPIRE search
The latest unpublished results are described in the Quark and Lepton Compositeness'' review.
See related review: Searches for Quark and Lepton Compositeness
SCALE LIMITS for Contact Interactions: $\Lambda\mathrm {( {{\mathit e}} {{\mathit e}} {{\mathit e}} {{\mathit e}} )}$ $>8.3$ TeV CL=95.0%
SCALE LIMITS for Contact Interactions: $\Lambda\mathrm {( {{\mathit e}} {{\mathit e}} {{\mathit \mu}} {{\mathit \mu}} )}$
SCALE LIMITS for Contact Interactions: $\Lambda\mathrm {( {{\mathit e}} {{\mathit e}} {{\mathit \tau}} {{\mathit \tau}} )}$
SCALE LIMITS for Contact Interactions: $\Lambda\mathrm {( {{\mathit \ell}} {{\mathit \ell}} {{\mathit \ell}} {{\mathit \ell}} )}$
SCALE LIMITS for Contact Interactions: $\Lambda\mathrm {( {{\mathit e}} {{\mathit e}} {{\mathit q}} {{\mathit q}} )}$ $>24$ TeV CL=95.0%
SCALE LIMITS for Contact Interactions: $\Lambda\mathrm {( {{\mathit \mu}} {{\mathit \mu}} {{\mathit q}} {{\mathit q}} )}$ $>20$ TeV CL=95.0%
SCALE LIMITS for Contact Interactions: $\Lambda\mathrm {( {{\mathit \ell}} {{\mathit \nu}} {{\mathit \ell}} {{\mathit \nu}} )}$ $>3.10$ TeV CL=90.0%
SCALE LIMITS for Contact Interactions: $\Lambda\mathrm {( {{\mathit e}} {{\mathit \nu}} {{\mathit q}} {{\mathit q}} )}$ $>2.81$ TeV CL=95.0%
SCALE LIMITS for Contact Interactions: $\Lambda\mathrm {( {{\mathit q}} {{\mathit q}} {{\mathit q}} {{\mathit q}} )}$
SCALE LIMITS for Contact Interactions: $\Lambda\mathrm {( {{\mathit \nu}} {{\mathit \nu}} {{\mathit q}} {{\mathit q}} )}$ $>5.0$ TeV CL=95.0%
MASS LIMITS for Excited ${{\boldsymbol e}}$ (${{\boldsymbol e}^{*}}$)
Limits for Excited ${{\mathit e}}$ (${{\mathit e}^{*}}$) from Pair Production $>103.2$ GeV CL=95.0%
Limits for Excited ${{\mathit e}}$ (${{\mathit e}^{*}}$) from Single Production $>3.000 \times 10^{3}$ GeV CL=95.0%
Limits for Excited ${{\mathit e}}$ (${{\mathit e}^{*}}$) from ${{\mathit e}^{+}}$ ${{\mathit e}^{-}}$ $\rightarrow$ ${{\mathit \gamma}}{{\mathit \gamma}}$ $>356$ GeV CL=95.0%
Indirect Limits for Excited ${{\mathit e}}$ (${{\mathit e}^{*}}$)
MASS LIMITS for Excited ${{\boldsymbol \mu}}$ (${{\boldsymbol \mu}^{*}}$)
Limits for Excited ${{\mathit \mu}}$ (${{\mathit \mu}^{*}}$) from Pair Production $>103.2$ GeV CL=95.0%
Limits for Excited ${{\mathit \mu}}$ (${{\mathit \mu}^{*}}$) from Single Production $>3.000 \times 10^{3}$ GeV CL=95.0%
Indirect Limits for Excited ${{\mathit \mu}}$ (${{\mathit \mu}^{*}}$)
MASS LIMITS for Excited ${{\boldsymbol \tau}}$ (${{\boldsymbol \tau}^{*}}$)
Limits for Excited ${{\mathit \tau}}$ (${{\mathit \tau}^{*}}$) from Pair Production $>103.2$ GeV CL=95.0%
Limits for Excited ${{\mathit \tau}}$ (${{\mathit \tau}^{*}}$) from Single Production $>2.500 \times 10^{3}$ GeV CL=95.0%
MASS LIMITS for Excited Neutrino (${{\boldsymbol \nu}^{*}}$)
Limits for Excited ${{\mathit \nu}}$ (${{\mathit \nu}^{*}}$) from Pair Production $>1.600 \times 10^{3}$ GeV CL=95.0%
Limits for Excited ${{\mathit \nu}}$ (${{\mathit \nu}^{*}}$) from Single Production $> 213$ GeV CL=95.0%
MASS LIMITS for Excited ${{\boldsymbol q}}$ (${{\boldsymbol q}^{*}}$)
Limits for Excited ${{\mathit q}}$ (${{\mathit q}^{*}}$) from Pair Production $> 338$ GeV CL=95.0%
Limits for Excited ${{\mathit q}}$ (${{\mathit q}^{*}}$) from Single Production $>6.000 \times 10^{3}$ GeV CL=95.0%
MASS LIMITS for Color Sextet Quarks (${{\mathit q}_{{6}}}$) $>84$ GeV CL=95.0%
MASS LIMITS for Color Octet Charged Leptons (${{\mathit \ell}_{{8}}}$) $>86$ GeV CL=95.0%
MASS LIMITS for Color Octet Neutrinos (${{\mathit \nu}_{{8}}}$) $>110$ GeV CL=90.0%
MASS LIMITS for ${{\mathit W}_{{8}}}$ (Color Octet ${{\mathit W}}$ Boson)
| 2020-01-27T18:22:10 |
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|
https://par.nsf.gov/biblio/10205041-robust-component-robustness-measure-incorporates-access-critical-facilities-under-disruptions
|
Robust component: a robustness measure that incorporates access to critical facilities under disruptions
The objective of this paper is to integrate the post-disaster network access to critical facilities into the network robustness assessment, considering the geographical exposure of infrastructure to natural hazards. Conventional percolation modelling that uses generating function to measure network robustness fails to characterize spatial networks due to the degree correlation. In addition, the giant component alone is not sufficient to represent the performance of transportation networks in the post-disaster setting, especially in terms of the access to critical facilities (i.e. emergency services). Furthermore, the failure probability of various links in the face of different hazards needs to be encapsulated in simulation. To bridge this gap, this paper proposed the metric robust component and a probabilistic link-removal strategy to assess network robustness through a percolation-based simulation framework. A case study has been conducted on the Portland Metro road network during an M9.0 earthquake scenario. The results revealed how the number of critical facilities severely impacts network robustness. Besides, earthquake-induced failures led to a two-phase percolation transition in robustness performance. The proposed robust component metric and simulation scheme can be generalized into a wide range of scenarios, thus enabling engineers to pinpoint the impact of disastrous disruption on network robustness. This research more »
Authors:
; ; ;
Award ID(s):
Publication Date:
NSF-PAR ID:
10205041
Journal Name:
Journal of The Royal Society Interface
Volume:
16
Issue:
157
Page Range or eLocation-ID:
20190149
ISSN:
1742-5689
| 2022-08-20T05:07:20 |
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|
http://dlmf.nist.gov/16.24
|
# §16.24(i) Random Walks
Generalized hypergeometric functions and Appell functions appear in the evaluation of the so-called Watson integrals which characterize the simplest possible lattice walks. They are also potentially useful for the solution of more complicated restricted lattice walk problems, and the 3D Ising model; see Barber and Ninham (1970, pp. 147–148).
# §16.24(ii) Loop Integrals in Feynman Diagrams
Appell functions are used for the evaluation of one-loop integrals in Feynman diagrams. See Cabral-Rosetti and Sanchis-Lozano (2000).
For an extension to two-loop integrals see Moch et al. (2002).
# §16.24(iii) $3j$, $6j$, and $9j$ Symbols
The $3j$ symbols, or Clebsch–Gordan coefficients, play an important role in the decomposition of reducible representations of the rotation group into irreducible representations. They can be expressed as $\mathop{{{}_{3}F_{2}}\/}\nolimits$ functions with unit argument. The coefficients of transformations between different coupling schemes of three angular momenta are related to the Wigner $6j$ symbols. These are balanced $\mathop{{{}_{4}F_{3}}\/}\nolimits$ functions with unit argument. Lastly, special cases of the $9j$ symbols are $\mathop{{{}_{5}F_{4}}\/}\nolimits$ functions with unit argument. For further information see Chapter 34 and Varshalovich et al. (1988, §§8.2.5, 8.8, and 9.2.3).
| 2014-10-25T20:41:18 |
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|
https://gea.esac.esa.int/archive/documentation/GEDR3/Data_processing/chap_cu5pho/cu5pho_sec_specProcessing/cu5pho_ssec_specExtCalib.html
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# 5.3.5 External calibration of the spectra
Author(s): Paolo Montegriffo
As the BP/RP spectra are not published in Gaia EDR3, the detailed description of this process is postponed to the forthcoming DR3 release. However, the externally calibrated mean BP/RP spectra have been used for the calibration of the BP/RP photometry (see Section 5.4.1), hence here a short summary is given on the instrument model used to calibrate the spectra and how it was applied.
The equation that describes the formation of the dispersed image in the focal plane of the BP and RP instruments can be summarised as follow:
$n_{p}(u)=\int_{0}^{\infty}n_{p}(\lambda)\,L(u-D(\lambda),\lambda)\,R(\lambda)% \,{\rm d}\lambda$ (5.1)
where:
• $u$ defines the location in the AL reference system, this is sometimes referred to as pseudo-wavelength;
• $n_{p}(u)$ is the internally calibrated mean source spectrum in units of $e^{-}s^{-1}$;
• $n_{p}(\lambda)$ is the photon flux of the source SED expressed in units of $photons~{}s^{-1}m^{-2}nm^{-1}$;
• $L(u,\lambda)$ is the effective monochromatic Line Spread Function (LSF);
• $D(\lambda)$ is the dispersion function;
• $R(\lambda)$ is the overall instrument response function;
The LSF model is based on a linear combination of the product of two sets of basis functions modelling respectively the AL and the wavelength dependency; these bases have been derived with the Generalised Principal Component Analysis on a large set of theoretical LSFs, where also the expanded wings are taken into account, and that can also be interpolated to obtain a more continuous representation.
Pre-launch dispersion functions of the BP/RP prisms based on chief-ray analysis were derived from fitting a $6^{th}$ degree polynomial to the unperturbed EADS-Astrium Gaia optical design. For each field of view, dispersion functions are provided for the centre of each CCD in the form of the coefficients $A_{i}$ of the expansion
$AL(\omega)-AL(\omega_{ref})=\sum_{i=0}^{N}A_{i}\omega^{i},$ (5.2)
where
• $AL=AL(\omega)$ denotes the AL image position in mm (in the direction of Y axis of the Focal Plane Reference System, see Section 3.4.13),
• $\omega=1/\lambda$ in $nm^{-1}$ denotes the inverse wavelength, and
• $\omega_{ref}=1/440~{}nm^{-1}$ for BP and $1/800~{}nm^{-1}$ for RP.
The mean instrument dispersion function model has been defined as
$D(\lambda)=d_{0}+d_{1}\cdot\left[\frac{1}{P_{AL}}\sum_{i=0}^{N}A_{i}\frac{1}{% \lambda^{i}}\right]$ (5.3)
where
• $D(\lambda)$ denotes the AL image position in pixel units;
• model parameters $d_{0}$ and $d_{1}$ represent respectively the wavelength zero-point and scale: the zero-point is by construction the AL position corresponding to the reference wavelength. The default values assumed are $d_{0}=30$ and $d_{1}=1.0$ for both XP instruments.
The dispersion function is provided for both BP and RP instruments as a single csv file tabulated for wavelengths ranging from 320 nm to 1100 nm and step 0.5 nm.
The response model is built as a combination between a model for the nominal response with a parametrised cut-off and a distortion model to account for the deviations between this and the current response
$R(\lambda)=R_{Nom}(\lambda)\times R_{d}(\lambda)$ (5.4)
The nominal photonic response for XP instruments is modelled as the product of the following quantities:
$R_{Nom}(\lambda)=T_{0}(\lambda)\,\rho_{att}(\lambda)\,Q(\lambda)\,T_{p}(\lambda)$ (5.5)
where
1. 1.
$T_{0}(\lambda)$ is the telescope (mirrors) reflectivity;
2. 2.
$\rho_{att}(\lambda)$ is the attenuation due to rugosity (small-scale variations in smoothness of the surface) and molecular contamination of the mirrors;
3. 3.
$Q(\lambda)$ is the CCD QE;
4. 4.
$T_{p}(\lambda)$ is the prism (fused silica) transmittance curve which includes filter coating on their surface.
Using standard stars (see Section 5.6), it is finally possible to reconstruct the model that allows to calibrate the mean spectra: Equation 5.1 can be rewritten in a more compact form as
$n_{p}(u)=\int\limits_{0}^{\infty}\,K(u,\lambda)\cdot n_{p}(\lambda)\,{\rm d}\lambda$ (5.6)
where the kernel $K$ is a combination of LSF, dispersion and response models, and $n_{p}(\lambda)$ denotes the source SED in unit of $photon~{}s^{-1}nm^{-1}m^{-2}$.
If the source SED is expressed in some parametric form, for instance as a linear combination of basis functions, this equation could in principle be solved. However, Equation 5.6 is a Fredholm integral equation of the first kind and its solution is complicated by the fact that the problem is essentially ill-conditioned: the observed spectrum $n_{p}(u)$ is affected by noise, hence there are many solutions which satisfy exactly an integral solution slightly perturbed from the original.
To overcome this problem, the fact that the left hand term of the equation is written as a linear combination of Hermite functions $\varphi_{i}$, can be exploited and it can be demonstrated that the source SED itself can be expressed as a linear combination of a special set of basis functions $\phi_{i}$ called inverse bases obtained by solving the integral equations:
$\varphi_{i}\left(\frac{u-u_{0}}{a}\right)=\int\limits_{0}^{\infty}\,K(u,% \lambda)\cdot\phi_{i}(\lambda)\,{\rm d}\lambda$ (5.7)
where $u_{0}$ is the AL centre of the Hermite functions and $a$ is a proper scaling factor used in the mean spectra representation. The advantage of this approach is that the left hand terms of Equation 5.7 are analytic functions not affected by noise, and hence numerically stable solutions can be derived for each inverse basis.
| 2021-07-26T17:57:38 |
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|
https://www.usgs.gov/media/images/settling-tube-lab
|
Settling tube lab
Detailed Description
For some projects, scientists want to calculate sediment settling velocity and need to measure particle size using gravity. We use custom-built settling tubes filled with water – three at 2 meters tall (like the one shown here) and one 3 meters tall.
Public Domain.
| 2023-01-26T23:11:07 |
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|
https://indico.fnal.gov/event/18104/timetable/?view=standard_numbered
|
# New Technologies for Discovery IV: The 2018 CPAD Instrumentation Frontier Workshop
US/Eastern
Rhode Island Convention Center
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
Description
Organized by the Coordinating Panel for Advanced Detectors of the Division of Particles and Fields of the American Physical Society
This workshop will explore and evaluate Detector R&D opportunities, needs, and the challenges ahead for High Energy Physics in the US within the context of the P5 plan.
New ideas are particularly welcome!
Support
• Sunday, December 9
• 7:30 AM
Breakfast East Prefunction
### East Prefunction
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• 1
Registration East Prefunction
### East Prefunction
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Plenary I
Convener: Prof. Ulrich Heintz (Brown University)
• 2
Welcome
Speaker: Jill Pipher (Brown University)
• 3
Speakers: Ian Shipsey (Oxford), Marcel Demarteau (Argonne National Laboratory)
• 4
Generic Next Generation R&D
Speaker: Dr Petra Merkel (Fermi National Accelerator Laboratory)
• 5
Dark Matter
Speaker: Prof. Scott Hertel (UMass Amherst)
• 10:00 AM
Coffee Break East Prefunction
### East Prefunction
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Plenary II
Convener: Dr Zhehui Wang (Los Alamos National Laboratory)
• 6
Neutrino Physics Overview
Speaker: Prof. Sowjanya Gollapinni (University of Tennessee, Knoxville)
• 7
Pixel R&D for Neutrino Detectors
Speaker: Dr Dan Dwyer (LBNL)
• 8
Quantum Sensing
Speaker: Carlton Caves (University of New Mexico)
• 9
Early & Late Universe
Speaker: Aritoki Suzuki (LBL)
• 12:30 PM
Lunch East Prefunction, Rotunda
### East Prefunction, Rotunda
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Parallel Session: Noble Element Detectors 552A
### 552A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• 10
Micro-Pattern Gaseous Detector Technologies for Energy, Intensity and Cosmic Frontiers: an overview of the CERN-RD51 Collaboration
Driven by the availability of modern photolithographic techniques, Micro Pattern Gas Detectors (MPGD) have been introduced in the 20th century by pioneer developments: Microstrip Gas Chambers (MSGC), Gas Electron Multipliers (GEM), Micro-mesh gaseous structure (Micromegas), followed by the thick-GEM (THGEM), resistive GEM (RETGEM), Micro-Pixel Gas Chamber (μ-PIC), and an integrated readout of gaseous detectors using solid-state pixel chips (InGrid). Nowadays, intensive R&D activities in the field of MPGDs and their diversified applications are pursued by the large CERN-RD51 collaboration. The aims are to facilitate the development of advanced gas-avalanche detector concepts and technologies and associated electronic-readout systems, for applications in basic and applied research. MPGD systems now offer robustness, very high rate operation, high precision spatial resolution (sub 100-micron), and protection against discharges. MPGDs became important instruments in current particle-physics experiments and are in development and design stages for future ones. They are significant components of the upgrade plans for ATLAS, CMS, and ALICE at the LHC, exemplifying the beneficial transfer of detector technologies to industry. Beyond their design for experiments at future facilities (e.g. FAIR, EIC, ILC, FCC), MPGDs are considered for rare-event searches, e.g. dark matter, double beta decay and neutrino scattering experiments. Detectors sensitive to x-rays, neutrons and light are finding applications in other diverse areas as material sciences, hadron therapy systems, homeland security etc. Since its early stages, the RD51 collaboration has paid attention to building a proper environment for performing high-quality advanced R&D on MPGDs; it continues to advance the MPGD domain with scientific, technological, and educational initiatives. It is a worldwide open scientific and technological forum on MPGDs, and RD51 has invested resources during ten years in forming expertise, organizing common infrastructure and developing common research tools. Originally created for a five-year term in 2008, RD51 was recently prolonged for a third consecutive five years term beyond 2018 (arXiv: 1806.09955). This talk will highlight recent MPGD technology advances, review RD51 collaboration activities, and address numerous MPGD applications at the Energy, Intensity and Cosmic Frontiers.
Speaker: Dr Maxim Titov (CEA Saclay)
• 11
NEXt
Speaker: Dr Justo Martín-Albo (Harvard University)
• 12
Dual-Phase LArTPC R&D for neutrino physics
The Dual-Phase Liquid Argon Time Projection Chamber (LArTPC) aims to open new windows of opportunity in the study of neutrinos. Dual-phase LArTPCs are one of the far detector technology options foreseen for the Deep Underground Neutrino Experiment (DUNE) at Fermilab. Dual Phase (DP) refers to the extraction of ionization electrons at the interface between liquid and gaseous argon and their amplification and collection in the gas phase. Recently, there are lots of ongoing R&D activities on Dual-Phase degin, namely 3x1x1 m3 pilot detector and protoDUNE-DP LArTPC detector at CERN. protoDUNE-DP will be operating at the CERN neutrino platform. It not only serves as the engineering prototype of the FD, but will also demonstrate the concept of a very large dual-phase LAr TPC and calibrate it with charged particle test beam. We will briefly discuss design, installation and status of the protoDUNE Dual-Phase detector at CERN.
Speaker: Dr Animesh Chatterjee (University of Texas at Arlington)
• 13
Recent results from R&D for the nEXO experiment
nEXO is a next-generation experiment to search for neutrinoless double beta decay ($0\nu\beta\beta$). The nEXO detector will consist of a homogeneous time projection chamber (TPC) filled with 5 tonnes of liquid xenon enriched to 90% $^{136}$Xe. nEXO is projected to reach a $0\nu\beta\beta$ half life sensitivity of $\sim$$10^{28}$ years, which will provide a search for lepton number violating processes with more than 2 orders of magnitude higher sensitivity than existing experiments. To reach these goals, the nEXO collaboration is engaged in R&D to develop novel charge and light sensors, cold in-LXe electronics and high-bandwidth readouts with ultra-low radioactivity, and optimized high-voltage designs for a large TPC. Recent results from this R&D demonstrating key requirements for the nEXO design will be discussed.
Speaker: Prof. David Moore (Yale University)
• Parallel Session: Photodetectors 553A
### 553A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• 14
Scaled Superconducting Nanowire Detectors in Photonic Circuits
I will report on our recent progresses on developing scaled superconducting single photon detectors embedded in integrated photonic circuits. Yale’s waveguide SSPD design utilizes the concept of evanescent complete absorption of light by a nanowire fabricated atop a waveguide (Fig.1). It overcomes the tradeoff between detection efficiency and speed in conventional meander SSPD designs [1,2]. These traveling wave micro-SSPDs can absorb 99% of the incoming light within 10m-long optical waveguide and have an order of magnitude less kinetic inductance than conventional meander wire detectors. Therefore, they simultaneously achieve high detection efficiency and high speed, and exhibit excellent detection performance: on-chip quantum efficiency, timing jitter, dark count, intrinsic bandwidth and high scalability. Our circuit-detector approach is fully compatible with scalable, high-yield semiconductor microfabrication processes. We further show that a large grid of individually addressable micro-SSPD can be fully integrated on a single chip, with each detector element integrated into independent waveguide circuit with custom functionality.[3,4] Such a detector array can be utilized for demonstrating quantum interference of single photons on a silicon photonic chip.[5] Further exploitation of the hybrid photonic and superconducting detector circuits also lead to the realization of on-chip single photon spectrometer with high channel capacity.
Speaker: Prof. Hong Tang (Yale University)
• 15
CMOS single photon detector
Speakers: Dakota Starkey (Dartmouth College), Eric Fossum (Dartmouth College)
• 16
Novel quantum and bio-inspired designs for photodetection
Photodetection plays a key role in basic science and technology, with exquisite performance having been achieved down to the single photon level. Further improvements in photodetectors would open new possibilities across a broad range of scientific disciplines, and enable new types of applications. However, it is still unclear what is possible in terms of ultimate performance, and what properties are needed for a photodetector to achieve such performance. In this presentation, I will discuss recent theoretical and experimental work to address this question. On the theoretical front, we present a new general framework to establish the fundamental properties of photodetectors from a fully quantum perspective, and show what basic features are needed to achieve high performance. Novel photodetector designs emerge from these considerations, and we present initial experiments to test these new designs. Interestingly, some of the new photodetector features are similar to those found in the human visual system.
Speaker: Dr Francois Leonard (Sandia National Laboratories)
• 17
Developing Charged Particle Time-of-Flight at the Fermilab Test Beam Facility Using Commercially Produced LAPPD modules
The rst commercially-produced LAPPDTM photodetectors[1] are now available from Incom, Inc[2]. An informal collaboration of Fermilab, Incom, and the University of Chicago (UofC) has been developing plans to optimize the timing resolution and to characterize the performance and life-time of several of the newly available Incom modules at the Fermilab Testbeam Facility . These modules will contain the entire beam prole. If successful this could lead to an upgrade of the Fermilab Testbeam Facility Time of Flightsystem to four stations of LAPPDs for particle ID. The goals are thus two-fold: 1) a substantial upgrade to particle identication at the Fermilab Test Beam Facility; and 2) a validation of a new commercially-available technology for future detectors at the Energy and Luminosity Frontiers. System designs for one, two, and four LAPPD modules and expected TOF performance will be discussed.
Speaker: Prof. Henry Frisch (University of Chicago)
• Parallel Session: Superconducting Detectors
Conveners: Dr John Mates (University of Colorado, Boulder), Dr Peter Barry (ANL), Dr Sherry Cho (SLAC)
• 18
Searching for 10meV-1GeV Dark Matter with Athermal Phonon Detectors
Speaker: Dr matt pyle (University of California Berkeley)
• 19
DM Radio: An Optimized Search for Axion and Hidden-Photon Dark Matter
Speaker: Mr Saptarshi Chaudhuri (Stanford University Department of Physics)
• 20
A scalable and experimentally verifiable photonic apparatus for dark photon detection with superconducting nanowire devices
Speaker: Jeffrey Chiles (NIST)
• 21
Development of Cryogenic Light Detectors for CUPID using an Ir/Pt transition edge sensor
• 3:30 PM
Coffee Break East Prefunction
### East Prefunction
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Parallel Session: Computing & Machine Learning
Conveners: Dr Oliver Gutsche (Fermi National Accelerator Laboratory), Sergei Gleyzer (University of Florida), Taritree Wongjirad (MIT)
• 22
QUBO for Track Reconstruction on D-Wave
D-Wave Systems Quantum Annealer (QA) finds the ground state of a Hamiltonian expressed as: $O(a;b;q)=\sum_{i=1}^N{a_i q_i} +\sum_{i}^N\sum_{j < i}^N{b_{ij} q_i q_j}$ This Quantum Machine Instruction (QMI) is equivalent to a Quadratic Unconstrained Binary Optimization (QUBO) and can be transformed easily into an Ising model or a Hopfield network. Following Stimpfl-Abele [“Fast track finding with neural network”](https://www.sciencedirect.com/science/article/pii/001046559190048P), we expressed the problem of classifying track seeds (doublets and triplets) as a QUBO, where the weights depend on physical properties such as the curvature, 3D orientation, and length. We generated QUBOs that encode the pattern recognition problem at the LHC using the [TrackML dataset](https://www.kaggle.com/c/trackml-particle-identification) and solved them using [qbsolv](https://www.dwavesys.com/sites/default/files/partitioning_QUBOs_for_quantum_acceleration-2.pdf) and the [D-Wave Leap Cloud Service](https://cloud.dwavesys.com/leap/). Those early experiments achieved a performance in terms of purity, efficiency, and TrackML score that exceeds 95%. Our goal is to develop a strategy appropriate for HL-LHC track densities by using techniques including improved seeding algorithms and geographic partitioning. We also plan to refine our model in order to reduce execution time and to boost performance.
Speaker: Ms Lucy Linder (Lawrence Berkeley National Lab)
• 23
Identification of Double-Beta Decay Events in a Large Liquid Scintillator Detector
I will discuss application of machine learning techniques for identification of a two-track single-vertex event topology of double-beta decay events in a liquid scintillator detector. Event topologies of background events differ in number of tracks and/or in number of verticies and, in some cases, by relative timing of secondary particles. These topological differences between signal and backgrounds are "encoded" in an ensemble of scintillation and Cherenkov photons created in each event. Using a simulation of a 6.5-meters radius liquid scintillator detector I will show performance of various event classification techniques that utilize differences in timing and spatial distributions of detected photo-electrons. Continuing development in photo-detection techniques suggests that increasingly precise characterization of individual photons may be possible at future experiments. I will discuss what are possible implications for event reconstruction techniques that come along with precision photon characterization.
Speaker: Andrey Elagin (University of Chicago)
• 24
End-to-end particle and event identification for regular and boosted topologies at the Large Hadron Collider
From heavy flavour jet identification to the discovery of the Higgs boson, machine learning algorithms have become an increasingly important tool for physics analysis and event reconstruction at the Large Hadron Collider (LHC). We present an innovative approach to particle and event reconstruction at the LHC, called end-to-end deep learning, that combines modern deep learning algorithms with low-level detector representation. Using two physics examples as references: quark and gluon discrimination and boosted top quark tagging, we demonstrate the performance of the end-to-end approach using CMS Open Data. We also offer insights into the role of various sub-detectors and describe how end-to-end techniques can be useful for event-level classification.
Speaker: Dr Emanuele Usai (Brown University)
• 25
Data Reconstruction Using Deep Neural Network for Liquid Argon Time Projection Chambers
Liquid Argon Time Projection Chambers (LArTPCs) are capable of recording images of charged particle tracks with breathtaking resolution. Such detailed information will allow LArTPCs to perform accurate particle identification and calorimetry, making it the detector of choice for many current and future neutrino experiments. However, analyzing such images can be challenging, requiring the development of many algorithms to identify and assemble features of the events in order to reconstruct neutrino interactions. In the recent years, we have been investigating a new approach using deep neural networks (DNNs), a modern solution to a pattern recognition for image-like data in the field of Computer Vision. A modern DNN can be applied for various types of problems such as data reconstruction tasks including interaction vertex finding, pixel clustering, and particle/topology type identification. We have developed a small inter-experiment collaboration to share generic software tools and algorithms development effort that can be applied to non-LArTPC imaging detectors. In this talk I will discuss the challenges of LArTPC data reconstruction, recent work and future plans for developing a full LArTPC data reconstruction chain using DNNs.
Speaker: Dr Kazuhiro Terao (SLAC National Accelerator Laboratory)
• Parallel Session: Photodetectors
Conveners: Adam Para (Fermilab), Prof. Lindley Winslow (MIT), Lindley Winslow (UCLA), Zongfu Yu
• 26
The Snowball Chamber: Neutron-Induced Nucleation in Supercooled Water
The cloud and bubble chambers have been used historically for particle detection, capitalizing on supersaturation and superheating respectively. We now present the snowball chamber, which utilizes supercooled liquid. In our prototype, an incoming particle triggers crystallization of purified water. We demonstrate that water is supercooled for a significantly shorter time with respect to control data in the presence of AmBe and 252Cf neutron sources. A greater number of multiple nucleation sites are observed as well in neutron calibration data, as in a PICO-style bubble chamber. Similarly, gamma calibration data indicate a high degree of insensitivity to electron recoils inducing the phase transition, making this detector potentially ideal for dark matter searches seeking nuclear recoil alone. We will explore the possibility of using this new technology for WIMP and low-mass dark matter searches.
Speaker: Dr Matthew Szydagi (University of Albany)
• 27
Calorimeters for particle physics experiments with integration time of a few ns will substantially improve the capability of the experiment to resolve event pileup and to reject backgrounds. In this paper the time development of hadronic showers induced by 30 and 60 GeV positive pions and 120 GeV protons is studied using Monte Carlo simulation and beam tests with a prototype of a sampling steel-scintillator hadronic calorimeter. In the beam tests, scintillator signals induced by hadronic showers in steel are sampled with a period of 0.2 ns and precisely time-aligned in order to study the average signal waveform at various locations with respect to the beam particle impact. Simulations of the same setup are performed using the MARS15 code. Both simulation and test beam results suggest that energy deposition in steel calorimeters develop over a time shorter than 2 ns providing opportunity for ultra-fast calorimetry. Simulation results for an "ideal" calorimeter consisting exclusively of bulk tungsten or copper are presented to establish the lower limit of the signal integration window.
Speaker: Dmitri Denisov (Fermilab)
• 28
Ultrafast Radiation Hard Inorganic Scintillators for Future HEP Experiments
In high energy physics (HEP) and nuclear physics (NP) experiments, total absorption electromagnetic calorimeters (ECAL) made of inorganic crystals are known for their superb energy resolution and detection efficiency for photon and electron measurements. A crystal ECAL is thus the choice for those experiments where precision measurements of photons and electrons are crucial for their physics missions. Future HEP experiments at the energy and intensity frontiers require ultrafast inorganic crystal scintillators to achieve excellent timing resolution at a level of a few tens ps and to face the challenge of unprecedented event rate. Very fast inorganic crystals may also find application for Gigahertz hard X-ray imaging. We report recent progress in ultrafast and fast inorganic scintillators in HEP experiments, such as a thin LYSO crystal layer for fast timing for the CMS experiment upgrade at the HL-LHC, and undoped CsI and yttrium doped BaF2 crystals for the Mu2e experiment and its upgrade at Fermilab. Applications of ultrafast inorganic scintillators for Gigahertz hard X-ray imaging for the proposed Marie project at LANL will also be discussed.
Speaker: Dr Ren-yuan Zhu (Caltech)
• 29
Wavelength Shifting Liquid-Filled Capillaries for Optical Electromagnetic Calorimetry Applications
WLS Capillaries are being developed for optical calorimetry applications, and particularly for sampling calorimetry configurations. The WLS dyes can be tailored appropriately to provide wave shifting for various scintillation materials. Fabricated from radiation hard quartz, these elements are capable of withstanding high radiation doses and could be used broadly for EM applications in fixed target and colliding beam experiments. Structure fabrication, optical characteristics and measurements of the behavior of these structures under gamma irradiation in doses up to 150Mrad will be presented.
Speaker: Prof. Randy Ruchti (University of Notre Dame and National Science Foundation)
• Parallel Session: Quantum Sensors 553A
### 553A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• 30
Optical clocks
Speaker: Ross Hutson (JILA)
• 31
Spin squeezing
Speaker: Graham Greeve (JILA)
• 32
Precision measurement with atomic clocks
Speaker: Prof. Shimon Kolkowitz (University of Wisconsin - Madison)
• 33
Quantum sensing with large 2D crystals of trapped ions
We trap and control 2D arrays of hundreds of ions and can measure nV/m and yN scale electric fields and forces. Our technique relies on coupling the motional and spin degrees of freedom, allowing us to sensitively measure the motion of the ion crystal by reading out the spin-state of the ions.
• Parallel Session: Superconducting Detectors
Conveners: Dr John Mates (University of Colorado, Boulder), Dr Peter Barry (ANL), Dr Sherry Cho (SLAC)
• 34
Superconducting Detectors for Precision Cosmology
Speaker: Dr Jason Austermann (NIST-Boulder / CU-Boulder)
• 35
SPT-3G: The Third-generation Camera on the South Pole Telescope
In January of 2017, the South Pole Telescope (SPT) was upgraded with the new SPT-3G camera to better observe the cosmic microwave background. The SPT-3G camera consists of 16,200 superconducting transition edge sensor (TES) bolometers, a factor of ten increase over the previously installed SPTpol camera. The bolometers are contained in 2710 tri-chroic pixels, with each pixel simultaneously measuring two orthogonal linear polarizations in frequency bands centered at 95, 150, and 220 GHz. The upgrade to the SPT-3G camera also included the replacement of the secondary optics, the installation of a new larger receiver, and the deployment of the newly developed readout electronics. I will discuss the technology of SPT-3G and its current status.
Speaker: Dr Tyler Natoli (University of Chicago)
• 36
Development of Antenna-Coupled Lumped-Element KID for CMB Observations
Kinetic Inductance Detectors (KIDs) have become an attractive choice of detector in the sub-mm and mm observing community due to their innate frequency multiplexing capabilities and simple lithographic processes. These advantages make KIDs a viable option for the $O(500,000)$ detectors needed for the next generation CMB experiments, such as Cosmic Microwave Background - Stage 4 (CMB-S4) experiment. We developed a novel design of an antenna-coupled lumped element KID design optimized for CMB detection. Light is focused via alumina lenses to polarization-sensitive dual-slot antennae. A Nb/SiN/Nb microstrip line carries the signal to an Al/Nb KID. We present the design, fabrication process, and preliminary performance of a prototype array, and comment on the current status and future plans of this design.
Speaker: Ms Qing Yang Tang (University of Chicago)
• 37
Status of SuperSpec, the On-Chip Spectrometer
SuperSpec is a new technology for millimeter and submillimeter spectroscopy. It is an on-chip spectrometer being developed for multi-object, moderate resolution (R = ~300), large bandwidth survey spectroscopy of high-redshift galaxies for the 1 mm atmospheric window. SuperSpec targets the CO ladder in the redshift range of z = 0 to 4, the [CII] 158 um line from z = 5 to 9, and the [NII] 205 um line from z = 3.5-7. All together these lines offer complete redshift coverage from z = 0 to 9. SuperSpec employs a novel architecture in which detectors are coupled to a series of resonant filters along a single microwave feedline instead of using dispersive optics. This construction allows for the creation of a full spectrometer occupying only 20 cm squared of silicon, a reduction in size of several orders of magnitude when compared to standard grating spectrometers. This small profile enables the production of future multi-object spectroscopic instruments required as the millimeter-wave spectroscopy field matures. SuperSpec uses a lens-coupled antenna to deliver astrophysical radiation to a microstrip transmission line. The radiation then propagates down this transmission line where upon proximity coupled half wavelength microstrip resonators pick off specific frequencies of radiation. Careful tuning of the proximity of the resonators to the feedline dials in the desired resolving power of the SuperSpec filterbank by tuning the coupling quality factor. The half wavelength resonators are then in turn coupled to the inductive meander of superconducting kinetic inductance detectors (KIDs), which serve as the power detectors for the SuperSpec filterbank. Each SuperSpec filter bank contains hundreds of titanium nitride TiN KIDs and the natural multiplexibility of these detectors allow for readout of the large numbers of required detectors. The unique coupling scheme employed by SuperSpec allows for the creation of incredibly low volume (2.6 cubic microns), high responsivity, TiN KIDs. Since responsivity is proportional to the inverse of quasiparticle-occupied volume, this allows SuperSpec to reach the low NEPs required by moderate resolution spectroscopy to be photon limited from the best ground-based observing sites. We will present the latest results from SuperSpec devices. In particular, detector NEPs, measured filter bank efficiency (including transmission line losses), and spectral profiles. In addition, we will present our developments toward a SuperSpec on-sky demonstration instrument for deployment on the Large Millimeter Telescope.
Speaker: Mr Jordan Wheeler (University of Colorado Boulder)
• 6:00 PM
Reception Rotunda
• 38
### 553A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Monday, December 10
• 7:30 AM
Breakfast East Prefunction
### East Prefunction
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Plenary III
Convener: Dr Petra Merkel (Fermi National Accelerator Laboratory)
• 39
Electron Ion Collider
Speaker: Thomas Ulrich (Brookhaven National Laboratory)
• 40
Energy Frontier
Speaker: Prof. Meenakshi Narain (Brown University)
• 41
Triggering Challenges at the Energy Frontier
Speaker: Dr Isabel Ojalvo (Princeton)
• 42
FPGA-accelerated machine learning inference as a solution for particle physics computing challenges
Resources required for high-throughput computing in large-scale particle physics experiments face challenging demands both now and in the future. The growing exploration of machine learning algorithms in particle physics offers new solutions to simulation, reconstruction, and analysis. These new machine learning solutions often lead to increased parallelization and faster reconstructions times on dedicated hardware, here specifically Field Programmable Gate Arrays. We explore the possibility that applications of machine learning simultaneously also solve the increasing computing challenges. Employing machine learning acceleration as a web service, we demonstrate a heterogeneous compute solution for particle physics experiments that requires minimal modification to the current computing model. First results with Project Brainwave by Microsoft Azure, using the Resnet-50 image classification model as an example, demonstrate inference times of approximately 50 (10) milliseconds with our experimental physics software framework using Brainwave as a cloud (edge) service. We also adapt the image classifier, for example, physics applications using transfer learning: jet identification in the CMS experiment and event classification in the Nova neutrino experiment at Fermilab. Solutions explored here are potentially applicable sooner than may have been initially realized.
Speaker: Dr Mia Liu (fermilab)
• 10:00 AM
Coffee Break East Prefunction
### East Prefunction
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Parallel Session: Photodetectors
• 43
Superconducting single photon detection
Speaker: Karl Bergren
• 44
Capacitively Coupled Single Photon Detectors: From Classical to Quantum Mechanical Devices
In recent years, the development of Si CMOS quanta image sensors (QIS) has enabled room-temperature, non-avalanche photon counting in the visible spectrum regime by transferring a photoelectron to a tiny capacitor (C~400 aF), thereby inducing a readable voltage change on the order of 0.4 mV using correlated double sampling method. These non-avalanche single photon detectors (SPDs), based on capacitive coupling, greatly benefit from the CMOS scaling and may inspire new ways of envisioning/optimizing electronic-photonic integration on Si. This talk will focus on two aspects: (1) Extending the spectral response of QIS devices (based on classical capacitive coupling) to infrared and ultraviolet regime. Different schemes of spectral extension will be discussed, including hot-electron devices and GeSn nanodots integrated with Si QIS readout methods. (2) Leaping from classical to quantum mechanical capacitive coupling to minimize the timing jitter and maximize the bandwidth of the non-avalanche SPDs. In these quantum capacitive photodetectors, the absorption of a single photon changes the wave function of a single electron trapped in a quantum dot(QD), leading to a charge density redistribution nearby. This redistribution translates into a voltage signal through capacitive coupling between the QD and the measurement probe or a nanoscale MOS gate. Using InAs QD/AlAs barrier as a model system, the simulation shows that the output signal reaches ~4 mV per absorbed photon, promising for high-sensitivity, sub-ps single-photon detection. We will also discuss the fundamental limits and advantages of capacitively coupled photodetectors over avalanche photodetectors in single photon detection and photon counting.
Speaker: Prof. Jifeng Liu (Dartmouth College)
• 45
Status update on Large Area Picosecond Photo-Detectors – LAPPD
The Large Area Picosecond Photo-Detector (LAPPD™) is a microchannel plate (MCP) based planar geometry photodetector featuring single-photon sensitivity, semitransparent bi-alkali photocathode, millimeter spatial and picosecond temporal resolutions and an active area of to 350 square centimeters. The “baseline” LAPPD™ employs a borosilicate float glass hermetic package. Photoelectrons are amplified with a stacked chevron pair of “next generation” large area MCPs produced by applying resistive and emissive Atomic Layer Deposition (ALD) coatings to glass capillary array (GCA) substrates. Signals are collected on microstrip anodes applied to the bottom plate. We report performance results achieved for fully functional sealed LAPPDs™. These results include electron gains of up to 107, low dark noise rates (15-30 Hz/cm2), single photoelectron (PE) timing resolution of 64 picoseconds RMS (electronics limited), and single photoelectron spatial resolution along and across strips of 2.4 mm and 0.8 mm RMS respectively and high (up to 25%) QE uniform bi-alkali photocathodes. While not fully optimized, these tiles are usable for applications by early adopters. Optimized LAPPDs can be employed in neutrino experiments (e.g. ANNIE, WATCHMAN, DUNE), particle collider experiments (e.g. EIC), neutrinoless double-beta decay experiments (e.g. THEIA), medical and nuclear non-proliferation applications. We will also discuss future prospects of the project and new developments in LAPPDs.
Speaker: Dr Alexey Lyashenko (Incom Inc.)
• 46
Development of fast-timing MCP-PMT/LAPPD for particle identification
Particle IDentification (PID) is fundamental to nuclear and particle physics experiments. Fast-timing MCP-PMTs are ideal candidate for PID sensors if the price is affordable. We report detailed design, fabrication and characterization of Argonne 6 × 6 cm$^2$ fast timing photodetectors based on next-generation microchannel plates (MCP). The whole assembly is made of low-cost borosilicate glass materials and hermetically sealed with a bialkali photocathode in a vacuum. The flexible photodetector design provides the potential of modifying individual components as well as the entire configuration to fit for different applications. Recently, low-cost, large area pico-second photodetector (LAPPD$^{TM}$), which shares the similar design as Argonne MCP-PMT was successfully commercialized by our collaborator Incom, Inc. Efforts were devoted to modify the standard configuration of the LAPPD$^{TM}$, and to validate the performance on Argonne 6 × 6 cm$^2$ MCP-PMTs. Experiment results show great improvement of the detector’s timing resolution and magnetic field tolerance, providing strong potential for PID applications. Results on high voltage, magnetic field strength and angle dependence will be presented in detail.
Speaker: Dr Junqi Xie (ANL)
• Parallel Session: Silicon Detectors 552A
### 552A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• 47
Pixel Sensors with Engineered Substates for Time and Space Resolution and Radiation Hardness
Future Particle Physics experiments will require detectors with increasingly precise spatial and time resolution. These issues are currently being addressed separately by Low Gain Avalanche Diodes (LGADs) and hybrid or CMOS pixel detectors. We will discuss how engineered silicon substrates, with doped epitaxial layers combined with AC coupling of the anode implant, can be used to produce radiation hard LGADs with high fill factor and arbitrary pixel geometries. We will also describe how small pixels enabled by 3D sensor/electronics integration can be utilized for both fast timing and event topology discrimination in thick or thin silicon detectors.
Speaker: Dr Ron Lipton (Fermilab)
• 48
3D sensors for charged particle tracking
Speaker: Julie Segal (Stanford)
• 49
Monolithic sensors for high energy physics
Speaker: Petra Riedler
• 50
Timing with Solid State Detectors
Speaker: Bruce Schumm
• Parallel Session: Superconducting Detectors
Conveners: Dr John Mates (University of Colorado, Boulder), Dr Peter Barry (ANL), Dr Sherry Cho (SLAC)
• 51
Towards the Next Generation of Frequency-Multiplexed TES Readout
TES bolometers have emerged as a very successful technology in part thanks to their exquisite sensitivity and ability to be fabricated in large monolithic arrays. O(10^6) TES bolometers are planned to be deployed in the 2020s for the cosmic microwave experiment CMB-S4, which will require advances in readout technology. Frequency-multiplexed (fMux) readout has been demonstrated to great success with an O(10) multiplexing factor, and is currently also operating successfully at a multiplexing factor of 68 on SPT-3G. We are developing a series of improvements that will greatly simplify the fMux readout architecture, improve performance, and increase the multiplexing factor. I will present results on several advances that include lossless bias generation and moving of the 4K SQUID amplifier to the sub-Kelvin stage.
Speaker: Dr Tijmen de Haan (LBNL)
• 52
Microwave SQUID multiplexing for high-energy physics experiments
Speaker: Doug Bennett (NIST)
• 53
Highly-multiplexed microwave SQUID readout using the SLAC Microresonator Radio Frequency (SMuRF) Electronics for Future CMB and Sub-millimeter Surveys
Speaker: Dr Shawn Henderson (SLAC National Accelerator Laboratory)
• 54
Microwave-multiplexed TES (uMUX) and Kinetic Inductance Detectors (KID) continue to have success in deployed instruments, and are being built in larger and larger arrays. Corresponding improvements in room temperature readout electronics are needed to keep pace with increasing multiplexing factors, as well as manage the power requirements and system complexity associated with the ever increasing total detector count in future instruments. In this talk, I review early work evaluating the commercially-available Xilinx RFSoC development board for use in uMUX/KID readout. This system integrates RF synthesis and sampling, an FPGA for signal processing, and a CPU for housekeeping tasks, all into a single chip. This results in significantly lower electrical power requirements than other solutions, which has the potential to reduce system complexity in ground-based installation, and significantly increases the potential for (sub-)orbital and space use.
Speaker: Dr Sean Bryan (Arizona State University)
• 12:30 PM
Lunch East Prefunction
### East Prefunction
• QIS Discussion
Convener: Prof. Meenakshi Narain (Brown University)
• 55
QIS Discussion
Speakers: Dr Helmut Marsiske (Office of High Energy Physics, U.S. Department of Energy), Prof. Randal Ruchti (National Science Foundation)
• Parallel Session: Computing & Machine Learning
Conveners: Dr Oliver Gutsche (Fermi National Accelerator Laboratory), Sergei Gleyzer (University of Florida), Taritree Wongjirad (MIT)
• 56
Tracker layout and track reconstruction synergy in collider environment with high pileup
Leading planned or considered hadron colliders are expected to produce data in collisions with average number of simultaneous interactions per beam bunch crossing of several hundred. These include both the high luminosity LHC upgrade currently in preparation and the possible high energy LHC upgrade as well as a future circular collider FCC-hh. Execution of charged particle track reconstruction for the general purpose detectors at these colliders is expected to be at least comparable in cost to the construction and operation of the tracking detectors. We show that the sensitive layer layout in the design of a tracking detector can play a vital role to reduce complexity and cost of the charged particle track reconstruction. Our case study is based on realistic simulation of a tracking detector similar to that of CMS to be operated in HL-LHC. We show that a typical layout with roughly equidistant layer separation is inferior to that with grouped layers with a smaller distance within a group, which allows for more performant track segment reconstruction. This synergy between the hardware and software choice can allow for a reduction of the total cost of a future collider experiment.
Speaker: Vyacheslav Krutelyov
• 57
Evaluation and Development of Algorithms and Techniques for Streaming Detector Readout
Experiments in Nuclear Physics (NP) have unique requirements on their data acquisition and computing due to the multiple channel and multi-dimensional challenges in their measurements. While there have been remarkable advances in microelectronics capabilities, computing, and data science over the last decade, the research model of NP has not changed for many decades. With the start of the 12 GeV program and the ongoing design of the Electron-Ion Collider in mind, we would like find out if the technological advantages of the last decade can fundamentally improve the research model of NP. We propose an exploratory study on three levels: 1. Rethinking the way measurements are compared to theory and would like to examine the capabilities of an event level analysis taking the multi-dimensional correlations in the data fully into account. 2. Rethinking the way experimental data are handled and would like to identify ways to speed up the analysis of the data in the context of an event level analysis. 3. Rethinking the way we read detectors and assemble the detector data into events and would like to investigate the capabilities of streaming readout in view of an event level analysis. Specifically, we prototype components of streaming readout and explore appropriate associated data models. The data model also must be appropriate for processing-intensive analyses of multi-dimensional correlations in NP data. Our development is done in such a way as to a) evaluate and quantify the possibilities and limitations of this approach with current hardware/software and identify where further developments are needed b) produce a prototype tool kit of hardware and software solutions that could be applied separately and in the short-term at Jefferson Lab and elsewhere.
Speaker: Dr Markus Diefenthaler (Jefferson Lab)
• 58
DNN based algorithm for CMS Level-1 muon reconstruction
In order to preserve its ability to do physics at the electroweak scale in the HL-LHC era, CMS experiment has to maintain low trigger thresholds that are robust against high intensity and large number of interactions per bunch crossing expected at the HL-LHC. Specifically, the muon trigger transverse momentum (pT) thresholds currently used cannot be maintained at the HL-LHC without improving the reconstruction algorithms and incorporating additional information into the L1 muon reconstruction. The biggest challenge in L1 muon reconstruction is the ability to have highly accurate determination of the muon pT in order to prevent lower transverse momentum muons, below the desired threshold, from saturating the trigger rate. We present studies of an alternative novel technique to improve L1 muon momentum resolution using advanced Machine Learning algorithms executed in FPGAs. The presentation will include simulation based studies to quantify performance improvements and bottlenecks of such a technique as well as a preliminary implementation of firmware with the goal of estimating required resources and latency.
Speaker: Jia Low (University of Florida)
• 59
Deep Machine Learning on FPGAs for L1 trigger and Data Acquisition
Machine learning is becoming ubiquitous across HEP. There is great potential to improve trigger and DAQ performances with it. However, the exploration of such techniques within the field in low latency/power FPGAs has just begun. We present HLS4ML, a user-friendly software, based on High-Level Synthesis (HLS), designed to deploy network architectures on FPGAs. As a case study, we use HLS4ML for boosted-jet tagging with deep networks at the LHC. We map out resource usage and latency versus network architectures, to identify the typical problem complexity that HLS4ML could deal with. We discuss possible applications in current and future HEP experiments.
Speaker: Dylan Rankin (MIT)
• Parallel Session: Noble Element Detectors
Convener: David Moore (Stanford University)
• 60
Q-Pix: Pixel-scale Signal Capture For Kiloton Liquid Argon TPC Detectors: Charge-Quantized Waveform Capture, Free-running Clocks, Dynamic Networks
We describe a novel ionization signal capture and waveform digitization scheme for kiloton-scale liquid argon Time Projection Chamber (TPC) detectors. The scheme is based on a pixel-scale self-triggering ‘charge integrate/reset’ block, free-running local clocks and dynamically established data networks. The scheme facilitates detailed capture of waveforms of arbitrary complexity from a sequence of varying time intervals, each of which corresponds to a fixed charge integral. An absolute charge auto-calibration process based on intrinsic 39Ar decay current is a major benefit. A flat electronic architecture with self-guided network generation provides very high resilience against single-point failure. The goal is optimized discovery potential. Much might be at stake.
Speaker: Dr Yuan Mei (LBNL)
• 61
Xenon doping of Liquid Argon for astroparticle detectors
Liquid Argon (LAr) has a widespread use in astroparticle experiments dedicated to neutrino studies and Dark Matter searches. LAr scintillation light is produced in the far Ultraviolet (128 nm), posing technical challenges for collection and detection. While there are available multiple technologies for this task, already tested and well functioning, new solutions are being searched for. An interesting possibility is to dope LAr with Xenon. Ar excitation can be passed to Xenon, which also emits light at larger $\lambda$=175 nm. Xe photons can be detected more easily than Argon ones, and they bring other advantages, like larger Rayleigh scattering length, and increased yield. These characteristics can significantly impact detection capabilities for large volume LAr-TPC neutrino experiments. My talk will review present knowledge; recent tests, including those performed at CERN in the framework of the CERN Neutrino Platform, and an outlook for future use in the DUNE far detectors.
Speaker: Andrea Zani (CERN)
• 62
Results of high voltage breakdown studies in liquid argon and xenon with XeBrA
As noble liquid time projection chambers grow in size, their high voltage requirements increase, and detailed, reproducible studies of dielectric breakdown and the onset of electroluminescence are needed to inform their design. The Xenon Breakdown Apparatus (XeBrA) is a 5-liter cryogenic chamber at the Lawrence Berkeley National Laboratory built to characterize high voltage behavior of liquid xenon and liquid argon. This talk will present the motivation and results from XeBrA that will serve to inform the future of noble liquid detector engineering.
Speaker: Dr Lucie Tvrznikova (Yale University / LBNL)
• 63
Ultra-low Energy Calibration of the LUX detector with pulsed D-D neutrons and 127Xe Electron Capture Events
The LUX dark matter experiment has measured the nuclear recoil charge and light yields in LXe down to 0.7 keVnr and 1.1 keVnr, respectively, in situ using a D-D neutron calibration source. Improvements in the D-D calibration have been possible by incorporating pulsing technique with narrow pulses (20 us / 250 Hz). This technique allows the suppression of accidental backgrounds in D-D neutron data and also provides increased sensitivity for the lower energy NR calibrations. I will report the improved NR absolute Qy and Ly measurements using the pulsed D-D calibration technique performed in situ in the LUX detector. I also present an absolute calibration of electron recoil (ER) charge yield using $^{127}$Xe electron capture events at energies down to the N-shell 186 eVee. These in situ energy calibrations, using D-D neutron and $^{127}$Xe sources, represent the lowest energy NR and ER that have been explored in liquid Xe and are accompanied by a significant improvement in calibration uncertainty.
Speaker: Mr Dongqing Huang (Brown University)
• 64
The Noble Element Simulation Technique (NEST) Version 2.0
The latest release of the Noble Element Simulation Technique (NEST) is presented here. Noble element target media have become common in rare event searches, and an accurate comparison model is critical for understanding and predicting signals and unwanted backgrounds. Like its predecessors, NESTv2.0 is a simulation tool written in C++ and is based heavily on experimental data, taking into account most of the existing ionization and scintillation data for solid, liquid, and gaseous xenon. Due to the large amount of precise data for liquid xenon, most theoretical models in NEST have been replaced with simple, well-behaved, empirical formulas, such as sigmoids and power laws. NESTv2.0 also uses an empirical, non-binomial, recombination fluctuations model. In addition, NESTv2.0 simulates S1 and S2 scintillation signals with correct energy resolutions in dual-phase xenon time-projection chambers, and this is done without using an external package. While NEST can be used with GEANT, NESTv2.0 is fully capable of operating as a stand-alone command-line tool.
Speaker: Gregory Rischbieter (SUNY Albany)
• Parallel Session: Quantum Sensors 553A
### 553A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
Conveners: Jason Hogan (Stanford University), Dr Salman Habib (Argonne National Laboratory)
• 65
Resonant absorption of bosonic dark matter in molecules, etc.
Speaker: Prof. Asimina Arvanitaki (Perimeter Institute)
• 66
Quantum pattern recognition for HEP
Speaker: Ms Lucy Linder (Lawrence Berkeley National Lab)
• 67
Quantum system engineering, axion detection
Speaker: Alexander Sushkov (Boston University)
• 68
Quantum sensors for light dark matter
Speaker: Prof. Kent Irwin (Stanford University and SLAC)
• Parallel Session: Silicon Detectors 552A
### 552A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• 69
Lithium doped Silicon Detectors for Particle Astrophysics
Speaker: Kerstin Perez (MIT)
• 70
Reinventing amorphous selenium avalanche photodetector for picosecond time-of-flight applications
Speaker: Amir Goldan
• 71
Silicon devices with single charge resolution
Speaker: Pitam Mitra
• 72
Charge-Coupled Devices Fabricated on Bulk Germanium
Speaker: Dr Christopher Leitz (MIT Lincoln Laboratory)
• 3:30 PM
Coffee Break East Prefunction
### East Prefunction
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Plenary IV
Convener: Maurice Garcia-Sciveres (LBNL)
• 73
Speaker: Vetri Velan (University of California, Berkeley)
• 74
Speaker: Carolyn Gee (University of California, Santa Cruz)
• 75
• 76
Speaker: Mr Dylan Temples (Northwestern University)
• 77
Speaker: Qing Xia (Yale)
• 7:00 PM
Conference Dinner Alumnae Hall (Brown University)
### Alumnae Hall
#### Brown University
Buses will pick up at the RICC between 6:30 and 7pm to go to the banquet location.
Buses will depart from the banquet location at 9:30pm and drop guests off at downtown hotels.
• Tuesday, December 11
• 7:30 AM
Breakfast East Prefunction
### East Prefunction
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Parallel Session: Computing & Machine Learning 553B
### 553B
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
Conveners: Dr Oliver Gutsche (Fermi National Accelerator Laboratory), Sergei Gleyzer (University of Florida), Taritree Wongjirad (MIT)
• 78
Submanifold Sparse Convolutional Networks for Sparse, Locally Dense Particle Image Analysis
From a breakthrough revolution, Deep Learning (DL) has grown to become a de-facto standard technique in the fields of artificial intelligence and computer vision. In particular Convolutional Neural Networks (CNNs) are shown to be a powerful DL technique to extract physics features from images: They were successfully applied to the data reconstruction and analysis of Liquid Argon Time Projection Chambers (LArTPC), a class of particle imaging detectors which records the trajectory of charged particles in either 2D or 3D volumetric data with a breathtaking resolution (~3mm/pixel). The CNNs apply a chain of matrix multiplications and additions, and can be massively parallelized on many-core systems such as GPUs when applied on image data analysis. Yet a unique feature of LArTPC data challenges traditional CNN algorithms: it is locally dense (no gap in a particle trajectory) but generally sparse. A typical 2D LArTPC image has less than 1% of pixels occupied with non-zero value. This makes standard CNNs with dense matrix operations very inefficient. Submanifold sparse convolutional networks (SSCN) have been proposed to address exactly this class of sparsity challenges by keeping the same level of sparsity throughout the network. We demonstrate their strong performance on some of our data reconstruction tasks which include 3D semantic segmentation for particle identifications at the pixel-level. They outperform a standard, dense CNNs in an accuracy metric with substantially less computations. SSCN can address the problem of compute resource scalability for 3D ML-based data reconstruction chain R&D for LArTPC detectors.
Speaker: Laura Domine
• 79
A Framework for Integrated Research Software Training in HEP
Speaker: Prof. Sudhir Malik (University of Puerto Rico Mayaguez)
• 80
E2E applications to boosted topologies
Speaker: Bjorn Burkle
• Parallel Session: Noble Element Detectors 553A
### 553A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• 81
Internal Calibration Source Injection Hardware for LZ
Self-shielding in ton-scale liquid noble detectors presents a unique challenge for calibrating the detector's innermost volume. Calibration isotopes must be injected directly into the active material to reach the central volume, and they must either decay away with a short half life or be purified out. I present a summary of the LUX-ZEPLIN (LZ) calibration hardware effort at UMass Amherst in which we are refining techniques for the injection and removal of precise activities of various calibration isotopes. This technology is generalizable to the liquid noble field as a whole.
Speaker: Christopher Nedlik (University of Massachusetts)
• 82
Noble liquid detector R&D with the LZ System Test platform at SLAC
LZ is a next generation dark matter search experiment designed to significantly extend our sensitivity to WIMP dark matter. At the core of the LZ design is a dual-phase Xe time projection chamber (TPC) with 7 tonnes of active volume. The LZ System Test platform has been constructed at SLAC and consists of three mid-size xenon detectors that, together, test and validate the performance of critical LZ subsystems at scales approaching or comparable to the LZ design. An overview of the test platform will be given, followed by recent results relevant to many noble liquid detectors.
Speaker: Kelly Stifter (Stanford University)
• 83
Recent Developments in Wavelength-Shifting Coatings for Noble Element Detectors
Charged particles generate copious amounts of scintillation light in the far ultraviolet when passing through the noble elements. Directly detecting these deep UV photons is challenging, and a common technique is to employ photofluorescent compounds as wavelength-shifters to convert this scintillation light into to the visible. A number of challenges continue to present themselves in the ongoing efforts to optimize designs in this detector paradigm, particularly in the realm of argon-based detectors. From new measurements to creative detector designs, I will summarize a variety of recent findings and innovative approaches in this area of active research.
Speaker: Prof. Denver Whittington (Syracuse University)
• 84
Summary of the R&D Results from Recent Analyses of LUX Xe TPC Data
LUX operated at Sanford Lab from 2013 to 2016 with a primary mission to search for dark matter using a dual-phase xenon TPC with a 250 kg target mass. It produced world-leading search results. Its data continues to be used for other rare event physics searches and to improve our understanding of the detailed behavior of Xe TPCs. Ongoing LUX analyses have significantly furthered the understanding of signal yields and signal detection in xenon and also identified competing radiogenic backgrounds. In this talk, I will detail recent results including pulse shape discrimination, results from the many new calibration techniques that were successfully exploited, and also summarize the improvements in the understanding of radiogenic backgrounds and efforts to extend the background model. These LUX analyses are being also being used to inform the upcoming LUX-ZEPLIN experiment.
Speaker: William Taylor (Brown University)
• 85
Photosensors for the DarkSide-20k Experiment
DarkSide-20k is a proposed 30-tonne fiducial mass liquid argon TPC that will perform an instrumental background-free search for WIMP dark matter. The TPC will be outfitted with 200,000 silicon photomultipliers (SiPMs) grouped into 8,280 single-channel, 25 cm$^2$ photosensors that are sensitive to single photoelectrons. We will present the cryogenic performance of the first DarkSide Motherboard, a 625 cm$^2$ module that houses 25 photosensors and their associated low-noise electronics. We will also discuss the strategy for producing the full complement of DarkSide photosensors, including the transition of wafer production to a commercial foundry and the construction of a dedicated, low-background packaging facility.
Speaker: Graham Giovanetti (Princeton University)
• Parallel Session: Silicon Detectors 552A
### 552A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• 86
Back-illuminated imagers with ns time resolution
Speaker: Andrei Nomerotski (Brookhaven National Laboratory)
• 87
High Density Interconnect Technology aka 3D Integration for Radiation Detection Circuits and Systems
High Density Interconnect Technology aka 3D Integration Technology is a transformative enabler for new forms of detectors integrating sensors with the processing electronics in pseudo-monolithic structures. The processing power, thanks to the integration of consecutive layers of active components and effectively tens of layers of routing metallization, allow building self-supporting, edgeless and robust detectors that permit extraction of higher level information directly on the detector through enabling inter-channel(inter-pixel) communication and in-hardware implementation of advanced algorithms. 3D integration technology, after a bit more than a decade of infancy, paved its way to the largest mainstream foundries, where giants, like TSMC or GlobalFoundries offer real 3D integration technology with wafer stacking and through silicon vias on process nodes 28 nm and below now. Of course, costs are high and only top and largest volume commercial producers can afford these services. Fortunately, in the most recent years, 3D integration technologies, initially developed in the industrial context, gained strong interests in National Laboratories, where the ingredients have been either licensed or developed in-house to be able to fulfil the requirements of federally funded detector research and development. Leveraging of these capabilities is attractive to the Department of Energy programs, for offices of High Energy Physics and Basic Energy Sciences, and efforts in this direction are underway with orientation on demonstrating strategic capabilities. Looking further into the future, i.e. into the 10nm integrations scales, it is believed that with 3D integration technologies with emphasis of heterogenous integration, it would be possible to build such devices that raw information will be transformed into less bandwidth occupying data, carrying only useful message for a user. The special attention is to be given to interconnection between sensing nodes, digitization and processing on the back of the focal plane, including data reduction, edge computing, information extraction, use of techniques, like neural network and neuromorphic algorithms of increased complexities. The objective is going from simple algorithms of increased resolution, correction of detection imperfection, extracting of secondary level information direction of arrival, distance to topological and abstract object recognitions and artificial intelligence interfaces. Introduction to the 3D capabilities, undertaken efforts , collaborations and the directions here-mentioned will be given in the presentation.
Speaker: Dr Gregory Deptuch (FERMILAB PPD/EED)
• 88
Low Gain Avalanche Detector development at BNL
Low-Gain Avalanche Diodes are gathering interest in the High-Energy Physics community thanks to their fast-timing and radiation-hardness properties, which are planned to be exploited, for example, in timing detectors for the upgrades of the ATLAS and CMS detectors at the High Luminosity LHC. This new technology has also raised interest for its possible application for photon detection in medical physics, imaging and photon science. The main characteristic of this type of device is a thin and highly-doped layer that provides internal and moderate gain, in the order of 10-20, that enhances the signal amplitude. A thin substrate of a few tens of microns allow fast carrier collection. We will detail on the fabrication technology, specifically developed at Brookhaven National Laboratory for the detection of minimum ionizing particles. The static electrical characterization and the gain measurements on prototypes will be reported too. Some devices have been irradiated with proton beam at the Tandem Van de Graaff facility at BNL, and post-irradiation studies will be reported.
Speaker: Dr Gabriele Giacomini (Brookhaven National Lab)
• 89
Technical Choices and Challenges of LSST Readout System
Speaker: Sven Herrmann (BNL)
• 90
Avalanche photodiode (APD) and high dynamic range (HDR) imaging
• 10:00 AM
Coffee Break East Prefunction
### East Prefunction
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Parallel Session: Noble Element Detectors 553A
### 553A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• 91
Prototyping the world's largest liquid argon TPC: ProtoDUNE Single Phase
Neutrino physics are a rich field of research with many unanswered questions. To continue exploring this field, liquid argon TPCs (LArTPC) are becoming increasingly popular because of their many advantages over other detector technologies. One of the largest future long-baseline neutrino oscillation experiments, DUNE, aims to build 4 x 10kt LArTPCs as its far detector. ProtoDUNE-SP is the single-phase DUNE Far Detector prototype that was built between Dec. 2015 and Jun. 2018 and is currently operating at the CERN Neutrino Platform. This experiment is a crucial part of the effort towards the construction of the first DUNE far detector module and is a significant experiment in its own right. With a total liquid argon mass of 0.77 kt, it is the largest monolithic single-phase LArTPC detector built to date. It has currently finished cumulating data from a new dedicated charged-particle test beamline at CERN and will continue running with cosmic data. Through the journey of the construction and activation of ProtoDUNE SP, we will explore how DUNE's goals can be reached.
Speaker: Dr Flor de Maria Blaszczyk (Boston University)
• 92
High-Pressure Gas TPC for DUNE Near Detector
The DUNE near detector will consist of several components, one of which is the high-pressure gaseous argon TPC (HPgTPC). As a promising neutrino detection technology, it is well-suited to improve the neutrino-nucleus systematic uncertainties for the neutrino oscillation measurements. In this talk, an overview of the on-going HPgTPC R&D efforts in the U.K. and U.S. will be presented.
Speaker: Tanaz Mohayai (Fermilab)
• 93
ArgonCube: Novel R&D for LArTPCs
ArgonCube is an international collaboration for LArTPC Detector R&D, with a focus on the technical needs for the DUNE physics program. The ArgonCube R&D program is currently aimed on detector modularization, pixelated charge readout, and innovative light detection for large LArTPCs. Modularization addresses a number of technical issues for large LArTPCs, including drift field stability, stored energy, and liquid argon purity. Pixelated readout has proven to deliver true 3D imaging of particle interactions, removing the ambiguities present for existing readout techniques. New approaches to light detection enable increased photon yields and provide improved localization of scintillation signals. The ArgonCube design has been adopted as the baseline LAr system for the DUNE Near Detector. The ArgonCube 2x2 Demonstrator, a 3-ton-active modular pixelated LArTPC, will serve as an engineering prototype for DUNE. It is currently under construction and will operate in the Fermilab NuMI neutrino beam in 2020.
Speaker: Dr Dan Dwyer (LBNL)
• 94
New Developments in Micropower ASICs for 3D pixelated charge readout of liquid argon Time Projection Chambers
True three-dimensional ionization charge detection and readout of liquid argon time projection chambers has recently been demonstrated. To achieve this, a 32-channel custom readout ASIC, LArPix, was used to read out a custom pixelated TPC anode immersed in liquid argon. This talk will discuss design and architectural details that enabled low-noise, low-power digitization of the charge signal. In addition, potential follow-on developments and improvements (e.g. increased number of channels, increased ADC dynamic range) will be discussed.
Speaker: Dr Carl Grace (Lawrence Berkeley National Laboratory)
• 95
Cold Electronics R&D
Operating the wire readout electronics for Liquid Nobel TPCs at cryogenic temperatures has a number of advantages. As demonstrated by the BNL group, the front-end amplifier noise is reduced both by the elimination of extra capacitance due to cables and by the improved transistor noise performance at low temperature. Digitizing and digital multiplexing in the cold is also advantageous in that it reduces the number of cryostat penetrations needed and leads to an overall simpler system. Nonetheless, cryogenic electronics presents a number of challenges including achieving the lifetime and reliability needed for long-term experiments and in some applications, the strict radiopurity requirements. Several groups are pursuing the development a full cryogenic readout chain. Among these, the SLAC ASIC group has recently submitted for the fabrication the mixed-signal "CRYO" ASIC, which combines the three functions of amplification, digitization and multiplexing onto a single ASIC. In this talk, I will describe the status of the global cold electronics R&D effort, including the design, planned testing and application of the CRYO ASIC in the Deep Underground Neutrino Experiment (DUNE) and the next phase of the Enriched Xenon Observatory (nEXO).
Speaker: Dr Mark Convery (SLAC)
• Parallel Session: Photodetectors 553B
### 553B
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
Conveners: Adam Para (Fermilab), Prof. Lindley Winslow (MIT), Lindley Winslow (UCLA), Zongfu You
• 96
Nanocomposite Materials for Microchannel Plate Detectors
Precisely controlled metal-metal oxide nanocomposite layers prepared by atomic layer deposition (ALD) exhibit material properties that can be tuned over a broad range by adjusting the metal content such as band gap, absorption coefficient, resistivity, and electrochemical corrosion resistance. Consequently, these metal-metal oxide nanocomposites are well suited especially as a resistive layers for microchannel plates (MCPs) functionalization. For resistive layers in MCPs, both resistance stability with respect to applied potential and the thermal coefficient of resistance (TCR) are the critical materials property because it dictates the range of allowable operating voltage and temperatures for devices (e.g. photon, neutron, or particle detectors) that incorporate the MCP for electron amplification. The ability to control the TCR will enable new applications such as cryogenic detectors or detectors that must endure large temperature changes during operation. To address this need, we have synthesized a variety of ALD metal-metal oxide nanocomposite layers by combining different metals (W, Mo, Ta, Nb, and Re) and metal oxides (Al2O3, ZrO2, TiO2, Ta2O5, Nb2O5, and HfO2). We studied the electrical transport properties of these ALD films and focused on their temperature dependence in order to extract the TCR. In all cases, the TCR is negative, so that the resistance drops with increasing temperature as expected for a semiconducting material. In addition, the magnitude of the TCR increases with the film resistivity, and depends on both the metal and the metal oxide components of the composite. This presentation will expound on these findings and explain the implications for MCP detectors.
Speaker: Dr Anil Mane (Argonne National Lab)
• 97
Development of the Air-Transfer Process for the `Gen-II' LAPPD
The Gen-II LAPPD is a 20$\times$20 cm$^2$ MCP-based photo-detector that has a monolithic ceramic detector base with an anode capacitively coupled through a thin metal film to an application-specific readout pattern outside of the vacuum package. We discuss the development of the *air-transfer* process for the Gen-II LAPPD assembly. In this process a hermetic seal between the top window with pre-deposited antimony layer and the detector base is made during the detector bake-out. Photo-cathode synthesis is then performed by introducing alkali metals into the sealed detector package through a small sealable vacuum port. We have demonstrated the feasibility of several critical process steps including demonstration of cesium transport from a source outside of the detector package to the entire surface of the detector window in the presence of two full-size 20$\times$20 cm$^2$ MCPs inside the detector.
Speaker: Andrey Elagin (University of Chicago)
• 98
3D digital SiPM development for large area photodetectors
Over the last years, we have worked on the concept of 3D digital SiPM and demonstrated critical steps towards there realization from CMOS design to fabrication process. We will review the main building blocks of the 3D digital SiPM, the development we have led and the forecasted and needed R&D. This will include CMOS design for arrays of ultra-low single photon timing resolution time-to-digital converter for time-of-flight experiments and for low power large area photodetector for noble liquid low background experiments (liquid xenon and argon). We will make the case that 3D digital SiPM has the potential to have superior performance over the 2D digital SiPM and its analog counterpart. We will discuss how this next generation detector can be disruptive in the field of radiation instrumentation and how it opens the door to new sciences.
Speaker: Prof. Serge A. Charlebois (Université de Sherbrooke)
• 99
On the Development of High Efficiency Si-Based Single VUV Photon Detector
Aside from a large variety of direct applications, Silicon-based photo-multipliers (SiPMs) are also replacing photo-multiplier tubes in the net generation of liquid noble experiments (Argon and Xenon). However, current photo-detection efficiency (PDE) values, at peak emission wavelengths for xenon (175 nm) and argon (128 nm), range between 5% and 25%, requiring in some instance the use of a wavelength shifting material. In this talk, we will discuss the ongoing effort to use molecular implantation on 3-Dimensionally integrated digital SiPMs (3DSiPMs) to boost the device PDE in the VUV regime to values >35%. Furthermore, we will discuss the dedicated effort in the selection of materials with optimal optical properties in the VUV range, which is fundamental for the construction of the ultimate single VUV photon sensitive photo-detector.
Speaker: Dr Pietro Giampa (TRIUMF)
• Parallel Session: Quantum Sensors 552A
### 552A
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• 100
Nano-mechanical resonators coupled to atoms
Speaker: Prof. Andrew Geraci (Northwestern University)
• 101
New Directions for Fundamental Physics Tests with Macroscopic Scale Atom Interferometers
Light-pulse atom interferometry—which uses optical pulses to split, recombine, and interfere quantum mechanical atomic matter waves—is a sensitive method for measuring inertial and gravitational forces, making it a valuable tool for a broad set of applications and fundamental physics tests. The sensitivity of an atom interferometer scales with its enclosed spacetime area, which is proportional to the product of the maximum spatial separation reached between the two interferometer paths and the interferometer duration. Motivated by this scaling, atom interferometers have been realized that cover macroscopic scales in space (tens of centimeters) and in time (multiple seconds). In this talk, I will discuss new experimental efforts to use macroscopic scale atom interferometers for fundamental physics tests. These include improved searches for new particles beyond the standard model by looking for deviations from the gravitational inverse square law and an improved measurement of Newton’s gravitational constant. Additionally, I will discuss work that the Matter wave Atomic Gradiometer Interferometric Sensor (MAGIS) collaboration is pursuing toward a large scale atom interferometer to search for ultralight dark matter and to detect gravitational waves in a frequency band complementary to those addressed by laser interferometers.
Speaker: Prof. Tim Kovachy Kovachy (Northwestern University)
• 102
Measurement of the fine structure constant as test of the Standard Model
Measurements of the fine-structure constant α require methods from across subfields and are thus powerful tests of the consistency of theory and experiment in physics. Using the recoil frequency of cesium-133 atoms in a matter-wave interferometer, we recorded the most accurate measurement of the fine-structure constant to date: α = 1/137.035999046(27) at 0.20 parts per billion accuracy. Comparison with Penning trap measurements of the electron gyromagnetic anomaly ge − 2 via the Standard Model of particle physics is now limited by the uncertainty in ge − 2; a 2.5σ tension may be a sign of physics beyond the Standard Model that warrants further investigation. In particular, we will discuss implications for dark-sector candidates such as dark photons.
Speaker: Prof. Holger Mueller (UC Berkeley)
• 103
ACME + precision measurements with polyatomic molecules
Speaker: Nick Hutzler (Caltech)
• 12:30 PM
Lunch East Prefunction
### East Prefunction
#### Rhode Island Convention Center
One Sabin Street Providence, Rhode Island 02903 United States
• Plenary V
Convener: Ian Shipsey (Oxford)
• 104
Speaker: Ian Shipsey (Oxford)
• 105
Photodetectors
• 106
Noble Element Detectors
Speakers: Prof. Sowjanya Gollapinni (University of Tennessee, Knoxville), Sowjanya Gollapinni
• 107
Silicon Detectors
Speakers: Alvaro Chavarria, Julia Thom-Levy (Cornell University)
• 108
Quantum Sensors
Speaker: Dr David Hume (NIST)
• 109
Computing & Machine Learning
| 2023-01-30T01:23:55 |
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|
https://pos.sissa.it/364/122/
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Volume 364 - European Physical Society Conference on High Energy Physics (EPS-HEP2019) - Detector R&D and Data Handling
Commissioning of the Belle II Pixel Vertex Detector
H. Ye* On behalf of the DEPFET and Belle II PXD collaboration
*corresponding author
Full text: Not available
Abstract
As an upgrade of the asymmetric e$^+$e$^−$ collider KEKB, SuperKEKB aims to increase the peak luminosity by a factor of 40 to 8×10^35 cm$^{−2}$s$^{−1}$. The upgraded Belle II detector allows the experiment to handle the much increased data rates, with the goal to explore new physics beyond the Standard Model at the intensity frontier. Belle II is expected to accumulate a dataset of 50 ab$^{−1}$ by 2027. The Belle II pixel detector (PXD) has been developed using the DEpleted P-channel Field Effect Transistor (DEPFET) technology, which combines low power consumption in the active pixel area and low intrinsic noise with a very small material budget. In this talk commissioning and performance of this novel detector measured with first collision data will be presented.
How to cite
Metadata are provided both in "article" format (very similar to INSPIRE) as this helps creating very compact bibliographies which can be beneficial to authors and readers, and in "proceeding" format which is more detailed and complete.
Open Access
Copyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.
| 2020-09-23T01:09:00 |
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https://pos.sissa.it/316/090/
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Volume 316 - XXVI International Workshop on Deep-Inelastic Scattering and Related Subjects (DIS2018) - WG3: Higgs and BSM Physics in Hadron Collisions
Probing BSM physics with electron-proton colliders
D. Curtin, K. Deshpande, O. Fischer, J.F. Zurita*
*corresponding author
Full text: pdf
Pre-published on: 2018 September 20
Published on: 2018 November 23
Abstract
In this talk I will illustrate with two examples (Higgsino dark matter and Exotic Higgs decays) how electron-proton colliders present unique opportunities to probe BSM scenarios where proton-proton colliders fall short due to the experimental difficulties in reconstructing the signal due to the large hadronic backgrounds. The \emph{leit-motiv} of these examples are long-lived particles (LLPs), which have received recently a lot of attention from both the experimental and theoretical communities. We find that the proposed $e^-p$ colliders can be competitive against their more energetic $pp$ incarnations for lifetimes between a millimeter and a micron, depending on the physics scenario under consideration.
DOI: https://doi.org/10.22323/1.316.0090
Open Access
Copyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.
| 2019-02-22T22:29:13 |
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https://lammps.sandia.gov/threads/msg70909.html
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LAMMPS WWW Site - LAMMPS Documentation - LAMMPS Mailing List Archives
Re: [lammps-users] Errors in lubricate/poly ?
# Re: [lammps-users] Errors in lubricate/poly ?
From: Ranga Radhakrishnan Date: Thu, 13 Jul 2017 12:14:27 +0100
Hi, Sorry for another email addressing the same issue. Maybe I am beating a dead horse here, but another way to highlight the same error in omega calculation in both the lubricate and lubricate/poly pair styles would be to do a two particle shearing example as described earlier and in the attached input script (with one particle at the bottom edge and the other in contact) and increase the simulation box size. Even if one assumes that there should be a force between the particles, it should surely not depend on the box size. However, there is a box size dependency with these lubricate pair styles. I also want to make it clear that the problem with omega is not the only problem with the current implementation of lubricate pair styles. Another interesting situation is when particles overlap when shearing (it can happen in simulations of dense suspensions paired with granular forces), where one has to be careful about how the lubrication force is calculated. There's also an issue with the non-symmetricity of the stress tensor due to lubrication force as currently calculated in LAMMPS. Specifically for lubricate/poly, there are other issues that I pointed out earlier. I can discuss all these issues in more detail if the LAMMPS strategy is to modify the current implementation. One clarification about one of my earlier comments. I quote from my earlier email. "4) a.The squeeze term in lubricate/poly is taken from the force given in Eq. 9. 33 of Ref. (1). According to the resistance matrix formulation, the first term in Eq. 9. 33 should be multiplied by a prefactor of "2/(1+\beta)" , and the second term by "\beta" (apologies for the mistake in my previous email). One simple way to see that is that the magnitude of the leading order terms given in Sec. 11.2.2 should be twice of Eq. 9. 33, which is not the case in the textbook." The first term between Eq. 9. 33 and Sec. 11.2.2 of Kim and Karrila is consistent, since they scaled the gap distance by particle radius in the first case, however the second term is still inconsistent between the two sections of the book. I think that the Chapter 11 is the correct version in the sense that the terms are consistent with Eq. (3.19a, b) of Jefferey and Onishi, J. Fluid Mech. (1984), wol. 139, pp. 261-290, which is the original research article. I've also cc'ed the LAMMPS mailing list this time, apologies for not doing in my last emails. Regards, Ranga On 11/07/17 18:56, Ranga Radhakrishnan wrote: Hi David, I was trying to illustrate a problem with the current lubricate implementation by using a specific example where we know what to expect. That is the reason that I chose to use fix nve/sphere and fix deform. According to LAMMPS documentation, the command "fix fid all deform 1 xy erate ${arg} remap v" will add a relative velocity (V=${arg}*box_length) only if the particles are across the periodic boundary. The way to get the particles that don't cross the boundary have a relative velocity with each other is to use a fix/nvt sslod, or another NEMD technique. So for the case that I was describing (using fix nve/sphere), both the top particle at (0,1.53,0) and the bottom particle (0,0,0) will have the same velocity (zero relative velocity) even with fix deform, and hence my problem with the lubricate force in LAMMPS. As I was describing earlier, this problem seems to be less important when "omega[i][0] += 0.5*h_rate[3]/domain->zprd;" etc. is corrected in pair_lubricate.cpp. On the other hand, if the particles are on opposite sides of the cubic box (length=10) at say (0,0.5,0) and (0,9.53,0), they have a relative velocity V between them and again we should be able to match this to expected result. In the dump file we may not be able to see that these particle have a relative velocity between them (at least on time step=1). Sorry for not ccing this discussion on the LAMMPS forum. Please let me know if I should. Regards, Ranga On 11/07/17 16:39, Heine, David R wrote: Ranga, Can you clarify a point for me? With particles separated in the y direction and shear in the xy direction, why do you say there is no relative velocity between the particles? The top particle will have a larger x velocity than the bottom particle in proportion to the shear rate. If you instead placed the second particle at (0,0,1.03), then they would have the same relative velocity in the presence of xy shear. David From: Ranga Radhakrishnan [mailto:[email protected].....] Sent: Thursday, July 06, 2017 12:54 PM To: Heine, David R; Steve Plimpton; Bolintineanu, Dan Stefan (-EXP) Subject: Re: [lammps-users] Errors in lubricate/poly ? Hi David, I think that the below example is sufficient to illustrate the importance of updating lubricate and lubricate/poly pair styles. Consider two particles of diameter 1.0 placed at (0,0,0) and (0,1.03,0) in a cubic box of length=10 with velocity=0, and only interacting with lubricate (/poly) pair style whose outer cutoff is 1.05, and inner cutoff is 1.001 (flagfld=0). If the box is not sheared, then the force acting between the two particles is 0. If we used fix nve/sphere for integration and the box is deformed in the xy direction, the force should still be equal to 0 since there is 0 relative velocity between the particles. However, this is not the result that one obtains from lubricate, instead, one gets a force that depends on the box deformation rate. Please see the attached collision.lmp input file for other details of my simulation setup. As proposed in my previous emails, I have developed a pair style that is based on the simplification of the Grand Resistance Matrix (GRM) given by Kim and Karilla's textbook. My latest document and code are on bitbucket ( https://bitbucket.org/rangr_x/lubrication). From my last email, I have made a few changes to the calculation of stress in my force class, and to the Stokes drag force calculation. I have verified my code against Tim Najuch's "lubricate/GRM" formulation as well as some analytical results. I hope this is useful. Regards, Ranga On 01/07/17 17:04, Ranga Radhakrishnan wrote: Hi David, Thanks for your quick reply. Indeed, I have developed and tested a lubrication force class called lubricate/Simple, and it is currently a hack of the lubricate/poly. The link for my code is here: https://bitbucket.org/rangr_x/lubrication I have took out most of the FLD parts of lubricate/poly since it is not needed for my purpose (dense non-Brownian suspensions). There are a few things that need to be included in my code as mentioned in the Readme. Hopefully, either you or some of the others in the LAMMPS community can help me with improving this code. I have been in contact with Tim Najuch on the GRM version of the pair_lubricate as well. He has done a major revision of his code recently, and we expect to do a comparison of the results between our codes in a couple of weeks time. As for a quick comparison of the two particle results, I have done them for the analytical forms used in lubricate/poly in Sec IV D of my pdf (also in the bitbucket site). Hope this helps. Regards, Ranga On 30/06/17 15:18, Heine, David R wrote: Ranga, Yeah, it looks like you have done your homework. Tim submitted a GRM version of pair_lubricate based on Chapter 11, but maybe we are better off using the equations you highlighted here. Do you have this implemented in LAMMPS? It would be interesting to compare the behavior of two near-contact spheres with the three versions of pair_lubricate we now have. David From: Ranga Radhakrishnan [mailto:[email protected]...] Sent: Wednesday, June 28, 2017 12:53 PM To: Heine, David R; Steve Plimpton; Bolintineanu, Dan Stefan (-EXP) Cc: LAMMPS Subject: Re: [lammps-users] Errors in lubricate/poly ? Hi David, Thanks for your reply. I have attached the pdf as per your request. I will try to address your email in a enumerated list to make my points clear. 1) \omega^\infty seems to have the wrong units. It is because "h_rate" has the units of length/time (Please correct me if I am wrong). Specifically, I am referring to lines: "omega[i][0] += 0.5*h_rate[3]; ..." which subtracts h_rate from omega. In case "h_rate" has the right units of 1/time, I am confused about the units of Ef (E^\infty) which should be the rate of strain tensor. 2) The results given in Chapter 9 of Ref. (1) are slightly misleading, because they cite Jeffrey and Onishi's work (doi: 10.1017/S0022112084000355) before giving the final formulae for the forces, and torques. In the original work by Jefferey and Onishi, the gap distance is non-dimensionalised by (radi+radj)/2. 3) Eqs. 9.26, and 9.27 in Ref. (1) are the solutions for force and torques for shearing of two surfaces only due to rotation. Why does the pump term account only for the torque? I don't think the current formulation of the force considers the shearing of two surfaces only due to rotation correctly. (Please see Sec. IV of the attached document). 4) a.The squeeze term in lubricate/poly is taken from the force given in Eq. 9. 33 of Ref. (1). According to the resistance matrix formulation, the first term in Eq. 9. 33 should be multiplied by a prefactor of "2/(1+\beta)" , and the second term by "\beta" (apologies for the mistake in my previous email). One simple way to see that is that the magnitude of the leading order terms given in Sec. 11.2.2 should be twice of Eq. 9. 33, which is not the case in the textbook. 4) b. The squeeze or the shearing terms should be independent of the particle velocities and rotations, so Chapters 9 and 11 of Kim and Karilla should be consistent with each other. In case they are not, I have tried to refer to the original research articles and verify the same. 5) I don't think we need to bring in volume fraction dependencies at the moment, because the issues that I have raised can be tracked down using just two particles of unequal sizes. The general solution of the problem of two unequal spheres in a fluid is given in Chapter 11 of Kim and Karilla, or originally in Jeffrey's research article (doi:10.1063/1.858494). In the attached pdf, I have mainly relied on Kim and Karilla as the reference. The results that you are referring to in Chapter 9 of Kim and Karilla can be derived as cases of the general result in Chapter 11 (as shown in Section IV of the attached pdf). As you rightly mention the grand (shear) resistance matrix formulation is slightly more involved to implement efficiently. However, one can get simplified expressions for forces and torques that are easier to implement in LAMMPS by considering only the first two leading order terms as shown in the attached document (Eqs. 12, or 13, and 23, or 24). Regards, Ranga On 28/06/17 14:51, Heine, David R wrote: Ranga, I didn’t get the attached pdf when the message was forwarded, so maybe sending it directly to me will help me understand the issue better. In general, I followed the equations in Chapter 9 to incorporate polydispersity into pair_lubricate. As I was discussing with Tim Najuch, the text assumes you have particle A approaching another particle B, so being consistent with them, the separation distance is scaled by the radius of particle A. In the lubricate implementation, the forces on A and B are calculated separately, hence the requirement that “newton” is set to off. The grand resistance matrix approach in Chapter 11 that Tim was working on assumes the particles are approaching each other at the same speed, which may be a better approximation, but I don’t have a sense of how big the difference is when modeling things like highly filled systems as opposed to semi-dilute solutions. If you haven’t already talked to Tim about the grand resistance matrix implementation, maybe that will address some of your issues. I don’t see the issues about specific terms you mention below, but again, maybe I need the pdf attachment to see your explanation. If you have a means of making this more generally applicable than what is provided in Kim and Karilla, then I am all in favor of it. Best regards, David From: Steve Plimpton [mailto:[email protected]...] Sent: Wednesday, June 21, 2017 10:23 AM To: Ranga Radhakrishnan; Heine, David R; Bolintineanu, Dan Stefan (-EXP) Cc: LAMMPS Subject: Re: [lammps-users] Errors in lubricate/poly ? I'm CCing Dan Bolintineanu and Dave Heine who can likely answer these Qs. Steve On Wed, Jun 21, 2017 at 4:54 AM, Ranga Radhakrishnan wrote: Hi, I think that I have a few issues with the lubricate/poly implementation in LAMMPS based on my reading of Microhydrodynamics book by Kim and Karilla [1]. 1) The gap-distance (h_sep) between the particles should be scaled by (radi+radj)/2 and not as radi, where radi, radj are the radii of the two particles. 2) The first term in the squeeze force seems to be missing a prefactor of 2. 3) \omega^\infty seems to have the wrong units. It is because "h_rate" has the units of length. 4) The pump term is also incorrect for particles of different sizes. Briefly, specific cases of calculation of torques in Ref. [1] cannot be used to write down a generalized version. Please look at the attached pdf for a more detailed explanation on why I raised these concerns, and how to implement a "corrected" lubrication force if you agree with my concerns. Just to be clear, I have looked at previous messages in the mailing list before I send this message, and I don't think any of the previous messages have answered my concerns. Regards, Ranga ------------------------------------------------------------------------------ Check out the vibrant tech community on one of the world's most engaging tech sites, Slashdot.org! http://sdm.link/slashdot _______________________________________________ lammps-users mailing list [email protected] https://lists.sourceforge.net/lists/listinfo/lammps-users
variable DIA1 equal 1.0
variable MASS1 equal (PI*(${DIA1}^3.0)/6.0) variable DIA2 equal 1.0 variable MASS2 equal (PI*(${DIA2}^3.0)/6.0)
variable FLD_VISC equal 1.0
variable T_STEP equal 0.00001
variable LEN equal 10
atom_style sphere
boundary p p p
newton off
comm_modify mode single vel yes
region reg prism 0 ${LEN} 0${LEN} 0 ${LEN} 0 0 0 units box create_box 2 reg neigh_modify delay 0 print "Vol=$(vol)"
create_atoms 1 single 0.0 1.43 0.0
group right type 1
velocity right set 0 0 0
set type 1 omega 0 0 0
create_atoms 2 single 0.0 0.5 0.0
group left type 2
velocity left set 0 0 0
set type 2 omega 0 0 0
set type 1 diameter ${DIA1} set type 1 mass${MASS1}
set type 2 diameter ${DIA2} set type 2 mass${MASS2}
timestep ${T_STEP} fix 1 all nve/sphere pair_style lubricate${FLD_VISC} 1 0 1.001 1.05 1 0
pair_coeff * *
#pair_coeff 1 1 1.001 1.05
#pair_coeff 2 2 1.4014 1.47
#pair_coeff 1 2 1.2012 1.26
compute mytemp all temp
compute mypres all pressure NULL pair
fix 2 all deform 1 xy erate 1 remap v
thermo_style custom step c_mytemp c_mypres[*]
thermo 1
thermo_modify lost ignore norm no
compute_modify thermo_temp dynamic yes
dump id all custom 1 poly.lammpstrj id type radius mass x y z vx vy vz fx fy fz tqx tqy tqz omegax omegay omegaz
run 50
The University of Edinburgh is a charitable body, registered in
Scotland, with registration number SC005336.
| 2018-08-14T10:33:42 |
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|
https://gea.esac.esa.int/archive/documentation/GDR2/Data_processing/chap_cu6spe/sec_cu6spe_input/ssec_cu6spe_auxdata.html
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# 6.2.3 Auxiliary data
The input data of the spectroscopic pipeline include also some auxiliary data. The auxiliary data are:
The ground-based radial velocities of standard stars are used in wavelength calibration to fix the zero point (Section 6.3).
The pipeline uses the 2568 standard stars described in Soubiran et al. (2018), for which the radial velocity has been obtained with high accuracy. In addition, another 5729 standard stars have been selected from XHIP measurements, having uncertainties $e_{\rm RV}<1$ km s${}^{-1}$ and quality A and B, and having a match in the master list in Crifo et al. (2010). The list of 5729 standard stars is the result of the cleaning done using the daily pipeline results. The RVS daily observations and the dry run of the spectroscopic pipeline permitted to measure the radial velocities of most of these stars in various transits; they were excluded from the list if the radial velocity measured with the RVS differed by more than 3 km s${}^{-1}$ from the one provided. Table 6.3 lists the catalogues of standard stars used for calibration, together with the catalogues used for validation.
## Atmospheric parameters
The knowledge of the atmospheric parameters of the stars is essential for the pipeline. The parameters are used to select the appropriate synthetic spectrum to generate a template as much as possible similar to the RVS spectrum, which is then used to estimate, via Pearson correlation with the RVS spectrum (Section 6.4.7), the spectroscopic radial velocity of the star. The atmospheric parameter information is also used to select the stars having a spectral type required by the calibration module. For example, wavelength calibration needs spectra with deep lines, and the input spectra selection criterium uses $T_{\rm eff}$: 4500 $<$ $T_{\rm eff}$ $<$ 6500 K (it uses also magnitude).
In Gaia DR2 the spectroscopic processing took place before the atmospheric parameters processing (Chapter 8) and could not have access to the $T_{\rm eff}$ produced with Gaia data. For this reason, a list of auxiliary atmospheric parameters obtained using ground-based data are used in the pipeline. The auxiliary parameter list contains: $T_{\rm eff}$ information for 1.8 million bright stars, some are taken from the literature and described in Soubiran et al. (2014), and some have been estimated using the 2MASS photometric catalogue, $\log g$ for 633 050 stars and [Fe/H] for 650 505 stars, all taken from the literature.
Approximately 15 % of the stars treated in Gaia DR2 have the auxiliary ground-based atmospheric parameters associated. The treatment for the other stars is described in Section 6.4.4.
## Synthetic spectral libraries
The synthetic spectra are used to produce the templates (i.e. the synthetic spectrum is convolved with the RVS LSF-AL, and re-sampled, see Section 6.4.7.
A large set of synthetic spectra has been calculated in Sordo et al. (2011), for both the low-resolution spectrophotometry and the medium-resolution RVS data. The RVS spectra have been recalculated in 2016; in particular the MARCS library grid has been extended to the cool stars, several line lists have changed and the continuum opacity treatment has been improved.
The spectroscopic pipeline uses 5256 spectra selected among the following grids:
• MARCS spectra: $T_{\rm eff}$: 2500–8000 K, step 100 K in the range 2500–3900 and 250 K in the range 4000–8000; $\log g$: -0.5–+5.0, step 0.5; [Fe/H]: -5.0, -4.0, -3.0, -2.5, -2.0, -1.5, -1.0, -0.75, -0.50, -0.25, 0.0, +0.25, +0.5, +0.75, +1.0;
• A-type spectra: $T_{\rm eff}$: 8500–15 000 K, step 500 K; $\log g$: 0.5–5, step 0.5; [Fe/H]: -0.5–+0.25, step 0.25;
• OB-type spectra $T_{\rm eff}$: 15 000–55 000 K, step 1000 K in the range 15 000–30 000 K, step 2500 K in the range 30 000–50 000 K; $\log g$: highest value: 4.75, lowest: approximately linearly from 1.75 at 15 000 K to 4.0 at 55 000 K; [Fe/H]: -0.3, 0.0, +0.3.
For more information on the synthetic spectra used in the spectroscopic pipeline see Blomme et al. (2017).
## Restricted library of template spectra
To reduce the computation time in some of the software modules, a subset of the synthetic spectra dataset (Section 6.2.3) was used, consisting of the 28 models listed in Table 6.2. This selection is based on the expected number of stars of a given spectral type/luminosity class, determined from the Gaia Universe Model Snapshot (Robin et al. 2012, specifically their Tables 16 and 17).
The subset is used notably in the modules DetermineAP (Section 6.4.4) and TodCor (Section 6.4.7).
| 2022-08-08T05:13:28 |
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|
http://mathonline.wikidot.com/properties-of-the-double-integral
|
Properties of The Double Integral
Table of Contents
# Properties of The Double Integral
We are now going to look at some properties of the double integral.
Theorem 1: Let $z = f(x, y)$ be a two variable real-valued function that is integrable over $D \subseteq D(f)$. Then: a) If $D$ has zero area, then $\iint_D f(x, y) \: dA = 0$. b) If $D$ has area $d$, then $\iint_D f(x, y) \: k = kd$. c) $\iint_D \left ( f(x, y) + g(x, y) \right ) \: dA = \iint_D f(x,y) \: dA + \iint_D g(x,y) \: dA$ (Addition Property). d) $\iint_D kf(x, y) \: dA = k \iint_D f(x,y) \: dA$ (Scalar Multiple Property). e) If $f(x,y) ≤ g(x,y)$ for all $(x, y) \in D$ then $\iint_D f(x,y) \: dA ≤ \iint_D g(x,y) \: dA$. f) $\biggr \rvert \iint_D f(x,y) \: dA \biggr \rvert ≤ \iint_D \mid f(x,y) \mid \: dA$. g) If $D_1, D_2, ..., D_n \subseteq D(f)$ are non-overlapping subsets of $D(f)$ that share no interior points with each other and $D = \bigcup_{k=1}^{n} D_k$ then $\iint_D f(x,y) \: dA = \sum_{k=1}^{n} \iint_{D_k} f(x,y) \: dA$ (Additivity of Domains Property).
Unless otherwise stated, the content of this page is licensed under Creative Commons Attribution-ShareAlike 3.0 License
| 2018-09-21T15:22:08 |
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https://math.wikia.org/wiki/Improper_integral
|
FANDOM
1,168 Pages
An improper integral (not to be confused with an indefinite integral) is the limit of a definite integral where the endpoints approach a given value. For a given improper integral to exist, it must converge, which it does if the limit exists. An example would be
$\int\limits_1^\infty\dfrac{dx}{x^2}$
This can be solved by taking a limit.
$\lim_{b\to\infty}\int\limits_1^b\dfrac{dx}{x^2}=\lim_{b\to\infty}\left[-\frac{1}{x}\Big|_0^b\right]=\lim_{b\to\infty}\left[-\frac{1}{b}+\frac{1}{1}\right]=1$
Improper integrals result in infinite values when the series is divergent. For instance,
$\int\limits_1^\infty\dfrac{dx}{x}=\lim_{b\to\infty}\int\limits_1^b\frac{dx}{x}=\lim_{b\to\infty}\left[\ln(|x|)\Big|_0^b\right]=\lim_{b\to\infty}\Big[\ln(|b|)-\ln(|1|)\Big]=\infty$
Improper integrals where both endpoints approach infinity can be solved by breaking them into two improper integrals. For example:
$\int\limits_{-\infty}^\infty\dfrac{dx}{1+x^2}=\int\limits_{-\infty}^0\frac{dx}{1+x^2}+\int\limits_0^\infty\frac{dx}{1+x^2}$
$=\lim_{b\to\infty}\int\limits_{-b}^0\dfrac{dx}{1+x^2}+\lim_{b\to\infty}\int\limits_0^b\frac{dx}{1+x^2}=\lim_{b\to\infty}\left[\arctan(x)\Big|_{-b}^0\right]+\lim_{b\to\infty}\left[\arctan(x)\Big|_0^b\right]$
$=\lim_{b\to\infty}\Big[\arctan(0)-\arctan(-b)\Big]+\lim_{b\to\infty}\Big[\arctan(b)-\arctan(0)\Big]=\frac{\pi}{2}+\frac{\pi}{2}=\pi$
Improper integrals can also be used when over a defined area when there is a vertical asymptote. For example,
$\int\limits_0^1\dfrac{dx}{\sqrt{x}}=\lim_{a\to0^+}\int\limits_a^1\frac{dx}{\sqrt{x}}=\lim_{a\to0^+}\left[2\sqrt{x}\Big|^1_a\right]=\lim_{a\to0^+}\Big[2\sqrt1-2\sqrt{a}\Big]=2$
Examples of improper integrals
Community content is available under CC-BY-SA unless otherwise noted.
| 2019-12-14T23:11:15 |
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https://www.zbmath.org/authors/?q=ai%3Afishburn.peter-c
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## Fishburn, Peter Clingerman
Compute Distance To:
Author ID: fishburn.peter-c Published as: Fishburn, Peter C.; Fishburn, P. C.; Fishburn, Peter; Fishburn, P.; Fischburn, Peter C.; Fischburn, P. C. more...less External Links: MGP · Wikidata · dblp · GND · IdRef
Documents Indexed: 423 Publications since 1964, including 10 Books 1 Contribution as Editor · 4 Further Contributions Biographic References: 5 Publications Co-Authors: 90 Co-Authors with 197 Joint Publications 3,257 Co-Co-Authors
all top 5
### Co-Authors
229 single-authored 31 Gehrlein, William V. 30 LaValle, Irving H. 13 Brams, Steven J. 13 Roberts, Fred S. 11 Trotter, William T. jun. 10 Erdős, Pál 8 Calderbank, Arthur Robert 7 Reeds, James A. 7 Shepp, Lawrence Alan 6 Lagarias, Jeffrey C. 5 Rabinovich, Asya 4 Luce, Robert Duncan 4 Odlyzko, Andrew M. 4 Wright, Paul E. 3 Bell, David E. 3 Chung, Fan 3 Fiorini, Samuel 3 Graham, Ronald Lewis 3 Keeney, Ralph L. 3 Rubinstein, Ariel 3 Sarin, Rakesh Kumar 2 Baker, Kirby A. 2 Balch, Michael 2 Dyer, James S. 2 Edelman, Paul H. 2 Falmagne, Jean-Claude 2 Farquhar, Peter H. 2 Hwang, Frank Kwangming 2 Kim, Jeong Han 2 Marcus-Roberts, Helen M. 2 Monjardet, Bernard 2 Pollak, Henry O. 2 Spencer, Joel H. 2 Steuer, Ralph E. 2 Tanenbaum, Paul J. 2 Tetali, Prasad 2 Trenk, Ann N. 2 Wallenius, Jyrki 2 Wei, Victor K.-W. 2 Winkler, Peter M. 2 Zionts, Stanley 1 Allais, Maurice 1 Amihud, Yakov 1 Aoki, Masahiko 1 Beck, István 1 Bejlegaard, Niels 1 Best, Mark R. 1 Bhat, U. Narayan 1 Bogart, Kenneth P. 1 Bolker, Ethan D. 1 Booth, E. T. 1 Brightwell, Graham R. 1 Burnashev, Marat V. 1 Campbell, Donald E. 1 Chipman, John S. 1 Churchman, C. West 1 Costello, Daniel J. jun. 1 Cowan, Thomas A. 1 Cyert, Richard M. 1 Deb, Kalyanmoy 1 DeGroot, Morris H. 1 Denardo, Eric V. 1 Doble, Christopher W. 1 Doignon, Jean-Paul 1 Doyle, Peter G. 1 Du, Ding-Zhu 1 Duel-Hallen, Alexandra 1 Edwards, Ward 1 Elmaghraby, Salah E. 1 Ewacha, Kevin 1 Felsner, Stefan 1 Ferejohn, John A. 1 Frankl, Péter 1 Freed, Daniel Stuart 1 Furedi, Zoltan 1 Gao, Biao 1 Glover, Fred W. 1 Gopinath, B. 1 Gorowitz, S. 1 Hagen, Ole 1 Hammer, Peter Ladislaw 1 Isaacs, H. H. 1 Isaak, Garth T. 1 Jeffrey, Richard C. 1 Kelly, Jerry S. 1 Kilgour, D. Marc 1 Kochenberger, Gary A. 1 Konishi, Hideo 1 Krantz, David H. 1 Langley, Larry J. 1 Larsson, Stig 1 Lasdon, Leon S. 1 Lee, Hikyu 1 Leinfellner, Werner 1 Lévy, Yannick 1 MacCrimmon, Kenneth R. 1 Mangasarian, Olvi L. 1 Marschak, Jacob 1 Maskin, Eric Stark 1 Mirkin, Boris G. ...and 22 more Co-Authors
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### Serials
32 Journal of Mathematical Psychology 25 Order 21 Discrete Mathematics 20 Discrete Applied Mathematics 18 Theory and Decision 17 Mathematical Social Sciences 16 Journal of Economic Theory 16 Operations Research 15 Econometrica 14 Social Choice and Welfare 13 Management Science 10 Journal of Risk and Uncertainty 9 Mathematics of Operations Research 9 SIAM Journal on Discrete Mathematics 7 Journal of Combinatorial Theory. Series B 7 Economics Letters 7 Annals of Mathematical Statistics 6 Journal of Mathematical Economics 6 SIAM Journal on Algebraic and Discrete Methods 5 Journal of Graph Theory 5 Annals of Operations Research 5 SIAM Journal on Applied Mathematics 5 Management Science. Ser. A, Theory Series 4 Computers & Mathematics with Applications 4 IEEE Transactions on Information Theory 4 International Economic Review 4 The Review of Economic Studies 4 Journal of Multi-Criteria Decision Analysis 3 Psychometrika 3 The Annals of Statistics 3 International Journal of Game Theory 3 Journal of Combinatorial Theory. Series A 3 The Journal of Mathematical Sociology 3 Computational Geometry 2 The Annals of Probability 2 Applied Mathematics and Optimization 2 Ars Combinatoria 2 Naval Research Logistics 2 The Quarterly Journal of Economics 2 Synthese 2 European Journal of Combinatorics 2 Operations Research Letters 2 Statistical Science 2 Discrete & Computational Geometry 2 European Journal of Operational Research 2 SIAM Review 2 Geombinatorics 2 Journal of Combinatorial Theory 2 Naval Research Logistics Quarterly 2 Theory and Decision Library 1 American Mathematical Monthly 1 Mathematics Magazine 1 The Fibonacci Quarterly 1 Geometriae Dedicata 1 INFOR. Information Systems and Operational Research 1 Journal of Approximation Theory 1 Journal of Number Theory 1 Journal of Optimization Theory and Applications 1 Journal of Pure and Applied Algebra 1 Mathematical Programming 1 Mathematical Systems Theory 1 Networks 1 Normat 1 Pacific Journal of Mathematics 1 Proceedings of the American Mathematical Society 1 Theoretical Computer Science 1 Journal of Classification 1 Graphs and Combinatorics 1 Algorithmica 1 Mathematical and Computer Modelling 1 Journal of the Ramanujan Mathematical Society 1 International Journal of Information and Management Sciences 1 Designs, Codes and Cryptography 1 Economic Theory 1 Journal of Combinatorial Designs 1 Mathematical Research Letters 1 Annals of the New York Academy of Sciences 1 Johns Hopkins Series in the Mathematical Sciences 1 Annals of Operations Research
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### Fields
261 Game theory, economics, finance, and other social and behavioral sciences (91-XX) 83 Order, lattices, ordered algebraic structures (06-XX) 68 Combinatorics (05-XX) 30 Operations research, mathematical programming (90-XX) 25 Probability theory and stochastic processes (60-XX) 19 Convex and discrete geometry (52-XX) 16 Statistics (62-XX) 12 Computer science (68-XX) 11 Information and communication theory, circuits (94-XX) 10 Mathematical logic and foundations (03-XX) 7 Number theory (11-XX) 6 Biology and other natural sciences (92-XX) 4 General and overarching topics; collections (00-XX) 4 Geometry (51-XX) 3 Measure and integration (28-XX) 3 Integral transforms, operational calculus (44-XX) 3 Numerical analysis (65-XX) 2 History and biography (01-XX) 2 Linear and multilinear algebra; matrix theory (15-XX) 2 Real functions (26-XX) 1 General algebraic systems (08-XX) 1 Difference and functional equations (39-XX) 1 Approximations and expansions (41-XX) 1 General topology (54-XX)
### Citations contained in zbMATH Open
375 Publications have been cited 5,434 times in 3,277 Documents Cited by Year
Utility theory for decision making. Zbl 0213.46202
Fishburn, P. C.
1970
Intransitive indifference with unequal indifference intervals. Zbl 0191.31501
Fishburn, P. C.
1970
The theory of social choice. Zbl 0253.92006
Fishburn, Peter C.
1973
Interval graphs and interval orders. Zbl 0568.05047
Fishburn, Peter C.
1985
Condorcet social choice functions. Zbl 0369.90002
Fishburn, Peter C.
1977
Betweenness, orders and interval graphs. Zbl 0216.30401
Fishburn, P. C.
1971
The foundations of expected utility. Zbl 0497.90001
Fishburn, Peter C.
1982
Lexicographic orders, utilities and decision rules: a survey. Zbl 0311.90007
Fishburn, Peter C.
1974
Nontransitive measurable utility. Zbl 0499.90006
Fishburn, Peter C.
1982
Decision and value theory. Zbl 0149.16203
Fishburn, P. C.
1964
Approval voting. Zbl 0537.90001
Brams, Steven J.; Fishburn, Peter C.
1983
Interval orders and interval graphs. A study of partially ordered sets. Zbl 0551.06001
Fishburn, Peter C.
1985
Intransitive indifference in preference theory: A survey. Zbl 0195.21404
Fishburn, Peter C.
1970
Nonlinear preference and utility theory. Zbl 0715.90001
Fishburn, Peter C.
1988
Multiple criteria decision making, multiattribute utility theory: The next ten years. Zbl 0825.90620
Dyer, James S.; Fishburn, Peter C.; Steuer, Ralph E.; Wallenius, Jyrki; Zionts, Stanley
1992
Interval representations for interval orders and semiorders. Zbl 0264.06003
Fishburn, Peter C.
1973
Rank- and sign-dependent linear utility models for finite first-order gambles. Zbl 0743.90009
Luce, R. Duncan; Fishburn, Peter C.
1991
Binary choice probabilities: on the varieties of stochastic transitivity. Zbl 0277.92008
Fishburn, Peter C.
1973
Partial orders of dimension 2. Zbl 0247.06002
Baker, K. A.; Fishburn, P. C.; Roberts, F. S.
1972
Multiple criteria decision making, multiattribute utility theory: recent accomplishments and what lies ahead. Zbl 1232.90228
Wallenius, Jyrki; Dyer, James S.; Fishburn, Peter C.; Steuer, Ralph E.; Zionts, Stanley; Deb, Kalyanmoy
2008
Interval orders and circle orders. Zbl 0663.06003
Fishburn, P. C.
1988
Transitive measurable utility. Zbl 0521.90018
Fishburn, Peter C.
1983
Time preference. Zbl 0506.90004
Fishburn, Peter C.; Rubinstein, Ariel
1982
Algebraic aggregation theory. Zbl 0622.90009
Rubinstein, Ariel; Fishburn, Peter C.
1986
Nontransitive preferences in decision theory. Zbl 0723.90004
Fishburn, Peter C.
1991
The axioms of subjective probability. Zbl 0604.60004
Fishburn, Peter C.
1986
Induced binary probabilities and the linear ordering polytope: A status report. Zbl 0751.90004
Fishburn, Peter C.
1992
Paradoxes of preferential voting. Zbl 0521.90006
Fishburn, Peter C.; Brams, Steven J.
1983
Analysis of decisions with incomplete knowledge of probabilities. Zbl 0137.36402
Fishburn, Peter C.
1965
Optimal portfolios with one safe and one risky asset: Effects of changes in rate of return and risk. Zbl 0325.90008
Fishburn, Peter C.; Porter, R. Burr
1976
Subjective expected utility: A review of normative theories. Zbl 0452.90004
Fishburn, Peter C.
1981
Stochastic dominance and moments of distributions. Zbl 0434.90014
Fishburn, Peter C.
1980
Axioms for lexicographic preferences. Zbl 0326.90005
Fishburn, Peter C.
1975
Expected utility hypotheses and the Allais paradox. Contemporary discussions of decisions under uncertainty with Allais’ rejoinder. Zbl 0468.90002
1979
Utility theory. Zbl 0155.28806
Fishburn, P. C.
1968
Sets uniquely determined by projections on axes. II: Discrete case. Zbl 0752.44002
Fishburn, P. C.; Lagarias, J. C.; Reeds, J. A.; Shepp, L. A.
1991
Norbert Wiener on the theory of measurement (1914, 1915, 1921). Zbl 0780.92029
Fishburn, Peter; Monjardet, Bernard
1992
SSB utility theory and decision-making under uncertainty. Zbl 0553.90017
Fishburn, P. C.
1984
Axioms for approval voting: Direct proof. Zbl 0397.90007
Fishburn, Peter C.
1978
Even-chance lotteries in social choice theory. Zbl 0257.90001
Fishburn, Peter C.
1972
Continua of stochastic dominance relations for bounded probability distributions. Zbl 0352.60015
Fishburn, Peter C.
1976
A study of lexicographic expected utility. Zbl 0227.90008
Fishburn, Peter C.
1971
A note on deriving rank-dependent utility using additive joint receipts. Zbl 0847.90024
Luce, R. Duncan; Fishburn, Peter C.
1995
Bipartite dimensions and bipartite degrees of graphs. Zbl 0861.05035
Fishburn, Peter C.; Hammer, Peter L.
1996
No-hole $$L(2,1)$$-colorings. Zbl 1032.05046
Fishburn, Peter C.; Roberts, Fred S.
2003
Noncompensatory preferences. Zbl 0357.90004
Fishburn, Peter C.
1976
Monotonicity paradoxes in the theory of elections. Zbl 0475.90009
Fishburn, Peter C.
1982
Approval voting. 2nd ed. Zbl 1124.91018
Brams, Steven J.; Fishburn, Peter C.
2007
Proper and unit tolerance graphs. Zbl 0830.05058
Bogart, Kenneth P.; Fishburn, Peter C.; Isaak, Garth; Langley, Larry
1995
Mathematics of decision theory. Zbl 0276.62012
Fishburn, Peter C.
1972
Semiorders and choice functions. Zbl 0313.90002
Fishburn, Peter C.
1975
The probability of the paradox of voting: A computable solution. Zbl 0351.90002
Gehrlein, William V.; Fishburn, Peter C.
1976
The discrete Radon transform and its approximate inversion via linear programming. Zbl 0879.68103
Fishburn, Peter; Schwander, Peter; Shepp, Larry; Vanderbei, Robert J.
1997
SSB utility theory: An economic perspective. Zbl 0553.90016
Fishburn, P. C.
1984
Dominance in SSB utility theory. Zbl 0542.90006
Fishburn, P. C.
1984
Going from theory to practice: the mixed success of approval voting. Zbl 1132.91305
Brams, Steven J.; Fishburn, Peter C.
2005
Preference structures and their numerical representations. Zbl 0914.68181
Fishburn, Peter
1999
A nonlinear, nontransitive and additive-probability model for decisions under uncertainty. Zbl 0633.90002
Fishburn, Peter C.; LaValle, Irving H.
1987
Linear discrepancy and weak discrepancy of partially ordered sets. Zbl 1004.06005
Tanenbaum, Paul J.; Trenk, Ann N.; Fishburn, Peter C.
2001
Aggregation of equivalence relations. Zbl 0607.62141
Fishburn, Peter C.; Rubinstein, Ariel
1986
A mixture-set axiomatization of conditional subjective expected utility. Zbl 0272.90008
Fishburn, Peter C.
1973
On the sphericity and cubicity of graphs. Zbl 0533.05055
Fishburn, Peter C.
1983
Representations of binary decision rules by generalized decisiveness structures. Zbl 0413.90005
Ferejohn, John A.; Fishburn, Peter C.
1979
Markovian dependence in utility theory with whole product sets. Zbl 0142.17304
Fishburn, P. C.
1965
Foundations of risk measurement. I: Risk as probable loss. Zbl 0552.90004
Fishburn, Peter C.
1984
On Harsanyi’s utilitarian cardinal welfare theorem. Zbl 0539.90008
Fishburn, Peter C.
1984
Probabilities of election outcomes for large electorates. Zbl 0399.90007
Gehrlein, William V.; Fishburn, Peter C.
1978
Nontransitive additive conjoint measurement. Zbl 0738.92026
Fishburn, Peter C.
1991
Signed orders and power set extensions. Zbl 0764.90009
Fishburn, Peter C.
1992
Finite linear qualitative probability. Zbl 0851.60002
Fishburn, Peter C.
1996
Probabilistic social choice based on simple voting comparisons. Zbl 0545.90004
Fishburn, P. C.
1984
Comment on the Kannai-Peleg impossibility theorem for extending orders. Zbl 0548.90003
Fishburn, Peter C.
1984
Generalizations of semiorders: A review note. Zbl 0896.06003
Fishburn, Peter C.
1997
Fixed-route cost allocation. Zbl 0515.90056
Fishburn, P. C.; Pollak, H. O.
1983
An analysis of simple voting systems for electing committees. Zbl 0471.90013
Fishburn, Peter C.
1981
Binary probabilities induced by rankings. Zbl 0718.60006
Fishburn, Peter C.
1990
Stochastic dominance on unidimensional grids. Zbl 0845.90022
Fishburn, Peter C.; LaValle, Irving H.
1995
Acyclic sets of linear orders. Zbl 0872.90003
Fishburn, Peter
1997
Context-dependent choice with nonlinear and non-transitive preferences. Zbl 0657.90004
Fishburn, Peter C.; LaValle, Irving H.
1988
Continua of stochastic dominance relations for unbounded probability distributions. Zbl 0449.90006
Fishburn, Peter C.
1980
Interdependence and additivity in multivariate, unidimensional expected utility theory. Zbl 0153.49302
Fishburn, P. C.
1967
Semiorders and risky choices. Zbl 0157.26603
Fishburn, P. C.
1968
Continuous nontransitive additive conjoint measurement. Zbl 0718.90010
Fishburn, Peter C.
1990
Non-cooperative stochastic dominance games. Zbl 0372.90133
Fishburn, P. C.
1978
Sets of uniqueness and additivity in integer lattices. Zbl 1105.92332
Fishburn, Peter C.; Shepp, Lawrence A.
1999
State-independent subjective expected lexicographic utility. Zbl 0762.90007
Lavalle, Irving H.; Fishburn, Peter C.
1992
Fair division of indivisible items between two people with identical preferences: Envy-freeness, Pareto-optimality, and equity. Zbl 1069.91502
Brams, Steven J.; Fishburn, Peter C.
2000
Full color theorems for $$L(2,1)$$-colorings. Zbl 1116.05027
Fishburn, Peter C.; Roberts, Fred S.
2006
Maximum planar sets that determine $$k$$ distances. Zbl 0868.52007
Erdős, Paul; Fishburn, Peter
1996
Linear discrepancy and bandwidth. Zbl 1004.06006
Fishburn, Peter C.; Tanenbaum, Paul J.; Trenk, Ann N.
2001
A correlational inequality for linear extensions of a poset. Zbl 0562.06002
Fishburn, Peter C.
1984
Foundations of risk measurement. II. Effects of gains on risk. Zbl 0562.92019
Fishburn, Peter C.
1982
Von Neumann-Morgenstern utility functions on two attributes. Zbl 0287.90001
Fishburn, Peter C.
1974
Geometric containment orders: A survey. Zbl 0935.06001
Fishburn, P. C.; Trotter, W. T.
1998
Sensitivity of decisions to probability estimation errors: A reexamination. Zbl 0164.20504
Fishburn, P. C.; Murphy, A. H.; Isaacs, H. H.
1968
One-way expected utility with finite consequence spaces. Zbl 0216.54001
Fishburn, P. C.
1971
Skew symmetric additive utility with finite states. Zbl 0704.90004
Fishburn, Peter C.
1990
Bell inequalities, Grothendieck’s constant, and root two. Zbl 0792.05030
Fishburn, P. C.; Reeds, J. A.
1994
Niche numbers. Zbl 0758.05092
Fishburn, P. C.; Gehrlein, W. V.
1992
Multiattribute nonlinear utility theory. Zbl 0555.90008
Fishburn, Peter C.
1984
Going from theory to practice: the mixed success of approval voting. Zbl 1348.91102
Brams, Steven J.; Fishburn, Peter C.
2010
Multiple criteria decision making, multiattribute utility theory: recent accomplishments and what lies ahead. Zbl 1232.90228
Wallenius, Jyrki; Dyer, James S.; Fishburn, Peter C.; Steuer, Ralph E.; Zionts, Stanley; Deb, Kalyanmoy
2008
Approval voting. 2nd ed. Zbl 1124.91018
Brams, Steven J.; Fishburn, Peter C.
2007
Full color theorems for $$L(2,1)$$-colorings. Zbl 1116.05027
Fishburn, Peter C.; Roberts, Fred S.
2006
Going from theory to practice: the mixed success of approval voting. Zbl 1132.91305
Brams, Steven J.; Fishburn, Peter C.
2005
Weak order polytopes. Zbl 1077.91016
Fiorini, S.; Fishburn, P. C.
2004
No-hole $$L(2,1)$$-colorings. Zbl 1032.05046
Fishburn, Peter C.; Roberts, Fred S.
2003
Fair division of indivisible items. Zbl 1073.91010
Brams, Steven J.; Edelman, Paul H.; Fishburn, Peter C.
2003
Facets of linear signed order polytopes. Zbl 1077.91017
Fiorini, Samuel; Fishburn, Peter
2003
Extendability of cyclic orders. Zbl 1036.06003
Fiorini, Samuel; Fishburn, Peter C.
2003
Probability weights in rank-dependent utility with binary even-chance independence. Zbl 1060.91045
Bell, David E.; Fishburn, Peter C.
2003
Acyclic sets of linear orders: a progress report. Zbl 1072.05501
Fishburn, Peter C.
2002
Pinwheel scheduling: Achievable densities. Zbl 1016.68007
Fishburn, P. C.; Lagarias, J. C.
2002
Subset comparisons for additive linear orders. Zbl 1082.06002
Fishburn, Peter C.; Pekeč, Aleksandar; Reeds, James A.
2002
Containment orders for similar ellipses with a common center. Zbl 1012.06003
Fishburn, P. C.; Trotter, W. T.
2002
Linear discrepancy and weak discrepancy of partially ordered sets. Zbl 1004.06005
Tanenbaum, Paul J.; Trenk, Ann N.; Fishburn, Peter C.
2001
Linear discrepancy and bandwidth. Zbl 1004.06006
Fishburn, Peter C.; Tanenbaum, Paul J.; Trenk, Ann N.
2001
A nail-biting election. Zbl 1069.91523
Brams, Steven J.; Fischburn, Peter C.
2001
Strong one-switch utility. Zbl 1232.91151
Bell, David E.; Fishburn, Peter C.
2001
Cancellation conditions for finite two-dimensional additive measurement. Zbl 1015.91057
Fishburn, Peter C.
2001
Fair division of indivisible items among people with similar preferences. Zbl 0980.91013
Edelman, Paul; Fishburn, Peter
2001
Almost connected orders. Zbl 0991.06003
Doble, Christopher W.; Doignon, Jean-Paul; Falmagne, Jean-Claude; Fishburn, Peter C.
2001
Signed orders, choice probabilities, and linear polytopes. Zbl 1051.91085
Fishburn, Peter C.
2001
Counting split intervals orders. Zbl 0989.06004
Reeds, James A.; Fishburn, Peter C.
2001
Fair division of indivisible items between two people with identical preferences: Envy-freeness, Pareto-optimality, and equity. Zbl 1069.91502
Brams, Steven J.; Fishburn, Peter C.
2000
Utility functions for wealth. Zbl 0961.91007
Bell, David E.; Fishburn, Peter C.
2000
Optimal linear arrangement of a rectangular grid. Zbl 0949.05044
Fishburn, Peter; Tetali, Prasad; Winkler, Peter
2000
Interference patterns in bijective colorings of 2-regular graphs. Zbl 1007.05044
Fishburn, Peter; Wright, Paul E.
2000
On an Erdős problem for distinct distances in convex polygons. Zbl 1112.52300
Fishburn, Peter
2000
Preference structures and their numerical representations. Zbl 0914.68181
Fishburn, Peter
1999
Sets of uniqueness and additivity in integer lattices. Zbl 1105.92332
Fishburn, Peter C.; Shepp, Lawrence A.
1999
Finite three-dimensional partial orders which are not sphere orders. Zbl 0941.06005
Felsner, Stefan; Fishburn, Peter C.; Trotter, William T.
1999
Split semiorders. Zbl 0935.06002
Fishburn, Peter C.; Trotter, William T.
1999
Competitive pricing of information goods: Subscription pricing versus pay-per-use. Zbl 0917.90041
Fishburn, Peter C.; Odlyzko, Andrew M.
1999
Cycle orders. Zbl 0963.06003
Fishburn, P. C.; Woodall, D. R.
1999
MCDA: Theory, practice and the future. Zbl 0920.90082
Fishburn, Peter C.; Lavalle, Irving H.
1999
Duplicated distances in subsets of finite planar sets. Zbl 0941.52014
Erdős, Paul; Fishburn, Peter
1999
Geometric containment orders: A survey. Zbl 0935.06001
Fishburn, P. C.; Trotter, W. T.
1998
Subjective expected lexicographic utility with infinite state sets. Zbl 0998.91013
Fishburn, Peter C.; LaValle, Irving H.
1998
Isosceles planar subsets. Zbl 0938.52013
Fishburn, P.
1998
Linear extensions of additive partial orders. Zbl 0904.06001
Fishburn, Peter
1998
Dimensions of split semiorders. Zbl 0904.06004
Fishburn, Peter C.; Trotter, William T.
1998
Utility of wealth in nonlinear utility theory. Zbl 0944.91020
Fishburn, Peter
1998
Interference-minimizing colorings of regular graphs. Zbl 0912.05036
Fishburn, P. C.; Kim, J. H.; Lagarias, J. C.; Wright, P. E.
1998
Subjective expected lexicographic utility: Axioms and assessment. Zbl 0907.90036
Fishburn, Peter C.; LaValle, Irving H.
1998
The discrete Radon transform and its approximate inversion via linear programming. Zbl 0879.68103
Fishburn, Peter; Schwander, Peter; Shepp, Larry; Vanderbei, Robert J.
1997
Generalizations of semiorders: A review note. Zbl 0896.06003
Fishburn, Peter C.
1997
Acyclic sets of linear orders. Zbl 0872.90003
Fishburn, Peter
1997
Failure of cancellation conditions for additive linear orders. Zbl 0911.92034
Fishburn, Peter C.
1997
On 1-rate wide-sense nonblocking for 3-stage Clos networks. Zbl 0890.68009
Fishburn, Peter; Hwang, F. K.; Du, D. Z.; Gao, B.
1997
Discount-neutral utility models for denumerable time streams. Zbl 0892.90015
Fishburn, Peter; Edwards, Ward
1997
Cancellation conditions for multiattribute preferences on finite sets. Zbl 0901.90018
Fishburn, Peter C.
1997
Distances in convex polygons. 1st ed. Zbl 0872.52008
Fishburn, Peter
1997
Distinct distances in finite planar sets. Zbl 0894.52007
Erdős, Paul; Fishburn, Peter
1997
Score certificates for tournaments. Zbl 0865.05044
Kim, Jeong Han; Tetali, Prasad; Fishburn, Peter
1997
Super Arrovian domains with strict preferences. Zbl 0876.90008
Fishburn, Peter C.; Kelly, Jerry S.
1997
Bandwidth edge counts for linear arrangements of rectangular grids. Zbl 0888.05049
Fishburn, Peter; Wright, Paul
1997
Bipartite dimensions and bipartite degrees of graphs. Zbl 0861.05035
Fishburn, Peter C.; Hammer, Peter L.
1996
Finite linear qualitative probability. Zbl 0851.60002
Fishburn, Peter C.
1996
Maximum planar sets that determine $$k$$ distances. Zbl 0868.52007
Erdős, Paul; Fishburn, Peter
1996
Minimal winning coalitions in weighted-majority voting games. Zbl 0858.90145
Fishburn, Peter C.; Brams, Steven J.
1996
Cardinal admissibility and optimability in finite nonarchimedean decision theory. Zbl 0851.90017
LaValle, I. H.; Fishburn, P. C.
1996
On the varieties of matrix probabilities in nonarchimedian decision theory. Zbl 0855.90002
LaValle, Irving H.; Fishburn, Peter C.
1996
Binary interactions and subset choice. Zbl 0912.90001
Fishburn, Peter C.; LaValle, Irving H.
1996
Convex nonagons with five intervertex distances. Zbl 0849.52014
Erdős, Paul; Fishburn, Peter
1996
Structuring and assessing linear lexicographic utility. Zbl 0870.90022
LaValle, Irving H.; Fishburn, Peter C.
1996
Structuring and assessing matrix-probability distributions. Zbl 0870.90023
LaValle, Irving H.; Fishburn, Peter C.
1996
Decision theory and discrete mathematics. Zbl 0856.90001
Fishburn, Peter C.
1996
Niche number four. Zbl 0871.05038
Gehrlein, W. V.; Fishburn, P.
1996
Quasi-linear utility in a discrete choice model. Zbl 0875.90210
Konishi, Hideo; Fishburn, Peter
1996
A note on deriving rank-dependent utility using additive joint receipts. Zbl 0847.90024
Luce, R. Duncan; Fishburn, Peter C.
1995
Proper and unit tolerance graphs. Zbl 0830.05058
Bogart, Kenneth P.; Fishburn, Peter C.; Isaak, Garth; Langley, Larry
1995
Stochastic dominance on unidimensional grids. Zbl 0845.90022
Fishburn, Peter C.; LaValle, Irving H.
1995
The invention of the independence condition for preferences. Zbl 0843.90011
Fishburn, Peter; Wakker, Peter
1995
Convex polygons with few intervertex distances. Zbl 0831.68112
Fishburn, Peter
1995
Joint receipt and Thaler’s hedonic editing rule. Zbl 0886.90029
Fishburn, Peter C.; Luce, R. Duncan
1995
Multiplicities of interpoint distances in finite planar sets. Zbl 0831.52008
Erdős, Paul; Fishburn, Peter C.
1995
Lexicographic order preservation and stochastic dominance. Zbl 0836.90018
LaValle, Irving H.; Fishburn, Peter C.
1995
Intervertex distances in convex polygons. Zbl 0831.52009
Erdős, Paul; Fishburn, Peter
1995
Covering properties of convolutional codes and associated lattices. Zbl 0834.94017
Calderbank, A. R.; Fishburn, Peter C.; Rabinovich, Asya
1995
Bell inequalities, Grothendieck’s constant, and root two. Zbl 0792.05030
Fishburn, P. C.; Reeds, J. A.
1994
Maximal three-independent subsets of $$\{0,1,2\}^ n$$. Zbl 0803.51016
Calderbank, A. R.; Fishburn, P. C.
1994
Utility and subjective probability. Zbl 0925.90099
Fishburn, Peter C.
1994
The smallest graphs with niche number three. Zbl 0804.05070
Gehrlein, W. V.; Fishburn, P. C.
1994
On “choice” probabilities derived from ranking distributions. Zbl 0799.92029
Fishburn, Peter
1994
Fairness and social risk. I: Unaggregated analyses. Zbl 0818.90001
Fishburn, Peter C.; Sarin, Rakesh K.
1994
A postscript on distances in convex $$n$$-gons. Zbl 0815.52006
Erdős, Paul; Fishburn, Peter
1994
A variational model of preference under uncertainty. Zbl 0799.90003
Fishburn, Peter
1994
The normalized second moment of the binary lattice determined by a convolutional code. Zbl 0803.94020
Calderbank, A. R.; Fishburn, P. C.
1994
The axioms and algebra of ambiguity. Zbl 0780.90004
Fishburn, Peter C.
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https://dust.trainhub.eumetsat.int/docs/msg_rgb.html
|
MSG SEVIRI RGB composites¶
This notebook provides you an introduction to Level 1.5 data from the SEVIRI instrument as part of the Meteosat Second Generation 0 Degree Service. It further provides you an introduction to the Python package satpy which allows for an efficient handling of data from meteorological satellite instruments, including SEVIRI and MODIS. At the end, a specific focus will be put on the SEVIRI Dust RGB, whose primary aim is to detect dust in the atmosphere.
The example features the saharan dust event during 5./6. February 2021, which brought massive amounts of Saharan dust into central Europe. See a more detailed description of this particular event here.
The Meteosat series have been providing crucial data for weather forecasting since 1977 and is a series of geostationary satellites providing imagery for weather forecasting and climate monitoring. Meteosat Second Genersation (MSG) is the current fleet of operational geostationary satellites. The Spinning Enhanced Visible and InfraRed Imager (SEVIRI) is MSG’s primary instrument and has the capacity to observe the Earth in 12 spectral channels. 11 channels provides measurements with a resolution of 3 km at the sub-satellite and one, the High Resolution Visible (HRV) channel, provides measurements with a resolution of 1 km.
The SEVIRI instrument allows for a complete image scan (Full Earth Scan) every 15 minutes. The 0 Degree Service is the main mission of MSG and provides High Rate SEVIRI image data in 12 spectral bands, processed in near real-time to Level 1.5.
Basic facts
Spatial resolution: 1 km at nadir
Spatial coverage: Latitude: -81 to 81 degrees, Longitude: -79 to 79 degrees
Revisit time: every 15 minutes
Data availability: since 2004
How to access the data
High Rate SEVIRI Level 1.5 Image Data is available for download via the EUMETSAT Data Store. You need to register for the EUMETSAT Earth Observation Portal in order to be able to download data from the Data Store.
import glob
import xarray as xr
import numpy as np
import matplotlib.pyplot as plt
import matplotlib.colors
from matplotlib.axes import Axes
import cartopy
import cartopy.crs as ccrs
from cartopy.mpl.gridliner import LONGITUDE_FORMATTER, LATITUDE_FORMATTER
from cartopy.mpl.geoaxes import GeoAxes
GeoAxes._pcolormesh_patched = Axes.pcolormesh
from satpy.scene import Scene
from satpy.composites import GenericCompositor
from satpy.writers import to_image
from satpy.resample import get_area_def
import pyresample
import warnings
warnings.filterwarnings('ignore')
warnings.simplefilter(action = "ignore", category = RuntimeWarning)
%run ../../functions.ipynb
MSG SEVIRI True color composite¶
Load and browse High Rate SEVIRI Level 1.5 image data¶
Meteosat Second Generation data are disseminated in the specific MSG Level 1.5 Native format. The Python package satpy supports reading and loading data from many input files. With the function available_readers(), you can get a list of all available readers satpy offers. For MSG data and the Native format, you can use the reader seviri_l1b_native.
available_readers()
From the EUMETSAT Data Store, we downloaded for severals hours from 5./6. February 2021 of High Rate SEVIRI Level 1.5 Image data. The data is available in the folder ../../eodata/1_satellite/meteosat/event/. Let us load one image scence for 6 February at 7.27 UTC. First, we specify the file path and create a variable with the name file_name.
file_name = glob.glob('../../eodata/1_satellite/meteosat/event/*2021020607*.nat')
file_name
In a next step, we use the Scene constructor from the satpy library. Once loaded, a Scene object represents a single geographic region of data, typically at a single continuous time range.
You have to specify the two keyword arguments reader and filenames in order to successfully load a scene. As mentioned above, for MSG SEVIRI data in the Native format, you can use the seviri_l1b_native reader.
scn = Scene(reader="seviri_l1b_native",
filenames=file_name)
scn
<satpy.scene.Scene at 0x7fdb8f7cda90>
A Scene object loads all band information of a satellite image. With the function available_dataset_names(), you can see the available bands available from the MSG SEVIRI satellite.
scn.available_dataset_names()
['HRV',
'IR_016',
'IR_039',
'IR_087',
'IR_097',
'IR_108',
'IR_120',
'IR_134',
'VIS006',
'VIS008',
'WV_062',
'WV_073']
The underlying container for data in satpy is the xarray.DataArray. With the function load(), you can specify an individual band by name, e.g. IR_108 and load the data. If you then select the loaded band, you see that the band object is a xarray.DataArray.
scn.load(['IR_108'])
scn['IR_108']
<xarray.DataArray 'reshape-7f46b2a2eee50e746a278c951ee5cd2d' (y: 3712, x: 3712)>
dask.array<truediv, shape=(3712, 3712), dtype=float32, chunksize=(3712, 3712), chunktype=numpy.ndarray>
Coordinates:
acq_time (y) datetime64[ns] NaT NaT NaT NaT NaT NaT ... NaT NaT NaT NaT NaT
crs object PROJCRS["unknown",BASEGEOGCRS["unknown",DATUM["unknown",...
* y (y) float64 -5.566e+06 -5.563e+06 ... 5.566e+06 5.569e+06
* x (x) float64 5.566e+06 5.563e+06 5.56e+06 ... -5.566e+06 -5.569e+06
Attributes: (12/17)
orbital_parameters: {'projection_longitude': 0.0, 'projection_latit...
units: K
wavelength: 10.8 µm (9.8-11.8 µm)
standard_name: toa_brightness_temperature
platform_name: Meteosat-11
sensor: seviri
... ...
name: IR_108
resolution: 3000.403165817
calibration: brightness_temperature
modifiers: ()
_satpy_id: DataID(name='IR_108', wavelength=WavelengthRang...
ancillary_variables: []
With an xarray data structure, you can handle the object as a xarray.DataArray. For example, you can print a list of available attributes with the function attrs.keys().
scn['IR_108'].attrs.keys()
dict_keys(['orbital_parameters', 'units', 'wavelength', 'standard_name', 'platform_name', 'sensor', 'georef_offset_corrected', 'start_time', 'end_time', 'reader', 'area', 'name', 'resolution', 'calibration', 'modifiers', '_satpy_id', 'ancillary_variables'])
With the attrs() function, you can also access individual metadata information, e.g. start_time and end_time.
scn['IR_108'].attrs['start_time'], scn['IR_108'].attrs['end_time']
(datetime.datetime(2021, 2, 6, 7, 15, 11, 201331),
datetime.datetime(2021, 2, 6, 7, 30, 10, 197941))
But for now, let us reload the data file from the beginning. We do not need the IR_108 channel for the next steps, but rather would like to focus on different RGB composites.
scn = Scene(reader="seviri_l1b_native",
filenames=file_name)
scn
<satpy.scene.Scene at 0x7f05fb7933a0>
Browse and visualize RGB composite IDs¶
RGB composites combine multiple window channels of satellite data in order to get e.g. a true-color image of the scene. Depending on the channel combination used, different features can be highlighted in the composite, e.g. dust. SatPy offers several predefined RGB composites options. The function available_composite_ids() returns a list of available composite IDs. You see that there are predefined composites for e.g. natural_color, snow or dust.
scn.available_composite_ids()
[DataID(name='airmass'),
DataID(name='ash'),
DataID(name='cloudtop'),
DataID(name='cloudtop_daytime'),
DataID(name='colorized_ir_clouds'),
DataID(name='convection'),
DataID(name='day_microphysics'),
DataID(name='day_microphysics_winter'),
DataID(name='dust'),
DataID(name='fog'),
DataID(name='green_snow'),
DataID(name='hrv_clouds'),
DataID(name='hrv_fog'),
DataID(name='hrv_severe_storms'),
DataID(name='ir108_3d'),
DataID(name='ir_cloud_day'),
DataID(name='ir_overview'),
DataID(name='ir_sandwich'),
DataID(name='natural_color'),
DataID(name='natural_color_nocorr'),
DataID(name='natural_color_raw'),
DataID(name='natural_color_with_night_ir'),
DataID(name='natural_color_with_night_ir_hires'),
DataID(name='natural_enh'),
DataID(name='natural_enh_with_night_ir'),
DataID(name='natural_enh_with_night_ir_hires'),
DataID(name='natural_with_night_fog'),
DataID(name='night_fog'),
DataID(name='night_ir_alpha'),
DataID(name='night_ir_with_background'),
DataID(name='night_ir_with_background_hires'),
DataID(name='night_microphysics'),
DataID(name='overview'),
DataID(name='overview_raw'),
DataID(name='realistic_colors'),
DataID(name='snow'),
DataID(name='vis_sharpened_ir')]
Let us define a list with the composite ID natural_color. This list (composite_id) can then be passed to the function load(). Per default, scenes are loaded with the north pole facing downwards. You can specify the keyword argument upper_right_corner="NE" in order to turn the image around and have the north pole facing upwards.
composite_id = ['natural_color']
A print of the Scene object scn shows you that it consists of one xarray.DataArray with the standard name natural_color.
print(scn)
<xarray.DataArray 'where-c726622c80224770c3c041125613789c' (bands: 3, y: 3712, x: 3712)>
dask.array<where, shape=(3, 3712, 3712), dtype=float64, chunksize=(1, 3712, 3712), chunktype=numpy.ndarray>
Coordinates:
crs object PROJCRS["unknown",BASEGEOGCRS["unknown",DATUM["unknown",E...
* y (y) float64 5.569e+06 5.566e+06 5.563e+06 ... -5.563e+06 -5.566e+06
* x (x) float64 -5.569e+06 -5.566e+06 ... 5.563e+06 5.566e+06
* bands (bands) <U1 'R' 'G' 'B'
Attributes: (12/20)
georef_offset_corrected: True
area: Area ID: msg_seviri_fes_3km\nDesc...
end_time: 2021-02-06 07:30:10.197941
platform_name: Meteosat-11
sun_earth_distance_correction_applied: True
... ...
optional_datasets: []
name: natural_color
_satpy_id: DataID(name='natural_color', reso...
prerequisites: [DataQuery(name='IR_016', modifie...
optional_prerequisites: []
mode: RGB
The function show() allows you to visualize a loaded composite or band. Let us e.g. visualize the natural_color composite. Once visualized, you see that the RGB composite highlights clouds in turquoise, but highlights specific features in their natural color.
scn.show('natural_color')
Generate a geographical subset for southern Europe¶
The visualization above looks nice, but in many cases you might want to highlight a specific geographical region. Let us generate a geographical subset for southern Europe. You can do this with the function crop() and specifying the keyword argument ll_bbox=(lon_min, lat_min, lon_max, lat_max). Let us take the following bounding box information with a focus over Portugal and Spain: (-5.0, 31.0, 20.0, 51.0).
Afterwards, you can visualize the cropped image with the function show().
scn_cropped = scn.crop(ll_bbox=(-5, 31, 20, 51))
scn_cropped.show("natural_color")
From the cropped image, you can load the area information that is stored as an attribute entry. The area attribute holds information related to the projection, number of columns / rows and area extent.
Note: the area extent key provides x and y values in meters from the nadir, which is the original projection unit.
scn_cropped['natural_color'].attrs['area']
Area ID: msg_seviri_fes_3km
Description: MSG SEVIRI Full Earth Scanning service area definition with 3 km resolution
Projection: {'a': '6378169', 'h': '35785831', 'lon_0': '0', 'no_defs': 'None', 'proj': 'geos', 'rf': '295.488065897014', 'type': 'crs', 'units': 'm', 'x_0': '0', 'y_0': '0'}
Number of columns: 750
Number of rows: 482
Area extent: (-454561.0796, 3151923.5257, 1795741.2947, 4598117.8516)
Another possibility is to crop the data with x and y values in original projection unit (x_min, y_min, x_max, y_max). In the case of MSG SEVIRI data, the projection unit is meters (distance from the nadir). Below we apply the funcion crop() again, but instead of ll_bbox, we use this time the keyword argument xy_bbox=(xmin, ymin, xmax, ymax) and slightly adjust the x and y values from the area extent attribute above.
When we visualize the cropped image again with the function show(), you see that the extent is more or less the same. The adjustment of ymin and ymax has increased the extent towards the north and the south.
scn_cropped = scn.crop(xy_bbox=(-5E5, 30E5, 20E5, 48E5))
scn_cropped.show("natural_color")
As a next step, let us store the area definition as variable and call it area. We can can use the area information to resample the loaded scene object in a next step.
area = scn_cropped['natural_color'].attrs['area']
area
Area ID: msg_seviri_fes_3km
Description: MSG SEVIRI Full Earth Scanning service area definition with 3 km resolution
Projection: {'a': '6378169', 'h': '35785831', 'lon_0': '0', 'no_defs': 'None', 'proj': 'geos', 'rf': '295.488065897014', 'type': 'crs', 'units': 'm', 'x_0': '0', 'y_0': '0'}
Number of columns: 835
Number of rows: 601
Area extent: (-502567.5303, 2998902.9642, 2002769.1132, 4802145.2669)
Cropping is nice and for our geographical area of interest the cropped image looks acceptable. However, when working with regions close to the marging of the scene, the cropped scene can look very distorted, due to the viewing angle of the satellite. For this reason, it is recommended to use the function resample() from the library pyresample, which resamples the loaded scene to a custom area and projection.
Pyresample offers predefined areas; a list of those can be found in the satpy package under /satpy/etc/ in the file areas.yaml. There is no predefined area for our region. For this reason, we can make use of the variable area, which we defined above and which has all the area information needed by the resample() function. Below, we simply pass the area variable to the resample() function.
scn_resample_nc = scn.resample(area)
scn_resample_nc.show('natural_color')
Visualize MSG SEVIRI true color composite with Cartopy features¶
SatPy’s built-in visualization function is nice, but often you want to make use of additonal features, such as country borders. The library Cartopy offers powerful functions that enable the visualization of geospatial data in different projections and to add additional features to a plot. Below, we will show you how you can visualize the natural_color composite with the two Python packages matplotlib and Cartopy.
As a first step, we have to convert the Scene object into a numpy array. The numpy array additionally needs to be transposed to a shape that can be interpreted by matplotlib’s function imshow(): (M,N,3). You can convert a Scene object into a numpy.array object with the function np.asarray().
The shape of the array is (3, 601, 667). This means we have to transpose the array and add index=0 on index position 3.
image = np.asarray(scn_resample_nc["natural_color"]).transpose(1,2,0)
image.shape
(601, 835, 3)
In a next step, we scale the values to a range between 0 and 1 and we clip the lower and upper percentiles. This process sharpens the contrast, as a potential contrast decrease caused by outliers is eliminated.
image = np.interp(image, (np.percentile(image,1), np.percentile(image,99)), (0, 1))
Let us now also define a variable for the coordinate reference system. We take the area attribute from she scn_resample_nc Scene and convert it with the function to_cartopy_crs() into a format Cartopy can read. We will use the crs information for plotting.
crs = scn_resample_nc["natural_color"].attrs["area"].to_cartopy_crs()
Now, we can visualize the natural_color composite. The plotting code can be divided in four main parts:
• Initiate a matplotlib figure: Initiate a matplotlib plot and define the size of the plot
• Specify coastlines and a grid: specify additional features to be added to the plot
• Plotting function: plot the numpy array with the plotting function imshow()
• Set plot title: specify title of the plot
# Initiatie a subplot and axes with the CRS information previously defined
fig = plt.figure(figsize=(16, 10))
ax = fig.add_subplot(1, 1, 1, projection=crs)
# Add coastline features to the plot
ax.coastlines(resolution="10m", color="white")
# Define a grid to be added to the plot
gl = ax.gridlines(draw_labels=True, linestyle='--', xlocs=range(-10,11,5), ylocs=range(30,50,5))
gl.top_labels=False
gl.right_labels=False
gl.xformatter=LONGITUDE_FORMATTER
gl.yformatter=LATITUDE_FORMATTER
gl.xlabel_style={'size':14}
gl.ylabel_style={'size':14}
# In the end, we can plot our image data...
ax.imshow(image, transform=crs, extent=crs.bounds, origin="upper")
# Define a title for the plot
plt.title("Natural color composite of southern Europe, recorded by MSG at " + scn_resample_nc.attrs["start_time"].strftime("%Y-%m-%d %H:%M"), fontsize=20, pad=20.0)
Text(0.5, 1.0, 'Natural color composite of southern Europe, recorded by MSG at 2021-02-06 07:15')
MSG SEVIRI Dust RGB composite¶
In a final step, we would like to have a closer look at the SEVIRI Dust RGB composite, whose primary aim is to support the detection of dust in the atmosphere. The dust composite makes use of three window channels of Meteosat Second Generation:
• Red: IR12.0-IR10.8
• Green: IR10.8-IR.8.7
• Blue: IR10.8
Let us first again load the image from 6 February 2021 at 7.27 UTC as a pytroll Scene object again.
file_name = glob.glob('../../eodata/1_satellite/meteosat/event/*2021020607*.nat')
file_name
Now, let us define a list with the predefined dust RGB composite and let us load this composite with the function load(). Remember, by specifying the keyword argument upper_right_corner='NE', you load the image with North facing upwards.
composite_id = ['dust']
The, we can directly resample the image to the area defined above. You can use the area object and the function resample() to resample the dust RGB composite to the area of interest.
scn_resample_dust = scn.resample(area)
And in a last step, we can visualize the dust composite with Satpy’s built-in visualization function show(). The colours of the dust RGB can be interpreted as follows:
• Magenta: Dust or ash clouds
• Black: Cirrus clouds
• Dark red: Thick, high and cold ice clouds
• Yellow: Thick mid-level clouds
• Darkblue: Humid air in lower levels
• Lilac: Dry air in lower levels
scn_resample_dust.show('dust')
| 2023-03-22T03:19:30 |
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|
http://herschel.esac.esa.int/Docs/AO1/OT1_accepted.html
|
## Solar System (14)
### HCl, HF and H2O+ in comets : probing solar nebula and coma chemistry
Proposal ID: OT1_dbockele_1
Principal Investigator: Dominique Bockelee-Morvan
Time: 25.1 hours priority 1
Category: Comets
Summary:
The composition of comets provides a record of the chemistry of the primitive solar nebula, in the region and at the time of their formation. The presence of interstellar-like organics and other exotic gases in cometary nuclei gives the definite impression that comets preserve a record of the interstellar composition characteristic of the presolar cloud, or that cometary and interstellar molecules formed by similar processes. We propose to take benefit of the unique capacities of Herschel in the sub-millimeter domain and the high sensitivity of HIFI to search for cometary molecules of cosmogonic interest that cannot be observed from the ground, namely HCl (both (35)Cl and (37)Cl isotopes) and HF. These species are the main reservoirs of fluorine and chlorine in the ISM, as measured from Herschel, and are locked onto grains in dense molecular clouds. Their survival during the collapse of the presolar cloud is uncertain, but both HCl and HF should have reformed readily from the released atomic Cl and F in the proto-planetary disk. We expect that these molecules condensed onto pre-cometary grains during the cooling phase of the Solar Nebula. In addition, observations of H2O+ are proposed to constrain the H2O chemistry in cometary atmospheres and to measure accurately the frequency of its 111-000 and 202-111 ortho transitions near 1115 and 742 GHz, respectively, for best interpretation of H2O+ interstellar data.
### Detecting the Largest Rings in the Solar System--Dust Rings from the Irregular Satellites
Proposal ID: OT1_ddan01_1
Principal Investigator: Daniel Tamayo
Time: 12.8 hours priority 1
Category: Solar System Other
Summary:
We propose to extend observations of Saturn's newly discovered Phoebe ring (Verbiscer et al. 2009) to new wavelengths and greater radial range to better characterize the dust properties and constrain the dynamics and particle size distribution of the ring. We will seek similar rings around both Uranus and Neptune. This work is important to understanding the transfer of material from the irregular satellites to the inner regular satellites, the outermost of which can have their surfaces completely transformed by this process. Furthermore, this dust represents an important analogue to the dust observed in debris disks around other stars.
The discovery of the Phoebe ring, as well as work by Turrini et al. (2009), Bottke et al. (2010), and Buratti et al. (1991), among others, suggests that the other giant planets should also possess rings supplied by their irregular satellites. We therefore propose searches for such rings at both Uranus and Neptune. Our proposal is aimed to return important science results for a modest time investment (12.8 hours)
### Probing the Enceladus torus with Herschel
Proposal ID: OT1_elellouc_1
Principal Investigator: Emmanuel Lellouch
Time: 27.2 hours priority 2
Category: Planets
Summary:
Observations of Saturn with HIFI, performed initially in June 2009 and in more details in June 2010 within the framework of the KP-GT Water and related chemistry in the Solar System", have revealed unexpected absorptions in the core of several emission lines of water from Saturn's atmosphere (557 GHz, 987 GHz, 1113 GHz and 1670 GHz). These absorptions cannot occur in Saturn itself; rather we show that they are due to absorption from water in the Enceladus torus", i.e. a cloud of material originating from Enceladus' active plumes, spreading around Saturn and forming a broad toroidal structure centered around Enceladus' orbit at 4 Saturn radii. Based on a comet-like fluorescent excitation model, our preliminary analysis of these data indicate line-of-sight water column densities of (1-3)x10^13 cm-2 and a radial extent of about 2.5 Saturn radii. This discovery provides an entirely new method to probe physical conditions (density, structure, and composition) in the Enceladus torus. Here we propose a detailed follow-up on these observations. The goals are (i) to monitor the variation of these absorptions with viewing geometry, taking advantage thatthe change of aspect in the Saturn system (with the satellite and ring system becoming progressively more open") over the upcoming years (ii) to search for H2O emission directly originating from the torus (iii) to search for several additional compounds such as NH3 (known to be produced by Enceladus' plumes), OH (seen in the UV from HST) and several ionized species (H3O+, H2O+, OH+, expected from torus ionization). The ensemble of data will hopefully provide us with (i) an improved understanding of the excitation conditions in the torus (e.g. on the role of electrons) (ii) an improved understanding of its composition and chemistry (iii) a detailed 3-dimensional view (radial, vertical and longitudinal) of the torus and the ability to directly test physically-based model torus models.
### Probing the extremes of the outer Solar System: short-term variability of the largest, the densest and the most distant TNOs from PACS photometry
Proposal ID: OT1_evileniu_1
Principal Investigator: Esa Vilenius
Time: 29.2 hours priority 1
Category: Kuiper Belt bodies
Summary:
Pluto was believed to be the outermost object in the Solar System until, at the end of the last Millenium, a number of similar objects were found on orbits beyond Neptune. These objects are now being designated as Trans-Neptunian Objects (TNOs) and are believed to be a reminder of a primordial population. The TNO population comprises a wide range of orbital types and spectral features, many of which are of icy nature. Their origin and evolution are still an open question and subject to debate. We propose repeated high-SNR PACS photometry observations of three extreme specimen of the TNO population: (136199) Eris, the largest dwarf planet, (90377) Sedna, the most distant body in the Solar System and (50000) Quaoar, the densest TNO observed so far. We request a total of 51.7 hours of Herschel observing time using different channels, aiming a SNR of 10 or higher. We intend to perform time-series photometry in order to refine physical properties, which have often been determined using coarse thermal models and single-band data in the past, to find hints of thermal IR lightcurves of Eris and Sedna and to make a high SNR observation of the entire lightcurve of Quaoar. Together with available optical lightcurves we can distinguish whether flux variations are due to shape effects or inhomogeneities of the object's surface. We will make use of existing thermal and thermophysical models to refine physical properties, which may be used to recompute density estimations for Eris and Quaoar and to model surface compositions. Herschel is highly suitable for this task, since it offers the highest sensitivity available to date in the far-IR regime, in which TNO emission peaks due their low surface temperatures. Our results will put constraints on some of the important questions concerning the Trans-Neptunian region and will therefore be of vital importance for observers and modelers in Solar System sciences.
### Properties of Jupiter Trojans from far-IR spectroscopy and photometry
Proposal ID: OT1_evileniu_2
Principal Investigator: Esa Vilenius
Time: 44.1 hours priority 2
Category: Asteroids
Summary:
The two swarms of Jovian Trojan asteroids, which librate around Jupiter's Lagrangian points L4 and L5, occupy an intriguing place between the predominantly rocky inner Solar System and its icy outer regions. Their dynamical and physical properties provide crucial constraints on our understanding of the origin and early evolution of the Solar System. When Spitzer enabled the first spectroscopic observations of these objects at mid-IR wavelengths, the spectral signature of fine-grained silicates was found on a number of bright Trojans (Emery et al., 2006; Mueller et al., 2010). This provided a surprising piece of observational evidence between the hypothesized genetic connection between Trojans and cometary nuclei. Thanks to the spectroscopic capabilities of PACS, a completely unexplored wavelength range is now opening up that contains diagnostic features of elusive materials such as crystalline water, hydrous silicates, or organic irradiation residues.
We here propose PACS spectroscopy observations of 4 Jupiter Trojans, the respectively two brightest objects in the L4 and L5 swarms: Hektor, Agamemnon, Patroclus, and Aneas. We also propose a small amount of time for PACS photometric observations in support of spectroscopy. Our sample is sufficiently large to provide our results credibility, but small enough to keep our observing time request modest. Our observations will provide new constraints on the amount of water ice on the surface (if any) and will shed light on the hypothesized previous cometary activity of these objects.
### An Irregular Dust Cloud around Uranus
Proposal ID: OT1_gkennedy_1
Principal Investigator: Grant Kennedy
Time: 16.5 hours priority 2
Category: Satellites
Summary:
The Solar System's irregular satellites have been grinding themselves to oblivion since their capture by the Giant planets billions of years ago. We have developed an evolutionary model of this collisional evolution that matches the known irregular populations and predicts that the cloud of small icy fragments created could be detectable. These circumplanetary clouds may also be detectable around extrasolar planets. We propose to use the SPIRE instrument on Herschel for 16.5 hours to observe a ~1 degree square region around Uranus in search of this cloud of icy particles. Because we expect the surface brightness to be fainter than the Zodiacal, galactic, and cosmic background this observation requires subtraction of two images taken one year apart. The first image is centered on Uranus, but a year later the planet has moved by 4 degrees and the same background is imaged the second time. Discovery of this cloud will be concrete evidence that the irregulars are collisionally evolved and allow a much better estimate of the size distribution between micron size grains and the largest irregulars. Dust cloud structure and asymmetry will provide information on grain properties and their fate, many of which are thought to coat the surfaces of outer regular satellites. The knowledge gained of the irregular satellite populations will allow more informed models of extrasolar circumplanetary swarms and pave the way for their discovery. It would be particularly apt that dust around Uranus is discovered by Herschel, as Uranus itself was discovered by William Herschel in 1781.
### Variability in Ice Giant Stratospheres: Implications for Radiative, Chemical and Dynamical Processes
Proposal ID: OT1_gorton01_1
Principal Investigator: Glenn Orton
Time: 17.1 hours priority 1
Category: Planets
Summary:
We will assess the rotational variability in the stratospheres of the ice giants, Uranus and Neptune, to understand the dynamical and chemical variability of the atmospheric structure of both planets as a function of longitude. This effort follows up observations by the Spitzer IRS that shows consistent evidence for rotational variability of stratospheric hydrocarbons in Uranus and intermediate-term variability in Neptune's emissions, neither of whose origins are not well understood. Herschel provides an opportunity to follow up these observations with its unparalleled sensitivity. Over the 17-hour periods characterizing the equatorial rotation periods of both planets a series of eight PACS dedicated line scans will be made of strategic lines of HD, methane and water vapor. An efficient scheme takes advantage of the simultaneous availability of Uranus and Neptune in Herschel's visibility window. These will assess the variability of hydrocarbons vs temperatures in both atmospheres to an unprecedented accuracy. The results will be analyzed by a team consisting of many members of the Key Project on Water and Related Chemistry in the Solar System'' who will apply their expertise with the data and its analysis, as well as researchers who discovered the Spitzer variability and ground-based inhomogeneity. The data will be examined in the context of models by team members who are experts in radiative transfer, photochemistry, and dynamical modeling of circulation and zonal thermal wave structure. By refining quantitative models for interactions between radiative, dynamical and chemical processes in these two cold but radiatively and dynamically diverse planets, a baseline will be created that will be useful in the interpretation of variability in the spectra of giant exoplanets. This work will also be programmatically useful in the evaluation of the variability of radiation from Uranus and Neptune, both which are key members of the Herschel flux calibration system.
### Nitrogen, Phosphorus and Sulphur Chemistry in Saturn's Atmosphere: Internal and External Origins for HCN, HCP and CS
Proposal ID: OT1_lfletche_1
Principal Investigator: Leigh N. Fletcher
Time: 8 hours priority 1
Category: Planets
Summary:
Our understanding of some of the fundamental physiochemical processes at work within Saturn's gaseous atmosphere is presently limited by the difficulties associated with detection of a number of atmospheric species. Based on our new understanding of Saturn's bulk composition and chemistry from the Cassini mission, Herschel/HIFI offers an unprecedented opportunity to detect these species for the first time, and to place constraints on their origins. Radiative transfer calculations have been used in tandem with chemical modelling to select optimal transitions of HCN, HCP and CS for study by HIFI. These species have never been detected before, but are expected to be important secondary repositories for nitrogen, phosphorus and sulphur in Saturn's atmosphere. Furthermore, the superb spectral resolution of heterodyne spectroscopy is ideal for distinguishing between broad tropospheric absorptions and narrow stratospheric emissions, allowing us to distinguish between internal and external origins for each species. Tropospheric abundances will be compared to expectations from state of the art thermochemical and photochemical models, in addition to predictions of lightning-induced shock chemistry. Stratospheric abundances will be interpreted in terms of external supply of N, P and S-bearing materials, either from large asteroidal/cometary impacts (where shock chemistry in impact plumes is also important) or influx of material from Enceladus, the rings or interplanetary dust particles. As a result, the HIFI search for the first signatures of Saturn's HCN, HCP and CS abundances will serve as vital constraints on internal chemistry and the coupling between Saturn's cold atmosphere and external environment, revealing the fundamental processes at work in the cold outer reaches of our Solar System.
### Analysis of OPRs and D/Hs of hydrogen sulfide in comets: Understanding their natal origin and constraining their place of formation in the protoplanetary disk.
Proposal ID: OT1_lpaganin_1
Principal Investigator: Lucas Paganini
Time: 20 hours priority 2
Category: Comets
Summary:
Measuring the relative amounts of individual species present in the nucleus of a comet can provide information on their formation mechanism, and thus on cometary origins. We propose to investigate ortho-to-para ratios (OPRs) of hydrogen sulfide and further survey its isotopologues (e.g. HDS) to evaluate deuterium-to-hydrogen ratios (D/Hs) of all suitable comets that become available over the performance period of this OT1. We seek to obtain a quantitative analysis of production rates of sulfur species, isotopic fractionation in H2S (HDS/H2S), and the ratio of nuclear spin species for H2S. This can provide a measure of the temperature at which the nuclear spins were last set prior to being incorporated into the nucleus. Comparison of these measurements in comets with those found in interstellar cloud cores, aided with predictions of nebular chemistry, will test the presence of legacy ice from the natal cloud core and the degree of processing experienced by pre-cometary ices.
### The chlorine cycle on Jupiter and Saturn
Proposal ID: OT1_nteanby_2
Principal Investigator: Nicholas Teanby
Time: 6.4 hours priority 2
Category: Planets
Summary:
Hydrogen halides provide key insights into giant planet atmospheres but their detection has so far remained elusive. Herschel/HIFI's low noise and high spectral resolution provides a unique opportunity to detect these species for the first time - with an estimated sensitivity at the sub part per trillion level - an improvement of over three orders of magnitude on the best measurements currently available.
Observing hydrogen halide species provides an exciting new avenue for studying chemical and dynamical processes at work on the giant planets. This proposal will focus on HCl - the halide with the highest predicted abundance and detectablity. HCl could have an internal or external origin - although models predict that an external origin from influx of extraplanetary material is the most likely.
The observed HCl abundances will be used to: (1) Determine the magnitude of external Cl sources and compare exogenic flux environments and physiochemical processes between Jupiter and Saturn. (2) For Jupiter, by comparing the Cl flux to the O flux (from H2O), we can determine the excess Cl flux and measure the proportion of Io's plasma torus that enters the top of the jovian atmosphere. This unique measurement would have implications for the whole Jupiter system. (3) Use the gradient of the vertical profile to determine the efficiency of HCl scavenging by NH3 in the stratosphere and constrain the stratospheric chlorine cycle. (4) Provide the most stringent test of interior thermochemical models to date, by determining limits on the abundance of HCl in the troposphere. This will help constrain the speed at which internal material is dredged up and the efficiency of HCl depletion by formation of ammonia salts. Comparing HCl abundances between Jupiter and Saturn will allow us to probe these processes under different internal and external environments, providing further insight.
### Confirmation of the first detection of HNC on Titan
Proposal ID: OT1_rmoreno_1
Principal Investigator: Raphael Moreno
Time: 12.4 hours priority 1
Category: Satellites
Summary:
Observations of Titan were performed on June 14, 2010 with Herschel/HIFI, as part of the Herschel guaranteed time key programme "Water and related chemistry in the Solar System" (PI: P. Hartogh). These measurements, targetted to the H2O 556.935 GHz line, have shown in addition an unanticipated line at 543.897 GHz. We attribute this emission to HNC(6-5), which would represent the first detection of HNC in Titan's atmosphere. Preliminary interpretation of the data suggests that HNC is confined to the upper atmosphere (above at least 300 km, and may be even higher). HNC is a plausible species in Titan's atmosphere, expected to be produced by dissociative recombination reaction of the ionospheric ion HCNH+ at altitudes above 1000 km. The loss process considered is HNC protonation by reaction with H-bearing ions and H atoms, yielding HCN. An accurate knowledge of the vertical distribution of HNC and HCN at altitudes above 800 km would provide a major constraint for the photochemical formation scheme of HNC. The goal of this proposal are (i) to spectroscopically confirm the presence of HNC in the upper atmosphere of Titan by observing another transition at 906 GHz (ii) to measure the narrow component of HCN at 532 GHz, in order to retrieve its abundance abundance profile over 400-800 km. The so-constrained HNC/HCN ratio in the upper atmosphere will permit us to discriminate between the different possible formation/loss schemes of HNC.
### Probing the atmospheres of Uranus, Neptune and Titan with CH4 lines
Proposal ID: OT1_rmoreno_2
Principal Investigator: Raphael Moreno
Time: 26.3 hours priority 1
Category: Planets
Summary:
Methane is a key species in the Outer Planets. It is the third most abundant molecule in all four Giant Planets, with an abundance of about 2 % in Uranus and Neptune, and reaching 5% (of N2) at the surface of Titan. Because of its large abundance, methane plays a dominant role in governing the atmospheric chemistry of all these planets. Indeed, the photolysis of methane by solar photons initiates a complex chemistry, giving rise to a wealth of hydrocarbons. In the case of Titan, the photochemistry of methane is even more complex, because of the coupled CH4-N2 chemistry taking place in Titan's upper atmosphere. Initial observations of Neptune and Titan, performed in the framework of the GT-KP Water and related chemistry in the Solar System'' (PI: P. Hartogh) have allowed the detection of CH4 emission at 119.6 micron and in several other lines, but with a low spectral resolution. These measurements have constrained the stratospheric abundance of CH4. In the case of Uranus, the PACS measurements of the CH4 line at 159 microns shows only tropospheric absorption, and with a low signal-to-noise ratio. The goal of this proposal is to use the high spectral resolution of HIFI in order to resolve the 1882 GHz methane lines on Neptune and Titan. These optically thick lines will allow to constrain the vertical temperature profiles in their stratospheres, and in Neptune's case, the vertical distribution of methane. For Uranus, we propose to observe again the methane line at 159 micron with PACS, but with a gain of a factor 3 in sensitivity, in order to confirm the detection and better constrain its abundance.
### Herschel portrait of Pluto: measuring the thermal lighcurve and the emissivity of volatile ices
Proposal ID: OT1_sprotopa_1
Principal Investigator: Silvia Protopapa
Time: 31.3 hours priority 2
Category: Kuiper Belt bodies
Summary:
Beyond the orbit of Neptune there exists a population of remnant bodies from the formation of the Solar System; i.e. the Transneptunian objects (TNOs) in the Kuiper belt. Scientific interest in these bodies arises because they are considered to retain the most pristine and least altered material of the Solar System. Improving the knowledge of these distant bodies thus extends the understanding of the origin and evolution of the Solar System. The Pluto/Charon system plays a key role in the study of the Transneptunian region. Much of what we understand of the physical constitution, composition and evolution of the objects in the Kuiper Belt is put into context by studies of Pluto. Herschel is the only facility which gives the opportunity to draw a portrait of the Pluto/Charon system using the thermal wavelength region. In particular we propose to measure Pluto/Charon thermal lightcurve and perform spectroscopic measurements of the system in the range (50-220) micron. These combined measurements will constrain thermal properties (thermal inertia) and emissivities (spectral and bolometric) of the different terrains on Pluto. The observations will provide constraints on the composition, the physical character (grain sizes, mixing characteristics, texture) and the temperature profile within the near-surface layers of Pluto. We intend also to search for signatures of yet unknown surface ices. Furthermore these observations give us the possibility to answer some open questions like: (i) is Pluto's surface changing? (ii) are nitriles and carbon dioxide ices present on the surface of Pluto as predicted? Answering these questions will provide a benchmark for understanding Pluto and all the large TNOs in the Kuiper Belt. Herschel gives the unique opportunity to complement NASA's New Horizons mission to Pluto, expected to arrive in 2015.
### The latitudinal and seasonal variations of D/H and O2 on Mars
Proposal ID: OT1_thencren_1
Principal Investigator: Therese Encrenaz
Time: 26.3 hours priority 1
Category: Planets
Summary:
We propose to use HIFI to determine latitudinal and seasonal variations of HDO, H2-18O, O2 and CO on Mars. The water data will be used to retrieve the D/H ratio and study its variations with latitude and season. The martian D/H ratio, presently poorly known, is a an important parameter as its excess on Mars (about 5 times the terrestrial value) is interpreted as the signature of an early outgassing of the martian atmosphere. In addition, models predict a possible variation of D/H with latitude and season, as an effect of condensation processes and surface/atmosphere interactions. The O2 and CO data will be used to study the cycle of these two non-condensible species as a function of the solar longitude. Results will be compared with climate models which predict significant variations of all these species. Our data will provide important constraints to photochemical models. H2O is known to be maximum at high northern latitudes during northern summer, while CO and O2 are expected to be maximum at high southern latitudes at the same time. Some CO variations have been observed in the infrared but not in the millimeter/submillimeter range so far. No information is presently known about the possibile variations of O2. Herschel is unique in its capability to observe O2 and H2O. We propose to observe Mars in three positions (North, Center and South) at two different seasons, with Ls close to 50 deg. and 120 deg. respectively. We will use AOT II-2 mode (raster scan with DBS) limited to 3 points. We have chosen high-frequency transitions to get the maximum spatial resolution. We propose to observe 3 settings: (1) H218O and HDO around 1630 GHz, (2) O2 and HDO around 1815 GHz and (3) 13CO and C18O around 1867 GHz. The total observing time is 26.3 hours.
## ISM / Star Formation (110)
### Unveiling the kinematics of the MWC49A's ionized disk and outflow with H-recombination line masers.
Proposal ID: OT1_abaezrub_2
Principal Investigator: Alejandro Baez Rubio
Time: 7.2 hours priority 1
Category: Circumstellar/Debris disks
Summary:
% MWC349A, the unique H-maser source observed so far, is a massive star with an ionized outflow believed to be generated in its photoevaporating rotating circumstellar disk. We plan to use the unique spectral capabilities provided by HIFI to perform observations of basically all of the H$\alpha$ recombination lines (from $H26\alpha$ to $H15\alpha$) covered by this instrument. Spectral resolved profiles will reveal essential kinematics inormation of the inner regions of the ionized outflow and the rotating disk. The observed line profile will be compared with the prediction of our non-LTE 3D radiative transfer model to constrain key parameters of the disk-outflow system. From the model's prediction we will stablish if the inner disk is rotating with a Keplerian law, the rotation of the outflow and likely the presence of radial motions (accretion/excretion) in the disk and the location of the lunching point of the outflow. These parameters will help to discriminate between the models proposed for the origin of the outflows and the evolutionary state (pre-main sequence or evolved B[e] stars) of the central star.
### Search for a correlation between planets and debris discs around retired A stars
Proposal ID: OT1_abonsor_1
Principal Investigator: Amy Bonsor
Time: 20.3 hours priority 1
Category: Circumstellar/Debris disks
Summary:
Planet formation leads to two detectable outcomes - planets and debris disks. No correlation between these outcomes has been found for main sequence FGK stars. However, planet formation outcome depends on spectral type. Furthermore, the higher incidence of both planets and debris for A stars makes correlations easier to detect. We propose to test for a debris-planet correlation around A stars, by observing 36 subgiants (retired A stars) with PACS to search for debris disk emission. All of these stars have been searched for planets, and 18 have detections. Our population models, calibrated to main sequence disk evolution statistics, predict that we should detect disks toward 23% of our sample. Comparison of debris incidences in the planet and control samples will quantify any debris-planet correlation, which would provide valuable constraints for planet formation models. Even without such a correlation, we expect to find 4 debris-planet systems, adding to the 10 currently known, which would provide a significant advance in our understanding of the dynamics of planet-disk interactions, and so of how these systems could have formed. Also, since the post-main sequence debris disk population is currently poorly known, any disk discovery (or lack of it) will provide important new constraints on the evolution of debris in this phase.
### Solving the beta Pictoris carbon puzzle by HIFI observations of CII
Proposal ID: OT1_abrandek_1
Principal Investigator: Alexis Brandeker
Time: 8.4 hours priority 1
Category: Circumstellar/Debris disks
Summary:
The nearby young A-star beta Pictoris is well known for its large circumstellar dust disk. The disk is also known to contain gas, which from absorption lines in the UV is found to be overabundant in carbon by a factor ~20. Recently, Herschel/PACS observed very strong emission from the CII line which seems to indicate that the disk is even more abundant in carbon than previously thought, up to a factor of 100 above other elements. This is unexpected, and we propose to investigate this with HIFI high-resolution spectroscopy of the CII 157um line profile. From the known Keplerian velocity field and the line profile, we will be able to constrain the spatial location of the carbon and thus the total carbon mass. The spatial location of the carbon gas will also give clues to its origin, in particular if it is related to the recently discovered planet in a ~10 AU orbit around beta Pic.
### Warm HCN in the planet-formation zone (R<50 AU) of GV Tau
Proposal ID: OT1_afuente_2
Principal Investigator: Asuncion Fuente
Time: 4.6 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
Spitzer NIR observations revealed the presence of warm C2H2 and HCN with large gas phase abundances in the disk around GV Tau N. The emission of these molecules has been interpreted as originated in the disk at R<50 AU, i.e., in the planet formation zone. Recent observations by our team of the HCN 1-0 and 3-2 lines using the IRAM 30m telescope and the Plateau de Bure Interferometer give further support to this interpretation. We propose to complete the mm and NIR observations by observing the HCN 7-6, 11-6 and 13-12 lines with the instrument HIFI on board Herschel. These detections will allow us to carry out a complete study of the HCN excitation, and to estimate the physical conditions (gas temperature and density), the radius and the kinematics of the emitting region. In addition, we will observe key CO and H2O lines in order to determine the amount of warm gas and derive the HCN and H2O abundance in the inner region of this young disk. To determine the physical conditions and chemical composition of this inner disk gas is the key to understand the evolution of the volatile material that becomes incorporated into the planet-forming regions.
### Herschel observations of solar−type stars with planets, planetesimals and dust
Proposal ID: OT1_amoromar_1
Principal Investigator: Amaya Moro-Martin
Time: 11.6 hours priority 1
Category: Circumstellar/Debris disks
Summary:
Similar to the Solar system, there are only 18 planetary systems known to harbor planets and planetesimals. This small sample is of unique value to our understanding of the diversity, dynamical history, and formation mechanisms of extra-solar planetary systems. Here we propose to observe seven of these systems, with spectral types F7-K2 and ages from 0.5-6.4 Gyr. They all show excess emission at 70 um but not at 24 um, implying the presence of an inner region depleted of warm dust, resembling the Solar System in its Jovian planets + Kuiper belt configuration. It is possible to characterize their planetesimal belts from the study of their dust disks. However, the disks SEDs are not known beyond 70 um. Long wavelength observations are of fundamental importance to determine the presence of cold grains, the only tracer of the outer edge of the dust-producing planetesimal belts. Because the latter is a critical parameter to understand the dynamical history and formation of these systems, we propose to carry out PACS 70/160 and SPIRE observations with the main goal of constraining the SEDs at long wavelengths. We have selected PACS 70 to take full advantage of the Herschel’s improved spatial resolution at 70 um compared to Spitzer, opening the opportunity to resolve the cold dust component that traces the planetesimal belt (which extent could be related to the dynamical history of the planetary system), and to detect extended halos (thought to arise from small dust grains on highly eccentric or hyperbolic orbits, that likely relate to the level of dynamical activity in the planetesimal belt). This proposal requires a total of 11.6 hours. The results will increase our understanding of the diversity of planetary systems, helping us place our Solar system into context. Herschel is the only observatory that can carry out the observation required for this study because of its high sensitivity in the wavelength range where the peak of the dust emission may be located.
### Dust and gas in brown dwarf disks: A multi-wavelength survey with Herschel
Proposal ID: OT1_ascholz_1
Principal Investigator: Alexander Scholz
Time: 13.6 hours priority 2
Category: Brown Dwarfs/Very Low-Mass Stars
Summary:
Disks around young brown dwarfs are a valuable test regime for our current understanding of star and planet formation. The disk sizes and masses are key indicators to assess the significance of dynamical encounters for the formation of very low mass objects. The disk mass, together with the properties of the dust, also constrains the potential for planet formation around brown dwarfs, which can be used to evaluate the diversity and ubiquity of planetary systems.
To tackle these science goals, we need constraints on the global characteristics of brown dwarf disks. This requires multi-wavelength observations of the far-infrared/submm continuum to trace the distribution and properties of the dust in the disk, as well as line spectroscopy to probe for the presence and amount of gas in the disk. Herschel is uniquely suited for such a project.
Here we propose to observe a well-characterised and carefully selected sample of 16 brown dwarfs with PACS and SPIRE photometry, complemented by PACS line spectroscopy for the 3 brightest objects. We expect to provide the first robust assessments of the masses and sizes of disks in the substellar regime. For the first time, we will be able to probe the dust opacity and the amount of gas in the brown dwarf regime, crucial parameters for the understanding of the disk physics. These observations will gain further value in synergy with planned submm interferometry campaigns with SMA and ALMA in the next year. Our project constitutes a significant step towards a solid characterisation of brown dwarf disks.
### Tracing global protoplanetary disk dispersal and evolution in Cep OB2
Proposal ID: OT1_asicilia_1
Principal Investigator: Aurora Sicilia-Aguilar
Time: 23 hours priority 2
Category: Circumstellar/Debris disks
Summary:
We propose to use Herschel PACS photometry observations at 70 and 160 microns to study the global structure of protoplanetary disks in different stages of evolution. Our goal is to determine the contribution of the various physical disk dispersal mechanisms (grain growth/settling, planet formation, photoevaporation) for a uniform sample of disks with different ages and stellar masses. Far-IR observations are extremely sensitive to the global disk properties (flaring, small dust grain depletion, total disk mass). The data will constrain the disk structure as well as the way evolution proceeds (inside-out evolution versus homologous depletion), revealing the effects of the different dispersal mechanisms and their interplay depending on the age and mass of the systems. We will study a large sample of disks in the Cep OB2 region, which contains three populations with ages 1, 4, and 12 Myr. Cep OB2 has been extensively studied at optical and IR(Spitzer) wavelengths, so the properties of these stars and their inner disks (including the presence of gas and accretion)have been determined. Millimeter observations are also available for 32 objects. The sample contains 59 disks (observed with IRS) plus ~120 additional cluster members for which we have optical, IRAC and MIPS data. The disks span a wide range of SED types, from flared, primordial disks with small grains to flattened objects without silicate features and transition objects with cleared or optically thin inner disks, and also show differences in the gas content and accretion. By combining the PACS photometry with our available multiwavelength data and our RADMC radiative transfer code for disk modeling, we will be able to trace the global disk structure/dust content of the objects. We will then examine the global trends of disk structure and evolutionary status within the full sample, checking its dependency of age and stellar mass in order to understand the effect of the different physical processes on disk dispersal.
### Physical conditions in PDRs
Proposal ID: OT1_atielens_1
Principal Investigator: Alexander Tielens
Time: 21.1 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
Luminous stars have a profound influence on their environment as their far-UV (6-13.6 eV) photons dissociate and ionize surrounding gas. The gas in these so-called PhotoDissociation Regions (PDRs) is heated by the photo-electric effect on polycyclic aromatic hydrocarbon (PAH) molecules and very small grains (VSG) and cools through emission in atomic fine-structure ([OI], [CII], [SiII]) and molecular rotational (H2, CO) lines. PDR models are known to have intrinsic problems and have moreover only been tested using observations with very large beams on complex regions. Herschel's high sensitivity, high spatial resolution, and wide wavelength coverage allows for the first time a study of the far-IR spectra of spatially resolved PDRs. We propose to map the key diagnostic, far-IR and sub-mm, atomic ([CII] 158μm, [OI] 63, 145μm) and molecular (CO) lines using PACS and SPIRE in a sample of edge-on, spatially resolved Galactic PDRs. The sources in this sample are all well-studied over a wide-wavelength range and have all been mapped by IRS/Spitzer in the rotational H2 lines, the [SiII] 34μm line, the PAH features and the VSG continuum. The goals of our combined Herschel/Spitzer study are to determine the density and temperature structure of the region, to quantify the gas energetics (cooling/heating efficiency), and to compare the gas (heating) characteristics with the emission characteristics of the (neutral & cationic) PAHs and VSGs. This will provide deep insight in the photo-electric heating of atomic gas which is central to the structure of PDRs, the phases of the ISM, and the structure of protoplanetary disks. In addition, these well-known Galactic PDRs provide natural laboratories for studies of the interaction of massive stars with their environment and a semi-empirical way of calibrating the infrared characteristics of regions of massive star formation and, thus, the observational characteristics of galaxies out to the early Universe.
### Testing Planetary Dynamics and Evolutionary History in the HR 8799 Planet/Disc System
Proposal ID: OT1_bmatthew_4
Principal Investigator: Brenda Matthews
Time: 9.8 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose to map the debris disc associated with the multi-planet system HR 8799 in order to constrain the current dynamical state of the planetary system and refine models for dust production in the disc, thereby testing models for the origins of the three known giant planets. Herschel's sensitivity and resolution make it possible to image both the cold planetesimal disc (posited to lie between radii of 90-300 AU) as well as the fainter extended halo (300 - 1000 AU radius) at multiple wavelengths. Direct detection of the edges of the cold belt of dust and an independent measure of the system's inclination will provide critical constraints on models of the planetary orbits within the system, particularly for the outer-most planet for which mass and orbit information can be constrained by simultaneous fits to the planet and disc.
The combination of three massive, coeval, and spectroscopically characterizable planets, together with the dust disc, makes this system a "Rosetta Stone" for planet formation studies. The disc is also important for differentiating between planet formation scenarios. Models predict variations in resonance structure for migration versus in situ formation, and multi-wavelength variations in observed structure within Herschel's wavelength range in the case of planetary migration. This proposal is at the very heart of Herschel's top science goal of understanding the mechanisms involved in the formation of stars and planetary bodies. The resolution, sensitivity and multi-wavelength imaging of Herschel are crucial to this program.
### Probing the physics and dynamics of the hidden warm gas in the youngest protostellar outflows
Proposal ID: OT1_bnisini_1
Principal Investigator: Brunella Nisini
Time: 53.7 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
We propose to obtain PACS and HIFI spectroscopic maps of five outflows driven by young and heavily embedded "Class 0" protostars, in selected transitions of [OI], CO and H2O. These species represent the main coolants of the warm (T ~ 100-2000 K) and dense (10^4 cm^{-3}-10^6 cm^{-3}) shocked gas that gives rise to most of the radiative luminosity of these systems. The immediate objectives of the proposed observations will be: 1) to detect, through a map of the [OI]63um line, the embedded atomic primary jet that should be responsible for the acceleration of the outflow; 2) to map the excitation structure of the molecular warm gas component and understand its role in the dynamics of the system; 3)to derive the spatial variations, as a function of the central source, of the H2O abundance and O/H2O abundance ratio, that will be tracing time-dependent chemical changes during the flow life-time. In order to maximize the scientific return from this program, we have selected sources that will be already mapped in the H2O 557 GHz line within the WISH Key Program. If added to the ground-based and space-borne spectral maps already available for the selected objects, the proposed Herschel observations will represent the first multi-wavelength spatial study of protostellar outflows covering the complete spectral domain of emission (from NIR to mm) of these objects. Such a data-base has a strong legacy value for both future missions and development of theoretical models and numerical simulations of shocks and outflows.
### Disk masses for ~10 Myr old brown dwarf disks
Proposal ID: OT1_briaz_4
Principal Investigator: Basmah Riaz
Time: 3 hours priority 1
Category: Brown Dwarfs/Very Low-Mass Stars
Summary:
We request SPIRE 200-500mu observations for two brown dwarf disks, 2MASSW J1207334-393254 (2M1207) and SSSPM J1102-3431 (SSSPM 1102), in the TW Hydrae Association (TWA). From our previous Spitzer observations, we had confirmed excess emission at wavelengths of ~5-38mu for both of these sources. With the SPIRE observations, we can probe the optically thin dust in the outer cooler regions of these disks. We have performed radiative transfer modeling for these systems. With the available mid-infrared observations, we find high degeneracies for the disk mass and outer disk radius estimates. Observations at far-infrared wavelengths can help constrain the model fits and obtain better estimates for the disk mass and outer radius for these disks. At an age of ~10 Myr, 2M1207 and SSSPM1102 are the oldest known brown dwarf disks. It is thus important to estimate the disk masses for these older disks, and to understand, in comparison with the younger Taurus systems, if brown dwarf disk masses show any decline with the age of the system.
We also request PACS 70mu photometry for another candidate brown dwarf disk in the TWA, 2MASSW J1139511-315921 (2M1139). This object shows an excess emission at 24mu, but none at shorter wavelengths. With 70mu observations, we can confirm if the disk flares up at longer wavelengths. If the presence of such a disk is confirmed for 2M1139, then this would be the first transition disk detected among the sub-stellar members of TWA.
### Do stars with rocky terrestrial planets also have Edgeworth-Kuiper Belts?
Proposal ID: OT1_bzuckerm_1
Principal Investigator: Ben Zuckerman
Time: 4.9 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose to measure with PACS the broadband far-infrared spectrum of some young A- and F-type main sequence stars with known, exceptionally luminous, mid-infrared emission. Such stars are uncommon but are of special interest because they point to and delineate the era of rocky terrestrial planet formation. Herschel observations will establish whether cool dusty regions analogous to the Sun's Kuiper Belt region accompany inner regions where terrestrial planet formation is occurring.
### A Search for Water Ice in Exo-Kuiper Belts
Proposal ID: OT1_cchen01_2
Principal Investigator: Christine Chen
Time: 20 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose to obtain PACS full range spectra of 6 bright debris disks (with 70 micron fluxes >0.5 Jy) that have been spatially resolved in scattered light. We plan to search for far-infrared emission features due to water ice and other species. Herschel PACS is expected to be the premier tool for characterizing dust around debris disks because the grains in debris disks are believed to be (1) large (with minimum blow-out sizes great than one a few microns) and (2) cold (with typical grain temperatures less than 70 K). Our proposed sources possess high albedos, suggestive of water ice. A Herschel detection of water ice would be the first definitive detection of water ice in an external Kuiper Belt.
### Peering into the protostellar shocks: NH3 emission at high-velocities
Proposal ID: OT1_ccodella_1
Principal Investigator: Claudio Codella
Time: 15.8 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
Ammonia and water are key molecules for determining the physical and chemical structure of star forming regions because of their large abundance variations. In shocked regions where jets driven by low-mass protostars impact the surrounding medium, the NH3 and H2O abundances undergo a dramatic enhancement due to ice grain mantle sublimation. Thanks to the very recent HIFI (CHESS KPs) observations performed towards the prototype L1157 outflow, we compared the line profiles due to the NH3(1_0-0_0) and H2O(1_10-1_01) transitions in the HIFI-band 1b. The high-spectral resolution provided by HIFI allowed us to observe a striking difference in profile between water and ammonia, with H2O emitting at definitely higher velocities. In Codella et al. (2010) we propose that such difference reflects different formation mechanisms: while NH3 is believed to be a direct product of grain surface reactions, water is enhanced by the release of the icy mantles as well as by endothermic reactions occurring in the warm (> 220 K) shocked gas, which convert all gaseous atomic oxygen into water.
We propose here the obvious next step, i.e. to observe the NH3(1_0-0_0) line at 572.5 GHz in a sample of 8 bright low-mass outflow spots already observed in the H2O(1_10-1_01) line within the WISH KP. The analysis of the profiles in such sample will allow us to: (i) determine whether the difference in profiles is unique to L1157 or a common characteristic of chemically rich outflows; (ii) provide clues to the physical characteristics of the shock and of the pre-existing material. Such analysis will be performed by using a suite of chemical, PDR, radiative transfer and shocks models which our team has developed.
The present proposal can be considered as a WISH+CHESS KPs synergy and indeed it gathers components of the teams leading the investigations of protostellar outflows in both CHESS and WISH Herschel GT-KPs.
### A Clearer View of Dust Evolution in Protoplanetary Disks
Proposal ID: OT1_cespaill_1
Principal Investigator: Catherine Espaillat
Time: 30 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose to quantify dust evolution in protoplanetary disks around low-mass pre-main sequence stars, the precursors of our own Sun. To this end, we will measure grain growth and settling, the first two steps towards planet formation, in disks located within the star-forming clouds of Taurus, Chamaeleon, and Ophiuchus. In addition to studying "full" disks we will also target objects which are in the process of clearing gaps in their disks, a phenomena which is most likely due to newly formed planets. By combining spectral energy distributions that employ mid-infrared Spitzer and submillimeter Herschel data with spatial brightness distributions obtained with interferometers in the millimeter (SMA, ALMA), we will provide a self-consistent analysis of the amount of dust growth, settling, and clearing in disks, which will also serve as a guide for future disk studies with JWST. The systematic, semi-empirical evidence obtained through this proposed study will provide needed insight and constraints to aid in theoretical modeling of dust evolution and planet formation, bringing us a few steps closer to understanding the origin of our own solar system.
### Settling an Icy Issue: Using Dust and Ice in Young Disks to Constrain Theoretical Models
Proposal ID: OT1_cespaill_2
Principal Investigator: Catherine Espaillat
Time: 20.8 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose to obtain PACS range spectroscopy to measure the amount of water ice and dust evolution in protoplanetary disks located within the ~1-2 Myr old Taurus, Chamaeleon, and Ophiuchus clouds. Theoretical works show that grain growth and dust settling are critical first steps in forming planets and that the ice content of disks plays an influential role in the coagulation process. However, the amount of dust evolution actually experienced by disks and their real ice content is largely unconstrained. To provide a quantitative link between theory and observations we will target 40 disks, many of which show signs of planet formation as inferred from gaps and holes in their dust distribution. We will use irradiated accretion disk models to do a self-consistent analysis of their spectral energy distributions utilizing multi-wavelength data from Spitzer and Herschel. This study will determine the degree of dust evolution experienced by the disks and their ice abundances which can serve as constraints for theoretical models of disk evolution and planet formation.
### Physics of gas evaporation at PDR edges
Proposal ID: OT1_cjoblin_1
Principal Investigator: Christine Joblin
Time: 9.8 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
Far-ultraviolet (FUV) photons in massive OB star-forming regions have a major impact on the structure, dynamics, chemistry and thermal balance of their associated molecular cloud. We propose to study the photoevaporation under FUV irradiation of dense filaments in prototype photodissociation regions (PDR) by mapping with the HIFI spectrometer the [CII] 158 micron line associated with the evaporating gas and high-J CO lines tracing the warm dense structures. The combination of the spectral range covered by Herschel and the very high spectral resolution of HIFI is unique to get insight into the process of mixing of cold molecular gas into warm atomic gas. This process governs the evolution of dense gas submitted to FUV photons in a wide variety of astronomical objects including protostellar and protoplanetary disks but is best studied in PDRs. We ask for 9.8 hours of observations in two PDRs, NGC7023 and the Horsehead nebula. NGC7023 is illuminated by a B2Ve star and hosts very diluted atomic gas and dense filaments. The Horsehead nebula is a PDR viewed nearly edge-on with a high gas density gradient at the edge that is illuminated by a O9.5V star and is immersed in an HII region. In these objects, there is evidence for dynamical processes that create a mixing layer between molecular and atomic gas, both from gas kinematics (first results with HIFI on the [CII] line) and chemistry. The first HIFI [CII] results clearly call for a larger spatial coverage of the region using OTF mapping mode with HIFI to obtain a more complete picture of the PDR morphology and dynamics. The 12^CO(8-7) and 13^CO(8-7) lines will be also targeted to trace the warm interfaces of the dense filaments/edges. The team gathers together specialists of the studied regions and of the Herschel instruments: HIFI (this proposal), SPIRE and PACS (complementary data). The team has strong expertise in the study of the physics and chemistry of PDRs, both in terms of data analysis and modelling using and developing the Meudon PDR code.
### Exploring the gaseous component of debris disks of high fractional luminosity : a deep [O I] 63.2 micron survey with Herschel.
Proposal ID: OT1_ckiss_1
Principal Investigator: Csaba Kiss
Time: 17.2 hours priority 2
Category: Circumstellar/Debris disks
Summary:
Gas-rich primordial disks and tenuous gas-poor debris disks are usually considered as two distinct evolutionary phases of the circumstellar matter. However, there is a very small interesting group of stars in our neighbourhood (49 Ceti, and our discovery HD 21997), which may represent the missing link between these phases as indicated by the unexpected presence of debris-like dust content and measurable CO gas component. With the aim of discovering and characterizing more of these spectacular objects here we propose to obtain [O I] 63 micron observations of a sample of carefully selected young (<50Myr) debris disks of high fractional luminosity with Herschel/PACS. Our objectives are to 1) discover and determine the incidence of 49 Ceti-like gaseous debris disks; 2) characterize disk structure; 3) determine the timescale of gas dispersal; 4) perform a detailed investigation of HD 21997. New discoveries would lead to the definition of a new subclass of circumstellar disks, the gaseous debris disks. We required 17.2h of Herschel time for the observations.
### Herschel characterization of the new class of dusty first-ascent giant stars
Proposal ID: OT1_cmelis_1
Principal Investigator: Carl Melis
Time: 13.1 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We have recently discovered a new class of first-ascent giants surrounded by substantial dusty and gaseous disks that are sometimes accreting onto the central star. These old stars, who are nearing the end of their lives, are experiencing a rebirth into characteristics typically associated with newborn stars. As such we dub them "Phoenix Giants". As a critical step to understanding these unique systems and the origin of their circumstellar material, we propose Herschel PACS and SPIRE imaging observations to characterize their dusty disks. We expect that Herschel observations of Phoenix Giant disks will establish a benchmark characterization of the outer disk regions of this recently discovered class of first-ascent giant stars.
### Investigation of the nitrogen chemistry in diffuse and dense interstellar gas
Time: 18 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
We propose to investigate the interstellar chemistry and physics of nitrogen through Herschel/HIFI observations of simple nitrogen-hydride molecules including NH, NH2, NH3, and related ions. The nitrogen chemistry is still rather uncertain and we therefore propose to compare and contrast the abundances and ortho/para ratios of nitrogen hydrides in the diffuse interstellar gas to the dense cores of molecular clouds. This comparison can be done very efficiently by observing excited-state transitions in selected cores that have previously been used in the PRISMAS program as background sources for absorption measurements in the ground-state transitions. In this way, we will determine whether nitrogen chemistry is dominated by gas-phase reactions or by processes on surfaces of dust grains, and whether the dominant chemistry is different in different parts of the interstellar medium. In summary, we propose HIFI observations of 5 transitions of simple nitrogen-bearing molecules in 8 sources, and 3 transitions in 2 sources. The total requested observing time is 26.2 hours.
### The neutral disk of MWC349
Proposal ID: OT1_cthum_1
Principal Investigator: Clements Thum
Time: 5.7 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We wish to study the circumstellar disk of the bright radiostar MWC349 with the aim to infer the evolutionary state of this prominent but enigmatic massive stellar object. We propose to make a full wavelength range scan with PACS and with the SPIRE spectrometer in order to determine the continuum spectrum of the disk, especially in the ill determined or unexplored wavelength region centered on 200-300 microns where the emission from the ionized wind and the warm circumstellar dust are comparably strong.
These spectral scans are at least 10x more sensitive than our ISO data, and permit a deep search for molecules like water and CO. The presence of water which is being found by Herschel in a range of accretion disks young stellar objects would be strong evidence for the nature of the MWC349 disk as due to accretion, whereas the absence of water is most easily explained if the disk results from mass loss in a strong stellar wind or ejection event. Our proposed investigation has thus the potential to resolve the half--century old question about the evolutionary state of MWC349.
### Deuterated water chemistry towards high-mass star-forming regions.
Proposal ID: OT1_cvastel_2
Principal Investigator: Charlotte Vastel
Time: 15.3 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
Observations of the HDO molecules are an important complement for studies of water, since they give strong constraints on the formation processes: grain surfaces versus gas-phase chemistry through energetic process as shocks. HIFI observations of multiple transitions of HDO in SgrB2(M) combined with ground-based observations allowed for the first time the determination of its abundance throughout the envelope. In the framework of the PRISMAS Key Program, a large sample of high-mass star-forming regions have been observed with the detection of many species in their line of sight. The HDO (111-000) fundamental transition has also been detected in absorption at the velocity of the hot core towards the 2 sources that have been observed so far, probably tracing the colder envelope in its surrounding.
We propose to observe higher energy level HDO transitions towards a sample of three compact HII regions that will be targeted by the PRISMAS Key Program (G34.3+0.1, W33A, W49N) in order to perform a full modeling from the hot core through the envelope using a spherical Monte Carlo radiative transfer code, RATRAN, which takes into account radiative pumping by continuum emission from dust. We will use for an optimum accuracy of the modeling the HDO and D2O collision rates with H2, recently computed within our group, that are not available in the public so far.
This study will hopefully give strong constrains on the formation processes of water, combining the proposed observations with published or soon to be published high resolution H2O observations with HIFI towards the same sources.
### Hot Dust within HII Regions
Proposal ID: OT1_cwatso01_1
Principal Investigator: Christer Watson
Time: 5.6 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
We propose observing thermal dust emission inside two wind blown bubbles identified by their PAH emission (N90 and N56 from a Churchwell et al., 2006) in all SPIRE and PACS bands. These bands sample emission from all dust grain sizes and temperatures thought to exist behind the post shocked gas. By measuring the emission across the face of the bubble and comparing with numerical simulations, we will determine how the grain size distribution changes with distance from exciting source. These results will help determine what dominant physics, sputtering or gas-dust friction, dominates grain processing within these sources. We will also measure emission from the cold, dense cloudlets proposed by Everett & Churchwell (2010) as the source of dust within these bubbles. By better characterizing these physical properties of dust grains, we will be able to better predict how dust grains affect the energetics of wind blown bubbles.
### The Conditions of Isolated Dark Clouds with Signs of On Going H2 Formation
Proposal ID: OT1_dli_2
Principal Investigator: Di Li
Time: 1.3 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
We propose to map three nearby isolated dark clouds, CB 45, B227, and L1574 with SPIRE. They are carefully selected based on their intriguing morphology of displacement between CO, 2MASS extinction, atomic gas traced HI Narrow self-absorption (HINSA),which is a unique tracer of cold atomic gas INSIDE molecular clouds. SPIRE maps will provide crucial dust emission information for quantifying dust column density, dust temperature and dust properties. SPIRE will provide much higher resolution than 2MASS extinction and is capable of tracing relatively diffuse dust structure missed by 2MASS. Combining HINSA, molecular gas, extinction, and dust emission data, we will have an unprecedented comprehensive data set for understanding the transition from atomic to molecular ISM. The spacial information and high sensitivity provided by SPIRE will enable us to construct time dependent H2 formation model for realistic clouds. Such a model will provide quantitive answers, for the first time, to fundamental questions in star formation, such as "How molecular are molecular clouds?" and "What is the age of a dark cloud?".
### Ammonia as a Tracer of the Earliest Stages of Star Formation
Proposal ID: OT1_dlis_2
Principal Investigator: Dariusz Lis
Time: 26.3 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
Stars form in molecular cloud cores, cold and dense regions enshrouded by dust. The initiation of this process is among the least understood steps of star formation. High-resolution heterodyne spectroscopy provides invaluable information about the physical conditions (density, temperature), kinematics (infall, outflows), and chemistry of these regions. Classical molecular tracers, such CO, CS, and many other abundant gas-phase species, have been shown to freeze out onto dust grain mantles in pre-stellar cores. However, N-bearing species, in particular ammonia, are much less affected by depletion and are observed to stay in the gas phase at densities in excess of 1e6 cm-3. The molecular freeze-out has important consequences for the chemistry of dense gas. In particular, the depletion of abundant gas-phase species with heavy atoms drives up abundances of deuterated H3+ isotopologues, which in turn results in spectacular deuteration levels of molecules that do remain in the gas phase. Consequently, lines of deuterated N-bearing species, in particular the fundamental lines of ammonia isotopologues, having very high critical densities, are optimum tracers of innermost regions of dense cores.
We propose to study the morphology, density structure and kinematics of cold and dense cloud cores, by mapping the spatial distribution of ammonia isotopologues in isolated dense pre-stellar cores using Herschel/HIFI. These observations provide optimum probes of the onset of star formation, as well as the physical processes that control gas-grain interaction, freeze-out, mantle ejection and deuteration. The sensitive, high-resolution spectra acquired within this program will be analyzed using sophisticated radiative transfer models and compared with outputs of state-of-the-art 3D MHD simulations and chemical models developed by the members of our team.
### Studying diffuse interstellar clouds with observations of hydrides
Proposal ID: OT1_dneufeld_1
Principal Investigator: David Neufeld
Time: 34.8 hours priority 2
Category: Interstellar Medium/HII regions
Summary:
With the use of the HIFI instrument, we propose to observe four simple hydride molecules - HF, OH+, H2O+, and H2Cl+ - in absorption towards five bright submillimeter continuum sources. The target sources, all located in the Galactic plane with sight-lines that intersect multiple interstellar clouds, are the massive star-forming regions W49N, W51, G29.96-0.02, W3(OH), and G330.95-0.17. This selection of sources samples sight-lines in the 1st and 4th quadrants of the Galaxy and in the outer Galaxy. The proposed observations will have integration times sufficient to obtain signal-to-noise ratios in the range 100 - 400 in a single spectral channel, providing great sensitivity to absorption by foreground material. We will thereby determine the molecular column densities in foreground clouds located in spiral arms that lie along the sight-lines to these continuum sources. The four molecules we will observe, all detected previously in the ISM in early Herschel observations, will provide critical information about the diffuse interstellar medium. In particular, HF will permit the identification and study of clouds with a very small H2 column density that may be virtually undetectable in the spectra of other molecules; OH+ and H2O+ will allow us to study clouds with a small molecular fraction (revealed by a large OH+/H2O+ ratio), and to determine the cosmic ray ionization rate as a function of Galactocentric radius; and H2Cl+ will probe the photoionization rate and its variation with position in the Galaxy.
### An accurate mass measurement for prestellar cores
Proposal ID: OT1_dnutter_1
Principal Investigator: David Nutter
Time: 11 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
Prestellar cores are crucial to our understanding of star formation. It is at this evolutionary stage that the stellar mass is set. If we are to understand the origin of the stellar IMF, we must therefore study the masses of the prestellar cores from which the stars are formed. There is currently a large uncertainty in the measured prestellar core mass that we obtain from far-IR and submillimetre observations. This uncertainty is caused by our inability to simultaneously determine the column density, temperature and dust emissivity index from photometric observations. Physical processes such as grain growth, or ice-mantle formation, which are affected by changes in density and temperature, will change the dust emissivity index. By simply taking a canonical value for the emissivity index, we cannot determine the correct mass for prestellar cores.
The SPIRE FTS allows us to break this degeneracy for the first time, and simultaneously measure the column density, temperature and dust emissivity index, and therefore determine accurate masses. We propose to map 16 prestellar cores with the SPIRE FTS, and hence generate accurate maps of their column density. We will map each core using the full FTS field of view. We will be able to determine the absolute value of the dust emissivity index, and also see whether it varies across each of the cores. We have selected cores in different environments in order to study the core-to-core, and cloud-to-cloud variations in the dust properties. We will be able use this information about the relation between the three measured parameters, to more accurately determine masses for a much larger sample of cores for which only photometric data are available.
### PACS Photometry of Nearby Warm Debris Disk Systems from the WISE All-Sky Survey
Time: 52.8 hours priority 1
Category: Circumstellar/Debris disks
Summary:
Debris disks trace the collisional breakdown of asteroid and comet parent bodies orbiting nearby main sequence stars. They are detectable in ~16% of FGK stars, nearly twice as often in A stars, and are almost unknown around M stars. The debris disks of sunlike stars are typically cold analogs of our Kuiper belt with emission peaking near 70 microns wavelength. However, a relatively small number of warm disks are known with emission at 24 microns. These systems are especially interesting because they trace dust in the region likely to host terrestrial planets, where the dust has a short dynamical lifetimes. They also tend to be young systems aged < 1 Gyr. This knowledge of warm debris disks - extrasolar analogs to our solar system's Zodiacal cloud - is based on the 25 year old IRAS survey and observations of selected targets with ISO and Spitzer.
The Wide-Field Infrared Survey Explorer (WISE) has just completed new, sensitive all-sky mapping in the 3.3, 4.6, 12, and 22 micron bands. Association of the WISE sources to Hipparcos and Tycho stars has led to the identification of 99 nearby main sequence stars with robustly detected warm 22 micron excesses not previously known. To determine whether these systems represent outbursts of asteroidal dust production (such as in the HD 69830 system), or simply the Wien side of emission from a cold outer dust belt, photometry at longer wavelengths is needed. We propose Herschel/PACS 70 and 160 micron photometry of this unbiased sample. These data will allow us to fully characterize the dust temperature and infrared luminosity of these systems, allowing them to be understood in the context of other debris disks and disk evolution theory. The sample includes field M stars as close as 12 pc, the first objects of this class seen to have warm dust emission. The results will strongly constrain our picture of the collisional history of inner planetary systems.
### A New Method to Determine the Gas Mass in Protoplanetary Disks
Proposal ID: OT1_ebergin_4
Principal Investigator: Edwin Bergin
Time: 21.1 hours priority 1
Category: Circumstellar/Debris disks
Summary:
The mass of planet-forming disks is one of its most fundanmental quantities and can determine the primary mode of planet formation. Because the dominant constituent, H2, is undetectable, we are forced to adopt indirect methods to trace the total gas content. The primary method used is to observe thermal dust continuum emission at submm/mm wavelengths where the dust emission is optically thin. However, mass estimates are highly uncertain because grain evolution can substantially alter the dust opacity coefficient and the gas-to-dust ratio, which are required to convert total flux to mass. We propose here a dedicated program to use PACS spectroscopy to search for the emission of HD J=1-0 at 112 microns and derive the gas mass from a tracer that uniquely probes H2. HD will co-exist with H2 in the gas phase and is the dominant reservoir of deuterium, carrying the cosmic D atom abundance. Our program is a comprehensive effort where observations will be combined with chemical theory and excitation modeling to enable the conversion of integrated emission to mass. This program offers a unique opportunity to derive disk gas masses via an independent method with important implications for the formation of planetary systems.
### A Systematic Survery of the Water D to H Ratio in Hot Molecular Cores
Proposal ID: OT1_ebergin_5
Principal Investigator: Edwin Bergin
Time: 18 hours priority 2
Category: Interstellar Medium/HII regions
Summary:
The D/H ratio of water and the enrichment of HDO relative to H2O in comets, oceans, and interstellar water vapor, has been posited as one of the primary links between chemistry in the cold (T = 10-20 K) dense interstellar medium (ISM) and chemistry in the Solar Nebula. However, there are only ~10 measurements of HDO/H2O, even in hot (T > 100 K) molecular cores, which have the most favorable chemistry (due to fossil evaporation of D-enriched ices) and excitation. In addition the existing measurements have a wide range of uncertainty, making it impossible to discern the presence of source-to-source variations, which could hint at the origin of deuterium enrichments in the dense ISM. We propose here to change this statistic with a systematic survey of HDO and H2O in a sample of 20 hot molecular cores spanning a two order of magnitude range in mass and luminosity. This will increase the number of known water D/H ratios by ~200%. This program is unique in scope for Herschel and requires the uniformity in calibration and high spectral resolution offered by the HIFI instrument. With the stability of HIFI we will be able to derive D/H ratios with significantly less uncertainty. Our observations will be combined with theoretical chemical models to explore the statistics offered by this sample. By looking at a large number of objects with a range of conditions we aim to unlock the secrets of water deuteration in the interstellar space.
### Low gas to dust ratio in proto-planetary disks: the Carbon content of CQ Tau, MWC 758 and MWC 480
Proposal ID: OT1_echapill_1
Principal Investigator: Edwige chapillon
Time: 6.4 hours priority 2
Category: Circumstellar/Debris disks
Summary:
The study of the transition from gas-rich protoplanetary disk to gas-poor debris disk is crucial to constrain the planetary formation mechanisms. Although it is a key parameter for big gaseous planet formation, the evolution of the gas-to-dust ratio with time and star properties is not yet known. One of the first steps to observationally constrain it is to determine independently the gas mass and the dust mass of disks. The dust content, determined from continuum emission, is better known than the gas content. As molecular hydrogen is not observable at the low temperatures of disks, the gas mass is usually derived from CO observation. However, CO may not be always the main carbon reservoir: it should freeze on grain mantles in the cold mid-plane of T Tauri disks, and be photodissociated in the upper layers by the UV field, leading to CI and CII, especially in disks surrounding A stars. We propose here to characterize the gaseous Carbon content in three disks (CQ Tau, MWC 758 and MWC 480) using the three main C carriers: CO, CI and C+. Previous CO observations indicates warm disks (the temperature being well above the CO freeze-out temperature). Two of them, CQ Tau and MWC 758, have very low CO content and may be in the transition stage between gas-rich and gas poor disks. A low CI content was also found for CQ Tau using APEX. We propose to take advantage of sensitivity of Hershel at 1900 GHz (157 um) and high spectral resolution provided by the HIFI instrument to observe C+ in these disks.
### The Herschel/HIFI insight on the CH+ puzzle
Proposal ID: OT1_efalgaro_1
Principal Investigator: Edith Falgarone
Time: 38.7 hours priority 2
Category: Interstellar Medium/HII regions
Summary:
Seventy years after its discovery in the diffuse interstellar medium, the origin of the CH+ cation is still elusive. Herschel/HIFI offers a unique opportunity to disclose the underlying gas dynamics at the origin of CH+ in the diffuse medium by allowing high sensitivity and high spectral resolution observations of the CH+ (J=1-0) transition, unreachable from the ground: it will be the leading and only instrument and the observations will bring a completely new look at this resilient puzzle.
The abundant CH+ ion is not only a sensitive tracer of the most tenuous phases of the interstellar medium but it is likely a specific tracer of turbulent dissipation, because its formation route is highly endoenergic. We propose absorption spectroscopy observations of mainly the CH+ J=1-0 line, against 10 background dust continuum sources, bright enough to allow us to sample a broad variety of galactic environments. The lines-of-sight will probe the outskirts of star-forming regions, including one InfraRed Dark Cloud, where turbulent dissipation is most intense, and diffuse gas at high galactic latitude where turbulence is milder. The primarily goal of this project is the comparison of the CH+ abundances with model predictions of turbulent dissipation regions, in which dissipation proceeds either in low-velocity shocks or intense velocity-shears. Another goal is testing the possibility that CH+ forms at the turbulent interface between the two thermally stable phases of the interstellar medium.
As HF, CH+ is a potential sensitive tracer of diffuse matter in the early universe. Understanding its origin and the dissipative processes that it traces will shed a new light on galaxy formation and evolution.
### Characterization of the long wavelength features of interstellar Polycyclic Aromatic Hydrocarbons
Proposal ID: OT1_epeeters_1
Principal Investigator: Els Peeters
Time: 9.4 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
Strong emission features at 3.3, 6.2, 7.7, and 11.2 um dominate the mid-infrared spectra of most interstellar objects. These IR features are due to vibrational fluorescence of large (50-150 C-atom) Polycyclic Aromatic Hydrocarbon molecules pumped by UV photons. These species will also have bands at far-infrared wavelength, notably due to 'drum-head' modes. We have performed experimental and theoretical studies that demonstrate that these bands carry unique information, particularly on the size of the emitting species that cannot be obtained from the shorter wavelength bands.
We propose to measure the far-IR spectra of a sample of well-studied PAH sources using PACS and SPIRE. The sample has been carefully selected to show strong mid-IR PAH bands, and a relatively weak dust continuum at the Herschel wavelengths to maximize the line-to-continuum ratio for far-IR PAH bands. These observations are designed to measure infrared bands to a level of 1% of the dust continuum. Together with the Spitzer/ISO studies, the full spectrum of the IR emission features from 3 to 600 um can be determined. In order to determine the implications for the emitting PAHs, we will compare these bands to the PAH database that we have compiled over the last 15 years and analyze the emission using the realistic PAH emission model that we have developed over the years.
### Investigating the origin of the far-infrared emission of the microquasar Cygnus X-1
Proposal ID: OT1_frahoui_1
Principal Investigator: Farid Rahoui
Time: 6.2 hours priority 2
Category: Galactic Other
Summary:
Microquasars are Galactic X-ray binaries exhibiting collimated outflows commonly called jets. In particular, the so-called compact jets are detected almost simultaneously in all the spectral domains, and are characterised by the existence of a spectral break at which they change their emission regime from optically thick to optically thin synchrotron. The determination of this cut-off frequency is fundamental for the understanding of the accretion-ejection processes as it is related to the black hole spin and mass, as well as to the accretion rate. In a previous Spitzer spectroscopic study of Cygnus X-1, we assessed the contribution of the compact jets to the mid-infrared continuum as well as their spectral break. Nevertheless, its accurate value appears to be dependent on the model used to describe the continuum of the companion star, which is the blue supergiant HD226868. Indeed, it changes whether we consider bremsstrahlung from the stellar winds or thermal emission from a circumstellar dust component. We therefore require photometric observations of Cygnus X-1 with PACS, in the blue, green, and red filters, in order to assess the flux density level of the source at 70, 100, and 160 microns. These measurements, combined with our Spitzer spectra, will allow us to discriminate between bremsstrahlung and dust, which will eventually lead us to the accurate determination of the spectral break of the compact jets exhibited by Cygnus X-1.
### Debris Disks around Planet-Bearing Stars
Proposal ID: OT1_gbryden_1
Principal Investigator: Geoffrey Bryden
Time: 67.2 hours priority 1
Category: Circumstellar/Debris disks
Summary:
The relationship between planets and debris disks is unclear. On one hand the direct imaging of planets in three systems with prominent debris disks (beta Pic, HR 8799, and Fomalhaut) suggests a direct link between the two phenomena. Indeed, the eccentric shape of the Fomalhaut dust ring is clearly driven by its shepherding planet, whose existence and eccentricity were correctly predicted based on the disk asymmetry. On the other hand, Spitzer surveys fail to find any correlation between cold debris at 10's of AUs and radial-velocity-detected planets in the inner system. Motivated by Herschel's advantages over Spitzer, we propose to further explore the planet-debris relationship by observing 67 stars known to have planets. For the 9 targets that are already known to have orbiting debris, we will resolve the disks, determining the location of the dust-producing planetesimals and measuring disk asymmetries that may be induced by neighboring planets. For the remainder of the targets we will search for new debris disks and then look within the overall sample for any correlations with planet properties.
### A Disk Census for New Low-Mass Members of TWA
Proposal ID: OT1_gherczeg_1
Principal Investigator: Greg Herczeg
Time: 9.2 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose to conduct a protoplanetary and debris disk survey of 14 recently-identified members of the benchmark (10 Myr) TW Hya Association (TWA). Our new sample expands the member census by tripling of the low-mass population (>M5; <0.2 M_sun). TWA represents a critical age where the longest-lived protoplanetary disks and the youngest debris disks overlap in the same population, so it offers a critical window into the formation and evolution of planetary systems. We specifically propose a PACS 70/160 micron photometric census to identify new disks, and followed by SPIRE 200/250/350 micron photometric observations of all newly-identified disk systems to characterize their SEDs and determine the nature of their circumstellar disks (protoplanetary or debris). Based on the disk fraction among known late-type members (3/6 = 50%), we estimate that 6-7 of our targets are likely to host circumstellar disks; these disks have been incredibly rare until now, so each will be a prime target for future studies of accretion, disk evolution, and planet formation.
### Using PACS and SPIRE photometry and spectroscopy to characterise the discs of Herbig Be stars: structure, gas content and cold crystalline dust composition.
Proposal ID: OT1_gmeeus_1
Principal Investigator: Gwendolyn Meeus
Time: 33.4 hours priority 2
Category: Circumstellar/Debris disks
Summary:
Herbig Be stars are the link between massive protostars and the intermediate-mass Herbig Ae stars. While for this last group the disc has been characterised in terms of flaring/flat geometries in which dust grains grow and settle towards the midplane, and the bulk of the gas dissipates after 5 Myr, the picture of a disc around a more massive star is less clear. Therefore, we propose to observe a sample of 40 Herbig Be stars, in an effort to determine their disc properties. In particular, we aim at answering the following questions: 1) How do these discs dissipate?, 2) Does grain growth and settling occur? 3) Can gas giant planets still form, and what is the stellar upper mass limit for their formation?, and finally 4) How do the Herbig Be discs differ the lower mass Herbig Ae and T Tauri discs? To answer these questions, we propose to use PACS and SPIRE in photometric mode for the whole sample, and in spectroscopic mode for a subset of the 6 brightest - most promising targets. We will complement the proposed observations with existing optical to mid-IR photometry, as well as mid-IR spectroscopy, to construct spectral energy distributions (SED). These SEDs trace the dust continuum and will be analysed with the aid of radiative transfer modelling. For part of the sample, we also have mid-IR images or interferometry, revealing the spatial extend at those wavelengths. In a next step we will relate the derived disc properties with stellar properties. In addition, for the 6 spectroscopic targets we will be able to make a detailed case study of their cold dust and gas content: the forsterite feature at 69 micron reveals the iron content in the crystalline dust, and gas lines of e.g. OI and CO will allow us to constrain the amount of gas still present in the disc, using both radiative transfer modelling as well as thermo-chemical models. The proposed observations will provide a valuable database for a better understanding of the disc structure and evolution in the more massive Herbig Be type stars.
### Water Formation and Destruction Processes in Molecular Clouds
Proposal ID: OT1_gmelnick_1
Principal Investigator: G.J. Melnick
Time: 10 hours priority 2
Category: Interstellar Medium/HII regions
Summary:
The study of water is one of the most compelling and unique science goals of the Herschel mission. Unfortunately, our understanding of water may not be limited by the quality of the data so much as by remaining uncertainties regarding the processes that govern the formation and destruction of water. We propose a set of focused observations designed to measure the depth-dependent distribution of water vapor, which is sensitive to a set of processes (e.g., photodissociation, photodesorption, grain surface reactions) that not only determines the distribution of water, but affects the abundance and distribution of many other gas-phase molecules. The knowledge gained will not only improve chemical models for which these processes are important, but will greatly improve our estimates of the true water-vapor abundance derived from all Herschel measurements. We propose a set of HIFI and PACS water maps, pointed observations, and strip scans toward three objects whose face-on or edge-on appearance makes them ideal laboratories for this study: Orion, Cepheus B, and DC 267.4-7.5. Our prior SWAS observations provide confidence in the presence of the water emission we seek to detect as well as proof that the proposed study is feasible. We also make use of ground-based molecular line maps that have already been obtained. This study is not a part of the WISH program, nor can it be carried out with WISH data. The choice of HIFI instead of SPIRE for this study is driven by the need for both sensitivity and velocity resolution - it would require > 2000 hours for SPIRE to obtain a sparsely-sampled map of the same area (23.5'x40') and sensitivity (9.E-18 W/m2, 10-sigma) as the fully-sampled 557 GHz map we propose toward Orion alone and, with HIFI, the water lines will be velocity resolved, which is key to the success of this study. Finally, a by-product of this study will be one of the largest velocity-resolved water maps to be made by Herschel. The total time required for this Herschel-unique program is 38.5 hours.
### Characterizing the evolved, planet-forming disks orbiting the old classical T Tauri systems V4046 Sgr and MP Mus
Proposal ID: OT1_gsacco_1
Principal Investigator: Germano Sacco
Time: 14.4 hours priority 1
Category: Circumstellar/Debris disks
Summary:
V4046 Sgr and MP Mus are the second and the third closest known classical (actively accreting) T Tauri systems, respectively (the intensively studied TW Hya being the closest). We have recently established that, like TW Hya, both systems are orbited by dusty, molecular disks. Given their proximity (d<100 pc), ages (~10 Myr), and masses (0.7-1.2 solar masses), these three systems represent readily-studied analogs of the young sun during the crucial, late phases of the star formation process, when the circumstellar disk still retains a significant gaseous component and giant planets likely are forming or have recently formed. Furthermore, the close binary V4046 Sgr affords an unusual opportunity to investigate planet formation within circumbinary disks. We propose to observe the V4046 Sgr and MP Mus disks using Herschel's PACS and SPIRE spectrometers with the complementary aims of (1) measuring the detailed spectral energy distribution of the continuum dust emission between 55 and 670 micron and (2) detecting the brightest atomic emission lines. These data, together with the comprehensive suite of X-ray, mid-infrared and radio observations we are already collecting for these two systems, will allow us to fully characterize the physical properties of both the dust and the gas components of their circumstellar disks and to investigate the effects of high energy emission from the central star on the evolution of the circumstellar, planet-forming environment.
### A Herschel Study of Star Formation Feedback on Cloud Scales
Proposal ID: OT1_harce_1
Principal Investigator: Hector G. Arce
Time: 51.5 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
We propose to conduct a study of the impact of radiative and mechanical stellar feedback on the surrounding medium of a cluster-forming cloud. Outflows and UV radiation from young stars affect the dynamics and the chemistry of the gaseous environment, thereby influencing the star formation process in the cloud. Herschel offers an extraordinary opportunity to observe unique tracers of these important physical and chemical processes. Our observations will mostly consist of unbiased HIFI, PACS, and SPIRE spectral maps of NGC1333, a nearby cloud, that harbors a cluster of protostars, many outflows and a couple of B stars, and it is commonly used as the prototypical cluster to model clustered star formation. These maps will allow us to conduct a study of an unbiased sample of shocks from outflows at different evolutionary stages within one cloud. We will use important shock tracers and coolants that typically cannot be observed from the ground to investigate the chemistry and physics of the outflow phenomenon in order to fully understand their impact on the natal cloud. Our study will provide the most complete estimate of the outflow energy and momentum input budget in a cluster. In addition, we will investigate how stellar UV radiation affect the water abundance, its formation and destruction, and the chemistry of the gaseous environment. Our proposed Herschel observations (and complementary ground-based data) will provide the best estimate of the water mass reservoir for star formation at the scales of the cloud. The resulting data sets for this cluster-forming region will surely provide a long term observational basis against which to test current and future models of cloud chemistry, stellar feedback and shocks.
### A Study of the Small Negative Molecular Ions CN-, CCH-, and OH- in the Interstellar Gas
Proposal ID: OT1_hgupta_1
Principal Investigator: Harshal Gupta
Time: 37.2 hours priority 2
Category: Interstellar Medium/HII regions
Summary:
The HIFI instrument on Herschel provides a unique opportunity to undertake an astronomical study of light negative molecular ions in the interstellar gas, as these are difficult or impossible to observe from ground based observatories. A sensitive search for the negative ions CN-, CCH-, and OH- with HIFI toward 6 galactic molecular sources is proposed. Three successive rotational transitions (J=6, 7, 8) of CN- and CCH- in HIFI bands 1 - 3, and the lowest rotational transition of OH- near 1.12 THz will be observed. The goals of this study are: i. to enlarge the number of known sources of light negative molecular ions; ii. to determine the abundances of the anions, as well as the anion-to-neutral ratios to assess theoretical models of the fractional ionization of molecular clouds; and iii. to assess the chemical environment of anions through parallel observations of neutral molecules (H13CN and HNC) and positive molecular ions (CO+ and H13CO).
### Planets, Debris Disks, and the Lambda Bootis Stars
Proposal ID: OT1_hmaness_1
Principal Investigator: Holly Maness
Time: 7.1 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose to explore the link between lambda Bootis stars, debris disks, and planetesimal formation and evolution. The lambda Boo stars are a rare type of peculiar A star (2%), which are Population 1 and metal poor. Planet bearing systems and debris disk stars appear unusually well represented in the lambda Boo class: for example, beta Pic, Vega, and HR 8799 are all lambda Boo candidates.
A small sample of 14 lambda Boo stars observed by Spitzer suggests an occurrence of infrared excess approaching 100%. Only two lambda Boo stars are included in the DEBRIS/DUNES Herschel key program debris disk surveys. We will use PACS/Herschel to make sensitive, high-resolution maps of 27 new lambda Boo stars. Like DEBRIS/DUNES, we will reach the stellar photosphere for all targets, enabling a measurement of the true rate of excess infrared emission among lambda Boo stars compared to normal A stars.
The depletion pattern of heavy elements in the atmospheres of lambda Boo stars suggests they may have accreted gas from which dust grains have condensed and been removed: this gas may be circumstellar gas that has formed planetesimals or dusty interstellar gas. While the circumstellar disk scenario predicts sizes of a few hundred AU, the cloud accretion scenario predicts 1000-2000 AU bow structures oriented in the direction of the relative motion of the cloud and star. With target distances of < 140 pc, these bow structures are expected to be resolved for all targets. These will be the first mid-infrared observations of lambda Boo stars outside of the low density Local Bubble: if interstellar medium interactions dominate the lambda Boo phenomenon then systematic variations in excess strength and morphology may occur with distance.
### Taming the Invisible Monster: The Disk of Epsilon Aurigae in the Far-Infrared
Proposal ID: OT1_hoard_1
Principal Investigator: D. W. Hoard
Time: 3.6 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose to obtain photometric flux density measurements of the remarkable binary star Epsilon Aurigae in all six of the PACS and SPIRE imaging bands. Epsilon Aur is seen close to edge on, and has long (2 yr) eclipses every 27.1 yr. The last eclipse, during 1982â1984, received world-wide attention from astronomers. During 2009â2011, the system is again in eclipse and is the focus of a world-wide observing campaign enlisting both professional and amateur astronomers. Epsilon Aur consists of a high luminosity post-AGB F0 star with a much less luminous stellar companion. The latter is newly proven by us to be surrounded by a solar system-sized disk of cool dust. This disk is a rare example of an evolved disk, composed of the remnants of the endgame of stellar evolution, rather than a "primordial" disk as found in T Tauri stars and A stars like Beta Pic. Gaps in the Epsilon Aur disk, reminiscent of the structure of the rings of Saturn, were recently inferred from ground-based time-series spectroscopic observations. By analogy to the role of shepherd moons in the rings of Saturn, this suggests that there could be planetesimals, dwarf planets, or even full-size terrestrial planets in the Epsilon Aur disk. The spectral energy distribution of Epsilon Aur is well-sampled from the far-UV to the mid-IR (0.1-70 microns), with one radio measurement at 1200 microns. However, it is currently unconstrained in the wavelength region spanned by PACS and SPIRE, which is dominated by the dust disk. These Herschel instruments are uniquely configured to provide high S/N photometry bridging the gaps between the mid-IR and radio regimes. These SED points are crucial to confirm if a non-blackbody slope is present, relating to dust grain emissivity, and if potentially bright emission features from molecular species might dominate. These observations will contribute to understanding stellar evolution in binary stars, as well as the formation, evolution, and rejuvenation of planetary systems.
### Understanding the Origin of Transition Disks via Disk Mass Measurements
Proposal ID: OT1_ipascucc_1
Principal Investigator: Ilaria Pascucci
Time: 43.8 hours priority 1
Category: Circumstellar/Debris disks
Summary:
Transition disks are a distinguished group of few Myr-old systems caught in the phase of dispersing their inner dust disk. Three different processes have been proposed to explain this inside-out clearing: grain growth, photoevaporation driven by the central star, and dynamical clearing by a forming giant planet. Which of these processes lead to a transition disk? Distinguishing between them requires the combined knowledge of stellar accretion rates and disk masses.
We propose here to use 43.8 hours of PACS spectroscopy to detect the [OI] 63 micron emission line from a sample of 21 well-known transition disks with measured mass accretion rates. We will use this line, in combination with ancillary CO millimeter lines, to measure their gas disk mass. Because gas dominates the mass of protoplanetary disks our approach and choice of lines will enable us to trace the bulk of the disk mass that resides beyond tens of AU from young stars. Our program will quadruple the number of transition disks currently observed with Herschel in this setting and for which disk masses can be measured. We will then place the transition and the ~100 classical/non-transition disks of similar age (from the Herschel KP "Gas in Protoplanetary Systems") in the mass accretion rate-disk mass diagram with two main goals: 1) reveal which gaps have been created by grain growth, photoevaporation, or giant planet formation and 2) from the statistics, determine the main disk dispersal mechanism leading to a transition disk.
### Massive Young Stars in W43: PACS/SPIRE SED Spectral Scans of MM1 to MM4
Proposal ID: OT1_jbally_2
Principal Investigator: John Bally
Time: 6.7 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
We propose to acquire complete spectral-scans of the four most luminous and massive young stellar objects (MYSOs) in the giant W43 giant HII region complex located at a distance of 5.5 kpc in the Galactic Molecular Ring. The SED modes of the PACS spectrometer and the high-resolution mode of the SPIRE FTS will be used to trace variations in chemical abundances, excitation conditions, and structure in the SEDs as functions of the evolutionary states of these four massive objects. While the central pixels record the spectra of the target MYSOs, the adjacent pixels will probe the spectral properties of the surrounding dense molecular clumps, additional massive YSOs that happen to fall within the aperture, PDRs, and adjacent ionized regions. W43 is one of the most luminous star forming regions in the Galaxy. It has undergone a mini-starburst' within the last few Myr. Massive star formation continues in at least 50 clumps spread over a 20 pc diameter region. The proposed observations will test evolutionary models for MYSOs.
### EPICS: Evolution of Protostellar Ices, Carbonates and Silicates
Proposal ID: OT1_jchiar_1
Principal Investigator: Jean Chiar
Time: 31.9 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
Dynamical and energetic processes that occur during the evolution of a protostar have a strong influence on composition and other characteristics of the dust and these can be well probed with far-IR spectroscopy using Herschel's PACS instrument. Physical evolution of protostars, driven by gravity, is accompanied by a dramatic evolution of the dust, driven by condensation and coagulation, thermal processing by the central star, and shocks driven by protostellar jets. Mid-IR spectroscopic studies of dust in protostellar environments reveal a wide diversity of dust components ranging from volatile ices, to carbonates to refractory crystalline silicates. However, the relationship between the dust evolution and the evolution of the protostar itself has not yet been studied. The evidence suggests that ices are connected to the deepest embedded phase, while crystalline silicates may trace the presence of disks. Carbonates may be either connected to processing of ices in the envelope of YSOs or result from disk processes. In order to probe this dust evolution that accompanies protostellar evolution, we have carefully selected a sample of well-characterized protostars spanning a wide range in evolutionary age and protostellar characteristics from the deeply embedded class 0 stage through the accretion disk (class I) and protoplanetary disk (class II) phases. We will employ PACS in SED mode to study the lattice vibration phonon modes of the ices, silicates and carbonates that occur in the 51 to 220 micron region. Our proposed study will allow us to address at what stage of protostellar evolution different dust signatures become apparent. In this way, we can address the (inter)relationship of these different compounds and the processes involved in their formation. Our study directly addresses Herschel's top-level goal of studying the ingredients in the dust throughout the evolution of a protostar that will then become part of the planetesimal and planet-forming process.
### Close Binaries with Infrared Excess: Destroyers of Worlds?
Proposal ID: OT1_jdrake01_1
Principal Investigator: Jeremy Drake
Time: 16.4 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We have recently used Spitzer to confirm that large IR excesses seen in about 20-30% of old close binary stars by IRAS correspond to very warm close-in dust that appears to originate from recent collisions of planets or planetesimals (Matranga et al. 2010). Somehow, close binaries seem to be destabilizing their planetary progeny, perhaps through secular shrinkage of the stellar separation caused by magnetically-driven angular momentum loss. The aim of this proposal is to use Herschel to search for excesses characteristic of Kuiper-belt-like cold dust or planetesimals in a sample of 88 close binaries from an approved Spitzer IRAC survey. Probing these larger radii in such systems will provide a robust sample of broad SEDs to understand debris disks in close binaries, provide insight into the possibly origin of the Earth mass or more of dust required, and give us a unique handle in understanding planetary formation in circumbinary disks.
### A 3-Dimensional view of the ionized and the warm neutral gas in Orion
Proposal ID: OT1_jgoicoec_4
Principal Investigator: Javier R. Goicoechea
Time: 27.7 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
While bolometric images provide a snapshot'' of the impact of high-mass star formation over entire molecular cloud complexes, it is only by pursuing large scale maps of different spectrally-resolved line tracers of the ionized and the warm neutral gas that we can probe and study the cloud dynamics and kinematics in detail.
We propose to use HIFI to carry out large scale mapping of the core of the Orion GMC (7.5'x11.5'), the closest high-mass SFR in the disk of the galaxy. Our goal is to study the impact and feedback of the high-mass star formation process on the parental molecular cloud by following the ionized, the warm neutral gas and the dense molecular gas over large scales and at high spatial resolutions. The global cloud dynamics, the kinematic interplay of the different gas phase components and their influence on the environment will be revealed by a series of velocity-resolved [NII], [CII], CH+, CH, high-J CO, HCO+ and HCN line maps that cannot not be observed from the ground.
### FOOSH: FU Orionis Objects Surveyed with Herschel
Proposal ID: OT1_jgreen02_2
Principal Investigator: Joel Green
Time: 21 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
We propose to utilize the unprecedented spatial resolution and sensitivity of Herschel at far-infrared and submm wavelengths to observe nearly all known FU Orionis objects, the dramatic result of burst accretion events in protostellar disks. The known FUors represent a vital window into a key process of star formation rather than a rare and peculiar event in the lives of a few stars. In addition, FUors provide a natural laboratory that probes the effect on enhanced heating on disk composition and structure. Our objectives are to (1) Study the structure of known envelopes and constrain the amount of remnant envelope material around the remainder; (2) characterize the physical and chemical properties of the disks and envelope, the parameters that set the initial conditions for planet formation in T Tauri disks; (3) observe solid-state, atomic, and molecular spectral features toward FUors in order to determine the effects of increased luminosity on mineralogy, disk chemistry, and envelope material. In order to do this we will use all three instruments onboard Herschel, providing a comprehensive survey of FUors.
### Low efficiency clouds and the minimum conditions for star formation
Proposal ID: OT1_jhatchel_1
Principal Investigator: Jennifer Hatchell
Time: 20.4 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
To understand the conditions required for star formation, the best regions to observe are regions where those criteria are only just fulfilled - molecular clouds with low star formation efficiencies (SFE). The Scorpius molecular complex contains 4000 solar masses of molecular gas, yet Spitzer observations show it contains only 11 young stellar objects hence an extreme SFE of less than 0.3%. Its low SFE can be contrasted with the rich L1688 protostellar cluster in nearby Ophiuchus and intermediate SFEs in Lupus, with which it shares a similar environment on the boundary of the Lupus-Sco-Cen OB association. We aim to map the Scorpius clouds with SPIRE and PACS to locate and characterise the dense cores, identifying gravitationally unbound, bound and protostellar cores. We aim to determine why regions such as this have such low SFE, the evolutionary path(s) for starless cores, and the minimum conditions for star formation. At 130 pc, Scorpius is among the closest star forming regions hence one of the best Herschel targets for this work.
### Very Large Debris Disks from the PLANCK submillimeter All-Sky Survey
Time: 5.6 hours priority 1
Category: Circumstellar/Debris disks
Summary:
Debris disks are analogs of our Kuiper Belt in the periphery of the Solar System, but are surrounding other main sequence stars. Comets in the Kuiper Belt, and more generally planetesimals in a debris disk, are left over from the early phase of planet formation according to the ''core-accretion" theory and are connected to a planetary system orbiting closer in. Differently, an alternative theory for the formation of giant planets distant from their star invokes ''gravitational instabilities'' in young, large, and massive protoplanetary disks, and predicts no left over planetesimal in a peripheral disk at the end this fast process. Hence, existence and sizes of debris disks are a central question in planet formation theory.
The PLANCK in-orbit observatory is conducting the first all-sky survey in the submillimeter and offers the first opportunity for an unbiased survey of very large, and cold debris disks. We have used the existing PLANCK data to identify debris disk candidates spatially unresolved with the PLANCK beam (4.2'). We propose to confirm their nature by spatially resolving them with the Herschel SPIRE camera, and to determine their sizes by imaging and dust temperature by sampling their SED at 250, 350 and 500$\mu$m. If successful, we would have identified a new population of very large, and cold debris disks characterized by distant planetesimals from their central star, supporting the ''core-accretion'' theory for giant planet formation.
### Cooling and chemistry in the most embedded massive protostars in the Magellanic Clouds
Proposal ID: OT1_joliveir_1
Principal Investigator: Joana Oliveira
Time: 34.6 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
Stars form from contracting molecular cloud cores, but this process relies heavily on the ability of the core to cool and to overcome the magnetic barrier; this, in turn, depends on the chemical composition and could therefore lead to drastically different outcomes at low metallicity. However, most of what we know about star formation is derived from studies of solar-metallicity YSOs in the Milky Way. To investigate the role of metallicity on the star-formation process we propose to observe a sample of early-stage massive young stellar objects in the metal-poor Small and Large Magellanic Clouds. These were selected from among sources with spectroscopic evidence of ice and/or maser emission, and comprise a range in luminosity. We propose to use PACS and SPIRE FTS to measure the strengths of key atomic and molecular lines, in order to measure the temperature, density, ionization state and abundances of the main cooling species in these objects. By comparing the SMC and LMC samples, and Galactic samples of YSOs, we will assess the effect of the reduced metallicity on the formation process of massive stars.
### How to produce warm dust around warm debris disks? - Testing the outer Planetesimal Belt Scenario
Proposal ID: OT1_jolofsso_1
Principal Investigator: Johan Olofsson
Time: 7.3 hours priority 1
Category: Circumstellar/Debris disks
Summary:
During the last decade, some peculiar objects emerged from mid-infrared observation campaigns: warm debris disks. These unique and rare objects have the same properties as "classical" debris disks, except that they display emission features in the mid-infrared, that are associated with warm micron-sized silicate grains. The origin of the warm dust component is still subject to discussion. According to the most recent studies, this dust population may be the consequence of two scenarios. The first explanation would be that a recent catastrophic collision took place in the inner regions of the disks, producing a large amount of micron-sized grains. The second possibility is that a cold outer planetesimal belt is feeding the inner regions, in a similar way as the Late Heavy Bombardment that took place in the Solar System. Such dynamical instability can possibly be triggered by giant planet's migration. We propose to use the PACS photometer, combined with SED modeling, for a unique set of 6 warm debris disks, than may host on-going planetary formation, in order to search for emission in excess at long wavelengths, that may reveal the presence of outer planetesimal belts.
### A Herschel Survey of Disks across the Stellar/Substellar Boundary in Taurus
Proposal ID: OT1_jpatienc_1
Principal Investigator: Jenny Patience
Time: 35 hours priority 1
Category: Brown Dwarfs/Very Low-Mass Stars
Summary:
With the exceptional sensitivity of the Herschel Space Observatory, we propose to map a complete sample of 124 low mass members of the Taurus star-forming region, spanning the transition from low mass stars to brown dwarfs. Taurus is the ideal population for this investigation since the low stellar density enables the detailed study of individual objects without contamination from nearby sources. The sensitive PACS 70um and 160um maps of all sources will provide a census of disks, ranging from primordial gas rich disks to transition disks and debris disks, and define a benchmark population study for comparison with objects of higher mass, older ages, and in different environments. For the 59 targets with evidence of disk excesses from Spitzer 24um images, we also propose to obtain SPIRE 250-500um scans to further characterize the disk properties. The Herschel data for all sources will be combined with existing photometry to construct SEDs over the optical to submm range, and we will fit the SEDs with a comprehensive grid of models developed with the state-of-the-art radiative transfer code MCFOST. The proposed Herschel data cover wavelengths inaccessible from the ground and over the important range associated with the transition from optically thick to optically thin emission. By comparing the well-sampled SEDs with an extensive grid of models, we will estimate key structural parameters such as radius, mass, scale height, and evidence of flaring or dust settling. These properties represent important observational constraints on models for brown dwarf formation and the viability of these disks as sites for future planet formation.
### Characterizing the life cycle of interstellar matter in the Magellanic Clouds with CII and CI
Proposal ID: OT1_jpineda_1
Principal Investigator: Jorge Pineda
Time: 59.6 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
The understanding of the processes governing the formation of interstellar clouds and subsequent star formation is key for our understanding of how galaxies evolve in our Universe. Special interest is given to the study of low-metallicity interstellar matter as it is thought to be representative of the environment where stars formed at earlier cosmological time. Unique targets for this study are the Large and Small Magellanic clouds, which are the closest low-metallicity star forming systems. We propose deep, velocity--resolved observations of the [CII] 158 um, [CI] 609um, and [CI] 370um lines towards 54 representative positions in the Large and Small Magellanic clouds with the HIFI instrument on board of Herschel. These will be combined with our MAGMA CO data to obtain a complete inventory of carbon in the Magellanic clouds. We selected positions to represent different ISM environments, based on whether they show: a) HI peaks with little or no 160um dust emission and no CO, b) HI and 160um peaks but still no CO, and c) CO peaks. We also include a sample of lines-of--sight observed by FUSE which have known H2 column densities, which will allow us to calibrate our use of [CII] as a tracer of HI and H2 column densities. Our sample therefore includes clouds in different stages of evolution going from diffuse atomic to diffuse molecular and to dense molecular clouds. We will use an excitation/radiative transfer code and a PDR model to derive the physical conditions of the line-emitting gas. Our observations have the potential to discover large quantities of dark H2 gas traced by [CII] and perhaps [CI] emission, as recently observed in [CII] emission in the galactic plane (Langer et al. 2010 and Velusamy et al. 2010).
### Protostellar Envelopes Resolved Inside and Out: A Close Look in the Far-IR
Proposal ID: OT1_jtobin_1
Principal Investigator: John Tobin
Time: 3 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
We propose to use Herschel PACS and SPIRE observations to develop a detailed characterization of the envelope temperature and density structure in four nearby (d ~ 200-300 pc) protostars. This will enable us to understand how the non-axisymmetric structure in the surrounding dusty envelopes affects the infall process and the structure of the inner envelope. The goal of this proposal is to take advantage of the superb spatial resolution in the far-IR and sub-millimeter to constrain envelope densities and temperatures over the wide range of spatial scales involved in protostar formation. The proposed observations will resolve the warm inner envelope around these protostars with PACS and map the cold outer envelope with PACS and SPIRE with unparalleled sensitivity and resolution. The multi-band Herschel data enable us to construct dust temperature and density maps which we will combine with our existing Spitzer/near-IR dust extinction maps and measurements of envelope mass and morphology. We will interpret our observations using radiative transfer models to provide the most comprehensive characterizations of protostellar envelope density and temperature structures with which to confront theory.
### Polycyclic aromatic hydrocarbons (PAHs) in protoplanetary disks around late-type T Tau stars in Orion Nebular Cluster
Proposal ID: OT1_kkim_1
Principal Investigator: Kyoung Hee Kim
Time: 31.3 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose a search for far-infrared features from polycyclic aromatic hydrocarbon molecules (PAHs) in a small sample of protoplanetary disks around late-type T Tau stars. These objects were identified in the course of our large Spitzer-IRS survey of the Orion A cloud to have mid-infrared PAH features with unusual profiles, which are far too bright to explain by photoexcitation by their host stars; they must be excited by ultraviolet light from their more massive neighbors. Recent laboratory spectra of PAHs demonstrate the variation of wavelength and strength with molecule size for the far-infrared features of PAHs, a sensitivity that is lacking in the mid-infrared features. The observation of such features in disks around low-mass stars, in which we frequently see the effects of coagulation and growth among the silicate-grain population, represents an opportunity to search for size variation among the PAH population, a congruence with the PAH molecules found in the primitive meteorites, and perhaps hints of the role played by carbonaceous molecules in the assembly of solid bodies in disks.
### Cool Herschel/Hot Spitzer: The distribution of water in protoplanetary disks
Proposal ID: OT1_kponto01_1
Principal Investigator: Klaus Pontoppidan
Time: 39 hours priority 1
Category: Circumstellar/Debris disks
Summary:
One of the key mission objectives of Herschel is to observe water in various environments, but in protoplanetary disks in particular. Water has an immediate relevance to the formation of planets and to our own origin. We propose to obtain deep PACS/SPIRE line spectra of water, OH and CO in protoplanetary disks already known to have strong rotational water vapor emission at mid-infrared (10-36 micron) wavelengths, as detected by Spitzer (the newly discovered mid-infrared molecular forest). The mid-infrared lines trace warm to hot gas formed within a few AU from the central star. The proposed observations will relate the oxygen chemistry and transport of water in the inner few AU with that of the cooler outer disk - 1-100 AU - as traced by the PACS water lines. The line ratios of water in the Spitzer spectral range suggest that water vapor may be strongly depleted in the disk surface beyond 1 AU although gas and dust temperatures are high enough to maintain abundant water out to at least 10 AU. It was suggested by Meijerink et al. 2009 that this depletion of water could be due to a cold finger effect'', in which the surface water vapor is carried downwards into colder regions of the disk where it freezes out and is bound in the disk mid-plane as part of the general dust growth and settling. If so, the surface abundance structure of water is a direct tracer of the mid-plane snow-line. Based on model fits to the mid-infrared lines, we predict very strong differences in the 50-200 micron water lines, depending on the distribution of water in the outer disk surface. Our program is unique in that 1) we specifically target disks known to have strong water emission from the inner disk and 2) we go significantly deeper than others ensuring that we can constrain the abundance of water vapor down to 10^-10 per hydrogen in the outer disk, thus putting very strong constraints of the efficacy of the proposed cold finger effect.
### Dusty Disks around Hot White Dwarfs: Debris Disks or Remnant of post-AGB Binary Disks?
Proposal ID: OT1_ksu_2
Principal Investigator: Kate Su
Time: 7.6 hours priority 1
Category: Circumstellar/Debris disks
Summary:
Dusty disks around hot (Teff > 100,000 K) white dwarfs are a new phenomenon discovered by Spitzer. The origin of such a disk is still in debate. We propose to obtain far-infrared photometry for 6 dusty disks around hot WDs identified from our Spitzer 24 micron survey. The Herschel far-infrared measurements will provide strong constraints on the outer boundary of the disk and its total dust mass in the system, crucial information necessary to differentiate the origin of the disks.
### Outflows from evolved Class II sources: an Herschel/HIFI insight into the kinematical/physical properties of the atomic and molecular component.
Proposal ID: OT1_lpodio_1
Principal Investigator: Linda Podio
Time: 26 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
Stellar jets are known to play a key role in the overall star formation process as they can remove angular momentum from the disk and disperse the parental envelope. A characteristic emission lines spectrum is produced by the shocks caused by the interaction of the ejected material with the surrounding medium. The collimated, fast and hot gas (T~2000-1e4 K) is traced by atomic and H2 lines, while the slow and cold swept-up material (T~10-20 K) can be probed through millimeter lines. Herschel opens a window on the "warm" component at 100-2000 K, which hold crucial information on the understanding of the connection between the outflow atomic and molecular components and the transfer of energy to the surrounding medium.
Preliminary results obtained from the analysis of GASPS/PACS data of Class II sources associated to jets detected at optical/NIR wavelengths show extended and velocity shifted emission in atomic ([OI]63um, [CII]157um) and molecular (CO, H2O) lines, suggesting that these lines are originating in the outflowing gas. However, also emission from the surrounding accretion disk may contribute to the emission in the unresolved star-disk region (PACS resolution ~9.4").
We propose to complement the GASPS/PACS data with HIFI observations of the [CII]157um, CO 10-9, and H2O at 556.9 GHz lines in a small sample of GASPS targets associated to outflowing gas sigantures. HIFI high spectral resolution (fraction of km/s) will allow us to observe line profiles and separate emission from the disk and the outflows. The [CII]157um line, with the [OI] lines detected by PACS, will probe the jet atomic component, while HIFI and PACS CO and H2O lines will allow us to derive kinematical/physical properties of the molecular component. The characterization of molecular gas component, as well as the estimates of the mass loss rate associated to the different component is crucial to test the magneto-hydrodinamical jet models and understand the interplay between accretion and ejection.
### An in-depth Herschel study of gas, dust, and ices in FU Orionis objects
Proposal ID: OT1_maudar01_1
Principal Investigator: Marc Audard
Time: 31.3 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
We propose to obtain the broad-band medium-resolution spectra of 15 known outbursting sources with Herschel PACS and SPIRE to cover the 50-650 micron range and to study both the continuum (and the spectral features of ices and dust) and the emission lines. Additional photometry with PACS and SPIRE will be obtained to better characterize the direct environment of the FU Orionis objects. The main goals are 1) to place the FU Ori objects in the context of young stellar evolution by looking for differences in infrared spectral diagnostics between FU Ori objects and regular young stars. To this end we plan 2) to study the composition and evolution of dust grains in FU Ori objects, 3) to look for the presence of ices, 4) to identify atomic lines, in particular faint lines not previously or barely identified with ISO and to use line ratios to constrain the emission mechanism, 5) to search for molecular lines of hydroxyl and water, and of high transition states of (J=13-30) of CO. The CO lines will be used to constrain the origin of the lines (outflow, disk), 6) to use the Herschel spectra and photometry with ground-based and Spitzer data to fit the spectral energy distributions with radiative transfer codes to derive the disk and envelope properties. The Herschel observations of our sample of outbursting sources will probe an important phase in the life of young stellar objects with the aim to better understand their differences and their common properties, and to better place them into the evolutionary sequence from Class I star to Class II stars.
### Understanding the Protostellar Mass Accretion Process: Herschel 100-500 micron Photometry of Low Luminosity Embedded Protostars
Proposal ID: OT1_mdunham_1
Principal Investigator: Michael Dunham
Time: 6 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
Spitzer Space Telescope surveys of nearby, low-mass star-forming regions have discovered a new class of very low luminosity objects (VeLLOs), protostars embedded within dense cores with luminosities less than or equal to 0.1 Lsun. VeLLOs represent the extreme low end of the protostellar luminosity distribution, which is comprised mainly of sources below about 1 Lsun. The standard model of star formation, which predicts a mass accretion rate constant with time, is inconsistent with such a large population of low luminosity embedded protostars, leading numerous recent authors to suggest that mass accretion is variable and/or episodic in nature. Further constraints on this mass accretion process require far-IR and submm data to fill in the gap between existing Spitzer mid-IR and ground-based millimeter continuum data. We propose to obtain Herschel PACS and SPIRE 100-500 micron photometry of 24 confirmed and candidate embedded protostars with L < 1.0 Lsun. With these data, we will: (1) calculate accurate evolutionary indicators, (2) provide essential inputs for source models that seek to constrain the properties of both the protostars and the dense cores in which they are embedded, and (3) confirm or reject candidates that have not been conclusively shown to be embedded protostars. The proposed observations will provide crucial data for further understanding the protostellar luminosity distribution and mass accretion process for a very modest (6.0 hours) allocation of observing time.
### Diffuse ISM phases in the inner Galaxy
Proposal ID: OT1_mgerin_4
Principal Investigator: Maryvonne Gerin
Time: 13 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
First HIFI and PACS observations obtained in the framework of the PRISMAS and HEXOS key programs have demonstrated the advantage of using absorption spectroscopy for studying the diffuse interstellar medium in the inner Galaxy. Detections of HF, OH+, H2O+, CH+, CH and the N-hydrides have significantly improved the knowledge of the diffuse molecular gas and started to open windows on the diffuse atomic gas. However the information on the diffuse ionized gas remains fragmentary. We propose to take advantage of the Herschel spectroscopic capabilities and further characterize the diffuse neutral and ionized interstellar medium along lines of sight already selected in the PRISMAS and HEXOS programs. We target the fine structure lines of ionized nitrogen and carbon, [NII] 1.46 THz, CII] 1.9 THz,and the ground state and first excited lines of neutral carbon at 492 GHz & 809 GHz. [NII] is tracing is diffuse ionized gas, while the neutral carbon lines reveal the diffuse neutral gas and probe the gas pressure and [CII] traces both the neutral and ionized matter . Towards strong far infrared sources such as our targets, we expect that the [CII] line profile will present a superposition of emission and absorption features, that can only be resolved by the high spectral resolution provided by HIFI. Even for [NII] and [CI], the profiles may show superpositions of absorption and emission features, justifying our request for HIFI spectra, since the gas and electron densities in the foreground material are much lower than in the background sources. We propose to take advantage of the sensitivity offered by absorption spectroscopy to determine the ionized carbon abundance with an unprecedented accuracy. The proposed observations will therefore bring new measurements of the abundances of neutral and ionized carbon abundances, neutral gas pressure, and ionized gas filling factor in the inner Galaxy that will provide a complete picture of the respective volume and mass filling factor of the ISM phases in the inner Galaxy
### Kinematics and Chemistry in Ultracompact HII regions: the case of Mon R2.
Proposal ID: OT1_mgonza01_1
Principal Investigator: Manuel Gonzalez
Time: 3.4 hours priority 2
Category: Interstellar Medium/HII regions
Summary:
Ultracompact HII regions are defined as regions of ionized gas with diameters smaller than 0.1 pc. Mon R2 is the only nearby Ultracompact HII region that can be resolved with Herschel. This source has already been observed and has been proved to host a dense photon-dominated region surrounding the Ultracompact HII region. For the simplicity of its geometry and the absence of shocks, this source is an excellent target to investigate the chemistry of extreme PDRs. Observations done with HIFI during the Prioritary Science Phase combined with previous observations from the IRAM 30m telescope permitted to constrain a simple scenario to describe this region: a dense PDR layer ($n\, =\, 5\times10^6\, cm^{-3}$) surrounded by a lower density ($n\, =\, 10^5\,cm^{-3}$ ) UV protected envelope. We propose to do maps of tracers of the regions of the PDR close to the HII region in order to characterize its movement. At the same time, we propose to observe some hydrides molecules, which chemistry is poorly known in such regions. HIFI is a unique oportunity to study such hybrides with fine/hiperfine structures, due to its high resolution. That way, with only 3.4 hours of observation and some work in modeling and interpreting the results we would be able to characterize the kinematics and chemistry of this region, that can be used as a template of similar objects, like the surface layers of circumstellar disks and/or the nuclei of starburst galaxies.
### Deep HIFI searches for cold water vapor in protoplanetary disks
Proposal ID: OT1_mhogerhe_1
Principal Investigator: Michiel Hogerheijde
Time: 46.8 hours priority 1
Category: Circumstellar/Debris disks
Summary:
Water vapor inside planet-forming disks is expected to show large variations. In the warm (~200 K) inner few AU of the disk all oxygen is locked up in water vapor. In the colder outer region water quickly freezes out onto dust grains. However, efficient photodesorption by stellar ultraviolet radiation will return an appreciable fraction back into the gas phase in the upper disk layers. This coupled water ice/vapor system explains the Spitzer observations of warm water in several disks, and predicts the presence of cold water vapor in the outer disk. Through the Water in Star Forming Regions' (WISH) Key Program, we have recently clearly detected the groundstate line of cold water vapor to TW Hya and very tentatively detected it to DM Tau. Both lines are factors 10-50 weaker than expected. We hypothesize that up to 99% of icy grains have settled to the disk's midplane thus freeze drying' the upper disk layers. The WISH data do not go deep enough to probe cold water vapor content now that we know that the outer disk is freeze-dried. The only clear detection is TW Hya, which has a distance of only 51 pc. At more typical distances of 100-140 pc, line strengths are lower by factors 5-8, beyond the sensitivity of WISH. We propose much deeper HIFI observations of the H2O 110-101 line at 557 GHz of four targets: DM Tau (to confirm or reject WISH's very tentative' detection), and HD100546, HD163296, and AA Tau. These disks are, after TW Hya, the closest and largest disks that offer the best chances of detection. Because of the sensitivity of H2O 110-101 to cold water vapor in the outer disk, our observations probe as-of-yet unexplored grain settling in the outer disk and enrichment of the midplane with icy grains. This can boost planet formation, since icy grains coagulate more easily. Our proposal also contains a small request for velocity-resolved CO 10-9 observations with HIFI to study warm (~200 K) gas in these four disks, and investigate if preferential settling of icy grains also affects CO.
### A Search for Cold Dust Orbiting GD 362, a Highly Polluted White Dwarf With Detected Warm Dust
Proposal ID: OT1_mjura_1
Principal Investigator: Michael Jura
Time: 1.1 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose to observe GD 362 to measure the amount of cold dust orbiting this white dwarf which is already known to possess warm dust. There are two models to account for the large amount of atmospheric hydrogen in this externally-polluted star whose atmosphere is largely helium. (1) The star is accreting from a single Mars-mass parent body. In this case there is no reason to expect cold dust. (2) The star is accreting from an ensemble of 100's of Ceres-mass asteroids; a large amount of cold dust likely is present. If so, the source could be detected with PACS.
### Crystal clear: revealing midplane dynamics of protoplanetary disks through the spatial distribution of crystalline dust
Proposal ID: OT1_mmcclure_1
Principal Investigator: Melissa McClure
Time: 28.7 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose to obtain PACS range spectroscopy to measure the vertical and radial distribution of crystalline silicates in 22 protoplanetary disks around pre-main sequence stars. Dynamical processes, such as nebular shocks and meridional flows, are predicted to generate crystals within the warm, inner-most parts of these disks and transport them further out into the planet-forming regions. Therefore the spatial distribution of crystals, which have broad, mid-infrared spectral features, can be used to trace such mechanisms. Since these processes influence core-building and migration, determining their scope is paramount to our understanding of planet-formation as a whole. Recent studies using Spitzer Space Telescope IRS spectra suggest crystals are distributed farther out in protoplanetary disks than can be accounted for by current theories. Over the Herschel PACS 51-73 micron range, the continuum is extremely sensitive to changes in crystallinity as a function of radius, while the dust emission features over this range and the continuum from 102-146 micron are sensitive to changes in crystallinity in the vertical direction. By using irradiated accretion disk models to do a self-consistent analysis of the combined PACS and Spitzer IRS spectra of our 22 targets, we will unveil the midplanes of these disks and trace the influence of inner disk dynamics on the planet-forming region.
### First steps toward star formation: unveiling the atomic to molecular transition in the diffuse interstellar medium
Proposal ID: OT1_mmiville_2
Principal Investigator: Marc-Antoine Miville-Deschenes
Time: 31.4 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
We propose to map molecular material that is forming in the diffuse insterstellar gas, exploiting the unique capabilities of PACS and SPIRE: large area mapping at high angular resolution, sensitivity, and wavelength coverage spanning the peak of the dust spectral energy distribution. The main scientific goal is to discover the physical conditions in cirrus clouds that lead to the formation of the seeds of molecular clouds. Molecular hydrogen formation is fundamental to understanding the structure of molecular clouds and the core mass function (CMF) in the framework of the turbulent, magnetized and thermally bi-stable interstellar medium.
Our strategy is to map two regions at high Galactic latitude with PACS and SPIRE and use the dust opacity deduced from Herschel data to map the total column density of matter. Then using our high resolution 21-cm data for these fields, the atomic-correlated contribution can be removed, leaving a map dominated by dust in the molecular gas. Statistical properties of the molecular structures will be related to the properties of interstellar turbulence, thermal instability, and CMF seen in molecular clouds. The H I data are essential to this project, not only to uncover the molecular gas but also to probe the dynamical conditions in which the molecular gas has formed.
Both fields are part of a large project of H I observations of high Galactic latitude fields. The Spider field, a faint cirrus cloud with highly filamentary structure, is representative of the formation of H2 in dynamical conditions dominated by interstellar turbulence, with an average amount of molecular gas for diffuse clouds (estimated at about 15-20%). The Draco nebula, the archetype of interstellar matter re-entering the local interstellar medium after being expelled into the halo via the Galactic fountain, has a strikingly clumpy structure induced by its bulk motion with respect to the local ISM. There is a wide range of conditions to be modeled, including patchy CO emission.
### Probing the mechanical and radiative feedback from young stars in the molecular clump containing HH 1/2 and NGC 1999
Proposal ID: OT1_mpuravan_1
Principal Investigator: Manoj Puravankara
Time: 13 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
We propose PACS spectroscopic observations in the line and range scan mode of the HH 1/2 jet, its driving source, and a nearby cloud cavity irradiated by a B9/A0 star in an intermediate-mass molecular clump in L1641. Our aim is to study the details of the mechanical and radiative feedback from new born stars on their immediate cloud environment and how it affects the structure, stability and star formation potential of the cloud clump from which they have formed. We will map the HH 1/2 outflow, and the newly discovered cavity in NGC 1999, in the far-infrared fine-structure lines of [C II] and [O I], and in several rotational lines of CO and H$_2$O. From these observations we will spatially separate the various sources of energy and momentum, and place strong contraints on the density and temperature of the emitting gas. We will follow the spatial variations in the shock structure along the jet to probe the interaction of the jet with the surrounding molecular gas. By constraining the temperature and density of the surface walls of the cavity in NGC 1999 we will test if the temperature is high enough to represent photoevaporation, and estimate the rate of photoevaporation.
### ASCII: All Sky observations of Galactic CII
Proposal ID: OT1_mputman_1
Principal Investigator: Mary Putman
Time: 10 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
The Milky Way and other galaxies require a significant source of ongoing star formation fuel to explain their star formation histories. A new ubiquitous population of discrete, cold clouds have recently been discovered at the disk-halo interface of our Galaxy that could potentially provide this source of fuel. We propose to observe a small sample of these disk-halo clouds with HIFI to determine if the level of [CII] emission detected suggests they represent the cooling of warm clouds at the interface between the star forming disk and halo. These cooling clouds are predicted by simulations of warm clouds moving into the disk-halo interface region. We target 5 clouds in this proposal for which we have high resolution HI maps and can observe the densest core of the cloud. The results of our observations will also be used to interpret the surprisingly high detections of [CII] for low HI column density clouds in the Galactic Plane by the GOT C+ Key Program by extending the clouds probed to high latitude environments.
### Hot CO in the Massive Star Forming Region DR21
Proposal ID: OT1_mrllig_1
Principal Investigator: Markus Röllig
Time: 11.6 hours priority 2
Category: Interstellar Medium/HII regions
Summary:
We plan to resolve the detailed physical and dynamical structure of the massive star forming (SF) region DR21~C which has a prominent bipolar outflow visible in 2 micron emission of vibrationally excited H2, tracing hot, shocked gas. While, the shock is hardly affecting most of the molecular line emission of the region (Lane et al. 1990, Ossenkopf et al. 2010), only [CII] is showing an additional broad blue wing indicating that the [CII] emission is not only originating from that warm gas, but also from the ionized wind in the blister outflow. H2 and CO are at least partly co-existent and hence should show similar signs of shocks, but surprisingly 13CO(10-9) doesn't, so many question remains:
- Is there any CO that is directly affected by the shock and if so, at at which AV does the shock excitation stop? - Why does CO up to 10-9 show no direct signature of shock heating or outflowing material? - Does the shock only affect H_2 and ionized material? - Which volume of the source is affected/heated by the shock? - Which volume of the source is heated by the UV radiation from the cluster?
The aim of this proposal is to understand how shock/outflow and UV radiation from the embedded OB cluster contribute to the excitation of the surrounding material and where exactly the transition from shocked to unshocked material occurs.
### Confirming a sample of luminous debris disk candidates identified in the Herschel ATLAS
Proposal ID: OT1_mthomp01_1
Principal Investigator: Mark Thompson
Time: 1.4 hours priority 1
Category: Circumstellar/Debris disks
Summary:
Debris disks are the remains of planetary system formation, tracing the existence of planetesimal-sized objects in orbit around main sequence stars. Current and planned surveys of debris disks (including the Herschel Key Projects DEBRIS and DUNES) are deep surveys aimed at characterising the typical population of disks and targeted at samples of a few hundred nearby objects. These deep narrow surveys are relatively insensitive to the rarities in the debris disk population, some of which may be luminous and/or massive disks that have undergone recent disruptive collisional events. We have recently shown that the primarily extragalactic Key Project, the Herschel-ATLAS, can be used as a wide and shallow survey of debris disks by combining its excellent optical coverage and statistical techniques more commonly employed to identify galaxies. The combination of Herschel-ATLAS, DEBRIS and DUNES thus forms a powerful nested tier of surveys that will be sensitive to disks across the spectrum from exosolar analogues to rare disks that cannot be inferred from local populations. In this proposal we seek time to image the three candidate disks that we discovered in the Herschel-ATLAS Science Demonstration Phase with PACS so that we may confirm them as true debris disks and model their SEDs to extract mass, temperature and fractional luminosity. We will confirm whether these disk candidates are in fact the most luminous disks yet detected.
### Characterizing the structure of an unusually cold high latitude cloud
Proposal ID: OT1_mvenezia_1
Principal Investigator: Marcella Veneziani
Time: 6.8 hours priority 1
Category: Galactic Other
Summary:
We propose a PACS and SPIRE photometric observation at 100, 160, 250, 350 and 500 micron to study an unusually cold cloud detected by the BOOMERanG experiment at high galactic latitudes (b = -31 deg). This cloud has a temperature of T = 7 +- 3 K and this measurement is confirmed also by Planck-HFI data. Even if the temperature is so low, other properties are not that extreme: it has normal HI column density, gas-to dust ratio and no molecular material. A closer look at 100 micron shows, at 4' resolution, a wealth of brighter clumps embedded in the cloud that could be mostly molecular, hence hidden from the large beam HI and CO surveys. They can be pre-stellar cores and this would explain the low temperature. We propose to map a 30'x30' area centered on the cloud to study the substructure and the composition of that region. The observation with the Herschel angular resolution and band coverage will improve the knowledge of the early stages of star formation and of the structure and composition of the interstellar medium at tens of arcseconds angular scale. This is particularly interesting as the region is located at high latitudes, in an area that is supposed to be poor of star formation activity. With Herschel data we will be able to characterize the properties of the clumps and of the dust around, like temperature, spectral index, mass and density in order to better determine the physical processes occurring in this region and structure and substructures composition.
### HYSOVAR: Circumstellar Disks Variability around Young Stellar Objects in the Orion Nebula Cluster with Herschel/PACS
Proposal ID: OT1_nbillot_1
Principal Investigator: Nicolas Billot
Time: 9.9 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
The variability of Young Stellar Objects (YSOs) have been demonstrated over half a century ago from optical observations. More recent time series photometry of YSOs in the thermal infrared have shown their great potential to probe the structure of inner circumstellar disks (r << 1 AU), in particular the presence of warps and clouds' in the disks which may owe their existence to the gravitational torques from close-in planets. For instance the YSOVAR program used the Spitzer IRAC instrument to monitor over 1400~YSOs and establish that 70% of them show significant variability in the mid-IR. Today the Herschel/PACS spectral coverage, sensitivity and stability offer a unique opportunity to access the wavelength regime sensitive to the dust thermal emission from the terrestrial habitable zone through the ice-line where gas giants are expected to form. We propose the HYSOVAR program, an expansion of YSOVAR with the Herschel/PACS Photometer, to monitor the flux variations of 100+ Class I YSOs in Orion over weeks-to-years time scales. This small (9.9 hours) exploratory program would greatly increase the statistics and sensitivity of previous studies in the far-IR, and it would help us identify the physical processes responsible for the observed infrared variability by placing strong constraints on existing models of star and planet formation.
### A Deeper Look at the 3-10 Myr Old Disks in the Orion OB1 Association
Proposal ID: OT1_ncalvet_1
Principal Investigator: Nuria Calvet
Time: 39.6 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
We propose to obtain deep 70/160 micron PACS Photometer observations of populations in the Orion OB1 association, spanning the critical 3 to 10 Myr range of ages when disks are supposed to dissipate and planets to form. Our ongoing large-scale survey of the Orion OB1 star-forming regions has allowed us to find the elusive low mass population in the older parts of the association, and secure the photometric and spectroscopic data to fully determine the stellar and accretion properties of these objects. We propose to obtain slow-speed scans of five 30'x30' fields, covering sections of the ~ 3 Myr old cluster sigma Ori, a ~ 5 Myr old group in the Ori OB1b subassociation, and the ~ 9 Myr old 25 Ori group, the most populous stellar group at this age within 500 pc. Our Spitzer IRAC and MIPS data for the proposed fields allow us to estimate that we will detect at least 62 disks in our PACS observations, 48% of which also have Spitzer IRS data. With the Herschel far-infrared fluxes and our mid-infrared and optical fluxes we will construct the most complete spectral energy distributions for a large sample of 3-10 Myr disks. The interpretation of these SEDs with our irradiated accretion disk codes, constrained by the stellar parameters and mass accretion rates determined independently from the UV excess, will allow the best characterization to date of disks in this age range, and provide essential constraints on theoretical models of disk evolution and planet formation.
### Pillars of creation: physical origin and connection to star formation
Proposal ID: OT1_nschneid_1
Principal Investigator: Nicola Schneider
Time: 31 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
Herschel SPIRE/PACS photometry observations performed within the HOBYS (Herschel imaging survey of OB Young Stellar objects) key program have revealed a wealth of interesting structures in high-mass star forming regions. The most spectacular of those are 'pillars' and 'globules'. These features -- partly known from Hubble Space telescope or Spitzer images -- are formed due to photoevaporation at the interface between a molecular cloud and an HII region, and are thus intimately linked to high-mass star formation. The process of how these pillars are created, and under which conditions low- or high-mass stars form within them, are not yet clear. Classical approaches (e.g. Rayleigh-Taylor) can not explain pillar formation, so we have embarked upon a dedicated project to fully simulate pillars and globules using the (magneto)-hydrodynamic code HERACLES that comprises gravity and ionization. The model is intended to be coupled with a radiative transfer photon dominated region code (KOSMA-tau).
We propose here to make use of the Herschel spectroscopy capacities to map/make single pointings, in a number of atomic and molecular lines, of selected pillars and globules in three different regions (Rosette, Cygnus, M16), spanning a large range in UV intensity and density. We intend to observe the important cooling lines of [CII] at 158 micron and [OI] at 63 and 145 micron with PACS, the [CI] finestructure lines at 370 and 609 micron and the mid-to high-J CO and HCO+ ladder with the SPIRE FTS. Spectrally resolved [CII] mapping with HIFI is also required to derive the velocity information. These observations will be compared to the large existing complementary data set for each source, to study the physics of pillars and will additionally serve as input for the models, to ultimately explain pillar formation and star formation within them.
### Herschel spectroscopic study of the extraordinary disk Gomez's Hamburger
Proposal ID: OT1_oberne_3
Principal Investigator: Olivier Berne
Time: 10 hours priority 1
Category: Circumstellar/Debris disks
Summary:
"Gomez's Hamburger" (GoHam) is a gas rich protoplanetary disk around a pre-main-sequence A star. Recent observations at infrared and millimeter wavelengths have reveal the extraordinary nature of this source: it is seen almost perfectly edge-on, it is massive and therefore intense in the infrared and millimeter: offering the possibility to detect key species (e.g. H2O, High J CO lines), it is large enough to be spatially resolved at most wavelengths, and it is likely in the process of forming planets. Overall, it appears that GoHam is a key object to study the mechanisms that lead to planetary formation, and it has been left behind in the guaranteed time. Here, we propose to observe this object with the three instrument onboard Herschel to complete the data set we have already gathered for this source. The team, composed of experts in molecular astrophysics, disks, radiative transfer, chemistry, and dust properties, will then make best use of these observations to probe the gas temperature, density, velocity and the dust size distribution as a function of the radial and vertical dimension of the disk. Such results are needed, in the end, to constrain the hydrodynamical models of planetary formation, and chemical models explaining the formation of complex molecules. The total requested time for this program is 10 hours.
### Spatially resolved far-infrared imaging of bright debris disks: studying the disk structure and the stirring mechanism.
Proposal ID: OT1_pabraham_2
Principal Investigator: Peter Abraham
Time: 14.8 hours priority 1
Category: Circumstellar/Debris disks
Summary:
A significant fraction of main-sequence stars are encircled by dusty debris disks. The short lived dust particles of these disks are believed to be replenished through destructive collisions between unseen planetesimals whose orbits are stirred up by some mechanism. In the literature three candidate mechanisms compete: the most commonly invoked self-stirring, the giant planet induced planetary stirring and close stellar flyby. Here we propose to study 10 carefully selected debris disks with Herschel/PACS and Herschel/SPIRE, where young age and a rough estimate of disk size from Spitzer observations hint for stirring mechanisms other than self-stirring. With the new observations we will resolve the debris disks at 70 micron (and in some cases at 100/160 micron as well) and will analyze in detail their structure and to identify stirring mechanism. In our programme we aim to 1) resolve the dust disks and characterize their spectral energy distributions; 2) to study the radial and azimuthal distributions of the cold debris; 3) to identify the stirring mechanism in the disks; 4) to perform a detailed investigation of HR 8799 a star with three large outer planets. The proposed observations will contribute to a deeper understanding of the stirring mechanisms by utilizing the superior spatial resolution of Herschel. The total requested time is 14.8 hours.
### A deep 70 micrometer study of cold circumstellar disks in rho Oph: down below the brown dwarf limit
Proposal ID: OT1_pabraham_3
Principal Investigator: Peter Abraham
Time: 12.8 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
Most stars form in clusters, and the nearest example of an embedded young cluster is the one in the L1688 cloud of the rho Ophiuchi region. It is one of the best explored star-forming region, an intermediate exemplar between the sparse regions of Taurus and the rich, massive cluster of Orion. With the aim of detecting brown dwarfs (BDs) with masses down to a few Jupiter masses, our group conducted a major preparatory observational project in L1688, where we have spectroscopically confirmed 28 new brown dwarfs. The new discoveries increased the known population of BDs by a factor of 3 and provided the so far most complete census of the (sub)stellar population of the rho Oph cluster. Here we propose a comprehensive study of the cold circumstellar disks of the pre-main sequence population, with particular emphasis on the very low mass objects and BDs. Utilizing the unprecedented far-infrared sensitivity and spatial resolution of Herschel, we will obtain deep 70 and 160 micrometer maps of a 1.6 deg^2 area centred on the L1688 cloud, covering also the location of the 28 new brown dwarfs. We intend to (1) study the most complete population of brown dwarf disks in rho Oph; (2) analyse disk properties and evolution across the stellar mass range; and (3) characterize the protostar population and its luminosity function. Our programme provides the opportunity to characterize the complete, homogeneous population of disks around both young BDs and low-mass stars in "the benchmark protocluster" of rho Oph. The produced deep 70 micrometer map of the region will also have a very high legacy value, since flux densities for sources to be discovered (e.g. new confirmed BDs) can be extracted in the future. The total Herschel observing time for the proposed programme is 12.8 h.
### Follow-up spectroscopy of two selected filaments found in the Herschel Gould Belt Survey: A turbulent shock origin ?
Proposal ID: OT1_pandre_4
Principal Investigator: Philippe Andre
Time: 58.3 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
One of the early discoveries made with Herschel during the science demonstration phase is the fascinating omnipresence of filamentary structures in the cold interstellar medium and the apparently intimate relationship between the filaments and the formation process of prestellar cloud cores. Our first results from the Gould Belt survey in the Aquila Rift and Polaris Flare regions suggest a picture of core formation according to which filaments form first in the diffuse ISM, probably as a result of interstellar turbulence, and then prestellar cores arise from gravitational fragmentation of the densest filaments. To get further insight into the formation of prestellar cores, it is crucial to clarify the origin and nature of the filaments seen in the wide-field SPIRE/PACS images. Here, we propose follow-up observations of the central parts of two selected filaments with the SPIRE and PACS spectrometers to characterize the physical conditions of the gas and test the hypothesis that the filaments are formed behind low-velocity interstellar shock waves associated with the dissipation of turbulent energy. If this is indeed the case, we expect to detect a number of emission lines such as [CII] (at 158 microns) and [CI] (at 609 microns), and several high-J CO lines which are primary coolants of the postshock gas.
### Galactic Origins of Star Formation in the W43 Complex (GLOW)
Proposal ID: OT1_pcarlhof_1
Principal Investigator: Philipp Carlhoff
Time: 10 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
Star formation is one of the most important processes in the universe, strongly influencing the evolution and structure of matter on all scales. Still the early phases are not totally understood. The progression from low density gas and dust to star forming cores still awaits a persistent description.
One model that aspires to explain molecular cloud formation is the "converging flows" model. The term refers to the convergence of HI streams that can naturally be driven by gas motion within Galactic arms. The theory of converging flows is the first one that can explain star formation self-consistently. It sets the stage for rapid dispersal (fragmentation into filamentary structures) of molecular clouds and explains naturally the observed short lifetimes of star forming stages which have, for long, been a problem.
We propose to map three parts of the giant molecular complex W43, that show examples of converging flows and filamentary structure in C+. This line is known to be a good tracer of the transitional phase between atomic and molecular gas, particularly the phase where the gas is already molecular, but CO has not formed yet. We strive to observe the selected targets with Herschels HIFI instrument, to obtain detailed spectral information. With the addition of large scale maps of 13CO, that we have taken with the IRAM 30m and JCMT, this will give us a coherent picture of the region, needed to investigate the fluctuation of the molecular gas and compare these results to the theoretical models of converging flows.
The main scientific questions of this project are: (a) How do colliding flows of molecular gas form and how do they form filamentary structures? (b) How do these flows affect the formation of dense cores and thus accelerate star formation? The results of this proposal, complemented by other projects, will give deep insight into unknown mechanisms of star formation and, beyond that, pave the way to follow-up observations with Herschel and other observatories.
### Molecular Oxygen in Orion
Proposal ID: OT1_pgolds01_4
Principal Investigator: Paul Goldsmith
Time: 12.1 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
Observations carried out to date for the Herschel Oxygen Project (HOP) indicate that the abundance of a potentially major oxygen-bearing species, O2 (molecular oxygen), predicted to be as high as 1e-4, is less than 1e-7. One extremely interesting exception is Orion. We have 2 hours of integration on the 487 Ghz and 774 GHz O2 transitions, and see statistically significant emission in two velocity features, at ~ 6 km/s and ~ 12 km/s. These data were taken at the Peak 1 position of strong H2 vibrational emission, approximately 40" from the KL/hot core position. Plambeck and Wright (1987) found that the Peak A position near the hot core is a strong source of HDO emission at ~12 km/s. Since HDO is thought to be released from recently warmed grains, this may be intimately connected with the low O2 abundance being a result of atomic oxygen being frozen on cold grains and hydrogenated to water ice. When released after grain heating, it produces a significant gas-phase abundance of water and molecular oxygen. The HOP project did not include the KL/hot core position (Peak A is within 5") due to concerns about line confusion. However, data from the HEXOS survey confirms that the the O2 lines are in relatively windows, and shows O2 emission at the same 6 km/s and 12 km/s velocities. The line intensities are a factor ~ 5 stronger than at the H2 Peak 1 position, although noise is very large due to limited integration time. This suggests that the emission is from the hot core (6 km/s) and Peak A (12 km/s). We thus request 12 hours of time to carry out deep integrations at the frequencies of the 487, 774, and 1121 GHz, O2 lines, pointing at a position that includes the hot core and Peak A. This will confirm the identification as molecular oxygen (with three transitions at matching pair of velocities) and give a good handle on the temperature of the region producing O2 emission and its total column density. The total time requested is 12.1 hours.
### The Structure of a Molecular Cloud Boundary
Proposal ID: OT1_pgolds01_5
Principal Investigator: Paul Goldsmith
Time: 17.3 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
Molecular clouds do not exist in a vacuum, but are embedded in a warm, diffuse interstellar medium containing hydrogen largely in atomic form, and ionized carbon. Based on theoretical modeling, dense, cold clouds are surrounded by an intermediate temperature envelope in which the hydrogen is molecular (due to efficient self-shielding) and in which carbon changes from ionized to atomic, to molecular (primarily CO) as one moves to regions of greater extinction. This cloud envelope is expected to have a major impact on the structure of dense cloud in which star formationtakes place, as it can add to the pressure support confining them, and can serve as a conduit for energy flowing into the molecular cloud that can be critical for sustaining observed turbulence. This boundary layer is not readily observable in CO since the abundance of this species has dropped dramatically, and it is also difficult to study in molecular hydrogen emission, as the temperature is too low to significantly populate even the lowest excited rotational states. The boundary, sometimes called "dark gas", possibly contains a significant fraction of the total mass of the dense ISM. Based on detection of weak H2 emission from the boundary of the Taurus molecular cloud by Goldsmith et al. (2010), we here propose to use the unique capabilities of Herschel to make a well-calibrated cut through the "linear edge" boundary region in Taurus in the 158 micron fine structure line of CII, and both the 492 GHz and 810 GHz fine structure lines of CI. Accurate calibration is essential and cannot be achieved using ground-based facilities. We propose to use the HIFI instrument to resolve the line widths and probe the kinematics in the boundary layer. The ratio of the CI lines yields the density, and these lines, together with the distribution of intensity of CII and H2 will allow us to develop a well-defined model for the boundary layer. This will address important questions about molecular cloud structure, total mass, and evolution.
### The Auriga-California Molecular Cloud: A Massive Nearby Cloud With Powerful Diagnostics For Early Stages of Star Formation
Proposal ID: OT1_pharve01_3
Principal Investigator: Paul Harvey
Time: 19.1 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
We propose to map the Auriga-California Molecular Cloud (AMC) with the same observing parameters as being used for the rest of the clouds in the Gould Belt by the Herschel GT team conducting that program. The AMC was not included in that program BUT is extremely important as a counterpoint to the Orion Molecular Cloud (OMC) because it is as large and massive as the OMC but has a factor of 10 lower level of star formation, most of which is concentrated at the southeast end near the LkHalpha 101 cluster. We already have complete Spitzer survey data on this cloud and are in the process of obtaining JCMT line and continuum survey observations. The OMC has informed our understanding of star clusters and massive star formation. It is essential, however, to test that understanding by observing other massive clouds with differing levels of star formation. The combination of Herschel data with our existing Spitzer and molecular line data is vital to understand the physical reasons underlying the large differences in star formation between these two regions. Herschel's combination of angular resolution and 5-band imaging for dust temperature and emissivity measurements permit a uniquely high level of analysis of the far-IR emission from the AMC and comparison with the OMC.
### The chemistry of nitrogen in dark clouds
Proposal ID: OT1_philybla_1
Principal Investigator: Pierre Hily-Blant
Time: 29.4 hours priority 1
Category: Galactic Other
Summary:
Nitrogen is the fifth most abundant element in the local Universe. It is essential component of molecules associated to Earth-type life. Yet, the reservoir of nitrogen in the dense ISM, where stars, and ultimately planets, form, is not known. This is for good reasons. The main reservoir of gas-phase nitrogen are expected to be N or N2, and it is likely that most of the nitrogen be indeed frozen-out on dust grains in the form of ammonia ices. However, N and N2 are not observable in the shielded environments characterizing the embryos of star-forming regions. Hence, all what is know about nitrogen must rely on indirect observations of N-bearing molecules, the lightest (and thus among the easiest to form) of which are hardly detectable from the ground. To date, and despite longstanding efforts, our comprehension of the chemistry of nitrogen remains elusive. The HSO/HIFI instrument is opening new avenues in this respect, allowing astronomers to readily detect nitrogen hydrides and several key species of the nitrogen chemistry. This is the aim of this proposal. We propose the observation of key species that are observable only with Herschel. Those include NH, NH2 and NH3 (in their ortho and para forms), as well as their deuterated isotopologues, and other pivotal species like CH and CH2. This corpus of observations in order will allow to assess our understanding of the chemistry of nitrogen in dark cloud conditions, and answer the fundamental and open question, whether dust processes are necessary catalysts in this chemistry.
### High-J lines of HCN as tracer of feedback processes in high-mass star formation
Proposal ID: OT1_pschilke_2
Principal Investigator: Peter Schilke
Time: 16 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
The mechanisms involved in the formation of massive stars, and particularly the process of feedback from already-formed stars, are not well understood. Recent models of star formation have started to investigate the role of mechanic (outflows) and radiative feedback, but observational evidence for these processes altering the star formation process has been lacking. In an analysis of the HEXOS data, we have found that high-J HCN lines are perfectly suited to study this phenomenon: in SgrB2(M), they show a reversal of the infall profile at high J, indicating that in the inner regions the onset of feedback is halting the inflow, and the gas is actually expanding again.
In this proposal, we want to apply this powerful technique to a sample of high-mass star-forming cores at similar stages of development as SgrB2(M).
### Luminosity and mass loss history of the high-mass protostar IRAS20126+4104
Proposal ID: OT1_rcesaron_1
Principal Investigator: Riccardo Cesaroni
Time: 11.5 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
The main goal of this project is to estimate the luminosity of the high-mass protostar IRAS20126+4104 and obtain a direct measurement of the mass loss rate of the associated bipolar outflow. This is a well studied object, where a 7 Msun protostar is surrounded by a Keplerian disk and powers a bipolar outflow. The relatively small distance (1.64 kpc) and the limited complexity of the surroundings of this object, combined with the unique angular resolution of HERSCHEL in the far-IR, make it possible to reconstruct the spectral energy distribution and thus obtain an accurate estimate of the stellar luminosity. Knowledge of the mass and luminosity will set constraints on the evolutionary stage of the young stellar object. We also want to observe the OI 63 micron line which is strictly related to the mass los rate of the outflow. The latter can thus be obtained independent of the usual drawbacks (uncertain molecular abundance, unknown outflow inclination angle) of the estimates obtained from CO and other typical outflow tracers. Moreover, since the outflow is precessing, one can also relate the position along the outflow with the time of ejection and reconstruct the mass loss rate history of this object. We will also observe the OI 145 micron line to verify possible opacity effects in the 63 micron line, from the ratio between the two lines. These data will be complemented with observations of the CI line to image possible photo dissociation regions, plus a number of CO lines observed with SPIRE, PACS, and HIFI, to reconstruct the excitation structure of the outflow, both in space and velocity.
### A Herschel SPIRE/PACS Imaging Survey of the MonR2 and CepOB3 Molecular Clouds
Proposal ID: OT1_rgutermu_1
Principal Investigator: Rob Gutermuth
Time: 41.3 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
We propose complete surveys of the MonR2 (830 pc) and CepOB3 (700 pc) molecular clouds with SPIRE and PACS on Herschel to complement extant surveys with NEWFIRM and Spitzer at near-IR and mid-IR wavelengths, respectively. These two clouds complement cloud surveys of Orion and the Gould Belt clouds, as they are actively forming both low and high mass stars, and they are found at different evolutionary states relative to Orion. They are also closer to the galactic plane than Orion, implying a higher density of background stars and more reliable extinction maps. This study will impact our knowledge of two essential problems in star formation: the physical factors which determine the star formation rate and the initial mass function. We will produce high resolution maps of the large-scale dust column density and temperature from the SPIRE data maps and compare these to the density of protostars to determine the rate of star formation per area relative to the gas column density. We will use this data to reconcile inconsistent star formation rate vs gas column density correlations recently reported in the literature by measuring this relationship by independent means in a single cloud. To study the IMF, and its possible dependence on environment, we will look at factors that may determine the IMF: the mass of the pre-stellar core and the protostellar luminosity (which has a significant contribution from accretion). Pre-stellar cores will be extracted and characterized in terms of structure and mass. By combining the protostellar SEDs from Spitzer with PACS photometry, particularly 70~$\mu$m, better characterization of protostar bolometric luminosity and temperature distributions can be produced and compared among the clouds observed. With this data, we can examine how the core mass function and protostellar luminosity function can vary with density of young stars and cores and with the local conditions of the molecular gas, and how these vary from cloud to cloud.
### PACS and SPIRE observations of Galactic anomalous emission sources.
Time: 13 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
Despite the increasing evidence that the anomalous emission is a new physical mechanism acting in the diffuse interstellar medium, the nature and distribution of this component remains elusive. The currently most favored models attribute the observed microwave excess to rotating very small dust grains (PAHs and VSGs). Nonetheless, the infrared properties of the sources which, to date, are known to exhibit this type of emission are very poorly known mostly due to the limited angular resolution and frequency coverage of DIRBE and IRAS data.
We propose HERSCHEL PACS and SPIRE mapping of three Galactic anomalous emission sources (LDN 1780, LDN 675 and LDN 1111). This data, when combined with ancillary NIR and mid-IR data of comparable angular resolution (mainly from Spitzer), and coupled with available dust models, will allow to set tight constraints on the radiation field in the emitting sources as well as in their immediate surroundings. Such constraints, in turn, will allow to estimate the abundances of PAHs, VSGs and BGs, hence to shed light on the potential link between these dust populations and the observed microwave excess.
### HIFI Observations of the C18O and C17O J = 5-4 to 15-14 Transitions in Hot Cores: A Direct Method to Obtain Total Column Densities
Proposal ID: OT1_rplume_1
Principal Investigator: Rene Plume
Time: 35 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
Using CO to trace the total H2 column density in molecular clouds is a common practice. This practice, however, can be fraught with difficulties. First of all, CO is often optically thick, especially towards the highest column density regions in molecular clouds (where stars are born) and so the analysis of CO emission requires complicated radiative transfer modelling. Second, the conversion from CO to H2 relies on an often unknown conversion factor and so a canonical value of 1:10,000 is usually assumed. This is especially problematic in cold (T < 20 K) dense gas, in which CO can be depleted onto dust grains. However, in warm gas surrounding massive or even low mass protostars (so called "hot cores''), depletion can be circumvented and the rarer isotopologues (13CO, C18O and C17O) are optically thin enough that they can be used as column density tracers.
We propose to use Herschel/HIFI to directly derive total C18O and C17O column densities in a number of high mass protostars. The method we will use offers an unprecedented opportunity to derive this fundamental quantity in a model independent fashion. The basic idea is simple. For an optically thin line the observed integrated emission is proportional to the column density in the upper state. This quantity can be derived without any assumptions regarding density or temperature. If you observe enough transitions of C18O one can simply estimate the total column from summing all the observed states and correcting for the missing population. In high mass star forming regions, the high densities and temperatures mean that the higher-J states can be significantly populated and an estimate of the total column density based on only a few low energy transitions can be seriously in error. With HIFI, we have access to > 7 high-J C18O transitions, and therefore we can calculate the total C18O column densities with great accuracy.
### Water emission from outflows and hot cores in the Cygnus X proto-stars
Proposal ID: OT1_sbontemp_1
Principal Investigator: Sylvain Bontemps
Time: 36.2 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
The impressive first results from the WISH GT key program by van Dishoeck et al. indicate that water emission is bright towards the embedded proto-stars of all masses. These emissions are tracing outflows and warm inner regions of the collapsing envelopes (radiatively heated hot cores) which are unique probes of the cooling of these regions and of the kinematics of the dense warm gas. But WISH is limited by the reduced number of targets, and by the unavoidable biases introduced by the stringent selection of sources. The intermediate to high mass range is critical to challenge protostellar evolution models, and we argue that water emission from a complete sample of proto-stars in this mass range will be an important piece of knowledge for outflows to trace indirectly accretion and for hot cores to follow their time of appearance. Only Cygnus X is nearby and rich enough to provide a large sample of such proto-stars. We propose here to dramatically change the level of significance of WISH results by observing as many as 92 proto-stars covering the (final stellar) mass range of 3 to 20 Msun in the single complex of Cygnus X.
### Conditions for Giant Planet Formation: a Herschel Study of Raw Materials in Selected Debris Disks
Proposal ID: OT1_sdodsonr_1
Principal Investigator: Sarah Dodson-Robinson
Time: 26.5 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
Due to the observational difficulties of spatially resolving protostellar disk midplanes near the ice line, where most giant planet formation is thought to take place, most constraints on the possible locations and methods of giant planet formation have come from theory. We propose to use Herschel PACS and SPIRE photometry, and PACS spectroscopy, to observe five debris disks around Solar-type stars, in order to (1) observe young systems where giant planets cannot form, and (2) identify the available raw materials for typical planet formation. We will constrain the range of dust temperatures, and search for crystalline forsterite grains, as well as indirect diagnostics of ice and refractory carbon through deep line scans for [C II] (158 microns) and [O I] 63.2 microns.
### Synchrotron Radiation in Stellar Flares
Proposal ID: OT1_shawley_2
Principal Investigator: Suzanne Hawley
Time: 30 hours priority 2
Category: Galactic Other
Summary:
Stellar flares emit copious radiation at X-ray, optical and radio wavelengths but have not yet been investigated in the far-infrared. Recent observations at millimeter wavelengths provide tantalizing evidence that a population of ultrarelativistic electrons may be accelerated during flares and may provide significant synchrotron radiation in the far-infrared and sub-millimeter wavelength regimes. Herschel observations of two very active stars with a history of strong, frequent and energetic flares will probe this wavelength regime for the first time. Ultrarelativistic electrons may hold the key to explaining the photospheric flare heating that is necessary to produce the observed white light flare emission which carries more than half of the total flare energy. Our team brings together experts in stellar flare optical and radio observations, particle acceleration and plasma physics, and radiative hydrodynamical atmosphere modeling. We propose to carry out a Herschel flare observing campaign together with several ground-based optical and radio observatories and to produce a new generation of flare models that include the ultrarelativistic electron population.
### Hi-GAL360: the crucial step toward a global understanding of star formation in the Milky Way
Proposal ID: OT1_smolinar_5
Principal Investigator: Sergio Molinari
Time: 276.8 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
Hi-GAL360 will use PACS and SPIRE in parallel mode to obtain a 5-band photometric survey of the Outer Galactic Plane (OGP, beyond the solar circle) in the longitude range complementary to the Hi-GAL Open Time KP, i.e., 68° < l < 288° in a 2°-wide strip in latitude following the mid-plane of emission.
Hi-GAL360 data will enable a complete census of temperature, mass, density, column density and luminosity of filaments, clumps, and cores in the less confused outer Galaxy, where the assembly of filamentary structures and clouds and their fragmentation into clumps and cores can be uniquely characterised in low-metallicity and HI-dominated environments that are so different with respect to the inner Galaxy.
A complete OGP survey is required to obtain a statistically significant sampling of Galactic diversity - the full range of spiral arm, inter-arm, dust cloud, and star formation region properties - avoiding biases introduced by the study of specific or limited regions.
Hi-GAL360, together with Hi-GAL, will chart the Star Formation Rate and Efficiency from the Galactic Center to the far outer Galaxy, mapping the location and properties of star formation thresholds, thus providing the much needed connection between global scaling laws and the diversity of physical processes at work in the Galaxy. It will lay the foundations for a predictive, quantitative model of how star formation is triggered and regulated on all scales in the Milky Way. Such a model is vital to a full understanding of galaxy formation and evolution.
The merged Hi-GAL360/Hi-GAL Atlas of the Galaxy' will provide essential ground truth' for the interpretation of Herschel data on other galaxies from the Local Group to the high-redshift Universe where these objects are blended, and it will be the Herschel legacy that will remain unsurpassed for decades as the definitive survey of far-IR emission from the Galaxy.
Given our demonstrated community-oriented approach, we again waive our proprietary period.
### Measuring Emissivity Indices of Dust in Dense Cores with the SPIRE/FTS
Proposal ID: OT1_sschnee_1
Principal Investigator: Scott Schnee
Time: 6.2 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
Maps of the thermal emission from dust in nearby star-forming regions have revealed an apparent similarity between the mass distributions of dense cores (CMF) and the stellar initial mass function (IMF). However, deriving the mass of a core from measurements of dust emission is not straightforward. The primary difficulty comes from uncertainty in the dust emissivity, and in particular the slope of the dust emissivity at long wavelengths (the emissivity spectral index). Ground-based observations of the continuum emission from cores suffer from atmospheric contamination, so the best way to derive the emissivity spectral index is from space-based observations. Here we propose to use SPIRE/FTS to map the spectral energy distribution (SED) in a sample of dense cores and constrain the emissivity spectral index of the dust emission. These observations will be supplemented with GBT ammonia observations to break the degeneracy between temperature and the emissivity spectral index inherent in SED fits. We will then be able to derive much more accurate core masses, test the similarity between the CMF and the IMF, and search for variations of the dust properties with environmental factors such as temperature and density.
### WATCH - WATer Chemistry with Herschel
Proposal ID: OT1_swampfle_1
Principal Investigator: Susanne Wampfler
Time: 19.4 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
Water is one of the most abundant species in star-forming regions and plays important roles in both the energy balance, acting as a coolant, and the chemistry of star formation. Many of the species involved in the water chemistry emit in the far-infrared and are thus not observable from ground based facilities because of atmospheric absorption. Therefore, the Herschel Space Observatory provides a unique opportunity to study the chemical reactions involved in the formation and destruction of water and to probe the energetic processes in star-forming regions. Previous results from Herschel have shown that two species, OH+ and H2O+, that were thought to be important in the water chemistry of young stellar objects, are now mainly attributed to foreground clouds. These results raised the question on which chemical paths the formation and destruction of water takes place in the interior of protostellar envelopes. In this proposal, we plan to observe the different formation and destruction routes of water in a sample of eight nearby young stellar objects, which were chosen to cover a broad range of masses, luminosities and evolutionary stages. We propose to observe H3O+ and HCO+, two species that are closely linked to the formation and destruction of H2O and require high temperatures for excitation, in serveral high-J lines. This effort is complementary to the observations of H2O and OH done in the 'Water in star-forming regions with Herschel (WISH)' key project. The combination of the information from the H2O, OH, H3O+ and HCO+ emission will tell us on which routes the formation and destruction of H2O in protostellar envelopes proceeds.
### Unraveling the Mysteries of Complex Interstellar Organic Chemistry using HIFI Line Surveys
Proposal ID: OT1_swidicus_1
Principal Investigator: Susanna Widicus Weaver
Time: 42 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
We propose HIFI spectral line surveys of interstellar clouds to probe the influence of physical environment on molecular complexity. We will observe a statistically-significant sample of sources, cover a range of physical environments, and target selected frequency windows containing transitions from several known complex organic molecules. The goal of these observations is to correlate the relative abundances of organic molecules with the physical properties of the source (i.e. temperature, density, age, dynamics, etc.). Our broader research goal is to improve astrochemical models to the point where accurate predictions of complex molecular inventory can be made based on a given source's physical and chemical environment. The information gained from our proposed Herschel observations will serve as a benchmark for these astrochemical models and holds the promise of significantly advancing our understanding of interstellar chemical processes.
### Probing the HH111 Molecular Outflow with Herschel
Proposal ID: OT1_tbell_1
Principal Investigator: Tom Bell
Time: 17.4 hours priority 2
Category: Star Formation/Young Stellar Objects
Summary:
Outflows play a crucial role in star formation, since they carry away angular momentum from the protostars that drive them, allowing accretion to continue and the protostars to grow. They also represent a fossil record of the mass loss from their young hosts, providing valuable insights to the processes that govern accretion and outflow. Though jets and molecular outflows have been the subject of much scrutiny, the mechanisms responsible for launching and collimating the gas are still unclear and the relationship between the narrow optical jets and larger molecular outflows they accompany has still to be determined.
In order to understand the vital role of outflows in star formation, a detailed characterization of their physical, chemical and kinematical properties is essential. Accurate values for the mass, mass transport rate and momentum in outflows can then be derived to test competing formation scenarios, and the shock conditions can be determined. The HH111 jet and associated molecular outflow and CO bullets represent an excellent prototype of these outflow phenomena in which to accomplish this. We therefore propose to obtain a complete physical, chemical and kinematical picture of the hot molecular gas in the HH111 jet with Herschel by performing HIFI observations of selected CO rotational lines, SPIRE FTS mapping spectroscopy of the outflow region and SPIRE and PACS photometric maps of the same region. Together, these observations will enable a comprehensive study of the molecular gas and dust contained in the HH111 outflow, allowing an unparalleled determination of its physical properties and the role it plays in the mass loss from the central protostar. This, in turn, will give key insights into the mechanisms that power outflow phenomena in general.
### Probing The Unique Environment Around Sgr A*
Proposal ID: OT1_tbell_2
Principal Investigator: Tom Bell
Time: 40 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
We propose to study the extreme conditions in the molecular gas surrounding Sgr A* by obtaining a full spectral survey of this source with Herschel/HIFI. This will provide a complete chemical inventory, containing multiple transitions spanning a broad range of excitation conditions, and will constitute a unique resource with which to explore the diverse physical processes at work and confront current models with important new constraints. The molecular gas in this circumnuclear disk also serves as a template for the study of central regions of other galaxies, helping to elucidate the properties in those distant sources. These data will also include absorption lines from many important hydrides in diffuse clouds along the line of sight, and we will also perform deep integrations at specific frequencies to target key metal hydrides, which will allow depletion, diffuse cloud chemistry and key chemical reactions to be probed. The plethora of emission and absorption lines that these observations will provide, across a frequency range that is largely inaccessible from the ground, will constitute a detailed chemical and physical portrait of the interstellar medium under a diverse and extreme range of conditions. As such, the proposed spectral survey and deep integrations represent a valuable legacy dataset for the future.
### Extinction towards the Galactic Center
Proposal ID: OT1_tfritz_1
Principal Investigator: Tobias Fritz
Time: 6.7 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
We want to use far infrared hydrogen recombination lines for 6.7 hours from the Galactic Center with Herschel/PACS. We then combine the far infrared measurements with existing near and mid infrared measurements of hydrogen lines for obtaining the differential extinctions between the lines. Above 100 microns the extinction is below 0.05 mag such that be obtain the absolute extinction over the full infrared.
Firstly the absolute extinction can be used for following goals:
Many of the bright stars in the Galactic Center are massive, young O- or WR-stars. Their stellar types and ages have been derived individually by means of atmosphere modeling.
Putting a reliable, absolute magnitude scale to the near infrared emission from Sgr~A* allows one to relate properly radio, submm, near infrared and X-ray data with each other.
The 'red-clump' feature in the HR-diagram is well visible for the Galactic Center stars. Its apparent magnitude combined with the extinction measures the distance to the Galactic Center, R_0, independent from other methods.
Secondly the extinction law in the whole infrared regime can be used for testing the surprisingly flat extinction law in the mid infrared found by previous work constraining. This extinction law can then constrain dust grain modells.
### PACS Imaging of the CepOB3b Cluster: Observing the Truncation of Disks in a Rich Young Cluster
Proposal ID: OT1_tmegeath_5
Principal Investigator: Tom Megeath
Time: 8.3 hours priority 1
Category: Circumstellar/Debris disks
Summary:
We propose deep PACS 70 and 160 micron imaging of the Cep OB3b cluster. After the Orion Nebula Cluster (ONC), Cep OB3b cluster is the 2nd nearest, large (2000 member), young (3-5 Myr) cluster to the Sun. It is older and more evolved than the ONC, making it a superb laboratory for studying the evolution of disks in the cluster environment. The cluster contains two distinct, coeval sub-clusters. Spitzer observations show a lower disk fraction in the sub-cluster containing an O7 star, suggesting that disks are being photoevaporated and destroyed by the UV radiation from the O star. The proposed PACS observations, coupled with near-IR and mid-IR photometry, will measure the truncation of the remaining disks by UV radiation. With these data, we will probe the truncation and alteration of disks in an environment which is likely to be similar to that experienced by the young Solar Sytem.
### FIR study of dust processing in the Carina region
Proposal ID: OT1_tonaka_2
Principal Investigator: Takashi Onaka
Time: 13.1 hours priority 2
Category: Interstellar Medium/HII regions
Summary:
We propose to study dust processing and search for a signature of dust properties associated with massive star formation in a region of the Carina nebula, where a clear variation has been found by mid-infrared spectroscopy. ISO/SWS and Spitzer/IRS observations indicate the presence and variation of the feature around 22 micron in an interface region between the ionized gas and molecular cloud in the Carina nebula. The feature appears to be strongest around the ionization front and significant dust processing is indicated to take place. We propose to study this highly interesting region by PACS SED and line spectroscopy modes and SPIRE spectroscopy. We investigate the variation in the dust size distribution and degree of coagulation and search for possible features associated with the massive star-forming region. The present observation will provide the systematic far-infrared data of the region where clear evidence of dust processing is indicated for the first time and give crucial information on the study of material evolution in the interstellar medium.
### Depletion and Deuteration of Ammonia in Pre-stellar Cores
Proposal ID: OT1_tpillai_1
Principal Investigator: Thushara Pillai
Time: 2.6 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
Molecular line studies of dense cores have shown that NH3 is an excellent tracer of pre-stellar gas, which is the earliest phase in the formation of stars. Unlike most other molecules (mainly CO), ammonia does not deplete out in dense cores. This apparent non-depletion is still a mystery. To make matters worse, ammonia abundance has been shown to increase at the highest densities. The answer might lie in the choice of ammonia transitions that have been observed to propose non-depletion. These are the para-NH3 23 GHz rotational transitions that have critical densities of ~ 10^4 cm^-3 while NH_3 depletion is expected to occur at densities two orders of magnitude higher! However, the NH3 ground state transition at 572.5 GHz observable with Herschel has a critical density few orders of magnitude higher, close to where we expect to see depletion. We propose to unravel the seeming'' ammonia non-depletion in dense cores by mapping the densest region of a pre-stellar core (with heavy CO depletion) in ammonia. The molecular depletion is closely linked to molecular deuteration. NH2D is expected to be abundant in cold regions with significant CO depletion. The D/H ratio derived from the ratio of NH3 and NH2D column densities is consistently higher than that derived from other molecules, most importantly N2H+. The discrepancy is worse for higher mass cores where NH2D/NH3 ratios of up to 0.8 have been found! While other astrochemical processes may be at play, one of the prime suspects is again the poor choice of para-NH3 (1,1) transitions as dense gas tracer. We believe that this leads to ammonia column densities being underestimate. Here, we propose to observe NH3 J_K= 1_0-0_0 toward a high mass core where very high deuteration ratio has been found and derive the "true" NH3 column density. This proposal will address two fundamental issues with our understanding of ammonia chemistry in dense cores, (i) the seeming ammonia non-depletion and (ii) very high ammonia deuteration.
### Under pressure: Revealing the thermal and spatial structure of strongly irradiated clouds in the Carina Nebula, the nearest laboratory of massive star feedback
Proposal ID: OT1_tpreibis_1
Principal Investigator: Thomas Preibisch
Time: 6.9 hours priority 1
Category: Star Formation/Young Stellar Objects
Summary:
The Carina Nebula contains some of the most massive and luminous stars in our Galaxy and is the best site to study in detail the physics of violent massive star formation and the resulting feedback effects, i.e.~cloud dispersal and triggering of star formation. We are engaged in a comprehensive multi-wavelength study of the Carina Nebula. Our new X-ray and near-infrared data, and mid-infrared data reveal and characterize the full stellar population. We also have used LABOCA at the APEX telescope to obtain a wide-field sub-mm map of the Carina Nebula; while it shows the morphology of the cold clouds in unprecedented detail, these single wavelength data do not permit to determine cloud temperatures, and thus cloud column densities and masses. Here we ask for 7.2 hours SPIRE/PACS time to map the full spatial extent of the clouds (5.4 square-deg.) simultaneously at 5 wavelengths. The HERSCHEL maps will yield fluxes at the critical far-IR wavelengths and allow us to reliably determine cloud temperatures, column densities, and thus cloud masses. This will yield a complete inventory of all individual clouds in the complex, down to cloud masses of 1 Msun, and allow us to detect the youngest and most deeply embedded protostars (down to 0.1 Msun). We will map large-scale temperature gradients and changes in the dust properties that are expected as a consequence of the strong feedback by the massive stars, and establish and compare the clump mass functions in different parts of the complex. By comparison with similar HERSCHEL data for other star forming regions, we can address the question of how the particularly high levels of massive star feedback influence the evolution of the clouds and the star formation process. These HERSCHEL data will also reveal the small-scale structure of the irradiated clouds and allow a meaningful comparison to our dedicated numerical simulations of the disruption of molecular clouds, the origin of the observed pillar-like structures, and the triggering of new stellar generations.
### Structure of translucent clouds observed with HIFI [CII] 1.9THz and in H2 in absorption by FUSE
Proposal ID: OT1_tvelusam_1
Principal Investigator: Thangasamy Velusamy
Time: 22.7 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
We propose HIFI observations of 1.9 THz (158 micron) [CII] line emission in selected 27 lines of sight (LOSs) which have been observed in H2 absorption in UV by FUSE, and three observed in [CII ]2325A absorption by STIS. [CII] observations provide a powerful probe of warm diffuse clouds, and [CII] is a useful as a tracer of their warm H2 content. By combining FUSE and STIS which directly detects H2 and C+ in absorption and the HIFI [CII] data we can better constrain many of the physical conditions in the cloud including the density and pressure of the C+ gas. The [CII] line emission spectra will be complimentary to those observed in absorption in UV and, in addition to its extremely high velocity resolution, help us resolve the narrow absorption features in the H2 and HI gas. A comparison of the molecular H2 column densities inferred from the 1.9THz [CII] line in the clouds along the FUSE/STIS LOS with those directly measured by them will validate the interpretation of the HIFI [CII] emission observed by larger scale Galactic surveys. We request 22.7 hrs of observing time on HIFI in band 7b.
### HIFI studies of the small-scale structures in the Galactic diffuse clouds with [CII] and [CI]
Proposal ID: OT1_tvelusam_2
Principal Investigator: Thangasamy Velusamy
Time: 33.2 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
The 1.9 THz [CII] observations provide a powerful probe of warm diffuse clouds, because they can observe them in emission and are useful as a tracer of their molecular H2 not directly traced by CO or other means. HIFI observations of [CII] provide a high resolution of 12 arcsec, better than that for single dish CO (> 30 arcsec) maps, and much better than HI (>30 arcsec). Thus with HIFI we have an opportunity probe the small scale structures in diffuse clouds in the inner Galaxy at distances > 3 kpc. To study the structure of diffuse ISM gas at small scales we propose HIFI maps of 1.9 THz (158 micron) [CII] line emission in a selection of 16 lines of sight (LOSs) towards the inner Galaxy, which are also being observed as part of the GOT C+ survey of [CII] in the Galactic plane. GOT C+ provides mainly single point spectra without any spatial data. Maps of [CII] will constrain better the cloud properties and models when combining [CII] and HI data. The proposed OTF X map will be along the longitude and latitude centered on 18 selected GOT C+ LOS over a length of 3 arcmin in each direction, which is adequate enough to provide sufficient spatial information on the small scale structures at larger distances (>3 kpc) and to characterize the CII filling factor in the larger beams of the ancillary (HI, CO, and CI data). The [CI] 609 & 370micron and the 12CO(7-6) (which lies within the CI band) are excellent diagnostics of the physical conditions of transition clouds and PDRs. We will use the ratio of the [CI] lines to constrain the kinetic temperature and volume density of the CII/CI/CO transition zones in molecular clouds using radiative transfer codes. We also propose OTF X maps in both the [CI] lines for all CII target LOSs. We anticipate fully resolved structural data in [CII] on at least 300 velocity resolved clouds along with their [CI] emissions. We request a total of 33.2 hrs of HIFI observing time.
### Tracing Remnant Gas in Planet Forming Debris Disks : Confronting Theories of Ice-Giant Planet Formation
Proposal ID: OT1_vgeers_2
Principal Investigator: Vincent Geers
Time: 4.9 hours priority 1
Category: Circumstellar/Debris disks
Summary:
Recent studies of gas emission lines with Spitzer and sub-millimeter telescopes have shown that 10-100 Myr old stars with debris disks have too little gas left to form Jupiter like gas giant planets. Whether enough gas remains in these systems to form ice giant planets is still unanswered. The [OI] emission line at 63 micron is the most sensitive tracer of gas in the ice-giant region of 10-50 AU in disks, and Herschel PACS is therefore uniquely suited to test theories of ice-giant planet formation. We propose to obtain PACS line spectroscopy of [OI] (63 micron) for a carefully selected sample of four young stars from the FEPS Spitzer Legacy Science Program with ages from 10 to 100 Myr. These extremely well systems harbour prominent debris disks that could be in the process of forming ice giants such as Neptune and Uranus. The proposed observations will probe down to gas masses of 0.3-4 Earth masses, and allow us to constrain prospects for ice giant formation, measure gas-to-dust ratios of 1-10 in evolved disks to compare with planet formation / disk evolution models, and put constraints on whether the dust dynamics in these systems is driven by the remnant gas or by the radiation.
### The origin of H2O+ in dense clouds
Proposal ID: OT1_vossenko_4
Principal Investigator: Volker Ossenkopf
Time: 18.1 hours priority 1
Category: Interstellar Medium/HII regions
Summary:
We try to resolve the chemical evolution of oxygen hydrides in radiatively heated dense clouds. This involves in particular H2O+ and chemically related species, which are formed by gas-phase reactions initiated by cosmic ray ionization in diffuse clouds, but may be predominantly produced by the evaporation of icy grain mantles and the subsequent ionization of water by UV radiation in heated dense clouds. We will investigate the full chain of species OH+, H2O+, H3O+, OH, and H2O, connected by gas phase reactions, to quantify the contribution of ice evaporation in dense clouds.
We propose to observe these species in the dense layers known to exist in two massive star-forming regions, DR21(C), where indications of H2O+ from hot gas were already found and where the hot layer is affected both by UV radiation and a strong shock from a bipolar outflow, and Mon R2, a PDR with similar parameters but no indications of shock processing of the hot layer.
Differences between the results from the two sources will provide an estimate for the impact of shocks on the H2O+ production. By comparing the observed abundances of OH+, H2O+, H3O+, OH, and H2O with steady-state PDR models, we will be able to quantify the amount of water that is fed into the gas phase by the evaporation or photodesorption of ice mantles from dust grains.
### The chemistry of CH+ in disks around HerbigAe stars
Proposal ID: OT1_wthi01_1
Principal Investigator: Wing-Fai Thi
Time: 1.5 hours priority 2
Category: Circumstellar/Debris disks
Summary:
Chemistry of protoplanetary disks have focused on the inner (R<5AU) or outer disk (R>100 AU) but not in the 5-30 AU region where giant planets are formed. The hot organic chemistry of 5-30 AU region can be explored with Herschel. We tentatively detected CH+ emission in four disks at 72.14 micron. CH+ is a starting ion in the reaction network leading to methane, HCN, of C2H2. Two of the disks are known to have an inner gap up to ~10AU. We propose to obtain deep observations of three rotational transitions of CH+ with Herschel-PACS. The aims of the proposals are: 1) confirm the detections, 2) study the excitation condistions of CH+ in disks, 3) explore the hot carbon chemistry in disks with our chemical code, 4) understand the role of inner gap in the disk chemistry.
### Herschel Imaging of the remnant of a hot disk that is gone.
Proposal ID: OT1_zwang01_1
Principal Investigator: Zhongxiang Wang
Time: 1 hours priority 1
Category: Circumstellar/Debris disks
Summary:
The millisecond pulsar (MSP) binary J102347.67+003841.2 is unique since it once contained an accretion disk around 2001, indicating that it is the first such binary found at the end of its transition from a low-mass X-ray binary to a radio MSP. The accretion disk was likely disrupted by the pulsar wind from the MSP. Using Spitzer, we have found mid-infrared excess emission in the source, probably arising from the remnant of the previous accretion disk. Here we request Herschel/PACS imaging of the binary, seeking to detect the source at 70 and 160 microns. The detection will help establish the general properties of the putative remnant, which is part of our effort to fully study this rare MSP binary system.
## Stars (31)
### Search for fallback disks around nearby, slowly rotating neutron stars
Proposal ID: OT1_bposselt_1
Principal Investigator: Bettina Posselt
Time: 15.5 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
We propose to observe eight nearby, slowly rotating, strongly magnetized neutron stars with the Herschel PACS detector to search for dusty fallback disks and infer their properties. Such disks are generally predicted to be created after the supernova explosion by ejecta that fail to escape and remain bound. However, despite several searches, neutron star fallback disks remain elusive. Only one possible fallback disk has been detected so far -- around the slowly rotating (P = 8.7 s) magnetar 4U 0142+61 at a distance of around 4 kpc. Our proposed target sample includes seven radio-quiet, middle-aged neutron stars with similar periods, P = 3 - 12 s, and strong magnetic fields, B = (1 - 3) x 10^(13) G (the so-called Magnificent Seven), and one radio pulsar with similar P and B. All targets are much closer than 4U 0142+61 (d < 1 kpc). Their slow rotations allow the fallback disks to survive and increase the chance for disk detections. Our targets belong to the class of neutron stars that is discussed as a link between the ordinary rotation-powered pulsars and the magnetars. The possession of a fallback disk is one of the key parameters for understanding these different populations.
### Dust processing and grain growht in Keplerian discs around binary post-AGB stars.
Proposal ID: OT1_cgielen_2
Principal Investigator: Clio Gielen
Time: 15 hours priority 2
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
We propose to use the Herschel-PACS/SPIRE instruments to study the far-infrared continuum emission of a sample of evolved stars, both in the Galaxy and the Large Magellanic Cloud (LMC). All these stars are proven or suspected binaries surrounded by a long-lived circumbinary disc. Our analysis of the SPITZER mid-infrared spectra of these stars showed that grain processing is very effcient in these discs, despite the very short evolutionary timescale of the post-AGB central star. Extending the spectral energy distribution (SED) to far-infrared wavelengths is an essential complement in constraining the disc characteristics. The long-wavelength flux is very sensitive to the amount of large grains, and thus the total dust mass, and grain-size distribution within the disc. The ultimate goal of our research is to study the structure, formation and evolution of the very common discs around evolved binary stars, and constrain their impact on the evolution of the binary systems.
### Far-IR bands of PAHs in the Red Rectangle
Proposal ID: OT1_cjoblin_2
Principal Investigator: Christine Joblin
Time: 24.8 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Observations in the far-IR window should make a major contribution to solving two major problems in molecular astrophysics - the identity of the carriers of the Aromatic Infrared emission Bands (AIBs) and the Diffuse Interstellar absorption Bands (DIBs). The DIBs are generally attributed to carbon-based molecules but none has been assigned. Polycyclic aromatic hydrocarbons (PAHs) are commonly accepted to be the carriers of the AIBs but the hypothesis suffers from the lack of identification of individual species. This seriously limits the potential of these spectral signatures as probes of astrophysical conditions and processes.
We propose to exploit the unique capabilities of Herschel to record the far-IR emission features of PAHs in the Red Rectangle. These features are very specific to the exact molecular identity and are a very attractive route for the spectroscopic identification of PAHs. Most of them carry a sharp Q branch increasing the contrast for their detection. We ask for 24.8 hours to perform deep PACS and SPIRE FTS spectroscopy to search for these Q branches.
The unique carbon-rich Red Rectangle nebula is in an active stage of dust condensation and displays the strongest AIBs known as well as emission bands connected to the DIBs. Small molecules are underabundant and the Red Rectangle is clearly the place where the formation of large molecules can be tracked and the link between the AIB and DIB carriers should be explored.
The analysis of the bands will be performed using spectroscopic data, both theoretical and experimental, as well as Monte Carlo modelling to simulate the emission process. Even in the worst case of no band identification, comparison of model predictions with the Herschel spectra will strongly constrain the PAH model. If some lines are identified, we will apply for follow-up observations with HIFI to resolve the hot band structure of the Q branches and structure in the P and R branches.
Considering the short life of Herschel, this proposal is therefore very timely.
### Molecular complexity of the O-rich pre-Planetary Nebula OH231.8
Proposal ID: OT1_csanch01_1
Principal Investigator: Carmen Sanchez Contreras
Time: 32.4 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Envelopes around evolved stars are extraordinarily efficient factories of complex molecules and dust particles that will eventually enrich the ISM. To date, most chemistry studies have focused on C-rich envelopes, expected to show the largest molecular variety and abundances. Recent observations suggest that O-rich shells may be as chemically diverse as their Carbon counterparts, however, no serious attempt has been made yet to perform a full frequency scan of such objects. We propose to carry out a line survey with HIFI of the well known, O-rich pre-PN OH 231.8, which displays fast (>400 km/s), bipolar outflows and a molecular richness unparalleled amongst O-rich AGB and post-AGB stars. Results from our exploratory mm line survey with the IRAM 30 m antenna of this object has led to the detection of hundreds of lines from different species that clearly point to non-equilibrium/shock-induced molecule formation processes in the fast flow. The HIFI could be potentially effective to reveal the dense and warm regions near the centre, which is strongly affected by shocks.
At its completion, this project will provide the sorely needed molecular inventory and abundance measurements in O-rich CSEs, which are required to obtain a better understanding of the intricate, non-equilibrium molecule formation processes in O-rich environments. We will use our radiative transfer and chemistry models to reproduce the observed spectra and empirically derived abundances, respectively, and constrain the nebular physical and chemical conditions in the envelope of OH231.
### The puzzle of water vapour in carbon-rich stars
Proposal ID: OT1_dneufeld_2
Principal Investigator: David Neufeld
Time: 28 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Using the HIFI instrument, we will address the puzzling - but widespread - appearance of water vapour in carbon-rich stars. Following up on detections of water in ALL SIX carbon-rich AGB stars observed to date in a pilot study performed in the HIFISTARS Key Program, we will target additional water transitions in four stars already observed or expected to show the most luminous water emissions. The target stars are CIT6, IRAC 15194-5155, V Cygni, and S Cep, and the additional transitions are the 4(22)-3(31) and 3(12) - 2(21) transitions at 916 GHz and 1153 GHz. Combined with spectra already obtained for the low-lying water transitions, and interpreted in the context of water excitation models, the proposed observations will place strong constraints upon the location of the emitting water. We will therefore be able to distinguish between various hypotheses that have been proposed for the origin of the observed water: the vaporization of orbiting comets or dwarf planets; catalytic formation on dust grains; or chemical processes initiated by the photodissociation of CO. In addition, we will carry out deep integrations to observe the lowest 1(11) - 0(00) transition of para-water at 1113 GHz in two carbon-rich AGB stars: IRAS+40540 and V Hya; here, ortho-water has been securely detected but existing observations of the 1113 GHz para-water line yield weak detections that lack the signal-to-noise ratio needed to constrain the ortho-to-para ratio.
### A detailed study of the physics and chemistry in the Planetary Nebula NGC7027
Proposal ID: OT1_Fherpin_1
Principal Investigator: Fabrice Herpin
Time: 19.4 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Molecular spectroscopy at sub-mm and FIR wavelengths is an extremely powerful tool to investigate the latest stages of stellar evolution. The process of mass loss from evolved stars is not well understood, and molecular emission offers a unique avenue to trace the kinematics and structures of such objects, from AGB stars and their successors, Planetary Nebulae (PN), to massive supergiants. In addition, circumstellar shells of evolved stars foster a remarkable chemistry, producing unusual molecular species not easily observed in other environments, including long carbon chains, anions, metal-bearing molecules, and phosphorus compounds. The mechanisms by which this chemical synthesis takes place, its relationship to dust formation, and its evolution during the AGB and post AGB-phases, are all important questions that have yet to be understood. This proposal and the related other proposals submitted by our collaborators seek to answer these questions. Through the study of the emission from specific species combined with selected spectral surveys towards the PN NGC7027, we aim at understanding more specifically the physics taking place in the beginning of the PN stage, more exactly to precise the physical conditions ruling the molecular envelope, the ionized region and the thin interface between both, i.e. the PDR, through the quantification of the UV and shocks influence.
### Clues to the Evolutionary History of the R Coronae Borealis Stars
Proposal ID: OT1_gclayton_1
Principal Investigator: Geoffrey Clayton
Time: 25.6 hours priority 2
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
The unexpected discovery that the R Coronae Borealis (RCB) stars have isotopic abundances of 18O which are up to 500 times greater than those seen in other stars has increased the likelihood that these rare hydrogen-deficient carbon stars are the result of a double degenerate white dwarf (WD) merger (DD) rather than a final helium shell flash (FF). But other pieces of the puzzle have yet to be explained. For instance, a few RCB stars, including R CrB itself, show enhanced Li abundances, which favors the FF scenario. Also, IRAS images show that several RCB stars possess large dust shells which are consistent with fossil Planetary Nebula (PN) shells where the gas is no longer ionized. If these are PN shells, then that would point strongly toward the FF scenario. But other explanations for the dust shells include the FF outburst itself and new dust from the recent RCB phase. In addition, newly acquired Herschel/Spire images have called into question the reality of the shells themselves. The much improved spatial resolution over previous IRAS and MIPS images shows that some or all of the R CrB 100-micron shell is due to a cluster of galaxies lying directly behind the star. It is imperative that new high spatial resolution PACS and Spire images be obtained to verify the existence of these RCB star dust shells, as well as to analyze the morphology of the shells to deduce their nature and help decide between the DD and the FF scenarios. Furthermore, the new Herschel images, covering the wavelength range 70-500 microns, will be used together with archival IRAS, Spitzer and other datasets to produce SEDs for each star which will be modeled using Monte Carlo radiative transfer codes to determine the total dust mass, and total mass loss over the lifetime of the stars. It is a very exciting prospect that the RCB stars could be shown to be the product of a WD merger. This small group of stars would become even more interesting as they would be low-mass analogies to Type Ia supernovae.
### How Cool Are Planetary Nebulae?
Proposal ID: OT1_hdinerst_1
Principal Investigator: Harriet Dinerstein
Time: 6.1 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
We propose to observe the [O III] 52 and 88 micron fine-structure lines with PACS in planetary nebulae, in order to investigate whether they contain a cold and possibly metal-rich component in addition to the ordinary hot (10,000 K) material. The presence of cold gas has been proposed in order to account for the excessive strengths of optical emission lines from recombining O++ ions, and low temperatures (500 - 5000 K) indicated by some diagnostics. If planetary nebulae truly have such inhomogeneous physical conditions and abundances, this calls into question our fundamental understanding of the composition of the nebular gas, a major source of recycled material to the ISM. The FIR [O III] lines offer a unique opportunity to address this issue because, due to their low excitation energies, they are emitted from both cold and hot gas, while the optical [O III] lines arise only from hot gas. The bright 52 and 88 micron lines were easily observed in some of our sample using less sensitive, large-beam instruments such as the Kuiper Airborne Observatory (by this P.I.) and ISO-LWS. For several targets the previous observations indicate O/H values greater than solar, supporting the idea that metal-rich gas is present, but the higher angular resolution of PACS is needed in order to discern whether the metal-rich material is concentrated towards the central regions, as claimed by optical studies. For several objects we propose to also measure the 88.8 micron 13–12 H I line, which will not only provide a measurement of H+, but also a probe of temperature by comparing its strength to that of shorter-wavelength H I lines. The latter will be taken from Spitzer-IRS maps (for a few targets), and optical integrated-field unit spectral maps either already obtained, or to be obtained, at McDonald Observatory. These observations may enable us to prove or disprove the presence of cold O-rich material in planetary nebulae.
### Additional Hpoint observations of large post-AGB sources from HIFIStars
Proposal ID: OT1_jalcolea_1
Principal Investigator: Javier Alcolea
Time: 13 hours priority 2
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
One of the most spectacular phases in the evolution of intermediate mass stars takes place at the end of their lives. At the end of the AGB, the central star dashes across the HR diagram from the red giant to the blue dwarf region. At the same time, the spherically symmetric and slowly expanding circumstellar envelopes around AGB stars become planetary nebulae (PNe), displaying a large variety of shapes and structures far more complex. This transformation takes place at the very end of the AGB, and it is due to the interaction of fast and bipolar molecular winds with the fossil AGB circumstellar envelope.
The origin of these post-AGB winds is still unclear, but we know that the resulting two-wind interactions are only active during a very short period of time, ~ 100 yr, but still they are able to strongly modify the kinematics of the nebulae and re-shape them. To better understand these processes we must study the warm molecular gas component of early post-AGB sources, both pre-planetary nebulae (pPNe) and young PNe. Herschel/HIFI is very well suited at this, because its spectral coverage, high velocity resolution, and superb sensitivity.
For these reasons, 10 pPNe and young PNe were included in the KPGT HIFIStars, were a large number of spectral lines are observed in a moderate number of frequency setups, but just at the central point. In many cases this is simply enough, since most of post-AGB sources in HIFIStars are compact. However there are three cases in which the non spherically symmetric structures seen in the warm gas are larger than the beam of the telescope: OH 231.8+4.2, NGC 7027 and NGC 6302. Therefore we propose to perform some additional pointing in these three sources in a selected sample of HIFIStars frequency setups, were we have detected strong lines of CO, H2O, NH3 and OH. These observations are crucial to understand the kinematics and interactions traced by these warm gas probes, and so gain insight in the intricate problem of the post-AGB dynamics.
### Characterising the Environment of Fullerene Formation
Proposal ID: OT1_jberna01_1
Principal Investigator: Jeronimo Bernard-Salas
Time: 6 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
The bulk of the dust that is injected into the interstellar medium is formed via a complex chemistry in AGB circumstellar environments, which transforms the atomic gas into molecules and dust. To date, more than 60 individual molecular species of both inorganic and organic nature and a handful of dust minerals have been identified in these outflows. These environments are also thought to be the birthplace for large aromatic species such as polycyclic aromatic hydrocarbons and fullerenes. Because of their remarkable stability, fullerenes have been predicted to survive the harsh conditions of the insterstellar medium. However, targeted searches for the presence of fullerenes in various astrophysical environments were unsuccessful or not conclusive, until now. The Spitzer mid-IR spectrum of Tc1, a young planetary nebula with a low excitation central star and a high C/O abundance ratio, shows clear traces of C60 and C70. This indicates that when conditions are favorable, fullerenes are formed in large quantities. The mid-IR spectra allow us to quantify the abundance of carbon in the fullerenes, estimate their temperature, and detect them in the solid state in circumstellar environments, but to date we have little information on the circumstellar dust or the composition of the gas. We propose to use the far-IR spectrum of Tc1 using the Herschel PACS spectrometer to study the energy balance and characterize the conditions in the circumstellar regions where fullerenes are formed.
### Molecular complexity in the circumstellar envelope of the O-rich evolved star VY CMa
Proposal ID: OT1_jcernich_5
Principal Investigator: Jose Cernicharo
Time: 54 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Envelopes around evolved stars are factories of complex molecules (neutrals, anions and cations) and one of the main sites for dust formation. Most chemical studies have focused on C-rich envelopes, in particular on IRC+10216. Recent observations of metal bearing species and hydroxides in O-rich shells suggest that the chemistry in these objects can be as richer as in C-rich circumstellar envelopes. We propose to perform a complete line survey of the prominent O-rich star VY CMa with HIFI.
This study will provide, in addition to all lines of CO, H2O, HCN, SiO, SO2, a complete inventory of the molecular gas in O-rich evolved stars. The comparison with the line survey of IRC+10216 (already carried out with HIFI/Herschel) will permit to distingush the different chemical processes in these objects and the subtle role of the C/O abundance ratio in the molecular composition of the gas at different distances from the central star.
We will use our radiative transfer and chemistry models to reproduce the observed spectra and to derive molecular abundances. The data will also allow a better understanding of the physical structure of the envelope.
### Shock Chemistry and Dust Processing in Interacting Supernova Remnants
Proposal ID: OT1_jhewitt_1
Principal Investigator: John Hewitt
Time: 18 hours priority 2
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Supernova remnants interacting with dense moelcular clouds provide astroc-hemical laboratories to study heating and cooling of the dense ISM, shock chemistry, destruction and sputtering of dust, and the reformation of molecules. Water is expected to be a major coolant for shocks into dense gas, yet the number of remnants in which IR lines of hydroxyl and water are detected is very limited. We propose Herschel PACS, SPIRE and HIFI observations of three remnants with particularly high shocked gas densities, high dust and IR line luinosities, and extreme ionization environments. The scientific objectives of this proposal are: (1) to determine the abundance and excitation of oxygen-bearing molecules, (2) to study the oxygen chemistry in dense molecular gas shocked by powerful supernova remnant blast waves, and (3) to directly measure dust processing and constrain the effects of dust on shocks and oxygen chemistry.
### A HIFI survery of Water Fountain stars: unveiling the inner structure of hit star envelopes.
Proposal ID: OT1_jrizzo_1
Principal Investigator: Jose Ricardo Rizzo
Time: 3 hours priority 2
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Water fountain'' stars (WF) are considered key objects to our knowledge of the sun-like star evolution processed. At some point soon after AGBs, WFs would develop very fast and highly-collimated outflows, which produces H$_2$O maser emission, spread over more than 100\,\kms, when hitting the AGB previous envelope. Very recently, our group has detected low-$J$ CO and $^{13}$CO line emission arising in the cold, outer parts of the envelope. Based on these results, we ask for HIFI observations of mid- and high-$J$ lines of CO, together with a set of thermal H$_2$O lines, and CI. With these data, we plan to probe the inner, hotter, and denser parts of the envelopes, and to give some insights about the mass-loss history and chemistry; possibles PDRs will also be tested. This information will provide valuable inputs to our models, such as the total mass, and temperature profile. Some physical parameters will be also constrained. We have selected the whole sample of known WFs, a total of 14 sources (two of them still unpublished), for this project.
### Measuring the electron spectrum generated by diffuse shock acceleration in the Pulsar Wind Nebula HESS J1632-478.
Proposal ID: OT1_mbalbo_1
Principal Investigator: Matteo Balbo
Time: 0.5 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Relativistic collisonless shocks propagating in plasmas are an essential ingredient to explain particle accelerators such as gamma-ray bursts, supernovae remnants, pulsar and stellar winds. Numerical simulations predict particle energy distributions but these are very difficult to test because of the lack of simultaneous observation over 20 decades of frequency, complex geometries or variability.
We propose to use SPIRE in the Small Map configuration to map the infrared emission of a very energetic and old pulsar wind nebula recently detected by HESS. Exploiting the unique resolution and sensitivity of SPIRE at 250, 350 and 500 $\mu$m, we aim at detecting the faint synchrotron emission that will be compared to existing measurements in the radio, X-rays and gamma-rays. These wavebands, located between the CMB and dust emission, are centered where the synchrotron emission from the predicted relativistic Maxwellian distribution peaks, providing a constraining flux measurement.
### Herschel PACS and SPIRE investigation of water fountains
Proposal ID: OT1_mguerrer_1
Principal Investigator: Martin A. Guerrero
Time: 17 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Water fountains (WFs) are late AGB and post-AGB objects that show the earliest known manifestation of collimated mass-loss in evolved stars, with jets that have dynamical ages of only 5-100 yr and sizes as small as 100-500 AU. These fast collimated outflows, impinging onto the circumstellar material at the end of the AGB phase, are presumably responsible for the shaping of asymmetric planetary nebulae (PN), with the highly asymmetric H2O-maser-emitting PNe being presumably the immediate descendants of WFs. Therefore, WFs and H2O-PNe are key objects to study the shaping of PNe. Since their thick envelopes make them strongly obscured in the optical and near-IR, their inner circumstellar structure would be best traced at longer wavelengths.
Here we propose the acquisition of Herschel PACS and SPIRE deep imaging photometric observations of all known WFs and H2O-PNe to be added to near-IR, mid-IR, submm, and mm data to continue building the spectral energy distribution (SED) of these sources, and to check for the presence of extended material. The characterization and theoretical modeling of their SEDs will be used to infer the presence of disks and to estimate the physical parameters of circumstellar disks and envelopes, which in their turn will impose constraints on the models for the generation of jets in evolved objects.
### Herschel SPIRE FTS observations of mass loss from a red supergiant in the Large Magellanic Cloud
Proposal ID: OT1_mmatsuur_1
Principal Investigator: Mikako Matsuura
Time: 7.7 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
We propose to observe submillimeter CO thermal lines in the brightest red supergiant (RSG) in the Large Magellanic Cloud (LMC). We will use Herschel/SPIRE in the FTS mode. The high sensitivity of this instrument enables us to detect CO thermal lines in a RSG beyond the Milky Way for the first time. The objectives of this programme are (1) to obtain the gas mass-loss rate from the RSG, (2) to evaluate the gas-to-dust mass ratio of the RSG, and (3) compare the gas-to-dust mass ratio of the RSG with that of the LMC interstellar medium (ISM). Those will place important constraints on whether RSGs are important contributors to the chemical enrichment of the ISM.
RSGs lose a large quantity of mass through stellar winds, and these winds consist mainly of molecules whose mass can be measured by the CO thermal lines. Using the newly obtained gas mass-loss rate, and the previously obtained dust mass-loss rate, we will estimate the gas-to-dust mass ratio of the circumstellar envelope (CSE) of the RSG. Of particular interest is whether the gas-to-dust mass ratio is affected by the metallicity of galaxies. The metallicity of the LMC is about half of the solar metallicity, and we will compare our measurements with those of Galactic RSGs. Dust grains are composed of metals, and we expect a higher gas-to-dust mass ratio in the LMC. Further, we will compare our measured CSE gas-to-dust mass ratio to the LMC ISM value. That would aid determining whether these dying stars are important sources of gas and dust in the ISM, or if dust grains gain mass from the gas phase in the ISM, using the dust injected by dying stars as seeds. If the dust mass increases in the ISM, the gas-to-dust ratios should differ between the CSE and the ISM. This will provide the first direct observational evidence of whether additional dust depletion is important in the ISM.
This small (7.7 hour) project will have a great impact on our understanding of both stellar physics and ISM evolution.
### Clumping in OB-star winds
Proposal ID: OT1_mrubio_1
Principal Investigator: Maria del Mar Rubio
Time: 9.4 hours priority 2
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Massive stars, their nature and evolution, play a important role at all stages of the Universe. Through their radiatively driven winds they influence on the dynamics and energetics of the interstellar medium. The winds of OB stars are the most studied case. Commonly, the mass-loss rates of luminous OB stars are inferred from several types of measurements, the strengths of UV P Cygni lines, H-alpha emission and radio and FIR continuum emission. Recent evidence indicates that currently accepted mass-loss rates may need to be revised downwards when small-scale density inhomogeneities (clumping) are taken into account. We argue that only a consistent treatment of ALL possible diagnostics, scanning different parts of the winds, and analyzed by means of ‘state of the art’ model atmospheres, will permit the determination of true mass-loss rates. To this end we have assembled a variety of multi-wavelength data, but one crucial observational set is missing: far-IR diagnostics of free-free emission, which uniquely constrain the clumping properties of the wind at intermediate heights. We propose, therefore, to use PACS photometric mode to fill this crucial gap, studying the 70 and 110 micron fluxes of a carefully selected sample of 29 O4-B8 stars. These observations will provide the missing information to derive the clumping properties of the entire outflow, to understand the wind physics, and to obtain reliable mass−loss rates.
### Hunting for missing evolved stars in the Galactic plane
Proposal ID: OT1_nflagey_1
Principal Investigator: Nicolas Flagey
Time: 39.6 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
We discovered more than 400 compact shells in the MIPSGAL 24 microns survey of the Galactic plane. While only 10% of them are detected at shorter wavelengths, about a third are visible in the MIPSGAL 70 microns survey. About 15% of all the objects have been identified previously as planetary nebulae, supernova remnants, Wolf-Rayet stars, luminous blue variables. Spectroscopic follow-ups on a limited sample in the near-IR and mid-IR have revealed several dust-free planetary nebulae with very hot central white dwarf as well as a significant increase in the number of WR/LBV candidates. The remaining 350 or so unknown bubbles are also expected to be evolved stages of low- to high-mass stars that could account for the "missing" evolved stars in the Galaxy. To determine the true nature of a significant fraction of the unidentified bubbles, we propose to observe 35 of the brightest objects in the MIPSGAL 70 microns images with PACS Range Spectroscopy. With these data we will constrain the origin of their far-IR emission. Comparing the proposed spectroscopic to those of known evolved stars from the MESS Guaranteed Time Key Program will allow us to unequivocally identify the MIPSGAL bubbles. The richness of the far-IR emission spectrum of these evolved stellar objects will also provide us with dust and gas (atomic and molecular) features, with which we will characterize in details the physical conditions within each bubble thanks to modeling of these features. "Unveiling hidden details of star and galaxy formation and evolution" is the Herschel observatory's statement, as the mission brochure's cover shows. The observations that we propose here are in perfect resonance with that statement as we aim at lifting the veil on evolved stars hidden in the Galaxy. Furthermore, we propose observations that will build a synergy between two Key Programs (HiGAL and MESS).
### Oxygen abundances in carbon-type Wolf-Rayet stars from PACS scan spectroscopy
Proposal ID: OT1_pcrowthe_1
Principal Investigator: Paul Crowther
Time: 8 hours priority 2
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
We seek 13.6 hours of spectral scans of the [OIII] 88 micron fine-structure line with PACS for a sample of Milky Way carbon and oxygen sequence Wolf-Rayet stars. The proposed observations will: (i) enable reliable oxygen abundances to be determined for WC stars for the first time, to test evolutionary predictions; (ii) refine the degre of clumpig in the outer stellar winds of these stars derived from existing ISO/SWS or Spitzer/IRS datasets.
### Physical properties of the dusty circumstellar envelopes of two bright classical Cepheids
Proposal ID: OT1_pkervell_1
Principal Investigator: Pierre Kervella
Time: 2.8 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
The recent discovery of circumstellar envelopes (CSEs) around Cepheids is an indication that many Cepheids, if not all, are surrounded by CSEs. The bright classical Cepheids RS Pup and delta Cephei are particularly interesting members of their famous class of variable stars, as they are known to be surrounded by large CSEs that can be resolved angularly by Herschel. The requested observations will probe the cold extensions of these nebulae, and will be the first observations of any Cepheid in this wavelength domain. The present proposal aims at characterizing the dust in the CSEs using Herschel/PACS and SPIRE imaging photometry. Our scientific goal is to understand the origin of the envelopes: were they formed through evolutionary mass-loss from the Cepheids or are they made of residual interstellar material pre-existing the formation of the Cepheid progenitor? This question is of critical importance both to understand the evolution of the Cepheids themselves (stellar physics) and for the future application of the period-luminosity relation in the thermal-IR domain with the James Webb Space Telescope (extragalactic distance scale). The formation mechanism of the large dusty nebula surrounding these Cepheids is currently unknown, but two hypotheses appear plausible: (A} - it is a result of evolutionary mass-loss from the star through stellar wind, possibly linked to pulsation, that condensed into dust at large distances from the star. (B) - it is a remnant of the interstellar medium from which RS\,Pup formed, blown away by the stellar wind from the Cepheid. Our goal is to test these two hypotheses and characterize physically the cold dust in the envelopes (mass, temperature, distribution, composition).
### Herschel's Opportunity to Solve the Nebular Abundance Problem While Creating a Legacy Planetary Nebulae Dataset
Proposal ID: OT1_rrubin_1
Principal Investigator: Robert Rubin
Time: 33.3 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Abundance surveys of a large sample of Galactic planetary nebulae (PNe) have led to the discovery of a group of super-metal-rich nebulae whose spectra show prominent optical recombination lines (ORLs) from C, N, O, and Ne ions. The heavy element abundances derived from ORLs for several PNe are a factor >10 higher than those derived from the traditional method based on collisionally excited lines (CELs). This ratio is called the abundance discrepancy factor (adf). A promising proposition to explain the nebular abundance problem posits that these nebulae contain (at least) two distinct regions - one of "normal" electron temperature, Te (~10000 K) and chemical composition (~solar) and another of very low Te (< 1000) that is H-deficient, thus having high metal abundances relative to H. The latter component emits strong heavy element ORLs and IR fine-structure (FS) CELs but essentially no optical/UV CELs. Efforts to directly detect these inclusions in PNe have been unsuccessful to date. However, there is mounting circumstantial evidence for their existence, such as presented in our recent paper that modeled the high-adf PN NGC 6153 using a 3-D photoionization code. The models that included the low Te, H-deficient knots fit most observations far better than did those models without the clumps. With the launch of Herschel, there is finally the capability to perform a test we've been dreaming of. Measurements have shown that the adf varies with position in a PN and is highest close to the central star. The very low Te inclusions must be cooled via FS IR lines. We propose to use Herschel to map the FS IR lines in 5 bright PNe on the largest adf list, to find if these lines peak where the adf peaks. These spectra will also provide a feast for our other team expertise/interests: a legacy dataset of molecular lines to explore PDRs, how the central star interacts with the AGB ejecta and shapes the PN, how the shocks are produced, what comprises the chemistry of the molecular ejecta, and how do PNe evolve.
### A Statistical Sample of Planetary Nebulae in the Galactic Bulge: Measuring Masses and Mass-Loss Rates
Proposal ID: OT1_rsahai_2
Principal Investigator: Raghvendra Sahai
Time: 25 hours priority 2
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
We propose to exploit Herschel's unprecedented sensitivity to obtain 100-500 micron photometry for a statistical, flux-limited (in the IRAS 60 micron band) sample of Galactic bulge planetary nebulae (GBPNe), using PACS and SPIRE. The Galactic Bulge volume, offers a unique, nearby environment where a statistical population of PNe, all at roughly the same well-established distance, can be studied in order to understand these objects, test theoretical models for their formation and evolution, and address the mystery of the constancy of the PN luminosity function (an important cosmological distance indicator). Much of the mass ejected during the preceding AGB phase is expected to lie outside the ionised shells in these objects, and can only be detected via the thermal emission from cold dust.
Herschel provides us the only platform to measure the mass budgets of a statistical sample of GBPNe, and thus help us address one of the longest standing astrophysical problem: the relationship between the birth mass of solar mass stars and the mass left at the end when they die. PNe are an important contributor to the total mass return to the ISM for the old Bulge population, and the proposed observations will allow us to infer the PN contribution to the total rate of mass loss in the Bulge, a crucial input to evolutionary models. The robust constraints to the progenitor masses of PNe from our study will allow elemental enrichments to be determined as a function of initial stellar mass, providing key information for models of AGB nucleosynthesis.
The proposed observations are a critical component of a broader study comprising existing and future ground- and space-based observations that will produce a combination of nebular masses, mass-loss rates, luminosities, physical sizes, morphologies, radial velocities, ages, and chemical abundances for a statistical sample of planetary nebulae, resulting in a unique dataset describing the final stages of stellar evolution in unprecedented detail.
### Searching for Interrupted Mass-Loss in AGB stars: A Herschel Survey
Proposal ID: OT1_rsahai_4
Principal Investigator: Raghvendra Sahai
Time: 13.5 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Although the massive winds of AGB stars are reasonably well understood as resulting from radiation pressure on dust grains, our knowledge of how the mass-loss rates change as stars ascend the AGB is very poor. A small number of carbon-rich AGB stars have been found with detached circumstellar shells that imply that their mass-loss rates dropped dramatically a few thousand years ago. This decrease has been hypothesised to result from a He-shell flash which is believed to occur periodically in these stars; the nucleosynthesis of carbon in this flash, and its subsequent dredge-up to the stellar surface, converts oxygen-rich stars to carbon-rich ones.
We propose to use Herschel's unprecedented far-IR sensitivity and angular resolution to make a systematic search for signatures of interrupted mass-loss such as detached shells in a list of 21 targets which includes C-rich, O-rich and S-type stars (C/O~1) to test this hypothesis. Our list has been constructed using the IRAS point-source catalog to identify objects which have "60-micron excesses": their 60 to 25 micron flux ratio is > 0.4 and thus significantly larger than the average ratio for AGB stars. This excess implies the presence of a cold, extended dust shell, and relatively little hot dust close to the star, as compared to the average mass-losing AGB star. The morphology of detached shells provides a clear indication as to its origin (circular rings due to interrupted mass-loss, paraboloidal bow-shock shaoes due to interaction of the AGB wind with the ISM): hence our proposed PACS observations will thus be able to distinguish between detached shells due to interrupted mass-loss and ISM interactions.
### Herschel/HIFI observations of water fountain sources
Proposal ID: OT1_rsoria01_1
Principal Investigator: Rebeca Soria Ruiz
Time: 17 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
One of the most intriguing aspects of the evolution of intermediate mass stars is how these simply spherical balls of gas can evolve resulting in the formation of PNe, which display a variety of shapes far from being isotropic. This transformation takes place after the end of the AGB, when some post-AGB flows collide with the CSEs of the former AGB star. These envelopes, which are spherical and expanding at a low velocity, are accelerated and re-shaped due to the interaction of the post-AGB flows, which are much faster and highly bipolar. Later, the star becomes much hotter, ionizing the surrounding material and forming the PN.
This wind interaction is active only during a very short times, ~ 100 yr, and to gain insight into the subject we need to study objects in which this transformation is taking place, or it has happened very recently. So far, the earliest post-AGB sources we know about are the "water fountains". These are OH/IR sources in which, contrarily to what happens in AGB stars, the H2O masers show very wide velocity ranges, wider than OH masers. VLBI observations tell us that in "water fountains" H2O masers trace very fast bipolar outflows, with kinematic ages as short as 40-100 yr, comparable to the expected duration of the post-AGB acceleration of the envelope.
Unfortunately, the main properties of water fountain nebulae are now well known, as the masers do not provide information on the density and temperature of the gas. The usual probe, low-J transitions of CO, becomes unusable in most cases, as these sources suffer from strong interstellar contamination. We can overcome these problems with Herschel/HIFI, by observing higher J-transitions of CO, where contamination is negligible, and the strong lines of H2O and OH available within the band. Here we propose to observe six water fountains in five frequency setups, to study the molecular envelope of these sources by means of the observation of several lines of these very abundant molecules in their envelopes.
### The Herschel view on supergiant High Mass X-ray Binaries: revealing the most obscured high-energy source of our Galaxy
Proposal ID: OT1_schaty_1
Principal Investigator: Sylvain Chaty
Time: 16 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Among the high-energy binary sources, a new type of sources has been recently discovered by the high-energy observatory INTEGRAL. They are constituted of intrinsically highly obscured supergiant High Mass X-ray Binaries, of which IGR J16318-4848, a compact object orbiting around a supergiant B[e] star, seems to be the archetype. These sources have been partly unveiled by means of multi-wavelength X-ray, optical, near- and mid-infrared observations. However the fundamental questions about these sources, namely their formation, their evolution, and the nature of their environment, are still unsolved. After the successful multi-wavelength observations that we have performed on these intriguing sources, we propose here to get Herschel/PACS photometric observations, in order to detect the presence and characterize the nature of absorbing material (dust and/or cold gas) enshrouding the whole binary systems. This study will allow us to get a better understanding of the formation and evolution of such rare and short-living high mass binary systems in our Galaxy.
### Measurements of the Atomic Carbon Isotope Ratio in Evolved Stars
Proposal ID: OT1_smilam_1
Principal Investigator: Stefanie Milam
Time: 16 hours priority 2
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
We propose to use Herschel-HIFI to observe the atomic carbon isotope ratios of evolved stars. The sample of circumstellar envelopes to be studied are being observed by the HIFISTARS program, where the oxygen isotope ratios will be measured via H2O. The proposed observations will allow us to determine the carbon isotope ratio in various types of stars (C-rich, O-rich, and S-type) as well as constrain chemical fractionation that may occur in the outer envelopes of these objects and/or provide insight into other nucleosythetic processes that may alter the CNO-isotopic abundances. The data in this program are complimentary and will employ the results obtained from the HIFISTARS program.
### The Homunculus: Clues to Massive Ejection from the Most Massive Stars
Proposal ID: OT1_tgull_3
Principal Investigator: Theodore Gull
Time: 24.3 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
Eta Carinae is a lynchpin between mass ejection by highly evolved massive stars and the enriched ISM. The Homunculus, a very dusty, neutral bipolar shell ejected in the 1840s, is known to contain at least 12 solar masses, based upon gas/dust=100. But this ejecta is very N-rich with C and O being 0.02 that of solar abundance. What dust formed and how much total mass was ejected? Our ultimate goal is to obtain the total ejected mass. We propose to obtain full spectral scans of the Homunculus with PACS and SPIRES and selected scans with HIFI. We will use these spectra to identify molecules and atomic species associated with this C- and O-depleted gas. While most of this depletion is due to CNO processing and conduction in stars > 60 solar masses, additional depletion is likely due to the first molecules and dust formed at high temperatures during the 1840s eruption. In line of sight we see overabundances of metals not ordinarily seen in the ISM: Sr, Sc, V. These metals have been trapped in atomic state due to limited O and C being available to form molecules. Yet dust has still formed. But what kind of dust? Through existing HST/STIS and VLT/UVES spectra combined with the proposed Herschel spectra and detailed modeling, we will gain much better insight on how molecules and dust can formed in depleted C,O conditions, and in turn provide an improved estimate of the total mass loss. Implications from this study apply to the first massive stars and the earliest dust in the Universe.
### Characterizing the Mid/Far-Infrared Excesses of Cataclysmic Variables
Proposal ID: OT1_tharriso_1
Principal Investigator: Thomas Harrison
Time: 7 hours priority 1
Category: Galactic Other
Summary:
Spitzer and IRAS observations have shown that cataclysmic variables (CVs) are sources of mid/far-infrared emission. While the excesses detected by Spitzer have been attributed to circumbinary disks (CB), as currently envisioned, such disks could not be reponsible for the IRAS detections. If due to dust, the IRAS detections imply much more extended CB disks then previously proposed, or perhaps, dust shells ejected by ancient classical novae eruptions. Alternatively, the Spitzer and IRAS detections may be due to synchrotron emission from these objects. Recent Spitzer and radio observations have now confirmed that CVs are synchrotron sources. If most CVs are synchrotron sources, this would solve the mystery of the unexpectedly large IRAS detection rate for CVs. Both CB disks and synchrotron emission can provide additional sources of angular momentum loss. Currently, there is considerable debate in the CV community over whether the commonly invoked mechanisms for momentum loss are sufficient to explain CV evolution. If most CVs have CB disks or synchrotron jets, they could provide the additional angular momentum loss required to keep CVs contact binaries. We propose to conduct a small survey spanning the major subclasses of CVs. All eight targets have mid/far-infrared excesses. Our program requires 7.0 hr of Herschel time.
### Imaging and Spectroscopy of the Infrared Shell Surrounding the Pulsar Wind Nebula G54.1+0.3
Proposal ID: OT1_ttemim_1
Principal Investigator: Tea Temim
Time: 8.9 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
We propose to obtain Herchel PACS imaging and spectroscopy of G54.1+0.3, a young pulsar wind nebula (PWN) surrounded by a shell of supernova (SN) ejecta and freshly-formed dust. The dust and gas seem to be illuminated by the expanding PWN and the members of a stellar cluster in which the SN exploded, making them observable at infrared wavelengths. Our recent Spitzer study suggests that the shell contains 0.1 solar masses of dust, possibly the largest amount observed to date, and that this dust has not yet been processed by supernova remnant (SNR) shocks. The proposed observations will allow us to 1) determine the composition, temperature, mass, and spatial distribution of pristine SN dust that has not been altered by shocks, 2) search for a colder dust component to constrain the total amount of dust in the system, and 3) measure composition and velocity of the surrounding SN ejecta that will provide information on the SN progenitor and the evolution of the PWN. A Hersche study of this unique system promises to shed light on the outstanding questions regarding the nature and quantity of dust produced in SNe.
### Far-IR Emission from Planetary Nebulae: Simultaneous Mapping and Spectral Probing of the Multi-Phased Dusty Gaseous System
Proposal ID: OT1_tueta_2
Principal Investigator: Toshiya Ueta
Time: 197.5 hours priority 1
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
We propose to undertake an ambitious Herschel large survey of planetary nebulae (PNs), mustering the full strengths of Herschel's broadband mapping, spectral mapping, and spatio-spectroscopic capabilities. Our proposed PN survey will exploit Herschel's unprecedented spatial-resolving power in the far-IR wavelengths to its fullest potential. We will perform (1) deep PACS/SPIRE broadband mapping to account for the coldest dust component of the nebulae in the target PNs and determine the spatial distribution of the dusty PN haloes, (2) exhaustive PACS/SPIRE line mapping in far-IR fine-structure and CO transition lines in two representative PNs to diagnose the energetics of the nebulae as a function of location in the nebulae, and (3) PACS/SPIRE spectral-energy-distribution spectroscopy at several positions in the target PNs to understand variations in the physical conditions as a function of location in the nebulae. This PN survey is distinguished from the existing MESS KPGT program by the extra dimension added by spectral mapping and spatio-spectroscopy that permit simultaneous probing of the gas and dust component in the target PNs. Through these investigations, we will consider the energetics of the entire gas-dust system as a function of location in the nebulae. Herschel will allow us to take this novel approach which has rarely been taken previously. The proposed Herschel survey will be conducted in collaboration with the recently-approved Chandra X-ray Observatory Large Project to furnish substantial PN data resources that would allow us - a community of PN astronomers - to tackle a multitude of unanswered issues in PN physics, from the shaping mechanisms of the nebulae to the energetics of the multi-phased gas-dust system surrounding the central white dwarf. The proposed Herschel survey and the approved Chandra survey, combined with the community assets from optical to mid-IR, will provide an extremely valuable and comprehensive compilation of PN resource that carries a significant Legacy value.
### Low-excitation atomic emission from young planetary nebulae
Proposal ID: OT1_vbujarra_4
Principal Investigator: Valentin Bujarrabal
Time: 24 hours priority 2
Category: Evolved Stars/Planetary Nebulae/Supernovae
Summary:
AGB stars evolve to form blue dwarfs in a very short time, about 1000 yr. Simultaneously, the circumstellar envelope around the AGB star, which is spherical and expands at moderate velocity, also evolves to form a planetary nebula (PN) around the dwarf, which usually shows axial symmetry and fast bipolar flows. This change is due to very strong shock interaction between the fossil AGB envelope and fast and collimated post-AGB jets.
The nature of the gas also changes: the AGB shells are molecular and cool, 50 - 500 K, while gas in evolved PNe is fully ionized and hot, about 10000 K. This change is thought to proceed progressively during the intermediate phase of protoplanetary nebula (PPN), in which an intermediate phase of low- or intermediate-excitation atomic gas is expected to develop, due to photodissociation (in a PDR) or to gas heating in the shocks. This neutral or slightly ionized atomic gas can only be observed by means of fine-structure lines of abundant atoms. ISO detected a few nebulae in such lines, but the relatively poor sensitivity of that instrument and the lack of spectral resolution prevented any deep study of this component. Herschel/HIFI can significantly improve those data, in particular yielding accurate line profiles, from which we will be able to identify the emission from the different nebular components. New observations will allow us to study the properties of low-excitation atomic gas in PPNe and, in particular, to discern the origin the molecular dissociation, in a PDR or in shocks, from analysis of the fine-structure line profiles.
We accordingly propose observations of the CII (158 microns), CI (609, 370 mic), and OI (63 mic, using PACS) lines in a sample 13 objects, mostly PPNe and young PNe, but also including a few red (super)giants and more evolved PNe for comparison.
## Galaxies / AGNs (62)
### SPIRE Photometry on Lensed Quasars
Proposal ID: OT1_abercian_1
Principal Investigator: Alicia Berciano Alba
Time: 10 hours priority 2
Category: Active galaxies/ULGs/QSOs
Summary:
Observations of different CO transitions in high-z quasars can help us to characterise the physical conditions of the star-forming gas, and improve current models of the co-evolution of star formation and SMBH growth. However, emission of the mm/submm continuum and/or CO lines with ground-based facilities has been observed only in a relatively
small number of QSOs, limiting our current knowledge of the dust and molecular gas properties of this important objects. We propose a low cost, high-return 10 hour detection experiment that will deliver SPIRE photometry in 3 bands for 103 targets with 0.45 < z < 4.8 (all currently known optical/radio selected QSOs lensed by foreground galaxies) as first step towards building candidate list for follow up studies.
### Origin of massive outer gas reservoirs in early-type galaxies
Proposal ID: OT1_acrocker_1
Principal Investigator: Alison Crocker
Time: 24 hours priority 2
Category: Nearby galaxies
Summary:
A surprising number (~50%) of field early-type galaxies (E and S0s) contain a cool interstellar medium phase detected through the 21cm hyperfine transition of neutral hydrogen. In some cases, this gas is distributed in extremely extensive outer distributions of up to a few 10^9 solar masses of HI. The origin and relation of such outer gas reservoirs to their host early-type galaxies is currently unknown. The gas may be directly accreted from the IGM, stripped during a tidal interaction, or acquired during a gas-rich merger. Alternatively, such gas may have been long associated with the early-type galaxy, not being exhausted due to a low star formation efficiency. In each of these cases the gas is expected to have a different enrichment history and thus a different present-day metallicity and dust-to-gas ratio. With Herschel PACS and SPIRE photometry, we propose to measure dust masses in the outer HI distributions of 15 nearby early-type galaxies. With interferometric HI data already in hand, we can then calculate dust-to-gas ratios and constrain the origin of such gas. The sample size and variety of HI masses, radial extents and morphologies will let us test if the dust-to-gas ratios vary among the sample in a way described best by a single accretion scenario. Additionally, the temperature derived for the dust in the outer gas will let us constrain the possible heating sources for the dust. In some sample galaxies, coincident UV emission suggests young stars are present. If heating from these young stars is important, we expect a variation of dust temperature in systems with and without UV emission.
### A definitive Herschel study of the most powerful local radio galaxy - Cygnus A
Proposal ID: OT1_aedge_4
Principal Investigator: Alastair Edge
Time: 5.9 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
Powerful radio galaxies have played a central role in our understanding of active galaxies over the past five decades. Cygnus-A, the brightest and most nearby FR-II source, has been a "Rosetta Stone" in this study. It appears to have the outward characteristics of a normal radio galaxy but it's proximity allows us to identify the more subtle properties of an obscured quasar. The energy provided by this very active galaxy is sufficient to launch the energetic jets we observe but the transport of the energy to the hotspots is poorly constrained and understood. The growing realisation that AGN directly affect their host galaxy through a direct feedback mechanism throughout the lifetime of the galaxy makes it especially important for the most nearby obscured quasar to be observed with the widest possible spectral coverage. We propose to use Herschel to reveal the heating of the central region and the energetics of the hotspots. We request observations of the atomic cooling lines [OI], [OIII] and [CII] that will allow us to compare the energetics of the ISM in Cygnus A with other local and more distant galaxies.
### Search for dust emission from circumstellar dust in Type Ia supernovae
Proposal ID: OT1_agoobar_1
Principal Investigator: Ariel Goobar
Time: 12 hours priority 1
Category: Extra-Galactic Other
Summary:
We propose a pilot program to investigate the nature of the non-standard extinction law of Type Ia supernovae through sub-mm observations near the supernova lightcurve maximum. If scattering and absorption by circumstellar dust contributes to the observed extinction, dust emission at sub-mm wavelengths is expected. Thus, we plan to target nearby reddened Type Ia supernovae around peak luminosity. A detection of sub-mm emission from the supernova location would dramatically improve our understanding of the processes behind the dimming of supernovae, with far reaching implications for their use as distance indicators in cosmology.
### Dust-Based Molecular Gas Maps of Nearby Low-Metallicity Galaxies
Proposal ID: OT1_aleroy_1
Time: 20.1 hours priority 1
Category: Nearby galaxies
Summary:
We propose deep PACS 100 and 160 micron imaging of three nearby, star-forming, low metallicity galaxies. These data will allow us to make sensitive, high-resolution estimates of dust mass. We will combine these measurements with our in-hand HI maps to measure the dust-to-gas ratio and estimate the molecular gas (H2) content in each galaxy. This is a challenging measurement that requires requires the resolution of PACS and good sensitivity, but H2 masses at low metallicity are very difficult to estimate by any other means. We will use these H2 measurements to test recent models of H2 formation in galaxies, improve the calibration of the CO-to-H2 conversion factor, and assess the efficiency of star formation from H2 at low metallicity. We will also be able to put constraints on the life cycle of dust at low metallicity from gradients in the dust-to-gas ratio. These are all open questions that can best be addressed by observing the molecular gas in low metallicity galaxies. Carrying out such an experiment outside the Local Group is necessary something that only Herschel can do.
### Probing the Interstellar Medium Conditions in High Redshift Starburst Galaxies
Proposal ID: OT1_apope_2
Principal Investigator: Alexandra Pope
Time: 21.9 hours priority 2
Category: Extra-galactic ISM
Summary:
Far-infrared and submillimeter emission lines trace the massive gas reservoirs which fuel the increased star formation seen at high redshift. While [CII] emission at 158 microns is the dominant cooling line in galaxies and directly traces the conditions in the interstellar medium, only a handful of studies have managed to detect CII at high redshift. We propose to double the number of published high redshift [CII] detections by observing 4 ultra-luminous infrared galaxies at z=1.2-2.5 with the SPIRE FTS. Our sample is unique in that it already has exquisite measurements of mid-IR spectral features and CO emission ensuring that we are observing gas-rich, starburst-dominated systems. Combining the [CII] measurements with line luminosities from CO and mid-IR spectroscopy we will complete a full diagnosis of the interstellar medium in these intensely star forming systems constraining the gas density, and the strength and source of the UV radiation field. This program is an excellent way to push the limits and showcase the capabilities of the SPIRE/FTS. We request a modest allocation of 21.7 hours (5.5 hours per source) to complete this detailed study of the astrophysical conditions in high redshift ultra-luminous infrared galaxies.
### Velocity resolved HIFI spectroscopy of water lines in actively starforming galaxies
Proposal ID: OT1_aweiss01_1
Principal Investigator: Axel Weiss
Time: 63.6 hours priority 1
Category: Nearby galaxies
Summary:
Recent Herschel spectroscopy has shown that water lines can be very prominent in the submm spectra of infra-red (IR) bright galactic nuclei. Water can efficiently be excited by the IR photons of the dust continuum and via collisions of shock-heated gas in starforming regions. In the later case H$_2$O contributes significantly to the gas cooling. So far, the relative importance of the processes driving the water excitation are largely unknown. This is mainly because the submm lines of water in extragalactic systems have only become accessible with the launch of Herschel.
Our first velocity-resolved HIFI spectroscopy of low-level water transitions in actively starforming galaxies shows that water line profiles are formed by a mix of emission and absorption features and that the line profiles strongly vary between different water transitions. This shows that a lot of information on the underlying ISM structure is imprinted on the line profiles. On the other hand this implies, that velocity resolved spectroscopy is required in order to investigate the water excitation and the underlying physical conditions of the ISM.
We here propose to observe a set of five medium and high energy water lines using HIFI in a sample of active galaxies which are representative for a wide range of nuclear environments. In conjunction with the low-level water lines form the HEXGAL GT-KP this line selection will allow us to model the water excitation in outstanding detail and to investigate the relative contribution of the water excitation channels as a function of environment, derive chemical abundances and to investigate the underlying physical parameters of the gas.
### New HErschel Multi-wavelength Extragalactic Survey of Edge-on Spirals (NHEMESES)
Proposal ID: OT1_bholwerd_1
Principal Investigator: Benne Holwerda
Time: 10.3 hours priority 2
Category: Nearby galaxies
Summary:
Edge-on spiral galaxies are a unique perspective on the vertical structure of spiral disks, both stars and the iconic dark dustlanes. The thickness of these dustlanes can now be resolved for the first time with Herschel in far-infrared and sub-mm emission.
Resolved far-infrared and sub-mm observations of edge-on spirals will impact on several current topics. First and foremost, these Herschel observations will settle whether or not there is a phase change in the vertical structure of the ISM with disk mass. Previously, a dramatic change in dustlane morphology was observed as in massive disks the dust collapses into a thin lane. If this is the case, the vertical balance between turbulence and gravity dictates the ISM structure and consequently star-formation and related phenomena (spiral arms, bars etc.). We specificaly target lower mass nearby edge-ons to complement existing Herschel observations of high-mass edge-on spirals. Secondly, the combined data-set, together with existing Spitzer observations, will drive the generation of spiral disk Spectral Energy Distribution models. These model how dust reprocesses starlight to thermal emission but the dust geometry remains the critical unknown. And thirdly, the observations will provide an accurate and unbiased census of the cold dusty structures occasionally seen extending out of the plane of the disk, when backlit by the stellar disk.
The proposed 10.4 hours of PACS and SPIRE observations of low- and intermediate-mass disks complement slated Herschel observations of massive edge-on spirals and existing Spitzer observations in the near- infrared.
### Physical conditions in disky U/LIRGs from [C II] and [O I] spectra - low-z analogs for high-z starforming galaxies
Proposal ID: OT1_bweiner_1
Principal Investigator: Benjamin Weiner
Time: 9.1 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
We propose to use Herschel/PACS spectroscopy of the [C II] 158 micron and [O I] 63 micron lines to observe a sample of 16 low-redshift infrared-luminous galaxies, at log L_IR = 11.8 to 12.3 Lsolar, that are distinguished by large size and non-merger structure. These galaxies are interesting because they have high star formation rate activity spread over a large physical area, rather than concentrated into extremely dense regions as in the nucleus of a major merger, as in most local ULIRGs. They are potentially good analogs for high-redshift IR-luminous galaxies, which appear to have far-IR spectral shapes different from local ULIRGs. [C II] is a major cooling line in photo-dissociation regions and [O I] and [C II] probe the physical conditions and UV intensity in IR-emitting regions. In a few extreme lensed high-z ULIRGs where [C II] can be measured, the high-z objects have L([C II])/L(FIR) ratios that are high, more like those of local starbursts than local ULIRGs. At z>1, much of the star formation in massive galaxies is occurring at LIRG and ULIRG levels, and U/LIRGs dominate the IR luminosity density. Understanding star forming regions in high-z IR-luminous galaxies is necessary to understand the conditions in which most of the stars in massive galaxies formed. The proposed measurements of [C II] and [O I] in this local sample of high-z analogs will test the hypothesis that redshift evolution in the IR SED shape and the [C II]/FIR ratio are due to different physical conditions in high-z IR-luminous galaxies, because of the larger physical extent of the star forming area.
### Coordinated Study of Flare Emission from Sgr A*, the Closest Supermassive Black Hole
Proposal ID: OT1_cdowell_2
Principal Investigator: C. Darren Dowell
Time: 27.5 hours priority 1
Category: Galactic Other
Summary:
Coordinated study of flare emission from Sgr A*, the closest supermassive black hole, reveals information about the hydrodynamics, energetics, and accretion behavior of matter within the innermost ten Schwarzschild radii. We propose to use the unique capability of Herschel/SPIRE and XMM in order to characterize flare emission simultaneously at many different wavelengths, the most important of which are completely unavailable from the ground. These measurements will explore the nature of emission at the peak of the spectrum of Sgr A* and will determine the transition wavelength at which the variable emission becomes optically thin. In particular, we will test the prediction that there will be time delay between X-ray flares and the peak emission at 250, 350, and 500 microns. We will take advantage of the calibration stability of Herschel resulting from the L2 placement to detect Sgr A* in SPIRE difference images. The proposed Herschel and XMM observations form the cornerstone of a multi-wavelength campaign that includes observations in near-IR and radio wavelengths. The cross correlation of flare emission at multiple wavelengths will have far-reaching implications for testing the emission mechanism of Sgr A* and for understanding the processes of accretion onto and outflow from the closest supermassive black hole. Lastly, a long flux monitoring of Sgr A* with Herschel over long and nearly continuous baselines will characterize the fraction of time that Sgr A* is active in submm wavelengths and will provide a legacy to unravel the key properties of the best example of a low-luminosity massive black hole.
### A Complete Herschel-Spitzer Legacy Survey of the low-redshift ULIRG Population
Proposal ID: OT1_dfarrah_1
Principal Investigator: Duncan Farrah
Time: 250 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
We propose to establish a large, complete Herschel spectroscopic atlas of the low-redshift ULIRG population, via PACS/SPIRE spectroscopy of 45 local ULIRGs. Our observations will combine with existing Herschel data to complete a purely flux limited sample of 52 ULIRGs at z<0.2. This sample comprises the most well-studied low-redshift ULIRGs in existence; they all have mid-IR spectra from Spitzer in both low and high resolution mode, many have HST imaging, and about half have X-ray observations. We will measure the physical & chemical properties of the starbursts and AGN in unprecedented detail, construct new mid/far-IR diagnostic diagrams, and determine robust calibrations for key observables of ULIRGs in the distant Universe. Our program will form a cornerstone of the Herschel spectroscopic legacy, providing (1) a comprehensive database for community exploitation, (2) a firm anchor for studies of ULIRGs in the high redshift Universe, and (3) one of the most important input catalogues for ALMA. As our intention is to create an atlas for the community, we waive all proprietary rights.
### Characterizing Molecular Clouds at Low Metallicity
Proposal ID: OT1_dhunter_3
Principal Investigator: Deidre Hunter
Time: 53.7 hours priority 1
Category: Nearby galaxies
Summary:
Molecular gas is difficult to detect from traditional millimeter CO transitions in dwarf galaxies below a certain metallicity. Yet, there is evidence for lots of molecular H_2 in these galaxies. Fortunately, Photo-dissociation Regions are a better tracer of the molecular material in low metallicity systems. In metal-poor galaxies, PDRs dominate the molecular core where CO is found, and in the current paradigm the PDR grows and the core shrinks as metallicity decreases. Thus, we expect critical differences in the molecular clouds of dwarfs compared to spirals, with the differences becoming more extreme with lower metallicity. Yet, understanding these differences and their consequences to star formation is essential to understanding the processes that drive star formation at low metallicities. Therefore, we propose to observe the PDRs in 5 regions in 5 typical metal-poor dwarf galaxies spanning a range in oxygen abundance. We will use these observations to characterize the molecular gas, examine the correspondence between the molecular clouds and the atomic gas and star formation characteristics, and determine the characteristics of the atomic ISM that are necessary for the formation of these dense molecular clouds. We will also test the molecular cloud structure paradigm as a function of metallicity.
### Herschel-GOALS: PACS and SPIRE Imaging of a Complete Sample of Local LIRGs
Proposal ID: OT1_dsanders_1
Principal Investigator: David Sanders
Time: 84.9 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
We propose to obtain high-quality, PACS (70, 100, 160 micron) and SPIRE (250, 360, 520 micron) images of a complete sample of 201 local (z<0.08) luminous infrared galaxies (LIRGs) from the Great Observatories All-sky LIRG Survey (GOALS). These systems are primarily interacting or merging disk galaxies undergoing enhanced star formation and AGN activity, and represent an important evolutionary phase in the lives of massive galaxies. Herschel will measure a critical wavelength range of the FIR/submm spectral energy distribution (SED), which will enable accurate determinations of bolometric luminosities, dust temperatures, IR surface brightness and star-formation rates within the GOALS targets on spatial scales of 2-5kpc. The high-resolution PACS data will better resolve binary nuclear regions, disks, and tidal bridges and tails of colliding galaxies at different interaction stages. SPIRE will probe the hidden cold component of the ISM and will constrain the total amount of gas and dust available to fuel the starburst and AGN activity. Studies of the FIR-submm SEDs will allow us to derive the relative amounts of warm and cold dust along the merger sequence. The proximity, size, and completeness of the GOALS sample makes it well suited for studying the full range of infrared properties for LIRGs as a function of dynamical age, infrared luminosity, spectral type and merger phase. Finally, this Herschel program will provide crucial statistical results for LIRGs and ULIRGs that will enable researchers to understand high- redshift infrared galaxies in the context of local, well-resolved objects.
### Comparing [CII] 158 micron Luminosities to Spectral Properties of Luminous Starburst Galaxies and AGN
Proposal ID: OT1_dweedman_1
Principal Investigator: Daniel Weedman
Time: 20.2 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
Herschel PACS spectroscopy of the [CII] emission line at 158 microns is proposed for a carefully selected sample of 123 sources that already have complete low and high resolution mid-infrared spectra between 5 microns and 35 microns from the Spitzer Infrared Spectrograph, and which also have spectral energy distributions (SEDs) from IRAS and Akari photometry. [CII] 158 um is the strongest far-infrared emission line and therefore crucial to compare with other features in luminous, dusty galaxies. Sources have 0.004 < z < 0.34 and 43.0 < log L(IR) < 46.8 (erg per sec) and cover the full range of starburst galaxy and AGN classifications. Obtaining these [CII] line fluxes with PACS will allow: 1. determining how precisely [CII] luminosity measures star formation rate by comparing to PAH features and emission lines that arise in starburst galaxies; 2. determining how [CII] luminosity and equivalent width changes with starburst/AGN fraction, by comparing with strength and equivalent width of PAH and [NeII] emission arising from starbursts, and with strength of high ionization lines [NeV] and [OIV] and silicate absorption or emission arising from AGN; 3. determining how [CII] luminosity and equivalent width changes with dust temperature and bolometric luminosity, as derived from spectral energy distributions, and whether this depends on the starburst/AGN fraction. These determinations will allow interpretation of high redshift sources for which the only available diagnostics are the luminosity and equivalent width of the [CII] line and the far-infrared rest-frame SED. The total observing program requires 20.2 hours of Herschel observing time.
### Constraining the nature of high redshift infrared-faint radio sources
Proposal ID: OT1_emiddelb_1
Principal Investigator: Enno Middelberg
Time: 6.4 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
One of the most puzzling discoveries of the Australia Telescope Large Area Survey (ATLAS) is the population of infrared-faint radio sources. While relatively bright at 1.4 and 2.3 GHz (10-20 mJy) these sources are neither seen on optical (r=25mag) nor on near- and mid-infrared (3.6-70 micron) Spitzer maps. Existing multiwavelength data, e.g. from SWIRE, suggests that these sources are high-redshift (2<z<5) radio-loud AGN, suffering from heavy obscuration of their optical/NIR emission. Therefore, powerful FIR re-emission is expected, but the FIR-submm maps obtained with Herschel (in the HERMES key project) are too shallow (50 mJy at 160 micron, 30 mJy at 250 micron) to detect these sources. If they are obscured high-z analogues of local templates like 3C48 the predicted 100-500 micron flux density is about 20 mJy, well detectable with Herschel. Therefore, we propose deep PACS 100+160 micron and SPIRE 250+350+500 micron maps of six representative sources, in order to determine the nature of these infrared-faint radio sources. This will provide crucial new insights on those radio-loud high redshift AGN, which cover a lower flux/luminosity range and are therefore more characteristic than the few extremely luminous high-z radio galaxies studied so far.
### Measuring the physical properties of submillimeter galaxies around high redshift QSOs
Proposal ID: OT1_fcarrera_1
Principal Investigator: F.J. Carrera
Time: 2.9 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
We have detected strong overdensities of submillimeter galaxies (SMGs) around a sample of z~2 QSOs using SCUBA 450 and 850 micron maps. In at least one case we have proved that most of those objects are indeed at the same redshift as the QSO, and hence related to it. If the other SMGs are also related to their entral QSOs they would represent high density peaks in the density of the early Universe, where present-day massive galaxies are thought to form. However, our understanding of the origin of such emission (expected to be due to thermal emission by dust heated by star formation) is very sketchy, since we only have one or, at best, two measurements of their far infra-red/submm Spectral Energy Distribution.
Small scan maps with PACS and SPIRE on-board Herschel would provide crucial data around the expected peak of the emission for those SMGs, allowing an unambiguous determination of its spectral shape and strength, and hence proving its origin and providing accurate estimates of the physical properties of the emitting dust. This in turn can be used to quantify the star formation rates and dust masses, to understand the evolutionary status of these objects.
Additionally, the high-sensitivity Herschel maps would probe the source counts around the QSOs in hitherto unexplored bands to unprecedented depth, providing vital clues to really understand the role of these objects in the formation of galaxies in these early peaks in the density of the Universe.
### Water and CO: Signatures of Microturbulent Shocks in NGC 891
Proposal ID: OT1_gstacey_4
Principal Investigator: Gordon Stacey
Time: 22.1 hours priority 1
Category: Nearby galaxies
Summary:
We propose to detect and map rotational line emission from water and CO in the edge-on spiral galaxy, NGC 891. Both water and CO rotational lines are important coolants for low velocity C-shocks resulting from micro-turbulence in molecular clouds. The water lines are of particular interest, as they are definitive shock tracers on galactic scales. Micro-turbulent shocks are an important process through which molecular clouds dispel their turbulent kinetic energy enabling them to collapse and to form stars. NGC 891 is the ideal source for detecting shock tracers from the more quiescent ISM within a normal spiral galaxy: it is presented to us edge-on so that column densities along the line of sight are quite large, and it is nearby so that the edge-on geometry still nearly fills the Herschel spectrometer beams. The combination of high columns, and good beam match enables the detection of particularly weak lines. Our search is motivated by our recent study of NGC 891 in its H2 rotational line and [OI], [CII], and [NII] fine-structure line emission that provides strong evidence for micro-turbulent shock excitation of the S(2) and S(1) rotational lines. These lines are bright, and within C-shock models, several water lines are predicted to be nearly equally bright, and readily detectable with Herschel/PACS and HIFI, and the rotational ladder of CO is detectable with SPIRE. The proposed Herschel observations of water CO will provide the first definitive indicators of the micro-turbulent shocks that along with H2 line emission are the dominant coolants for molecular cloud interiors. Herschel is the only facility that can observe these water lines that are totally obscurred by the Earth's atmosphere even at aircraft altitudes.
### Herschel study of black hole and galaxy evolution: The z<0.3 QUEST AGN sample.
Proposal ID: OT1_hnetzer_1
Principal Investigator: Hagai Netzer
Time: 15.6 hours priority 2
Category: Active galaxies/ULGs/QSOs
Summary:
We propose 15.6 hours of Herschel time to secure high quality data,over the entire 70-500 micron range, for a group of 27 local, luminous active galactic nuclei (the QUEST AGN sample). The sources represent well the optically selected PG-QSO sample with redshifts up to z=0.3, and have been investigated, in great detail, in almost all other wavelength bands. The new far infrared (FIR) data set will be ideal to study various fundamental questions related to the connection and co-evolution of AGN and their host galaxies. Our previous Spitzer/IRS work on the sample has already revealed a clear relationship between the total AGN luminosity and the star formation rate (SFR) in their hosts. However, the previously undetected FIR sources may be situated in red-and-dead hosts and the Herschel observations can find these objects and allow a direct comparison of their AGN properties, like black hole (BH) mass and accretion rate, with those of the sources with high SFR. The observations will also provide unique information about the "intrinsic infrared AGN spectrum" with consequences to dust properties and distribution in such objects. Our sample is a needed ingredient in any Herschel-based studies that combine FIR-selected (IRAS, Spitzer, Herschel) and optically selected samples with their different biases. Its later comparison with similar high redshift observations will provide invaluable information about the cosmological evolution of AGN and star forming galaxies.
### Black hole growth and star formation in the early universe: the z=4.8 sample
Proposal ID: OT1_hnetzer_2
Principal Investigator: Hagai Netzer
Time: 13 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
We propose to secure Herschel PACS and SPIRE observations for a unique sample of 44 z=4.8 active galactic nuclei (AGNs). This is a genuine optically-selected flux limited sample that was observed by us from the ground thus providing reliable black hole (BH) and accretion rate estimates based on the properties of the strong MgII 2800A line. Reliable BH mass estimates at z>2 can only be obtained in narrow redshift bands at around z=2.3, z=3.3, z=4.8 and z=6.5. Our z=4.8 sample is thus a corner stone for answering any question related to galaxy and BH evolution, in particular the co-evolution (if any) of BHs and star formation (SF) in the early universe. The Herschel observations will provide invaluable information about the SF rate (SFR) in the host galaxies of the z=4.8 AGNs which, when combined with observations in the other redshift bands will trace the growth of the most massive BHs and the stellar mass in their hosts. SPIRE observations will provide SFRs (or upper limits on the SFR) in all sources. PACS observations of the more luminous sources in the sample will provide a. priors for the SPIRE observations that will allow us to go below the confusion limits and b. unique information about the 17-40 micron (rest) emission by warm (200K) dust close to the centers of these sources.
### Ram pressure-induced shocks in stripped Virgo spirals
Proposal ID: OT1_iwong_2
Principal Investigator: Ivy Wong
Time: 22 hours priority 2
Category: Nearby galaxies
Summary:
We propose to investigate the presence of ram pressure-induced shocks in three Virgo cluster galaxies with clear evidence for on-going ram pressure stripping, from a wealth of radio continuum, optical, infrared, and HI data. To achieve our aims, we will perform PACS spectroscopy to measure the [OI] and [CII] emission line strengths of three outer-disk regions located along the leading edge of interaction between the hot intracluster medium (ICM) and the cooler galaxy interstellar medium (ISM). The ionization state of the ISM gas within the leading edges will be revealed by the ratios of these two emission lines since they are the dominant coolants in the neutral and ionised ISM at low temperatures. Previous Spitzer IRS observations hinted at the presence of shock-excited molecular Hydrogen. Hence, these proposed PACS spectroscopy observations will provide independent confirmation of ram pressure-induced shocks in the cold ISM along the leading edges of these ram pressure-stripped galaxies. Evidence for shock excitation throughout the ISM may also explain the enhanced global radio-toratios observed in galaxies which are experiencing strong ram pressure.
### Do Ultraluminous X-Ray Sources Really Require Intermediate Mass Black Holes?
Proposal ID: OT1_jbregman_1
Principal Investigator: Joel Bregman
Time: 11.4 hours priority 1
Category: Extra-Galactic Other
Summary:
Ultraluminous X-ray sources are non-nuclear sources in normal disk galaxies that are second only to AGNs in point-source luminosity. Their X-ray luminosities exceed the Eddington limit for stellar mass black holes (15 Msun), suggesting the need for intermediate mass black holes. This inference depends on the X-ray emission being isotropic, an assumption that we test here. X-ray spectral studies show that much of the soft X-ray emission is absorbed by gas and dust, which will be reemitted isotropically in the far-infrared. The ratio of the absorbed X-ray luminosity to the FIR luminosity is a direct measure of the anisotropy of the X-ray emission. Our previous study with Spitzer, which focused on PAH emission, suggests that the X-ray emission is highly anisotropic. However, if the X-rays destroyed the PAHs, we should focus on the longer wavelength emission, where MIPS observations indicate weak detections. The limitations of the MIPS observations were the poor point spread function and short exposure time, which will be improved upon by the proposed PACS 70 um observations of three highly luminous and nearby ULXs. These data will determine whether ULXs are sub-Eddington or super-Eddington emitters.
### NGC 1266: Probing an extraordinary phase of galaxy evolution with Herschel
Proposal ID: OT1_jglenn_1
Principal Investigator: Jason Glenn
Time: 6.3 hours priority 1
Category: Nearby galaxies
Summary:
Two important, coupled questions in galaxy evolution are: how did gas-rich galaxies deplete their interstellar media to become gas poor and how do feedback mechanisms from star formation and active galactic nuclei (AGN) regulate star formation and supermassive black hole growth? Thus, observing galaxies with substantial gas content, nuclear activity, and outflows can make a significant impact on our understanding of galaxy evolution. Recently, observations of an early-type galaxy, NGC 1266, an S0 LINER, revealed a powerful molecular outflow associated with a compact (300-pc radius) and massive reservoir (of order 10^9 solar masses) of molecular gas. The outflow velocity exceeds the galaxy escape velocity, with an estimated flow of 40 solar masses per year. At this rate, the galaxy will deplete its molecular gas within 30 Myrs. There is evidence for an AGN, but the star-formation activity is weak given the gas surface density and no companion galaxy is visible. These unusual characteristics make NGC 1266 an excellent candidate for detailed study of the molecular gas with Herschel to help characterize gas depletion and feedback mechanisms in galaxies. With HIFI and the SPIRE FTS, the CO spectral lines will be measured, from J = 5 4 to J = 13 - 12, which, combined with detailed models of the line emission, will yield precisely the temperature, density, optical depth, and mass of the molecular gas in the core and outflow. High signal-to-noise line detections and good velocity resolution, provided by HIFI, will enable the core line emission to be robustly separated from the outflow line emission, and to study the dynamics of the outflow. With the SPIRE-FTS, a full low resolution spectral view from 4501500 GHz will be obtained to detect tracers of dense gas, such as HCN, HCO+, and HNC. The dense fraction of the gas can be assessed and the dust continuum emission can be used to infer an independent measure of molecular gas mass. Herschel is the only facility capable of making these observations.
### A Population of Dusty B Stars in the SMC: The First Extragalactic Debris Disks?
Proposal ID: OT1_jsimon01_1
Principal Investigator: Joshua Simon
Time: 9 hours priority 1
Category: Local Group galaxies
Summary:
Using data from the Spitzer Survey of the SMC, we have discovered a population of 120 main sequence B stars with large 24 micron excesses. Optical spectroscopy and the IRAC SEDs demonstrate that they are not ordinary YSOs or Be stars. We suggest instead that these objects may be debris disks around massive main sequence stars. Confirmation of this hypothesis would provide one of the only ways to study the process of planet formation in a low-metallicity external galaxy. We have measured the mid-IR SED of the dust emission with IRS spectroscopy and determined that both cold and warm dust is present. We now propose PACS photometry at 70 microns to unambiguously separate the dust into its warm (and therefore circumstellar) and cold (possibly interstellar) components. These data will enable us to determine how much of the dust is warm and better constrain the temperature distribution; any targets with substantial amounts of warm dust are almost certainly debris disks. If the B stars do indeed host debris disks, they provide perhaps the only plausible method for constraining planet formation in an external galaxy for the foreseeable future.
### Beyond the Peak: Resolved Far-Infrared Spectral Mapping of Nearby Galaxies with SPIRE/FTS
Proposal ID: OT1_jsmith01_1
Principal Investigator: J.D. Smith
Time: 149.4 hours priority 1
Category: Nearby galaxies
Summary:
We propose a spatially-resolved far-infrared spectroscopic survey of a sample of 23 nuclear and extranuclear regions within 22 nearby galaxies, selected to represent the broadest range of key physical properties, including luminosity, gas and stellar mass, star-formation density, and infrared activity. Combined with our wealth of ancillary imaging and spatially resolved spectroscopy from the heritage of SINGS/KINGFISH and related surveys (ultraviolet, optical, infrared, low-J CO, and radio), the proposed SPIRE/FTS dataset will provide key insights into the processes that shape the interstellar medium and govern star formation. Detection of the continuum emission from large grains over 200-650 microns will place new constraints on the long-wavelength behavior of dust emissivity. The richness of the emission line spectrum in this wavelength regime will allow us to quantify the excitation conditions of CO over a wide range of environments, and to characterize the physical properties of warm and dense gas within galaxies on kiloparsec scales, interpreting these properties using models of photo- and X-ray-dissociated gas, and comparing directly with resolved tracers of star formation, heating, and AGN activity. With capabilities unmatched by existing or planned ground- or space-based facilities, SPIRE/FTS mapping of a well-studied sample of nearby galaxies will serve as a crucial, unique, and lasting foundation for interpreting ALMA observations of galaxies at high redshift.
### A benchmark study of Active Galactic Nuclei
Proposal ID: OT1_jstevens_1
Principal Investigator: Jason Stevens
Time: 55.1 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
We propose Herschel observations of a sample of 176 AGN selected over a narrow redshift range (0.9<z<1.1) but spanning 5 magnitudes in optical luminosity. This selection allows us to decouple luminosity dependent effects from evolutionary effects in a sample selected close to the peak of AGN activity. Combined with our existing multiwavelength dataset (Spitzer, XMM-Newton, SWIFT, UKIRT...) the Herschel observations will provide a benchmark for all future high-redshift AGN studies. We have three primary science goals: (1) to determine the evolutionary status of the AGN by measuring their stellar masses, black-hole masses and star-formation rates, (2) to determine how the spectral energy distributions of the AGN vary as a function of luminosity, and (3) to determine the evolutionary status of the galaxy clusters' known to be forming around the AGN. The aims of this proposal can only be achieved with pointed observations made with the Herschel Space Observatory.
### A Herschel Survey of [OI]63um in 1<z<2 Submillimetre Galaxies in the ECDFS: A Bridge to ALMA
Proposal ID: OT1_kcoppin_1
Principal Investigator: Kristen Coppin
Time: 26.3 hours priority 1
Category: Extra-galactic ISM
Summary:
Luminous obscured galaxies likely dominate the total bolometric emission from star-formation at the early epochs of z~2-3, and are most efficiently identified through their (sub)millimetre emission and are so-called submillimetre galaxies (SMGs). The intense starbursts in SMGs are fuelled by their large observed H2 gas reservoirs, as traced by CO interferometric surveys, although the details of how their immense luminosities (L_fir>5x10^12 Lsun) and star-formation rates (~100-1000 Msun/yr) are powered are not well understood: Are SMGs just scaled up ULIRGs with star-formation occurring in a highly-obscured nuclear region (with perhaps some contribution from an AGN)? Or does the star-formation occur in a more extended, cooler component, such as in "normal" star-forming galaxies. One route to tackling this question is to construct a data set of the brightest fine-structure ISM emission lines ([CII] and [OI]) in a well-defined sample of SMGs, which with ancillary CO data, will allow us to study the physics of the ISM and its interplay with the heating source. Similar benchmark data sets are being compiled by several Herschel programs for local LIRGs and ULIRGs, which will act as a link to help interpret the high-redshift SMG observations. Here we propose a timely and systematic study with the PACS spectrometer of [OI]63um in a flux-limited sample of SMGs with secure spectroscopic redshifts between 0.7<z<2 in the ECDFS - the premier cosmological survey field for ALMA due to its southern declination and wealth of existing ancillary datasets. The combination of these Herschel data ([OI]) and future ALMA data ([CII] and CO) with state-of-the art PDR modelling will reveal new insights into the typical physical conditions of the ISM in the most active high-z star-forming population of galaxies, including the average gas temperature, density, abundance, and radiation field strength integrated over the galaxy.
### Tidal Tales of Dark Gas: Searching for [CII] in CO-Deficient Star Forming Tidal Tails
Proposal ID: OT1_kknierma_1
Principal Investigator: Karen Knierman
Time: 9.4 hours priority 1
Category: Nearby galaxies
Summary:
How is star formation in tidal debris affected by gas properties? To probe the molecular gas properties of 3 tidal tail regions, we propose to use the PACS spectrometer on Herschel to observe the [CII] 158 micron line. Two particular tidal tail regions of interest are Clump II in the M81 group and the western tail of NGC 2782. These two regions are HI-rich and have young blue stars or star clusters detected in optical broadband and narrowband H-alpha imaging; however, observations of CO 1-0 show non-detections down to low limits. In contrast to these two regions, the base of the eastern tail of NGC 2782 is rich in HI and CO and has young star clusters. Although the non-detection of CO suggests that there is no molecular gas in Clump II and NGC 2782W, we expect the molecular gas to have a higher fraction of "dark gas" or mostly unobservable molecular hydrogen and C+. One way to observe this "dark gas" is to use the far infrared fine structure line of [CII] at 158 microns. Using these [CII] observations and previous data in optical, near-infrared, submillimeter, and radio, we will compare the measurements of gas and young stars in Clump II and NGC 2782W to those in NGC 2782E to examine the dependence of star formation in tidal tail regions on gas properties.
### ISM Heating and Cooling in Massive Galaxies: The Andromeda Galaxy as Fundamental Calibrator
Proposal ID: OT1_ksandstr_1
Principal Investigator: Karin Sandstrom
Time: 47.1 hours priority 1
Category: Local Group galaxies
Summary:
M31, the nearest massive galaxy, affords a unique opportunity to draw up the energy balance of the star-formation (SF) process on the spatial scales (<50 pc) of individual SF regions and of the presumed SF energy deposition. For the heating terms', UV to near-IR data from the Pan-chromatic Hubble Andromeda Treasury (PHAT) provide a direct census of all young stars in M31; for the cooling terms', a rich set of existing multi-wavelength data (far-UV to HI) provide many of the cooling diagnostics for the gas and dust. Here we propose to obtain the crucial missing link in the overall ISM energy budget by mapping the dominant, and hence indispensable, cooling lines of the neutral medium, [CII] and [OI].n Specifically, we propose PACS [CII] and [OI] line mapping of several selected (700pc x 700pc) regions in M 31 with ongoing SF, complemented by [N II] observations. These data will enable a foundational study of the energy budget and feed-back of star formation. The data will also provide a stringent calibration of the [CII] line as a local star-formation indicator. Finally, the data set provides the opportunity to understand the sub-grid physics that is needed both for galaxy formation simulations and for interpreting the enormous wealth of gas and dust diagnostic data in more distant galaxies.
### Balancing the Energy Budget in LIRGs: A PACS Spectroscopic Survey of Luminous Infrared Galaxies in GOALS
Proposal ID: OT1_larmus_1
Principal Investigator: Lee Armus
Time: 154 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
Luminous Infrared Galaxies (LIRGs; having LIR > 10^11 Lsun), emit a significant fraction of their bolometric luminosity in the far-infrared and are a mixture of single galaxies, interacting systems and advanced mergers, exhibiting enhanced star formation rates and a higher fraction of Active Galactic Nuclei (AGN) compared to less luminous galaxies. With the Great Observatories All-sky LIRG Survey (GOALS), we are measuring the properties of a large, complete sample of 202 low-redshift LIRGs across the electromagnetic spectrum using Spitzer, HST, Chandra, GALEX and a number of ground-based observatories. Here, we propose to measure the [CII] 157.7, [OI] 63.2 and [OIII] 88 micron far-infrared emission lines and the OH 79 micron absorption feature in the GOALS sample with the PACS on the Herschel Space Observatory. We will target 154 LIRGs in [CII], [OI], and OH and 66 LIRGs in [OIII] for a total requested time of 166.9 hrs. The PACS data will allow us to penetrate the dust and measure the spatial distribution, dynamics and overall energy budgets in a large sample of LIRGs at low redshift for the first time. In addition to providing a measure of the physical conditions in the warm, neutral and ionized interstellar medium (ISM) in LIRGs, these data will allow us to establish a precise, quantitative FIR-based measure of the star formation rate that can be used across a wide range of galactic luminosities, even in the presence of powerful AGN. GOALS, with its rich ancillary dataset that covers X-ray through millimeter wavelengths, provides the perfect sample for this study. Our proposed observations will greatly extend the work started with ISO, and lay the foundation for high-redshift galactic studies with future facilities (e.g., ALMA) that will target the FIR and sub-mm spectral regions over the next decade.
### Completing the PACS coverage of the Herschel Reference Survey
Proposal ID: OT1_lcortese_1
Principal Investigator: Luca Cortese
Time: 50.8 hours priority 2
Category: Nearby galaxies
Summary:
The Herschel Reference Survey (HRS) is a Herschel Key Program focused on the study of the interplay between dust and star formation in the local universe. The HRS represents the only volume- and magnitude-limited Herschel survey of resolved nearby galaxies, spanning the whole range of morphological types (ellipticals to late-type spirals) and environments (from the field to the center of the Virgo Cluster).
Here we propose to use Herschel to acquire PACS 100 and 160 micron maps for 235 HRS galaxies. This will complete the coverage of the HRS in the spectral range 100-500 microns, currently biased towards early-type, cluster galaxies. These data are essential to characterize the far-infrared and sub-millimetre dust spectral energy distribution (SED) and to investigate how it varies with internal properties and environment. With complete PACS coverage, the HRS will be the ideal sample for statistical studies in the FIR/submm regime at z~0 and the reference for investigations at cosmological distances. In particular, we plan to combine the Herschel observations with UV, HI, CO, optical and near-infrared data already available to investigate the interplay between the interstellar radiation field and dust, to study the effects of the environment on dust content and star formation activity, to carry out the first complete morphological study of local galaxies in the far-infrared and to provide the community with the largest catalogue of UV-to-radio continuum integrated and resolved (at a kpc scale) SED. Thanks to its selection and multi-wavelength coverage, the HRS will thus represent a legacy for galaxy studies for many decades to come.
### Measuring the ISM Content of a Large Volume Limited Sample of Nearby Quasars
Proposal ID: OT1_lho_1
Principal Investigator: Luis Ho
Time: 43.2 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
The coevolution of central black holes (BH) and their host galaxies driven by starbursts and the feedback of AGN are major elements of recent galaxy evolution models. Here we propose to investigate these processes in a volume limited sample of PG QSOs, by examining if and how their ISM properties reflect the evolutionary stages of the host galaxy, and the mass of the central black holes. PG QSOs are ideal for such a study because there are complete and uniform data on their BH masses, X-ray to MIR SEDs, NIR and MIR spectral characteristics as well as HST imaging. As such their accretion rates are well known. Here, we request 43.2 hours of PACS and SPIRE observations to measure the full FIR SEDs for a complete sample of 87 PG-QSOs. These data will provide unique sampling of the ISM content of the hosts with measurements of the dust masses, luminosities and temperatures. For objects at the mean redshift of z = 0.2, the proposed PACS photometry will be used to constrain the mass of hot (~60 K) and cold (~25K) dust down to 3e5 and 3e7 Solar Masses respectively, that is total ISM masses similar or less than the Milky Way. As such the proposed data will provide extremely impressive measurements of (1) the ISM masses and luminosities present in the PG-QSO hosts and (2) the relative amounts of gas in high activity (hot dust -- star-formation or AGN) versus low radiation field environments. These data will provide the fundamental dataset for studies of the IR radiation from optical QSOs and understanding the host galaxy properties. The goals of this proposal mesh well with one of Herschel's main mission statements: "Unveiling hidden details of star and galaxy formation and evolution".
### The Interstellar Medium, Star Formation and Galaxy Evolution in Early-Type Galaxies
Proposal ID: OT1_lyoung_1
Principal Investigator: Lisa Young
Time: 60.7 hours priority 1
Category: Low-z galaxies
Summary:
We propose spectroscopic observations of the primary ISM cooling lines and the high-J CO ladder in a well-defined sample of nearby elliptical and lenticular galaxies. FIR line and line/continuum ratios will be used in conjunction with PDR models to constrain the physical conditions (gas density and strength of UV radiation field) in the ISM of these early-type galaxies. Similar work has been done extensively for spiral galaxies and (U)LIRGS but has only sporadically been done for quiescent ellipticals and lenticulars. We already have a broad suite of ancillary data for our targets, including HI and CO maps, high density molecular tracers, maps of the stellar populations (ages and metallicities) and optical emission lines. Our targets make an important bridge between normal star-forming spirals and cooling flow cluster galaxies, as they have some properties in common with both other types. Thus, this project is essential for placing other Herschel approved projects into the broader context of the interactions between gas and stars across the entire Hubble sequence.
### The Impact of Quasars on their Host Galaxies: Gas Conditions and Star Formation in the Central Kiloparsec
Time: 43.7 hours priority 2
Category: Active galaxies/ULGs/QSOs
Summary:
We propose to study the impact of powerful quasars on the star-forming gas in their host galaxies' central kiloparsec with a 44-hour program using the PACS and SPIRE spectrometers. We are targeting four intrinsically luminous and gravitationally-lensed AGN systems in the z~2-4 era which show evidence of obscured star formation in their hosts. We will measure the five bright far-IR fine-structure transitions: [SiII] 35, [OI] 63, [OIII] 52 & 88, and [CII] 158 which are the dominant interstellar gas coolants in galaxies. We will combine the Herschel line fluxes with Z-Spec measurements of the peak of the CO spectrum to provide a complete census of the atomic and molecular gas mass and cooling in the central kpc of these systems.
Our datasets will allow us to perform two key experiments: 1) What heats the gas in the central kpc? When compared with one another and the dust continuum, the line measurements distinguish between UV-photon heating in photo-dissociation regions (PDRs) and bulk heating due to X-rays and/or cosmic rays. Relative to the PDRs, the bulk heating sources are very efficient at heating the gas and produce strong line-to-continuum ratios as well as an enhanced [SiII] / [CII] ratio. If X-rays or cosmic rays are really an important heating source, we will see unusually strong [SiII] and [OI] in these systems.
2) Is the stellar mass function biased toward high masses in these systems? It has been proposed that bulk heating mechanisms are likely to impact the stellar IMF, boosting the characteristic mass by as much as an order of magnitude relative to the Galaxy. Our measurements of the [OIII] transitions, when compared with the far-IR continuum or [CII] which trace total star formation provide a measure of the fraction of very massive stars in the stellar IMF. Similarly, comparison of the [OIII intensities and lower-ionization species (including upper limits) probe the stellar effective temperature through comparison with nebular models.
### Death by Debris: Testing a new picture of Star Formation Quenching in Compact Groups
Proposal ID: OT1_mcluver_2
Principal Investigator: Michelle Cluver
Time: 80.6 hours priority 2
Category: Nearby galaxies
Summary:
Recent studies show that compact groups appear to follow an evolutionary sequence, linked to gas depletion, caused by interactions in the dense environment. Spitzer photometry of Hickson Compact Groups show a distinctive gap in IRAC colour-colour space, suggesting rapid evolution from dusty to dust-free systems which seems to correlate with HI-depletion in the galaxies, but the mechanism responsible is poorly understood.
Originally ram-pressure stripping, by analogy with clusters, was thought to be responsible, but the HI depletion is uncorrelated with the presence of hot X-ray gas. Based on our recent Spitzer spectroscopy of a sample of HCGs, we propose a new hypothesis that connects the colour evolution to the HI-depletion seen in the group galaxies. In this scenario, galaxies collide with previously stripped tidal debris, that either heats the disk ISM or strips it, thus shutting off star formation and accelerating the transition from dusty, gas-rich disks to gas-poor, dust-free systems. PACS deep [OI]63 and CII[158] maps allow us to look for smooth bow shock or clumpy shock signatures to discern between heating and stripping of the disk gas. SPIRE cold dust imaging will allow us to search for additional evidence of disk disruption and truncation. This project requires 80.6 hours of observing time.
### The Herschel Legacy of powerful 3C radio galaxies and quasars at z<1
Proposal ID: OT1_mhaas_2
Principal Investigator: Martin Haas
Time: 20.5 hours priority 2
Category: Active galaxies/ULGs/QSOs
Summary:
We propose Herschel observations of a complete sample of 3C radio-galaxies and quasars at redshift z<1. For all sources Spitzer mid-IR spectra are available. The aim is to quantify the orientation-dependence of AGN radiation (AGN unification), to investigate the interplay between accretion onto the central black-hole and star-formation in the hosts, and to understand the evolution of the black-hole/stellar-bulge relation. The low-frequency radio-selection provides us with powerful and massive active galaxies free from any orientation/obscuration bias, a requirement for testing AGN unification. The properties of the 3C sources are well known throughout the electromagnetic spectrum, except in the far-IR/sub-mm, where most of them were hitherto outside the capability of space missions to reach reliable measurements. We propose PACS 70-160 micron photometry of 72 sources supplemented by SPIRE 250-500 micron photometry of 11 sufficiently bright sources, in order to measure their detailed spectral energy distributions between available Spitzer and SCUBA/MAMBO data. Depending on redshift of the sources and predicted flux, the filter choice is optimised to provide best rest-frame FIR coverage. The rest-frame FIR emission serves as an isotropic calorimeter and the MIR/FIR luminosity ratio is determined by the relative strength of the AGN and star-forming contributions combined with dust obscuration. These observations will return crucial new information on the energy processes in powerful AGN and their hosts at z<1, providing an essential anchor for studies of galaxy and AGN evolution, in particular for a consistent comparison with Herschel observations of several (radio-loud) AGN samples at cosmic epochs z>1.
### GRB Afterglow Photometry with Herschel Infrared Cameras
Proposal ID: OT1_mhuang01_1
Principal Investigator: Maohai Huang
Time: 23.6 hours priority 2
Category: Extra-Galactic Other
Summary:
GRB Afterglow Photometry with Herschel Infrared Cameras (GRAPHICS)
Gamma-ray bursts (GRBs) are the most luminous explosions in the universe. It has been difficult to obtain a full spectral picture of the phenomena in the short period when GRBs become alive'', i.e. when they generate bursts in Gamma-ray and produce afterglows in other wavelengths. Between NIR (12micron) and submillimeter (850micron) there lies nearly two orders of magnitude of spectral range where GRB afterglows have never been detected. Herschel is unique in its cutting edge sensitivity, efficiency, and readiness in FIR observations, and is capable of detecting GRB afterglows. Observing GRB afterglows with Herschel would greatly enrich our understanding of GRB physics and conditions of the Universe in early epochs.
We propose Target of Opportunity studies using the SPIRE and PACS instruments of Herschel to observe 3 bright GRB afterglows, each within a few hours to a few tens of days after burst. We will make follow-up observations after the initial one to photometrically measure GRB light curves and IR SEDs. We will make ground optical observations to compliment Herschel data, and have the the GRB community informed. Observing the forward shock peak in the FIR light curve and compare it (both the flux and time) with those in the optical and radio bands would give a unambiguous test to the fireball model, and offer a direct measurement of the density profile of the circumburst material. Catching the short-lived reverse shock emission and measure its magnitude would lead to constraints on some important parameters of the GRB ejecta and address the unknown composition of GRBs, baryonic vs. magnetic.
### The Nature of Star-formation in Halos: The HI bridges in the M81/M82 group
Proposal ID: OT1_mlehnert_1
Principal Investigator: Matthew Lehnert
Time: 21.6 hours priority 2
Category: Extra-galactic ISM
Summary:
We have now reached a relatively mature understanding of the physical processes that regulate the interstellar medium in galaxies, but we are woefully ignorant of the details of the cycles between gas in and outside of galaxies. This is unfortunate because understanding the gas physics in a wide variety of environments is the key to determining the relevance of the physical mechanisms that have been invoked for driving galaxy evolution -- from the feeding of star formation through accretion of cold gas to the regulation of star formation through the mechanical energy ejected by massive stars and AGN.
To help to overcome our ignorance about the nature of star-formation in different environments, in this case in a galaxy halo, we propose to use PACS to observe [CII] in many selected regions of the "bridges" of HI in the nearby group of M81, one of the nearest intergalactic gas flows. The M81 group is an excellent target for this type of study because it has a wide range of HI column densities and stars have recently formed in the gas flow between its galaxies. [CII] is the main coolant and an excellent tracer of the cold neutral medium in galaxies. By combining these data with dust maps from Spitzer and Herschel and HI observations, we will investigate the mass balance between the warm and cold neutral medium to constrain the role of turbulence in regulating this balance, which is key to the cooling and fragmentation of gas and to regulating star formation. N-body/SPH simaulations of the interaction will be used to constrain the overall injection of energy in the tidal streams which powers this turbulence and hence the overall phase balance in the gas. Investigating the nature of star-formation in a halo of a galaxy or group is one of the critical first steps in understanding what occurs during the cosmological accretion of gas and thus help determine what processes drive the evolution of the ensemble of galaxies.
### Star Formation in X-ray Absorbed QSOs through cosmic time
Proposal ID: OT1_mpage_1
Principal Investigator: Mat Page
Time: 3.1 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
The nature of the connection between the growth of a black hole via accretion and that of its host galaxy bulge via star formation remains a fundamental question in galaxy evolution. SCUBA/850micron observations of matched samples of high redshift X-ray absorbed and unabsorbed QSOs demonstrated that the X-ray absorbed QSO were far more likely to be detected suggesting that their host galaxies had very high star formation rates. This result implies that the z~2 X-ray absorbed QSO population are undergoing the transition from the main star forming phase and the QSO phase of a massive galaxy. Follow-up X-ray observations of the absorbed X-ray QSOs found that the X-ray absorption is due to an outflowing, ionized wind which is potentially the feedback invoked by theorists to terminate star formation in the host galaxy. However, no QSOs from the samples, X-ray absorbed or unabsorbed, were detected with SCUBA below z=1.5. We propose SPIRE and PACS observations of a sample of 10 X-ray absorbed QSOs in the 1<z<1.5 redshift range, with the aim of identifying the star-formation properties of their host galaxies as well as their locus within the luminous infrared galaxy population at these redshifts. Our sample is selected such that it will enable us to probe the transition between the star-formation and QSO phases of massive galaxies to lower redshifts than previously and hence allow us to assess the differences (if any) in the relationship between accretion and star formation in massive galaxies as a function of cosmic epoch.
### Determining the structure of blazar jets with joint SPIRE and PACS observations
Proposal ID: OT1_msikora_1
Principal Investigator: Marek Sikora
Time: 21 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
The current time-resolved broad-band spectral data for jet-dominated active galaxies cover spectral ranges from radio to gamma-ray bands, with the notable absence of far infrared to sub-millimeter observations. Those observations are absolutely essential in studies of physics and structure of relativistic AGN jets. They will allow to determine the characteristic frequency of synchrotron self-absorption of the radiating material and probe the electron energy distribution in the critical region below the break associated with the synchrotron luminosity peak. Such measurements are required to determine the location and the spatial structure of the dissipation region of the jet. Here, we propose a series of short observations by both SPIRE and PACS of two blazars, PKS 1510-089 and AO 0235+164, repeated every 2 weeks during a 6-week visibility period over two consecutive visibility windows to provide time-resolved history of broad-band spectra in the IR/sub-mm bands. Those observations, together with data in other bands - which will be available via our on-going monitoring programs covering radio, optical, X-ray, and gamma-ray ranges - will provide a unique data set that will greatly advance our understanding of the blazar jets.
### Herschel Spectroscopic Survey of Warm Molecular Gas in Local Luminous Infrared Galaxies
Proposal ID: OT1_nlu_1
Principal Investigator: Nanyao Lu
Time: 83.5 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
We propose to survey CO spectral line energy distribution (SLED), from J=4-3 up to J=13-12, on 93 local luminous infrared galaxies (LIRGs; L_{IR} > 1.0E11 L_{sun}) with Herschel SPIRE FTS spectrometer. These galaxies, plus 32 additional LIRGs that will have similar data from existing Herschel programs (mainly the HerCULES project), form a flux-limited subset of the Great Observatories All-Sky LIRGs Survey (GOALS) sample. Our proposal is built on the legacy of GOALS and extends beyond the existing Herschel HerCULES program, which emphasizes more on ULIRGs, to a much needed sample coverage of the more numerous and diverse population of less luminous LIRGs. The data from the proposed observations will not only provide much needed local LIRG templates for future ALMA studies of high-redshift counterparts, but also lend us a powerful diagnostic tool to probe the warm and dense molecular gas that are more closely related to the starburst or AGN activity in the nuclei of LIRGs. The data from this proposal will provide important statistical clues to the interplay between the cold and warm molecular gas, IR luminosity, star formation rate and efficiency, and the diverse properties of LIRGs. Specifically, using the homogeneous CO SLED data from this proposal, together with ground-base, low-order CO line data (mainly J=1-0) and other data that have been compiled for the GOALS sample, we will address the following questions: (1) What is the dominant nuclear power source in individual sample galaxy: starburst or AGN? (2) What are the typical physical properties of warm molecular gas in the nuclei of LIRGs? (3) How do the nuclear warm gas components correlate to the cold gas component, star formation rate and efficiency, dust temperature, etc? and (4) How does molecular gas excitation change along a merger sequence?
### Characterizing the Dense Molecular Gas in M82 and NGC 1068: Star Formation versus AGN
Proposal ID: OT1_nrangwal_1
Principal Investigator: Naseem Rangwala
Time: 4.4 hours priority 1
Category: Nearby galaxies
Summary:
We propose to use HIFI to observe high-J rotational transitions of HCN, HNC and HCO+ in M82 and NGC 1068. These molecules are excellent tracers of dense molecular star-forming gas. Their high-J transitions (> J = 4-3), which have never been observed before, trace the densest and warmest regions of the molecular clouds, and their detection is only possible with Herschel. M82, a starburst galaxy with no detectable AGN, and NGC 1068, which harbors a luminous AGN, are ideally suited to test models that discriminate between the energy inputs from star-formation versus X-ray radiation from an AGN. The two sources produce significant differences in the gas physics and chemistry in the interstellar medium, and hence can be distinguished by deriving the physical properties of the molecular gas, and looking at diagnostic line ratios. These two galaxies are also important templates for understanding the physical processes in luminous star-forming and supermassive black hole-forming galaxies at high redshifts, which are too faint and highly obscured by dust. In 4.4 hours, we can obtain a total of 22 spectral lines for these molecules for the two galaxies. Combining these high-J observations with low-J measurements from the ground will provide at least 16 lines per galaxy for non-LTE modeling -- an unprecedented number that will put tight constraints on the physical parameters such as gas kinetic temperature, density, column density and mass. The models will also produce line optical depths, excitation temperature, and level populations providing insight into the excitation mechanism. We will use the line ratios of these molecules in the two galaxies to distinguish between excitation from a starburst and AGN by comparing them to the predictions from models in the literature. These two galaxies are also being observed as a part of the VNGS guaranteed time key project with SPIRE-FTS. The CO lines from FTS will probe and characterize the diffuse molecular gas, and will powerfully complement the results of this proposal.
### Coeval Black Hole and Host Galaxy Growth in High Redshift Radio Galaxies
Proposal ID: OT1_nseymour_1
Principal Investigator: Nicholas Seymour
Time: 26.8 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
High-redshift radio galaxies (HzRGs) are unique markers of the most massive and powerful galaxies in the early Universe, showing signatures of both active galactic nuclei (AGNs) and extreme starbursts. Hence, if the radio-loud AGN phase has a strong effect on the evolution of the host galaxy, it will be most evident in HzRGs. We used Spitzer to carry out a comprehensive survey of 71 HzRGs uniformly covering the redshift range 11e11Msun) out to the earliest epochs probed, and mid-infrared AGN luminosities consistent with the most powerful QSOs. To fully understand the evolutionary state of these HzRGs, we now require accurate star formation rates (SFRs), a measurement which is only possible with Herschel. By combining our Spitzer and ground-based sub-millimeter data with five photometric data bands from PACS and SPIRE, we will separate the AGN and star-forming contributions to the total infrared luminosities. Comparing parameters such as specific SFR against AGN power and radio power, and SFR normalised by accretion rate (from the AGN IR luminosity) against radio jet size, we will test theories of how the radio-loud phase stimulates or suppresses star formation (e.g., 'feedback'). HzRGs also reside in large dark matter over-densities, and are often found in rich (proto-)clusters. The most efficient SPIRE observing mode provides a five arcminute diameter map, which is well matched to our Spitzer data, thereby allowing environmental studies of the HzRGs. Above z=2, Spitzer and SPIRE colours will allow us to select candidate cluster members with redshifts similar to the HzRG. In total, we request 26.8 hours of PACS and SPIRE imaging of the 62 (out of 71) HzRGs which are not in the ROL. These data will enable us to investigate the interplay between AGN and star-formation activity in the early Universe, which in turn will allow us to test predictions of AGN-driven feedback at this crucial epoch. We will also study the HzRG environments.
### Understanding the physics of cold gas in the nearby proxies of distant cooling cores
Proposal ID: OT1_nwerner_1
Principal Investigator: Norbert Werner
Time: 23.9 hours priority 1
Category: Low-z galaxies
Summary:
We propose to observe nine nearby Halpha and X-ray bright giant elliptical galaxies to study the physical properties of their coldest gas phases. Recent CO and IR observations reveal that giant elliptical galaxies contain large amounts of cold dust and gas. These systems also often exhibit powerful Halpha emission, but relatively little star formation. These nearby massive galaxies are the lowest redshift proxies of the more distant cluster cooling cores. The first goal of the proposed observations is to understand the physical properties of the coldest gas phases in the nearest, most massive giant elliptical galaxies and to correlate them with the X-ray properties of these systems to understand why this cold gas does not proceed to star-formation. Furthermore, in these galaxies a tight correlation has been found between the their Bondi accretion rate of hot gas and the jet power. An important question, that we seek to answer is: is this correlation so tight because of a steady accretion of hot gas only, or is there another tight correlation between the hot and cold gas phases, leading to an apparent correlation between the Bondi accretion and the jet power? In order to address these question, we will use Herschel to target the atomic cooling lines of [CII] and [OI]. The proposed Herschel PACS observation in combination with existing and upcoming CO, NIR, optical, UV, X-ray, and radio data, will allow us to test our ideas about the mixing of the cold and hot gas phases in the nearest, brightest giant elliptical galaxies and to discriminate between models of heat input into the cold gas by mixing layers and alternative models, such as heating by conduction or shock heating from colliding clouds. In combination with existing and upcoming CO observations, we will be able to determine the mass of the cold gas in the cores of these giant elliptical galaxies. This will enable us to look for a possible relation between the hot and cold gas phases.
### Charting the Cooling Pathways in High-Speed Extragalactic Shocks
Proposal ID: OT1_pappleto_1
Principal Investigator: Philip Appleton
Time: 37.2 hours priority 1
Category: Nearby galaxies
Summary:
Following in the footsteps of ISO, recent observations with Spitzer have revealed a population of galaxy systems which emit a huge amount of luminosity in their pure rotational mid-IR molecular hydrogen lines, in some cases reaching 10-30 percent of the bolometric luminosity. These large line-luminosities are believed to be powered by galactic-scale shocks, which efficiently transfer kinetic energy to smaller dense clouds in the turbulent post-shock medium. However, nothing at all is known about the other important cooling channels for the shocked gas, such as [OI], H2O, OH, and CO, some of which can rival H2 as a coolant. We propose deep PACS and SPIRE spectroscopy of the Giant Shock in Stephan's Quintet and the Taffy Galaxy bridge to quantify the most important cooling channels and determine the physical state of the gas being shocked. The results have implications for understanding the importance of molecular cooling at higher redshift where turbulence and shock-heating may play a role in galaxy formation.
### What inflates the torus? Probing the physical properties of geometrically-thick buried AGN with high J CO lines
Proposal ID: OT1_pgandhi_1
Principal Investigator: Poshak Gandhi
Time: 20.6 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
The most significant new population of active galactic nuclei (AGN) discovered in recent years is the 'buried AGN' population, uncovered by the Swift satellite. Sensitive X-ray spectroscopy shows characteristics of heavily obscured AGN in these sources, in addition to a very low scattering fraction of low energy photons, which is interpreted as a result of the AGN being buried in dust and gas tori which have an atypically high geometrical thickness. Comprising up to 20 per cent of the entire AGN population, this class constitutes a very important new family of sources, which may be at an interesting evolutionary phase in the AGN life cycle. Yet, very little is known about them, and usual isotropic indicators such as the optical [OIII] forbidden emission line fail to probe their intrinsic powers. The geometrically thick torus picture can result in 1) high gas and dust masses in the tori; 2) increased velocity dispersions and elevated temperatures and pressures; 3) a broad-band spectral energy distribution dominated by cool optically-thick clouds. Far infrared lines provide excellent probes of the physical conditions in the torus, and we intend to use several high J rotational CO lines to test the above picture with Herschel for the first time on several buried AGN for which detailed X-ray spectroscopy exists. These observations will also enable us to search for dynamical signatures of motion in the torus.
### Dust in shocks and star-forming regions outside galaxies: PACS and SPIRE photometry of Stephan's Quintet
Proposal ID: OT1_pguillar_1
Principal Investigator: Pierre Guillard
Time: 13.3 hours priority 2
Category: Extra-galactic ISM
Summary:
Stephan's Quintet (SQ) is an extensively studied compact group of galaxies, where tidal interactions have displaced large amounts of gas into the inter-galactic medium (IGM). Spitzer IRS observations revealed an extremely bright H2 line emission from warm molecular gas, coexisting with a giant (40 kpc), X-ray bright shock, attributed to a high-speed (1000 km/s) galaxy collision. The weakness of PAH and mid-IR dust continuum shows that the H2 gas is not associated with star formation (SF) in the shock, in sharp contrast with standard galaxies. Spitzer photometry suggests that most of the SF rather happens outside the center of the shock and galatic disks. Moreover, an extended FIR component, not connected with the galaxies, but coincident with the X-ray halo of the group, may have been revealed by MIPS, but its poor resolution make this identification difficult. This dust may contribute to cool the hot gas, and thus to fuel SF in the halo. In this context of understanding the processes that control SF in the group, we propose to map the thermal dust emission in all the PACS and SPIRE bands. This will allows for the first time to (1) estimate the total cold gas content in the IGM independently from our CO measurements, (2) make use of the Herschel high spatial resolution to separate the dust emission coming from SF regions, the shock, and the X-ray halo, in order to elucidate the origin of the dust emission in the group and its potential role in cooling the intra-cluster gas, and (3) compare the FIR SED in the different regions of the group to dust models in order to constrain the dust size distribution and the structure of the molecular gas. These observations, together with a companion spectroscopy proposal, will provide the missing pieces of the overall energetic bugdet of the main coolants of the galaxy collision. The results will have important consequences on our understanding of the energetics and the role of dust in high-redshift mergers, and in the formation of the first stars and galaxies.
### Radio Jet Feedback on Molecular and Atomic Gas in Radio Galaxies
Proposal ID: OT1_pogle01_1
Principal Investigator: Patrick Ogle
Time: 68.2 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
We propose Herschel SPIRE and PACS atomic and molecular line spectroscopy and photometry of 23 H2-luminous radio galaxies. Most of these galaxies are IR-weak, such that the kinetic energy output of the radio jet dominates over the radiative output from the AGN accretion disk and star formation in the host galaxy. This new class of galaxies, discovered by Spitzer, has unique MIR spectra with very strong H2 rotational emission lines but weak PAH features compared to normal star-forming galaxies. We may be seeing the direct effects of AGN radio jet feedback, dramatically and fundamentally disturbing the host galaxy interstellar medium in a way that suppresses star formation. Herschel spectroscopy and photometry are essential to inventory the mass and energetics of the atomic and molecular ISM over a wide range of densities and temperatures, and thereby obtain a better understanding of the radio jet feedback mechanism that regulates massive galaxy evolution. We will use shock models to interpret the [O I] and CO emission line spectra and determine the density, temperature, and energetics of shocked molecular gas. Herschel photometry will probe the peak of the IR SED and yield estimates of the total mass of cold dust and cold molecular gas. This will allow us to assess what fraction of the molecular ISM is disturbed by shocks, and understand why and to what extent star formation is suppressed by radio jet feedback.
### Strong AGN feedback onto the ISM and its effects: A SPIRE FTS view of the molecular gas in 3C293
Time: 6.1 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
We propose to use the SPIRE FTS to study the large molecular gas reservoir of the powerful radio galaxy 3C293, the scene of a very strong AGN jet-gas interaction, and the first known case of shock-powered luminous mid-J/high-J CO lines. These were discovered during our large ground-based CO line survey of Luminous Infrared Galaxies (LIRGs) and AGN hosts, and set this object apart as that with the most excited molecular gas of the entire survey, yet with its large gas reservoir (~2x10^9Msol) surprisingly idle in terms of star formation rate (SFR~4Msol/yr). A deep SPIRE FTS spectrum will complete our ground-based CO Spectral Line Energy Distribution (SLED) of this remarkable system and allow excellent constraints to be placed on the thermal state of its molecular gas reservoir and possible suppressing effects of the AGN on star formation in the host galaxy. It will also be the first opportunity to study, locally, powerful AGN mechanical feedback onto the interstellar medium of host galaxies, which will occur frequently in the Early Universe during galaxy formation in the deep gravitational wells of proto-clusters marked by such powerful radio galaxies.
### Herschel spectra of low-z QSOs: measuring radiative feedback, radiation pressure and star formation
Proposal ID: OT1_pvanderw_4
Principal Investigator: Paul van der Werf
Time: 28.1 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
Observations with the SPIRE FTS of the ULIRG-QSO Mrk231 have shown that the CO rotational ladder can be used to separate the contribution of Photon-Dominated Regions (PDRs), powered by star formation, from that of X-ray-Dominated Regions (XDRs), powered by the AGN.
We propose to apply this diagnostic to a sample of 5 low-z QSOs with detections in CO, in order to:
(1) derive size, density, column density and X-ray illumination of the circumnuclear medium;
(2) measure radiative feedback and derive radiation pressure by the AGN on the surrounding medium, in order to probe its ability to drive the recently discovered molecular outflows and disperse the nuclear gas, and to assess its importance for the dynamical support of the circumnuclear medium, which will affect dynamical black hole mass measurements;
(3) determine the importance of star formation in the host galaxy for the observed infrared luminosity.
Our observations consist of SPIRE-FTS spectra of 5 QSOs, and PACS spectra to measure the higher CO lines in the brightest object only. These observations will address the evolutionary relation between QSOs and ULIRGs and the role of QSOs as drivers for the transition between actively star forming and passive galaxies. They will also constitute a low-z benchmark for future CO observations of high-z QSOs with ALMA, which can only be provided by Herschel, and which is not covered in the current Herschel programme.
### Gas excitation through black hole accretion and star formation in the centers of active galaxies.
Proposal ID: OT1_rmeijeri_1
Principal Investigator: Rowin Meijerink
Time: 22.4 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
Stunning observations with SPIRE FTS of Mrk 231 have shown that CO lines are very bright up to J=13-12, and there is no sign of a decline in the CO Spectral Line Energy Distribution (SLED). Our SPIRE FTS spectra show that this is a common feature of AGN type galaxies. Therefore, we propose to observe a set of 4 very high-J CO line transitions using the PACS spectrometer, for 5 of these well studied proto-typical (Ultra-)Luminous Infrared Galaxies ((U)LIRGs) and one starburst galaxy. The question of the relative role and contribution of AGN to the far-infrared luminosities of local (U)LIRG systems has long been a problem in our understanding of the evolutionary path of these objects, and as well for the interpretation of deep far-infrared surveys.
Our SPIRE FTS and our ground-based CO line observations together with the PACS observations in this program will allow us, for the first time, to complete a full CO SLED for a set of (U)LIRGs. Combining this with our models of Photon Dominated Regions (PDRs) and X-ray Dominated Regions (XDRs), we will then be able to determine the physical state of the interstellar medium and estimate the starburst/AGN contribution to the total energetics of these systems.
### Determining the Bolometric Luminosity of AGN
Proposal ID: OT1_rmushotz_1
Principal Investigator: Richard Mushotzky
Time: 59 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
Determining the bolometric luminosities of AGN is key to understanding their evolution. Uncertainties in the total radiation from AGN translate into uncertainties in their lifetimes, Eddington ratios, mass accretion rates, the form of their radiation, and the predicted black hole spin. However, we still have major problems in measuring this critical quantity. AGN and their host galaxies emit a large fraction of their light in the MIR to FIR, but the origin of this radiation and the connection to the AGN are not well understood. It is not clear whether this radiation is associated with the AGN or with star formation in the galaxy.
We propose to use Herschel's unique capabilities to establish the properties of the Swift-BAT all sky sample of local AGN selected at 15-195 keV. We will measure the MIR to FIR (65-500 microns) properties of a complete low-redshift sample (309 objects at z<0.05). The Swift-BAT survey is the least biased all sky survey for AGN with respect to host galaxy properties and obscuration in the line-of-sight, and thus it is superior to optical, IR, or radio surveys for understanding the the nuclear component of the MIR to FIR radiation from active galaxies. The low redshift of our sample, the uniformity of selection, and the large amount of parallel data which have already been obtained (Spitzer, optical, and X-ray spectra, and optical and UV imaging) will allow the most precise determination of the physical origin (AGN versus star formation) of the light. The low redshifts allow the best possible angular resolution for spatially separating star-formation and nuclear components, while only requiring short Herschel exposures.
The Herschel BAT survey will provide a comprehensive database for determining the bolometric light of AGN and will be an invaluable reference sample for analyzing higher redshift AGN. It will be a powerful resource for many years to come. We will make it available in a comprehensive and accessible form as rapidly as possible.
### Comparing the Dust Emission from High Redshift Lyman Break Galaxies with their Best Low Redshift Analogs discovered by GALEX
Proposal ID: OT1_roverzie_1
Principal Investigator: Roderik Overzier
Time: 28.6 hours priority 1
Category: Low-z galaxies
Summary:
We propose to use PACS to characterize the dust emission in UV-selected starburst galaxies at z<0.3 from our on-going survey of "Local Lyman Break Analogs" (LBAs). This survey was specifically designed to find and study rare, nearby galaxies from the GALEX all-sky survey that are most similar to the population of Lyman Break Galaxies (LBGs) at z>2-3. The LBAs are similar to LBGs in terms of mass, SFR, age, metallicity, attenuation, size, morphology, kinematics, and ISM. Because of these remarkable similarities, we can perform a much more straightforward comparison of their properties.
Specifically, we will use PACS to sample the far-IR dust emission from 28 LBAs, and study its relation to other physical properties of these starbursts to a level of accuracy that can not be achieved for similar UV-selected starbursts at high redshift. We will address the following questions:
(1) What are the contributions from hot/cold dust emission to the total (UV+IR) energy budget, and how do these compare with LBGs? (2) How do LBAs relate to their IR-luminous counterparts in the local Universe? (3) Do LBAs follow the locally calibrated "beta-IRX relation" that is commonly used to calculate dust-corrected SFRs at high redshift? (4) Can we understand offsets from the beta-IRX relation in terms of other properties (e.g., complex star formation histories or modified extinction laws)? (5) What are the star formation efficiencies in LBAs as a function of their triggering mechanism, and are these similar to those inferred for LBGs?
Combined with our existing broad based, multi-wavelength observations from GALEX, SDSS, HST, Spitzer, VLT, Keck, XMM, and the VLA these data will provide crucial information on the interplay of stars, gas and dust in the LBG analogs. This will aid us in our understanding of their UV-luminous counterparts at high redshift, just as our understanding of local ULIRGs has been fundamental for the study of the most IR-luminous sources at high redshift.
### Testing the XDR/High-J CO Paradigm in Nearby Galaxies
Proposal ID: OT1_shaileyd_1
Principal Investigator: Steven Hailey-Dunsheath
Time: 32.2 hours priority 1
Category: Nearby galaxies
Summary:
One of the most exciting first results from SPIRE and PACS spectroscopy is the detection of high-J CO emission in galaxies. Such emission has long been proposed as a tracer of X-ray dominated regions (XDRs) produced by AGN, and as a powerful diagnostic tool for future millimeter-wave study of AGN at high redshift. The shortest wavelength submillimeter CO lines detected by SPIRE-FTS in the X-ray luminous ULIRG Mrk 231 are interpreted as arising from an extended XDR, providing strong observational support for the XDR/high-J CO connection. However, our group (SHINING; PI E. Sturm) has used PACS to detect even higher-J far-IR CO emission in a few nearby galaxies, including 2 starburst galaxies with little evidence of a luminous AGN. Can high-J CO emission also be produced in gas heated by the UV radiation or mechanical output of a starburst? To address this question we propose to measure a set of far-IR CO lines in 4 nearby AGN and 4 starburst galaxies, as well as in 2 merging systems with large masses of shock-heated molecular gas. Does the high-J CO line SED reflect the different excitation mechanisms in these template objects? We additionally propose to use OH line observations to estimate the abundance of this molecule, which is a sensitive tracer of X-ray-driven chemistry. The OH line profiles will also be used to search for evidence of molecular outflows, which may drive shock heating. Each of these galaxies will have SHINING GT observations of the set of far-IR fine-structure lines, which includes important tracers of UV-, X-ray-, and shock-heated gas. The AGN subsample is restricted to the most nearby systems, where the high spatial resolution of PACS is sufficient to separate the nuclear AGN-heated gas from the circumnuclear star-forming regions. The PACS CO data obtained here will provide the first well-sampled far-IR extragalactic CO line SEDs, and will be an essential reference for future high redshift studies.
### The physical conditions of star formation at low metallicity: the Magellanic clouds as corner stones
Proposal ID: OT1_shony_1
Principal Investigator: Sacha Hony
Time: 79 hours priority 2
Category: Extra-galactic ISM
Summary:
How galaxies convert their gas reservoirs into stars is a stumbling block in understanding galaxy evolution. The far IR and submm cooling lines arising from photodissociation regions (PDRs) are the key diagnostics of the interplay between star formation and the evolving ISM throughout the course of the history of the universe. While effort has been put into physics of PDRs and star formation in the Galaxy and other metal-rich galaxies, little attention has been put into understanding the effects of the lower metal abundance on the these processes. Here we propose PACS ([CII] 158 um, [OI] 63 um, [OI] 145 um, [OIII] 88 um, [NII] 122 um) and SPIRE FTS spectroscopy towards carefully selected star forming sites in the nearest low metallicity galaxies, the Magellanic Clouds (MCs) as a benchmark study to calibrate the primary diagnostics of low metallicity environments which are crucial for ALMA high redshift science. The proximity of the MCs allows Herschel to resolve molecular clouds at 3 pc scale. Our targeted regions span a wide diversity of environments, including dense molecular gas and ionised regions. These new data, together with existing IRS spectra, Herschel and Spitzer photometry, and a wealth of ground−based data including the MAGMA CO data, will allow us to address important unresolved issues: 1) the amount of molecular gas hidden in a low extinction phase where CO is photodissociated and thus not detected; 2) the dependence of the FIR fine structure lines, CO excitation and gas thermodynamics on environment; and 3) the structure of PDRs at low metallicity. Our results will be key to interpreting FIR fine structure lines and CO observations of more distant systems. We will produce PDR models tested at low metallicity, a library of CO excitation at low metallicity, and a calibration of the amount of "CO−free" molecular gas as a function of environment. In addition, multi−line maps covering the main coolants of the atomic and molecular gas, represent a data product with lasting legacy value.
### Exploring the Dust Content of Galactic Winds with Herschel
Proposal ID: OT1_sveilleu_2
Principal Investigator: Sylvain Veilleux
Time: 48.7 hours priority 1
Category: Nearby galaxies
Summary:
We propose a PACS imaging survey to study galactic winds from nearby starburst galaxies. We will obtain very deep PACS 70/160 micron data to map the detailed distribution of cold (T<100 K) dust in a small but representative sample of galaxies that are known to host outflows. These data will be compared to state-of-the-art, 3D numerical simulations of superwinds and predicted PACS fluxes. Direct and indirect evidence shows that dust is present on large (kiloparsec) scales in outflows in some starburst galaxies. However, this dust has never been mapped at wavelengths of 70-160 microns, and its geometry, mass, and energy are almost completely unknown. Recent spectacular SPIRE results on M82, as well as our own Spitzer IRAC 8-micron and MIPS 24-micron maps of the targeted wind galaxies, suggest that this survey will yield exciting new insights on the cold dust in these outflows. We will ascertain the significance of dusty superwinds in the context of outflow physics and the impact of the outflows on the host galaxies and the intergalactic medium. We will compare the distribution, mass, and energy of the cold dust to optical emission-line and absorption-line, mid-infrared, X-ray, and radio data compiled by us and other groups. We note that several of our targets are being mapped with PACS and SPIRE as part of key programs (KPs). However, the objectives of these programs are heterogeneous and often neglect the importance of outflow science. This is reflected in the depth of the observations at the critical shorter wavelengths, near the peak of the IR SED: the PACS KP data will not be able to detect the FIR emission expected from a M82-like wind in our galaxies. There is currently no plan to address this problem but one is necessary to take full advantage of Herschel in this field. The proposed PACS survey will go nearly an order of magnitude deeper than the KP data and will complement the SPIRE portion of the KPs, while providing many advantages over the SPIRE data.
### Molecular Outflows in Gas-Rich Mergers
Proposal ID: OT1_sveilleu_3
Principal Investigator: Sylvain Veilleux
Time: 32.5 hours priority 1
Category: Active galaxies/ULGs/QSOs
Summary:
The role of galactic winds in gas-rich mergers is of crucial importance to understand galaxy and supermassive black hole evolution. In recent months, our group has had two major scientific breakthroughs in this area: (1) the discovery from our SHINING guaranteed-time PACS survey of ultraluminous infrared galaxies (ULIRGs) of a 1400-km/s molecular OH wind in the nearest quasar, Mrk 231. (2) The independent discovery from mm-wave CO interferometric observations in the same object of a spatially resolved molecular wind with estimated mass outflow rate 4-10x larger than the star formation rate. Remarkably this CO outflow coincides spatially with blueshifted neutral gas in our optical spectra. This powerful outflow may be the long-sought "smoking gun" of quasar mechanical feedback purported to transform gas-rich mergers. However, our SHINING survey contains only 2 other warm quasar-dominated late stage mergers like Mrk 231 (one of them also shows a high-velocity OH outflow, while the other has not yet been observed). So here we request 32.5h to obtain high-S/N OH 119 um spectra of 15 additional quasar-dominated late stage mergers. We have a comprehensive set of multiwavelength data on all of these objects, including crucial spatially resolved optical Na ID absorption spectroscopy. The combined sample of 20 cold ULIRGs and 18 warm ULIRGs/QSOs will allow us to address the role of mechanical feedback in mergers after the first peri-passage, i.e. when mechanical feedback from the starburst/QSO is predicted to be at its maximum. We will look for trends between the basic measured properties of OH (incidence of absorption, kinematics, column densities) and host/evolutionary indicators. In cases of kinematic match between OH features and spatially resolved neutral-gas clouds, we will be able to infer the masses and kinetic energies of these outflows. Measured velocities in excess of ~1000 km/s or inferred mass outflow rates much larger than the star formation rates would be telltale signs of AGN-driven winds.
### Hydrogen Fluoride Absorption Toward Luminous Infrared Galaxies
Proposal ID: OT1_tphill01_1
Principal Investigator: Thomas Phillips
Time: 40.5 hours priority 2
Category: Nearby galaxies
Summary:
We propose to carry out a HIFI survey of the fundamental transition of HF at 1.232 THz toward 24 relatively nearby IR-bright galaxies to probe their ISM physical conditions. HF is a very new tracer of the diffuse and dense ISM, with its use originating with the ISO detection of the J=2-1 transition in absorption toward Sgr B2. Widespread HF J=1-0 absorption toward galactic starforming regions has been recently detected by HIFI and HF emission in an extragalactic nucleus has been detected at low spectral resolution by SPIRE. We intend to make use of this unique probe by conducting a high spectral resolution (10-20 km/s) HIFI absorption survey toward continuum-bright external galactic nuclei exhibiting a wide range of physical properties (AGN, starbursts, mergers). HF is chemically very strongly bound and therefore resistant to photodissociation. Our study is facilitated by this resistance of HF molecules to destruction, which will occur in the extreme environments in the galactic nuclei. HF will thus be a very useful probe in regions of the ISM where more traditional gas probes, such as CO, are more prone to error (e.g., the use of the X-factor). With the simplifying assumption that all fluorine is likely to be locked up in HF, and that the HF molecules will reside in the ground rotational state, we can measure the hydrogen column density and mass of the nearby IR-bright galaxies. Observations of the local galaxies proposed here are the first step toward using HF as a tracer of the gas in high-redshift galaxies. By looking at extragalactic continuum-bright nuclei, we will also be able, through the use of the HIFI Wide Band Spectrometer, to simultaneously search for absorption through the Milky Way halo cloud population. Here, the rapid formation rate of HF and its strong molecular bond will allow us to detect HF absorption toward the tenuous and quiescent mostly HI clouds making up the galactic halo. These diffuse, cold regions may not otherwise be detectable in CO emission or other commonly uses tracers.
### Monitoring of the far-IR SED of two archetypical quasars
Proposal ID: OT1_tsavolai_1
Principal Investigator: Tuomas Savolainen
Time: 6.8 hours priority 2
Category: Active galaxies/ULGs/QSOs
Summary:
We propose quasi-simultaneous multiband photometry with Herschel and other ground- (VLBA, Effelsberg, SMA, OAGH, NOT) and space-based (Swift, Fermi) facilities to obtain an unprecedented coverage of spectral energy distribution (SED) of two archetypical radio-loud quasars 3C273 and 3C279 and follow evolution of the SED on monthly timescale. The wide wavelength coverage of the Herschel instruments PACS and SPIRE will allow us to sample the region of the synchrotron peak of the SED in these sources and monitor its variability, which provides a way to distinct between various emission components expected in this region (one or more synchrotron components, thermal emission from dust). The combination of the Herschel data with the other facilities will provide almost completely sampled SEDs that will put strong constraints on the blazar emission models.
### Unveiling the dark side of the Gamma-Ray Bursts with Herschel Far Infrared Photometry
Proposal ID: OT1_vd_1
Principal Investigator: Valerio D'elia
Time: 28.1 hours priority 1
Category: Extra-Galactic Other
Summary:
Dark gamma-ray bursts (GRBs) are bursts with a detected X-ray afterglow but not detected optical afterglow in spite of deep follow-up observations. Approximately 40% of all bursts belong to this category. Possible explanations for the lack of an optical detection are a high redshift (z>7), which however can not account for the whole dark population, and extinction due to the host galaxy dust. We plan to take advantage of the Herschel capabilities to spot for the first time these objects in the far infrared band, using PACS. The requested observations will shed light on the nature of dark GRBs, allowing us to put constraints on the dust content, on the afterglow physics and to search for the host galaxies of these elusive sources.
### Molecules in the Distant Universe: Herschel Spectroscopy of Damped Lyman-alpha Quasar Absorbers
Proposal ID: OT1_vkulkarn_1
Principal Investigator: Varsha Kulkarni
Time: 36.8 hours priority 1
Category: Extra-galactic ISM
Summary:
Observations of interstellar molecules in distant galaxies are essential for investigating the chemical evolution of galaxies. Absorption line systems in quasar spectra, especially the damped Lyman alpha (DLA) absorbers, provide excellent venues for directly studying the interstellar matter (ISM) in distant galaxies, selected independently of the galaxy luminosities. A few cold, dusty absorption systems have been discovered using radio surveys and the Sloan Digital Sky Survey. These absorbers, far richer in dust/molecules than the general DLA population, give us rare opportunities to probe molecular clouds at high redshift. Here we propose Herschel observations of 4 quasars with such DLAs at z < 1.5 to further observe their molecular content. These DLAs exhibit H I 21-cm absorption and other signatures of cold ISM such as the 2175 A bump from carbonaceous dust or low spin temperature. Furthermore, we have detected 9.7 micron silicate absorption toward two of these DLAs with Spitzer IRS. We request HIFI spectroscopy to observe absorption lines of CO, CN, NH, H2O, and SPIRE photometry of the 4 quasars to determine the continuum accurately. In addition, we request SPIRE photometry of 10 other quasars with strong absorbers rich in dust/metals, in order to identify bright targets for future Herschel spectroscopy. Our overall science goals are: (1) to estimate molecular abundances and kinematics of the absorbing gas; (2) to constrain isotopic ratios such as 12C/13C from 12CO/13CO or 12CN/13CN; (3) to estimate the cosmic microwave background temperature at the absorber redshifts. Finally, (4) the proposed program will help to further constrain the cosmic variation of fundamental constants such as the electron-to-proton mass ratio.
### Major-merger, starburst.... what next?
Proposal ID: OT1_vwild_1
Principal Investigator: Vivienne Wild
Time: 4.7 hours priority 1
Category: Low-z galaxies
Summary:
A popular scenario to explain the increase in number of quiescent, elliptical galaxies over cosmic time is one in which gas-rich major mergers lead to strong starbursts which exhaust fuel supplies and transform the morphology of galaxies from disks to spheroids. In this proposal we describe how PACS+SPIRE photometry can directly test this scenario. We present a unique sample of massive starburst-to-post-starburst galaxies in the local Universe (z<0.05), which have undergone a starburst between 10Myr and 1Gyr ago. The sample is drawn from a statistically complete sample of Sloan Digital Sky Survey (post-)starburst galaxies, i.e. they have experienced the same strength starburst. Together with CO molecular gas masses (already obtained), we will use the Herschel photometry to track the evolution of dust mass, dust temperature and dust-to-gas ratios for 1Gyr following the starburst. This will allow us to directly test (1) how star formation is quenched following a starburst: gas exhaustion, expulsion or change of gas state; (2) whether massive starburst galaxies are the progenitors of red-sequence galaxies. Additionally, we will use our accurate starburst ages to test whether supernovae or post-AGB stars contribute significantly to the enrichment of the interstellar medium (ISM) with dust. By combining with results from similar studies of local merger- or IR-selected galaxy samples we will calculate a "duty-cycle" for IR bright galaxies, crucial for understanding the selection of high-z galaxy samples. By combining our (post-)starburst galaxy sample defined upon the physical properties of starburst age and strength, with the diagnostic capabilities of CO and dust emission for probing the physical state of the ISM, this dataset will provide the best observational constraints to date on the merger+starburst evolutionary pathway from star-forming spiral to quiescent elliptical galaxy.
### Keeping the cool gas in galaxy clusters warm.
Proposal ID: OT1_wjaffe_1
Principal Investigator: Walter Jaffe
Time: 24.9 hours priority 1
Category: Extra-galactic ISM
Summary:
We propose SPIRE FTS spectra to determine the source of heating of the cool/warm (100-300 K) gas in the Brightest Cluster Galaxy NGC-1275, the brightest of all cluster cool-core galaxies. The heating mechanism in BCGs is unknown and crucial to understanding analogous "negative feedback" processes in star-forming galaxies at high redshift. Our current mm-CO, PACS, nearIR and optical data on this cluster indicate that the SPIRE measurements will detect many CO lines and possibly H2O+ and OH+ lines that will determine the temperature, and density of the most important component of this warm gas. The ratios of the CO lines, and the presence or absence of the ionized lines, and the dependence of these lines with distance from the central AGN should allow us to choose between the several possible heating and excitation mechanisms: soft X-rays, cosmic ray ionization, and C- and J- shocks from AGN induced turbulence.
## Cosmology (24)
### Spectroscopy of a Highly Magnified Galaxy Behind the Bullet Cluster
Proposal ID: OT1_agonza02_1
Principal Investigator: Anthony Gonzalez
Time: 12.8 hours priority 1
Category: High-z galaxies
Summary:
Initial Herschel results have demonstrated the power of the observatory for characterizing the properties of ultraluminous, star-forming galaxies during the peak era of star formation. Even with Herschel; however, the only way to spectroscopically study the properties of more typical, lower luminosity systems is by using gravitational lensing to augment the capability of the telescope. We request 12.8 hrs to obtain PACS and HIFI spectroscopy for a single, exceptionally magnified luminous infrared galaxy at z=2.791 that is lensed by the Bullet Cluster. This system, a dusty luminous infrared galaxy, is magnified by a factor of 100 and has a star-formation rate of 100 solar masses per year. It is the lowest stellar mass, lowest intrinsic luminosity galaxy known at z>2 that is magnified sufficiently to enable Herschel spectroscopy, providing our best chance of studying in detail a typical star-forming galaxy at this epoch. The primary goals with the current observations are (1) to obtain a high-fidelity determination of the warm gas mass in this sytem via molecular hydrogen rotational lines, and (2) to constrain the properties of the HII and photodissociation regions via fine structure lines, including the [CII] cooling line. The global objective is to obtain a detailed view of the ISM in this galaxy -- which is likely to yield the best information that we will have for any low mass galaxy at this epoch.
### Tracing the Evolution of Star Formation Activity in High Redshift Galaxy Clusters
Proposal ID: OT1_apope_1
Principal Investigator: Alexandra Pope
Time: 54.7 hours priority 2
Category: Galaxy clusters/Lensing clusters
Summary:
Recent observations suggest a reversal in the star formation rate density relation at z>1 such that the average star formation rate in galaxies increases with increasing local galaxy density; the epoch at which this transition occurs is poorly constrained. Two high redshift clusters have shown an increased fraction of actively star forming galaxies towards the center of the cluster, albeit with small number statistics. We propose a statistical study of the dust-obscured star formation activity in a mass limited sample of 12 clusters from z=1.1-1.8 with PACS imaging at 100/160 microns. With 54.7 hours of observing time, we will detect ~150 cluster galaxies down to 100 solar masses per year and many more field galaxies. Our sample spans the fundamental redshift range during which massive clusters show signs of transitioning from a stage of active formation to passive evolution. We will determine the role of the cluster environment on the evolution of infrared luminous galaxies as a function of redshift. These Herschel observations will allow us to map out the star formation activity in galaxy clusters and constrain their mass assembly epoch.
### Probing the Interstellar Medium of ULIRGs/SMGs at high redshift
Proposal ID: OT1_AVERMA_2
Principal Investigator: Aprajita Verma
Time: 77.3 hours priority 1
Category: High-z galaxies
Summary:
Early results from Herschel have shown we are entering a new and exciting era in the study of the interstellar media of galaxies. Using the far-infrared cooling lines, we have demonstrated the capability of the PACS spectrometer in deep integrations reaching line sensitivities of 3 sigma sensitivities of 3e-18 W/m/m in <~2 hours exposures on resolved lines, reaching as low as 1e-18 W/m/m in ~7 hours with the red detector allowing us to probe the ISM of galaxies in place at the peak of star-formation and AGN activity in the Universe (Sturm et al. 2010). This proposal builds on these first studies by performing PACS spectroscopy of a sample of bright and strongly lensed infrared/sub-mm galaxies at moderate to high redshift. By virtue of the magnification due to lensing we are able to probe intrinsically lower luminosity galaxies which would normally be beyond the reach of the Herschel spectro- meters, and, for the first time, constrain the physical processes and state of the ISM in these high-redshift galaxies.
### Herschel Observations of the Coma Cluster
Proposal ID: OT1_csimpson_1
Principal Investigator: Chris Simpson
Time: 27.2 hours priority 1
Category: Galaxy clusters/Lensing clusters
Summary:
We propose to make deep PACS observations of a 1.75-square degree region of the Coma cluster which encompasses both the dense core and the southwest infall region, and covers a factor of 100 in galaxy density. In combination with SPIRE data from the Herschel-ATLAS Key Project, these data will provide the first reliable measurements of the dust properties in a rich galaxy cluster. We have assembled a vast multi-wavelength dataset over this region of Coma that has allowed us to compute reliable stellar masses for nearly 2,000 spectroscopically-confirmed cluster members. We will (i) measure the far-infrared luminosity function and determine whether the turnover seen in Virgo is also present in Coma; (ii) measure the dust masses and temperatures of all galaxies brighter than this turnover; (iii) derive reliable *total* star-formation rates for all galaxies from a combination of UV, H-alpha, and far-IR imaging, and hence address the controversy surrounding optically-classified "post-starburst" galaxies; (iv) relate these important properties of the cluster galaxies to quantities such as stellar mass, galaxy morphology, local galaxy density, and the density of the intra-cluster medium, to determine which physical processes are responsible for the transformation of galaxies from late-type to early-type. We will also search for intra-cluster dust which is expected to be produced via stripping of material from infalling galaxies.
### SPIRE Spectroscopy of the Brightest High-Redshift Submillimeter Galaxies
Proposal ID: OT1_dmarrone_1
Principal Investigator: Daniel Marrone
Time: 4.1 hours priority 1
Category: High-z galaxies
Summary:
The South Pole Telescope has conducted a large survey of the southern sky at millimeter wavelengths and discovered a population of high-redshift strongly-lensed dusty star forming galaxies. Both the lensing and the long wavelength selection biases these sources to the highest redshift and their apparent luminosity makes them the most best possible candidates for SPIRE FTS spectroscopy. By combining the unique capabilities of SPT as a survey machine and Herschel as a followup spectroscopy machine, we propose to obtain spectra for five of the brightest lensed sources in the sky. These observations will open a new astrophysical window into the study of young star forming galaxies. The ratios of far-IR lines will provide ground-breaking physical information about this earliest stage of galaxy evolution, including the best measures of how star formation is proceeding, dust emission and absorption properties, the detailed physics of the ISM, and also the quantitative contribution of the emission that comes from black hole accretion in an obscured AGN for these high redshift sources.
### Characterizing the Interstellar Medium in 'Normal' High Redshift Galaxies
Proposal ID: OT1_driecher_1
Principal Investigator: Dominik Riechers
Time: 24 hours priority 2
Category: High-z galaxies
Summary:
One of the most astounding recent discoveries is that 'normal' high-z star-forming galaxies are very gas-rich, and often dominated by a massive, cold molecular interstellar medium (ISM) component. The extended morphology, low gas excitation and low star formation efficiency in these galaxies suggest that they maintain widespread, long-lasting star formation. Thus, the overall conditions for star formation are consistent with nearby spiral galaxies, although scaled up by 1-2 orders of magnitude in gas mass and star formation rate. Building upon our comprehensive study of the molecular ISM in these galaxies, we here aim to explore a new regime of star formation diagnostics in the brightest galaxy in our sample with Herschel, exploiting the unprecedented spectral line sensitivity in the widely unexplored far-infared wavelength regime that is inaccessible from the ground. Using PACS and SPIRE, we aim to detect, for the first time, the seven brightest neutral and low ionization state fine structure ISM cooling lines of C, N, and O in a 'normal' high-z galaxy. These lines will provide a critical piece of evidence for the scenario that the ISM properties in these galaxies are indeed comparable to nearby spirals (rather than extreme starbursts) by constraining the UV radiation field, densities, temperatures, and composition (atoms/ions/molecules) of the gaseous component in our target. Such Herschel data are the last missing piece in a full characterization of the ISM in 'normal' star forming galaxies during the peak epoch of galaxy formation. Together with our extensive ground-based dataset, this will provide a unique template for studies of such galaxies at z>3 with ALMA (where a few of the targeted lines become accessible from the ground).
### SPIRE Snapshot Survey of Massive Galaxy Clusters
Proposal ID: OT1_eegami_4
Principal Investigator: Eiichi Egami
Time: 27 hours priority 1
Category: Galaxy clusters/Lensing clusters
Summary:
For deep imaging longward of 100 um, confusion noise sets the fundamental sensitivity limits achievable with Herschel, and these limits cannot be improved by integrating longer. To penetrate through this confusion limit and detect faint high-redshift galaxies, gravitational lensing by massive galaxy clusters offers a very powerful and yet cheap solution. For this reason, we are currently conducting a PACS/SPIRE imaging survey of ~40 massive lensing clusters as one of the Herschel Key Programs, "The Herschel Lensing Survey" (PI: Egami, 292.3 hrs). Although this program is producing many exciting results as reported in our 5 Herschel special-issue papers, one thing is becoming clear: it is extremely difficult to find lensed galaxies that are bright enough (> 200 mJy in SPIRE bands) to perform spectroscopy with PACS/SPIRE. This disappointment, however, was quickly overcome by the serendipitous discovery of an exceptionally bright (~500 mJy@350 um) z=2.3 galaxy lensed by a massive cluster at z=0.325. This discovery suggests that if we survey a large enough cluster sample, we will find similarly bright lensed sources that make all kinds of exciting follow-up observations possible. Here, we propose to conduct such a survey by taking advantage of the Millennium Cluster Sample constructed from the ROSAT All-Sky Survey with many years of extensive follow-ups. More specifically, we will conduct a SPIRE snapshot survey of 279 X-ray-selected clusters. SPIRE's great sensitivity and observing efficiency means that we can complete this program in only 27 hours while achieving a nearly confusion-limited sensitivity of 10 mJy (1 sigma). Such a depth will allow all kinds of secondary science projects as well. Although SPIRE wide-area surveys like H-ATLAS will also discover many bright lensed galaxies, these sources are mostly lensed by galaxies and not clusters, which makes our approach an economic alternative to investigate a different type of lensed systems.
### A PACS Redshift 1-2 Oxygen Survey: Leveraging the ZEUS [CII] Detections
Proposal ID: OT1_gstacey_3
Principal Investigator: Gordon Stacey
Time: 45.7 hours priority 1
Category: High-z galaxies
Summary:
We propose to use PACS spectroscopy to observe the [OI] 63 um, [OIII] 88 and 52 um, and [OIV] 26 um fine-stucture lines, and PACS/SPIRE photometry to measure the far-IR continuum from 12 IR-bright galaxies in the z = 1 to 2 redshift range. These are galaxies from which we have detected emission in the 158 um [CII] line using our grating spectrometer, ZEUS, on the CSO. We have found that the most luminous starburst-dominated systems in this epoch are characterized by kpc-scale moderate intensity star formation, while the AGN-dominated systems host similarly extended, but much more intense starbursts. The proposed oxygen survey addresses two key questions stimulated by our [CII] results: (1) To what extent are luminous star-forming galaxies at z = 1 to 2 simply scaled-up versions of local starbursts? (2) Why are the starbursts in AGN-dominated systems so much more intense? The oxygen sequence combined with our [CII] detections will have powerful diagnostic capabilities, yielding the strength and hardness of the ambient UV radiation fields, and the density, pressure, and mass of the ionized and neutral atomic components. This data will allow us to characterize the size and age of the starburst, and the importance of the central engine. The ultimate goal is to understand what drives the apparently galaxy-wide starbursts in both star-formation-dominated and AGN-dominated systems, and help identify the connection between starbursts and AGN in the early Universe. This survey is important and unique. We cover the redshift interval from 1 to 2 near the peak of the star formation per unit co-moving volume in the Universe, and it is within this redshift interval that the ZEUS and PACS sensitivities are well matched to enable the detection of the [CII] line together with the oxygen sequence in a wide variety of systems.
### Measuring the Epoch of Reionization
Proposal ID: OT1_jcarls01_3
Principal Investigator: John Carlstrom
Time: 79 hours priority 1
Category: Cosmology/Extra-galactic surveys
Summary:
We propose to take advantage of the unique capabilities of both SPIRE and SPT to measure for the first time the kinetic SZ contribution'' to the CMB power spectrum. By doing so we will be able to detect, or severely constrain, a signal arising from the scattering of CMB photons off bubbles of ionized IGM during the epoch of reionization, thus providing a first glimpse of the universe as it emerged from the dark ages. To make this measurement we will map the 100 sq. deg. SPT Deep Field with SPIRE and conduct a joint CMB-style analysis of the SPIRE and SPT maps. The high-precision measurements of the CIB fluctuations provided by SPIRE are essential to isolate of the reionization signal. By adding SPIRE observations to the already-reduced SPT data, we will improve the existing constraints on this signal by an order of magnitude. Comparable constraints on the epoch of reionization are unlikely to come from any other combination of facilities prior to the next generation of 21 cm surveys. The combination of the SPT and proposed SPIRE maps will also enable numerous auxiliary studies.
### Resolved Herschel photometry and line spectroscopy for the brightest lensed galaxy at z~2
Proposal ID: OT1_jrigby_1
Principal Investigator: Jane Rigby
Time: 19.2 hours priority 1
Category: High-z galaxies
Summary:
We propose to obtain deep, spatially--resolved Herschel PACS and SPIRE photometry and PACs and HIFI spectroscopy of the brightest (in the rest-UV) lensed galaxy yet discovered, RCS0327 at z=1.7038. The goal is to characterize the dust--reprocessed spectral energy distribution (SED) of a typical star--forming galaxy at the epoch when half the Universe's stars formed. Because RCS0327 extends across 38 arcsec, Herschel will spatially resolve it, and thus will measure spectral energy distributions in multiple spatially--distinct regions. The resulting SED will serve as one of very few templates of low--extinction star forming galaxies beyond the local universe. We will measure the far-infrared luminosity and thus infer a star formation rate, which we will compare to rates measured from the optical/nIR. Finally, we will measure the luminosities of the [O I] 63 and [C II] 158 micron lines, which with the far-IR luminosity constrain the densities, pressures, and radiation fields of the photo-dissociation regions. Such observations are impossible for Herschel in the distant universe without lensing amplification.
### Revealing the most luminous dusty star forming galaxies
Proposal ID: OT1_jvieira_4
Principal Investigator: Joaquin Vieira
Time: 25.6 hours priority 2
Category: High-z galaxies
Summary:
The South Pole Telescope has surveyed 1000 square degrees at millimeter wavelengths down to milli-Jansky levels with the aim of constraining cosmological parameters. One of the most interesting and unanticipated results of this survey was the discovery of a population of high redshift strongly lensed sub-millimeter galaxies (SMGs). The magnification of these objects and the long-wavelength selection makes these source the best window we have to directly investigate massive galaxy formation in the early universe. Here we propose to observe a flux-limited sample of 65 of these sources with PACS and SPIRE for a total of 25.6 hours. These observations will span the peak of the SEDs at all redshifts, determine the redshift distribution and temperatures for these sources, and enable detailed study of molecular and fine structure lines of high-redshift galaxies. These observations are the best method for constraining the properties of the highest redshift SMGs, and we expect to find a minimum of 3 sources at z>5. As these sources are in the southern hemisphere they are ideal targets for ALMA early science observations and will provide an invaluable sample of sources for the community.
### Unveiling the dust mass in the host galaxies of Gamma-Ray Bursts
Proposal ID: OT1_lhunt_2
Principal Investigator: Leslie Hunt
Time: 28.1 hours priority 2
Category: High-z galaxies
Summary:
Gamma-Ray Bursts (GRBs) are so luminous that they can shine through highly obscured galaxies, nearby and in the remote universe. GRBs enable identification of galaxies independently of their luminosity, thus singling out a population that is a potentially powerful probe of galaxy evolution. Only a minority of the host galaxies of GRBs (GRBHs) have been so far detected at sub-millimeter (submm) or mid-infrared (mid-IR) wavelengths; however, in this minority the inferred star-formation rates (SFRs) can be as high as ~500 Msun/year, implying that they are similar to submm galaxies. On the other hand, the frequent non-detections argue against a population dominated by massive and strongly starbursting galaxies. One way to resolve this dilemma would be warm dust. At redshifts 2-4, warm dust (40-50K) would be difficult to detect in the submm bands because its peak would be too blue, and also in the mid-IR, because its peak emission would be far too red. We propose to break this possible dust-temperature redshift "conspiracy" with Herschel PACS+SPIRE photometry of 14 GRBHs with redshifts reaching 4.4. The sample was selected on the basis of prior Spitzer IRAC (or MIPS) detections. We already have in hand a large amount of ancillary multiwavelength data with which we can determine stellar ages and masses. We will construct spectral energy distributions from the UV to the far-IR and use them to derive bolometric luminosities and SFRs, and constrain dust mass, dust temperature, and grain properties. We will compare the dust properties with the stellar component of the galaxies, and analyze the GRBHs in the context of other high-z galaxy populations. Such a program is now possible thanks to the unique ability of Herschel to study dust emission in galaxies over a wide range of redshifts. Ultimately our proposed study of GRBHs will open a new window on the study of galaxy formation and evolution.
### Dissecting the nature of the Planck-HFI high-z blobs
Proposal ID: OT1_lmontier_1
Principal Investigator: Ludovic Montier
Time: 11.6 hours priority 2
Category: High-z galaxies
Summary:
Ultra luminous dusty galaxies radiating most of their energy in the far IR are now known from Spitzer IR and submillimeter observations to dominate the integrated luminosity at redshift 2 to 3. The behavior of this population at higher redshifts remains poorly constrained. This proposal is based on the use of the Planck all sky survey at millimeter and submillimeter wavelengths to find new and rare high-z candidate sources. The limited angular resolution requires a specific data processing to extract good candidates. The Cosmic Infrared Background (CIB) is observed with high signal to noise by Planck after a specific component separation. An algorithm detecting cold spots on the CIB (thus potentially high z dominated) compatible with point sources has been developed. These high z blobs have been shown to be a mixture of different type of objects. Among these, new high z ULIRGS at the high end of the luminosity function or lensed, or high z large scale structures are very interesting for galaxy evolution. We performed comparison of the Planck data with new unidentified sources found by SPT near the upper end of their luminosity function and we detected a few of them. Furthermore, the stacking in Planck of 34 of these SPT sources is easily detected in Planck and gives a typical SED in the Planck bands for these sources. We thus selected sources with this type of SED in the Planck data and produced a list of 10 candidates proposed in this program for observations with SPIRE and PACS. We propose an observation allowing to study the nature of these 10 cold blobs in three cases covering well the possible contributors to this Planck detected high z blobs (single source, cluster of 10 to 20 sources, structure of the cold CIB spot if a small number of sources has not been found). This should be a very interesting contribution to the study of this new emerging population. Furthermore this program should allow us to use best the Planck all sky survey later to find more candidates.
### The Last of the Titans: The Nature of Super-Starbursts at z~1.5
Proposal ID: OT1_mswinban_1
Principal Investigator: Mark Swinbank
Time: 6.7 hours priority 1
Category: High-z galaxies
Summary:
We have recently discovered a population of 'super-starbursts' at z~1-3-1.5. These rare galaxies are selected from the zWiggles spectroscopic survey, and rest-frame UV and H-alpha spectroscopy suggests star-formation rates 100-500Mo/yr. These apparently high-luminosity, but low stellar mass (log(Mstar)~10Mo), gas rich (f_gas~60%) galaxies forming extremely quickly in an extended starburst are suggestive of late time proto-galaxies, but uniquely, are selected from their nebular emission lines. We have obtained three dimensional spectroscopy of 13 galaxies and mapped the two dimensional dynamics on ~kpc scales. The galaxies show extended star-formation on 4--16kpc scales, with dynamics which may resemble rotating systems and clumpy and intense star-formation which may indicate bulge formation. However, the impact of dust obscuration is unknown, and if these galaxies are confirmed as high luminosity ULIRGs, it would argue that these are instead mergers with structures dust, and instead comprise the low-redshift tail of the 'archetypal' high-z ULIRGs and SMGs seen at z~2.3. We propose short Herschel SPIRE observations of this sample of 13 galaxies. We conservatively predict 250um fluxes >12mJy, which should yield detections viable in just ~7mins each. Our total request 6.7 hours.
### The Most Luminous Obscured Galaxies and Quasars Revealed by WISE
Proposal ID: OT1_peisenha_1
Principal Investigator: Peter Eisenhardt
Time: 10.0 hours priority 1 and 20.4 hours priority 2
Summary: High-z galaxies
In the past week, the Wide-field Infrared Survey Explorer (WISE), has completed its first coverage of the entire sky at 3.4, 4.6, 12 and 22 microns (W1, W2, W3, and W4), reaching sensitivities hundreds of times deeper than IRAS. Also in the past week, we have obtained spectroscopy of over 50 WISE sources with unusual colors, including 14 with z > 1.8. Nine of these 14 sources were selected by requiring strong W4 detection combined with insignificant W1 and W2 detection: W1/W2 drops. After rejecting optically bright W1/W2 drops, only 4 sources at z < 1.8 are present. These sources have in excess of 1E13 solar luminosities, and possibly 1E15. We request 64.1 hours of Herschel time to observe a sample of 88 W1/W2 drops, augmented by 5 other WISE sources at z > 1.8, from 70 to 500 microns with PACS and SPIRE. The resulting SEDs will enable us to extend the obscurations, luminosities, and star formation rates associated with ultra-luminous infrared galaxies (ULIRGs) into uncharted terrain.
### A Star formation oasis in the middle of a cluster desert
Proposal ID: OT1_ppopesso_1
Principal Investigator: Paola Popesso
Time: 97.4 hours priority 1
Category: Galaxy clusters/Lensing clusters
Summary:
One of the most fundamental correlations between the properties of galaxies in the local Universe is the so-called morphology-density relation. In the local Universe late type star forming galaxies favor low density regimes and giant ellipticals reside in the cluster cores. Much of the debate centers on whether the relation arises early on during the formation of the object, or whether it is caused by environment-driven evolution. To shed ligth on this issue, we propose to map with PACS at 100 and 160 um the field of 8 clusters in the cluster desert'' at 1.4 < z < 1.8, at the epoch when clusters are accreting galaxies and galaxies are still undergoing their own formation process. Our goal is to observe each system down to log(LIR)=11.5 to observe almost the entire LIRGs and the complete ULIRGs population and to sample the bulk of the star formation. The 8 systems are all X-ray detected, spectroscopically confirmed and with large amount of multi-wavelength ancillary data. The X-ray detection ensures that these are well established, bound structures, which represent the missing link between the protoclusters at z > 2 and the well formed clusters in the local Universe. Our sample spans almost a decade in X-ray luminosity and dynamical mass, comprising relatively young systems and already old and relaxed clusters. This hetereogenity allows us to link the level of star formation activity to the global properties of the systems to shed light on which environmental process, if any, can affect the galaxy star formation activity. All systems are covered by medium-deep and deep XMM and Chandra data, crucial to reveal X-ray faint AGNs, and to study the connection between AGN feedback and star formation activity. The availability of accurate stellar mass estimates allows to relate the SF activity to the environment in different mass bins, thus disentangling the mass- from the environment-driven galaxy evolution.
### Unveiling the nature of strong galaxy activity in an X-ray detected galaxy cluster at z=2.07
Proposal ID: OT1_rgobat_1
Principal Investigator: Raphael Gobat
Time: 17.7 hours priority 1
Category: High-z galaxies
Summary:
We have recently discovered the most distant X-ray luminous galaxy cluster known to date, a z=2.07 strong overdensity of red passively evolving ellipticals with extended X-ray emission seen by XMM-Newton. Several cluster members are detected by MIPS at 24 micron with fluxes above 100 microJy, implying high luminosities in the mid-IR rest frame. If due to star formation activity this would correspond to ULIRG-like luminosities, and would imply a very high degree of forming activity in the cluster core. However, the MIPS detected galaxies have elliptical like morphologies and SEDs, suggesting in turn that the mid-IR emission is due to a huge amount of heavily obscured AGN activity. We propose deep imaging with PACS and SPIRE in the cluster that will clarify the AGN or SF nature of the activity in the cluster. Our results will have important implications on the understanding of the early phases of cluster galaxy assembly. This project will push the study of galaxy activity in established clusters to the highest possible redshifts.
### SPIRE and the formation and evolution of galaxy clusters
Proposal ID: OT1_rhuub_1
Principal Investigator: Hubb Röttgering
Time: 16.7 hours priority 1
Category: Galaxy clusters/Lensing clusters
Summary:
The progenitors of local galaxy clusters ("proto-clusters") are powerful laboratories for tracing the emergence of large scale structure and studying the evolution of galaxies in dense environments.
We propose to use SPIRE's excellent sensitivity and survey speed to obtain, for the first time, a large sample of dust-obscured, star forming, proto-cluster galaxies in an area encompassing the entire proto-cluster and its environment.
The 8 proto-clusters in the sample cover the key redshift range 2 < z < 4 and have a wealth of existing, multi-wavelength data and a large number of spectroscopically confirmed proto-cluster galaxies. The masses of the proto-clusters are typically a few times 10^14 - 10^15 solar masses and the cores are up to 40 times denser than the field.
Matching the SPIRE sources with upcoming LOFAR and EVLA radio observations, we will constrain the photometric redshifts to better than 0.3, resulting in a complete sample of dusty proto-cluster galaxies with very low (<5%) contamination.
The proposed SPIRE observations will be compared to our extensive simulations of forming proto-clusters, allowing us to: (i) unveil and characterize the (dust-obscured) star-forming galaxies in the proto-clusters and constrain their star formations rates and dust temperature; (ii) relate these properties to their optical morphologies, stellar masses and location in the proto-cluster and investigate the differences between proto-cluster galaxies and field galaxies; (iii) ascertain whether red proto-cluster galaxies are passive galaxies or dusty starbursts; (iv) determine the structure and size of the proto-clusters, in particular, distinguish whether galaxies are distributed homogeneously or in filaments; (v) trace the evolution and contraction of large-scale structures from z=4 to z=2.
The proto-cluster targets are ideally located for follow-up spectroscopy and high-resolution imaging with submm observatories such as APEX and ALMA.
### Characterising the ISM of bright, lensed star-forming galaxies across cosmic time with the SPIRE FTS
Proposal ID: OT1_rivison_1
Principal Investigator: Rob Ivison
Time: 94.1 hours priority 1
Category: High-z galaxies
Summary:
We have shown that Herschel is capable of exploring high-redshift galaxies spectroscopically, provided those galaxies are sufficiently bright.
Here, we propose to exploit the wide wavelength coverage of the SPIRE FTS to study the powerful diagnostic rest-frame FIR cooling lines from a unique and complete sample of 25 bright, gravitationally-lensed - but intrinsically typical - submm galaxies (SMGs). We can thus perform the first detailed analysis of their ISM, tracing their density structure and searching for variations in line strengths compared to local counterparts.
Our targets span 1 < z < 3.1 (where [C II] is not accessible to ALMA) and a good range of L(FIR) (12 < log L(FIR) < 13.5), and are selected from panoramic Herschel imaging surveys that are uniquely capable of providing a large, reliable sample at S(350um) > 200mJy, with excellent ancillary data.
We will detect or place sensitive limits on the key atomic cooling lines, e.g. [C II], [O I], [O III], and combine these with ground-based observations of 12CO, 13CO, C I and dense-gas tracers to model their ISM and thence understand their energetics and evolution. Using these data we will:
1) map the evolution of the gas content as a function of redshift, via the sensitivity of [C II]/L(FIR) to M(H2); 2) search for changes in the properties of the star-forming gas as a function of redshift and L(FIR); 3) coadd the spectra in the rest frame to delve up to 5x deeper still, to search for faint lines, e.g. H2O and [O I]145.5, allowing a complete characterisation of the average emission; 4) conclusively address the issue of the contribution of AGN to the immense luminosities of submm galaxies.
Goals 1-3 drive the requirement for a sample of 25 SMGs. All our goals require Herschel and cannot be addressed by other facilities.
We stress that the scientific legacy of ISO and Spitzer has in large part been based on the wealth of data in their spectroscopic archives and the same is likely to be true for Herschel.
### Measuring the PAH emission in a z=6.1 star forming Submillimetre Galaxy
Proposal ID: OT1_schapman_1
Principal Investigator: Scott Chapman
Time: 4.8 hours priority 1
Category: High-z galaxies
Summary:
We have discovered a z=6.1 Submillimetre Galaxy from a detailed survey of 0.5 sq deg in GOODS-N, FLS, and LockmanEast. HDF259 was originally detected by SCUBA and the VLA, but recently constrained through Herschel-SPIRE detections. The redshift is confirmed through a Keck spectroscopic redshift, an optical-near/mid-IR photo-z (as an I-band dropout with a rising stellar bump at 1.6um), and through template fitting with a most likely T_dust in the SPIRE through 1.2mm wavelengths. Even if the optical data incorrect redshift, an extreme range of T_dust secures the redshift as lying from z=4-8.
This SMG represents the first opportunity yet to study the rest-frame 7.7um region PAH features in a z>6 star forming galaxy, using the PACS spectrometer (where the 7.7um strong PAH feature comes into the PACS 51-70um and 70-105um bands only at z>5.9).
The strength of the PAH, estimated both from extrapolated flux measurements from Spitzer-MIPS, and from the z~2 L_IR-L_PAH relation (Pope et al. 2008) ensures that a typical PAH in this SMG will be well detected in 4.8hrs total programme duration.
### THE HERSCHEL-AKARI NEP DEEP SURVEY: the cosmological history of stellar mass assembly and black hole accretion
Proposal ID: OT1_sserje01_1
Principal Investigator: Stephen Serjeant
Time: 73.5 hours priority 2
Category: High-z galaxies
Summary:
We propose a far-IR and submm mapping survey of the premier AKARI deep field in the North Ecliptic Pole, in PACS/SPIRE parallel mode. This is the only major deep infrared field not yet covered by Herschel guaranteed or open time key projects. The outstanding and unparalleled continuous mid-IR photometric coverage from AKARI, far better than equivalent Spitzer surveys, enables a wide range of galaxy evolution diagnostics unachievable in any other survey field (including Herschel HerMES/PEP fields), by spanning the wavelengths of redshifted PAH and silicate features and the peak energy output of AGN dust tori. The investment by AKARI in the NEP represents ~10 percent of the entire pointed observations available throughout the lifetime of AKARI. Our proposal remedies the remarkable omission from Herschel's legacy surveys of the premier extragalactic deep field from another IR space telescope.
We will simultaneously identify and find photometric redshifts for the Herschel point source population, make stacking analysis detections of the galaxies which dominate the submm extragalactic background light as a function of redshift, determine the bolometric power outputs of the galaxies that dominate the submm background, compare the UV/optical/mid-IR continuum/PAH/far-IR/submm/radio star formation rate estimator in the most comprehensive IR survey data set to date, and track the coupled stellar mass assembly and black hole accretion throughout most of the history of the Universe.
### Dust in the wind: the role of dust in ram-pressure stripped gas and intracluster star formation
Proposal ID: OT1_ssivanan_1
Principal Investigator: Suresh Sivanandam
Time: 10.4 hours priority 1
Category: Galaxy clusters/Lensing clusters
Summary:
We propose to detect dust associated with ram-pressure stripping through deep Herschel PACS/SPIRE imaging of a carefully chosen set of cluster galaxies that show strong signs of on-going stripping and intracluster star formation. Several lines of evidence, such as the existence of cold molecular gas and intracluster star formation in ram-pressure stripped tails, strongly point towards the existence of dust in these tails. Herschel is the only telescope that has the sensitivity to detect the emission from dust blown out into the intracluster medium (ICM). With our proposed observations we aim to: 1. quantify the temperature, mass, and lifetime of dust blown out into the ICM; 2. understand the role dust plays in the existence of molecular hydrogen in the ICM and intracluster star formation. Our program will carry out deep Herschel observations of five galaxies in high pressure environments with highly extended (~20-80 kpc) multi-phase gaseous tails. The Herschel observations will expand our already large multi-wavelength dataset and finally provide complete inventory of the gas and dust associated with ram-pressure stripping. This will provide a more complete picture of the impact of ram-pressure on galaxy evolution.
### Cold Gas and Dust in the Filamentary Complexes of Cluster Cooling Flows
Proposal ID: OT1_sveilleu_1
Principal Investigator: Sylvain Veilleux
Time: 7 hours priority 1
Category: Galaxy clusters/Lensing clusters
Summary:
We propose to obtain deep PACS + SPIRE far-IR photometry and 2D PACS [C II] 158 um spectroscopy of 7 cooling-flow clusters with extended Halpha filaments to constrain the properties of the dust and cooling gas in these systems. Our targets are part of a large sample of clusters that were imaged at Halpha using the Maryland Magellan Tunable Filter (MMTF) as part of a comprehensive multiwavelength survey. The superb sensitivity and resolution of the MMTF data have uncovered, often for the very first time, spectacular filaments of warm ionized gas extending as far as 50 kpc from the cluster core. The origin and heating source of these filaments remains a mystery. Our MMTF images have served as a guide to extract on-filament X-ray and optical spectra for a large sample of clusters, leading to the discovery that the X-ray ICM is cooling at a highly accelerated rate in the vicinity of these filaments. This direct link between the warm and hot phases may be the first direct evidence for the purported cooling flow. Given the high FIR fluxes detected in cluster cores, it is possible that dust grain cooling plays an important role in the cooling flow process. However, it remains unclear whether the observed dust is associated with the warm filaments or limited to the center of the brightest cluster galaxy (BCG). Current key programs cannot address this question given their lack of information on the Halpha filaments. Our proposed Herschel observations of the 7 cooling-flows clusters from our sample with the most extended Halpha filaments will directly address this question and help us determine: a) the role of dust cooling in the cooling-flow process, b) whether the observed dust is associated with the BCG or the warm filaments, and c) whether gas is cooling below 10^4 K, the temperature probed by Halpha. Providing answers to these questions will improve our understanding of the cooling processes in galaxy clusters and constrain the role of heating processes, such as AGN feedback, in preventing such cooling.
### A deep PACS survey of AKARI-Deep field south: Revealing the connection between AGN and star formation
Proposal ID: OT1_ttakagi_1
Principal Investigator: Toshinobu Takagi
Time: 34.5 hours priority 1
Category: High-z galaxies
Summary:
We propose a deep PACS imaging survey of a prestigious far-IR survey field, AKARI-Deep field south, which has the lowest cirrus background in the sky and has been observed with most of the major IR and submm telescopes, such as AKARI, Spitzer/MIPS, BLAST and Herschel/HerMES, covering 7-12 deg^2. We also conducted one of the widest and deepest millimetre survey using ASTE/AzTEC within this field, covering 0.25 deg^2. Although there are many (sub)mm survey fields in different parts of the sky, ADF-S has a unique data set from AKARI/IRC at 2.4, 3.2, 4.1, 7, 11, 15 micron, i.e. filling the wavelength gap between Spitzer/IRAC 8 micron and MIPS 24 micron. We utilize this comprehensive mid-IR coverage to identify obscured AGNs and derive the bolometric AGN luminosity, based on the type-independent X-ray-to-mid-IR luminosity relation. PACS photometry is necessary to derive accurate star formation rate (SFR) in starburst-AGN composite system. We investigate the relative importance of AGN in SMGs and other mid-IR selected ULIRGs, as a function of SFR, stellar mass, and redshift. Ultimately, we will determine the role of AGN in galaxy formation and the regulation mechanism for co-evolution of stellar mass assembly and central black hole. Also, deep PACS images allow us to identify millimeter-selected SMGs at very high redshifts, which will be prime targets of ALMA.
| 2015-04-25T21:44:09 |
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https://www.r-bloggers.com/2019/10/five-levels-of-analytical-automation/
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[This article was first published on R – Dataviz – Stats – Bayes, and kindly contributed to R-bloggers]. (You can report issue about the content on this page here)
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I have been thinking more about how programming that requires minimal human input is a virtue in computer science, and hence machine learning, circles. Although there’s no doubt that is one of the central goals of programming a computer in general, I’m not convinced this extends to data analysis, which needs some thought, contextual knowledge and curation. The contextual knowledge can be broken down further into understanding where the data came from and its weaknesses, what question we are really trying to answer, and where the findings are going: the statistical literacy of the audience and how their decisions should be influenced by the findings.
Let’s imagine a sliding scale of code autonomy. At one end is work that requires humans to do everything, most typically by operating a point-and-click graphical user interface (GUI) such as many users of Tableau, SPSS, etc are familiar with. That is completely non-reproducible in the sense that it can only be reproduced if you have a willing and suitably informed human to do it, and I think that makes it an island off the end of the sliding scale. Let’s note it and then restrict consideration to data analysis that is coded in some way so that the machine can re-run at least part of it without human intervention.
There’s no question that this is a good idea. You should be able to show where your results came from (an audit trail). Also, it’s very common to reach what you think is the end of the analysis only to be asked to run it again on some corrected or extended data; being able to just replace the data file and press Go is a huge time saver, and helps avoid typos.
But just how far down the scale do you need to go? I suggest five levels along the way to complete autonomy; let’s look at each in turn with a simple example. I use R here but the same ideas translate to every software tool and language.
### Level one:
• hard-coded results mean it won’t give different answers with new data
• it doesn’t look for changes in the size of the input data
• it doesn’t check for violations of data assumptions
• it doesn’t take arguments to control algorithm parameters, random number generator (RNG) seeds, or outputs such as file names or graphics captions
mydata <- read.csv("datafile.csv") myregression <- lm(outcome ~ riskfactor + confounder, data=mydata) prediction <- 0.213 + 0.918*mydata$riskfactor + 0.301*mydata$confounder png("results.png") plot(mydata$riskfactor, mydata$outcome, main="Regression findings") points(mydata$riskfactor, prediction, pch=19) dev.off() Even if you don’t know R, you can see that this reads in a CSV file with a certain name, runs a linear regression using some particular variables in the data (“outcome”, “riskfactor” and “confounder” — economically-trained readers might prefer to think of “confounder” as “endogenous_variable”), calculates predicted values of the outcome variable by hard-coding in the regression coefficients (presumably, after running the lm() line, the analyst printed the summary(myregression) and looked at the coefficients before typing them in), and then makes a plot of the observed and predicted values with a certain title, storing that in a PNG file with a certain name. This is all fine for giving an audit trail. You could re-run this on the same data and get the same results, and with some effort, you could go through and change options and see how that affects the results (for example, you could include an interaction term between “riskfactor” and “confounder”). I say “with some effort”, because you’d have to change the lm() line and the prediction line, and to avoid confusion, you’d probably want to add a caption to the plot too. When the boss calls you up and tells you that – “great news” – they found some more data and want to re-run the analysis, you’d have saved some time over using a GUI, but you’d still have to make some amendments to the code, and that would cost you time, plus the risk of typos. Let’s say that takes half a day to amend, run and check. The boss is satisfied, unless you made a typo and have to retract it later, in which case they are definitely not satisfied. ### Level two: • fix the hard-coding This is low-hanging fruit, really. In the case of regression coefficients, nobody would write the prediction line because you could just have: prediction <- predict(myregression) and that would take care of any changes to the lm() formula or the data. But in more complex settings, you might want to get the coefficients (or equivalents for other analyses) and calculate something a bit more bespoke from them. You should really do this by pulling out the relevant values returned by the regression function. In R, Python or Julia, most functions like this return a list (or whatever they call it) of all sorts of scalars, vectors, matrices and strings, and in there is something you need. In Stata, which I use a lot, such things go into the r() or e() lists of macros and you can copy them from there before the next estimation command replaces them. Other software might not provide flexible return values like that; if so, that software is not going to be helpful for reproducible and semi-autonomous analysis. mycoef <- myregression$coefficients prediction <- mycoef[1] + mycoef[2]*mydata$riskfactor + mycoef[3]*mydata$confounder
You can get more smart-ass about it, but the principle is clear.
prediction <- mycoef * model.matrix(model.frame(~riskfactor+confounder, data=mydata))
And the same thing applies to any hard-coding.
### Level three:
• examine and respond to the size of the input data; what if there are suddenly more variables than before?
It’s generally not an issue if the number of observations (rows) changes, but you ought to watch out for future situations where you need to add an extra column. Here, the balance of cost and benefit starts to become contested. If you are going to add a new predictor to a linear regression, you’d better check for missing data, multicollinearity and such before you proceed. So, is it better to allow a regression with unspecified inputs or to force the user to stop and think? On the other hand, some analytical methods can handle all sorts of inputs, and you might feel more relaxed about them (notably, those that get used in autoML are like this: random forests and boosted trees do well with minimal data processing, while regressions, artificial neural networks and clustering are sensitive to the transformations and filtering of the input data that, in the ML world, they call feature engineering; perhaps tellingly, I see very little unsupervised learning in autoML products for this reason).
In reality, coding up analysis that’s flexible to columns can be quite hard work. There’s often some kind of syntactical structure that requires you to type out all the constituent parts, like those formulas in R or layering of twoway graphs in Stata. If you can supply a matrix instead, you’re going to have more flexibility straight away. It might be worth looking for a different package / library / command that can do what you want with the right kind of input.
### Level four:
• check for violations of data assumptions
Who said the data supplied would always be numeric? Or factors? Or ISO8601 dates and times? The fact you’ve only received strings “Yes” and “No” in a variable so far does not mean some buffoon isn’t about to start typing “n”, “y”, “yup”, or even “see notes”. You better check for that and halt the process if you find departures from your assumptions. Remember to write nice, informative error messages for yourself, and others in the future. Every programming language (Ok, maybe not those weird ones) has functionality to check some logical comparison and halt with an error message if the check fails.
### Level five:
• make it a function / command / subroutine / macro that receives arguments
To give yourself (or others) real flexibility in re-running this analysis, but on different data, and with somewhat different settings, you need one function that takes the data and the settings as inputs, and returns the results. It might look like this:
runanalysis(data_file="Nov2016.csv", outcome_column=3, predictor_columns=c(5,7,8), gamma=0.3, test_sample=0.2, iterations=1000, log_file="week_31_run.txt", image_folder="week_31_images/", regression_option="glmnet")
I leave the precise meaning to your imagination. The point is, you can try out a range of different settings by looping over different values of those arguments. You can run different versions of runanalysis() on different CPU cores, or groups of cores, or virtual machines. You can plug in new data, or new settings.
Finally – and I think this is very cool because I’m interested in how we communicate our work to non-quants – you can make a GUI for your new function. R has some nice tools for this and there’s a book too.
Note that any of these levels can be automated to run at scheduled intervals, looking for new data at a certain location (they’re not limited to CSV files, they might query databases or other APIs), or they could periodically check for the appearance of a new data file and run when they find it (when the data collection team drop it into the folder ready for analysis). That’s an important part of automation but actually not the same dimension as this scale of code autonomy, I think.
Having reached level five, you can now go in two ways for near-complete autonomy, and they’re not mutually exclusive.
One is to build a package that contains code like this for a whole suite of relevant analyses that your organisation uses, so that you can specify what data to use, what the variables of interest are, what algorithms to use (you might want to run a GAM, regression tree, and random forest, for example), where to store the results, which of the organisation style templates to use for the text and tabular outputs, and lists of algorithm-specific tuning parameters. There might be a top-level function that calls one of the underlying runanalysis() functions. Or one overarching GUI (and at that point, you’ve come close to developing your own statistics software; you might even consider trying to sell it).
Another is to take an autoML approach, where you have your code run a variety of different analyses and select one on the basis of some performance metrics. If this interests you, watch out for my series of test drives of cloud analysis front-ends, coming to this blog soon.
Tikal temple five, photo by Arian Zwegers. CC-BY-2.0. flickr.com/photos/azwegers/15339110573
| 2021-07-24T01:25:47 |
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http://dergipark.gov.tr/gujs/issue/37206/318604
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## A New Method for Generating Initial Solutions of Capacitated Vehicle Routing Problems
#### Kenan KARAGÜL [1] , Michael G. KAY [2] , Sezai TOKAT [3]
##### 94 110
In vehicle routing problems, the initial solutions of the routes are important for improving the quality and solution time of the algorithm. For a better route construction algorithm, the obtained initial solutions must be basic, fast, and flexible with reasonable accuracy. In this study, initial solutions improvement for CVRP is introduced based on a method that is introduced in the literature. Using a different formula for addressing the gravitational forces, a new method is introduced and compared with the previous physics inspired algorithm. By using the initial solutions of the proposed method and using them as RTR and SA initial routes, it is seen that better results are obtained when compared with various algorithms from the literature. Also, in order to fairly compare the algorithms executed on different machines, a new comparison scale for the solution quality of vehicle routing problems is proposed that depends on the solution time and the deviation from the best known solution. The obtained initial solutions are then input to Record-to-Record and Simulated Annealing algorithms to obtain final solutions. Various test instances and CVRP solutions from the literature are used for comparison. The comparisons with the proposed method have shown promising results.
Constructive Routing Heuristics, Vehicle Routing Problem, Initial Routing Solutions, Physics-Inspired Optimization, Capacitated Vehicle Routing Problem
• Baker, B. M., & Ayechew, M. (2003). Agenetic algorithm for the vehicle routing problem. Computers & Operations Research, 787 – 800.
• Battarra, M., Benedettini, S., & Roli, A. (2011). Additional Material for “Leveraging saving-based algorithms by master-slave genetic algorithms”. Engineering Applications of Artificial Intelligence, Appendix A. Supplementary data.
• Battarra, M., Benedettini, S., & Roli, A. (2011). Leveraging saving-based algorithms by master–slave genetic algorithms. Engineering Applications of Artificial Intelligence, 555-566.
• Chatterjee, A., Mahanti, G. K., & Pathak, N. (2010). Comparative Performance of Gravitaional Search Algorithm and Modified Particle Swarm Optimization Algorithm for Synthesis of Thinned Scanned Concentric Ring Array Antenna. Progress In Electromagnetics Research B, 331–348.
• Cordeau, J.-F., Gendreau, M., Laporte, G., Potvin, J.-Y., & Semet, F. (2002). A guide to vehicle routingheuristics. Journal of the Operational Research Society, 512-522.
• Ding, D., Qi, D., Luo, X., Chen, J., Wang, X., & Du, P. (2012). Convergence analysis and performance of an extended central force optimization algorithm. Applied Mathematics and Computation, 2246–2259.
• Duman, S., Güvenç, U., & Yörükeren, N. (2010). Gravitational Search Algorithm for Economic Dispatch with Valve-Point Effects. International Review of Electrical Engineering, 2890-2895.
• Formato, R. A. (2007). Central Force Optimization: A New Metaheuristic with Applications in Applied Electromagnetism. Progress In Electromagnetics Research, 425-491.
• Groer, C. (2015, 5 5). VRPH. Retrieved from COIN-OR Home: http://www.coin-or.org/projects/VRPH.xml
• Groer, C., & Golden, B. (2015, 5 5). Parallel and Serial Algorithms for Vehicle Routing Problems. Retrieved from UMD, PhD Thesis, 2008: http://drum.lib.umd.edu/bitstream/1903/9011/1/Groer_umd_0117E_10068.pdf
Konular Fen Computer Engineering Yazar: Kenan KARAGÜLÜlke: Turkey Yazar: Michael G. KAYÜlke: United States Yazar: Sezai TOKATÜlke: Turkey
Bibtex @araştırma makalesi { gujs318604, journal = {Gazi University Journal of Science}, issn = {}, eissn = {2147-1762}, address = {Gazi Üniversitesi}, year = {}, volume = {31}, pages = {489 - 513}, doi = {}, title = {A New Method for Generating Initial Solutions of Capacitated Vehicle Routing Problems}, key = {cite}, author = {TOKAT, Sezai and KAY, Michael G. and KARAGÜL, Kenan} } APA KARAGÜL, K , KAY, M , TOKAT, S . (). A New Method for Generating Initial Solutions of Capacitated Vehicle Routing Problems. Gazi University Journal of Science, 31 (2), 489-513. Retrieved from http://dergipark.gov.tr/gujs/issue/37206/318604 MLA KARAGÜL, K , KAY, M , TOKAT, S . "A New Method for Generating Initial Solutions of Capacitated Vehicle Routing Problems". Gazi University Journal of Science 31 (): 489-513 Chicago KARAGÜL, K , KAY, M , TOKAT, S . "A New Method for Generating Initial Solutions of Capacitated Vehicle Routing Problems". Gazi University Journal of Science 31 (): 489-513 RIS TY - JOUR T1 - A New Method for Generating Initial Solutions of Capacitated Vehicle Routing Problems AU - Kenan KARAGÜL , Michael G. KAY , Sezai TOKAT Y1 - 2018 PY - 2018 N1 - DO - T2 - Gazi University Journal of Science JF - Journal JO - JOR SP - 489 EP - 513 VL - 31 IS - 2 SN - -2147-1762 M3 - UR - Y2 - 2018 ER - EndNote %0 Gazi University Journal of Science A New Method for Generating Initial Solutions of Capacitated Vehicle Routing Problems %A Kenan KARAGÜL , Michael G. KAY , Sezai TOKAT %T A New Method for Generating Initial Solutions of Capacitated Vehicle Routing Problems %D 2018 %J Gazi University Journal of Science %P -2147-1762 %V 31 %N 2 %R %U ISNAD KARAGÜL, Kenan , KAY, Michael G. , TOKAT, Sezai . "A New Method for Generating Initial Solutions of Capacitated Vehicle Routing Problems". Gazi University Journal of Science 31 / 2 489-513.
| 2018-12-12T16:28:16 |
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https://www.khronos.org/registry/vulkan/specs/1.2-extensions/man/html/VkQueue.html
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## C Specification
Creating a logical device also creates the queues associated with that device. The queues to create are described by a set of VkDeviceQueueCreateInfo structures that are passed to vkCreateDevice in pQueueCreateInfos.
Queues are represented by VkQueue handles:
// Provided by VK_VERSION_1_0
VK_DEFINE_HANDLE(VkQueue)
## Document Notes
For more information, see the Vulkan Specification
This page is extracted from the Vulkan Specification. Fixes and changes should be made to the Specification, not directly.
Copyright 2014-2021 The Khronos Group Inc.
SPDX-License-Identifier: CC-BY-4.0
| 2021-04-19T00:50:22 |
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https://wiki.bnl.gov/TECHQM/index.php?title=Partonic_Energy_Loss
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# Work Plan of the Hard Physics Working Group
The Hard Physics Working Group has decided to focus initially on the following problems:
# Purpose and Formulation of the QGP Brick Problem
In the recent past, several individual research groups arrived at apparently satisfactory descriptions of the nuclear modification factor by modeling jet quenching with one or only a few model parameters. Despite these individual successes, quantitative conclusions about the properties of the matter produced in heavy ion collisions have remained unclear so far. In particular, different groups arrived at phenomenologically successful descriptions by quoting values for the jet transport parameter, which differ by as much as an order of magnitude.
The different research groups in the Hard Physics working group have agreed to perform a set of simplified benchmark calculations. The aim of this exercise is to arrive at a common standard for comparing different models of jet quenching. This will clarify the origin of the large numerical discrepancies between different groups, thus providing a basis for quantitative conclusions.
The first problem is the “static QGP brick” problem, which will be completed within the coming months.
• Input Consider a brick of QGP without any time-evolution (static case). Consider a quark of 10 and a quark of 100 GeV energy, produced in the brick. The parton propagates over a length of either L=2 fm or L = 5 fm through this medium. If possible, choose a fixed coupling constant alpha_s = 0.3, to ease comparison. [If not possible, specify fully the choice of your running coupling constant.] The virtuality of the initial parton should be Q=E.
• Task 1 Plot in your model the probability distribution P(\Delta E) for the value of model parameters, for which the fraction of the average energy loss <\Delta E>/E is equal to 0.05, 0.1, 0.2, 0.4.
• Task 2 Specify for the above calculation the relation of your model parameters to the temperature of medium.
• Task 3 Plot for each probability distribution P(\Delta E) the corresponding single inclusive gluon energy distribution [or, alternatively, the primary distribution from which P(\Delta E) was calculated
Proposal (Berndt Mueller):
I propose that we expand the brick problem effort to permit parton cascade codes to participate.
There are currently at least 4 different codes in which the energy loss dE/dx in a thermal gluon bath can be calculated: MPC (Molnar), VNI/BMS (Bass et al), Ghi Shin's code, and the code written by Xu and Greiner. A first plot of dE/dx as a function of parton energy has been published by the last group in arXiv:0806.1169 [1].
# Brick Results
The results of different groups for the Brick Problem are given here:
• GLV
• WHDG
• GLV-WMC: (D)GLV to High Orders in Opacity, ${\displaystyle \scriptstyle {1\,\leq \,n\,\leq \,9}}$
• AMY
• Higher-Twist
• YaJEM
• ASW
Output format for the computed energy loss distributions.
Comparison of the ASW/BDMPS and WHDG/GLV brick results
Proposed common definition of qhat, lambda and mu as a function of T.
# PCM Brick Results
The results of different groups on the Parton Cascade Model Brick result are given here:
APC = Andong Parton Cascade - nucl-th/0207041
# TECHQM Notes and Discussion Forum
The password-protected area for TECHQM Notes and discussion is here.
Public notes:
| 2022-08-12T05:57:59 |
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https://zbmath.org/authors/?q=ai:smale.steve
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# zbMATH — the first resource for mathematics
## Smale, Steve
Compute Distance To:
Author ID: smale.steve Published as: Smale, S.; Smale, Stephan; Smale, Stephen; Smale, Steve; Smale, Steven Homepage: http://ttic.uchicago.edu/~smale/vita.html External Links: MGP · Math-Net.Ru · Wikidata · dblp · GND · MacTutor Awards: Fields Medal (1966) · Wolf Prize (2007)
Documents Indexed: 157 Publications since 1957, including 11 Books Biographic References: 19 Publications
all top 5
#### Co-Authors
88 single-authored 19 Shub, Michael 12 Cucker, Felipe 10 Zhou, Dingxuan 6 Blum, Lenore 5 Hirsch, Morris W. 3 Chern, Shiing-Shen 3 Jetter, Kurt 3 Niyogi, Partha 3 Poggio, Tomaso A. 3 Rajapakse, Indika 3 Weinberger, Shmuel 2 Caponnetto, Andrea 2 Devaney, Robert L. 2 Lashof, Richard K. 2 Smale, Nathan 1 Abraham, Ralph Herman 1 Bartholdi, Laurent 1 Berry, Michael Victor 1 Bouvrie, Jake 1 Christmann, Andreas 1 Dedieu, Jean-Pierre 1 Guo, Xin 1 Gurdian, Rodolfo 1 Jaffe, Arthur Michael 1 Khesin, Boris A. 1 Khovanskiĭ, Askold Georgievich 1 Koiran, Pascal 1 Mumford, David Bryant 1 Palais, Richard S. 1 Palis, Jacob jun. 1 Renegar, James 1 Rosasco, Lorenzo A. 1 Schick, Thomas 1 Sevryuk, Mikhail Borisovich 1 Shen, Wenjun 1 Tabachnikov, Serge L. 1 Tu, Loring W. 1 Varchenko, Alexander Nikolaevich 1 Williams, Robert F. 1 Wong, Hau-San 1 Xiao, Quanwu 1 Yao, Yuan 1 Yau, Shing-Tung 1 Zhou, Ding-Xuan
all top 5
#### Serials
8 Annals of Mathematics. Second Series 8 Foundations of Computational Mathematics 7 Journal of Mathematical Economics 6 Bulletin of the American Mathematical Society. New Series 4 American Journal of Mathematics 4 Journal of Complexity 4 Analysis and Applications (Singapore) 4 Bulletin of the American Mathematical Society 3 Uspekhi Matematicheskikh Nauk [N. S.] 3 The Mathematical Intelligencer 3 Proceedings of the American Mathematical Society 3 Notices of the American Mathematical Society 3 Oberwolfach Reports 3 Proceedings of Symposia in Pure Mathematics 2 Journal of Mathematical Biology 2 Inventiones Mathematicae 2 SIAM Journal on Computing 2 Theoretical Computer Science 2 Transactions of the American Mathematical Society 2 Constructive Approximation 2 International Journal of Bifurcation and Chaos in Applied Sciences and Engineering 2 Journal of Mathematics and Mechanics 1 American Mathematical Monthly 1 Communications on Pure and Applied Mathematics 1 Mitteilungen der Deutschen Mathematiker-Vereinigung (DMV) 1 Annales Scientifiques de l’École Normale Supérieure. Quatrième Série 1 Boletín de la Sociedad Matemática Mexicana. Segunda Serie 1 Commentarii Mathematici Helvetici 1 Duke Mathematical Journal 1 Econometrica 1 Gazette des Mathématiciens 1 IEEE Transactions on Automatic Control 1 Journal of Differential Geometry 1 Mathematical Programming 1 SIAM Journal on Numerical Analysis 1 Synthese 1 Physica D 1 Journal of Symbolic Computation 1 Discrete & Computational Geometry 1 Journal of the American Mathematical Society 1 Proceedings of the National Academy of Sciences of the United States of America 1 SIAM Review 1 Applied and Computational Harmonic Analysis 1 Journal of the ACM 1 La Gaceta de la Real Sociedad Matemática Española 1 Annali della Scuola Normale Superiore di Pisa. Scienze Fisiche e Matematiche. III. Ser 1 Mathematical Medley 1 Japanese Journal of Mathematics. 3rd Series
all top 5
#### Fields
43 Computer science (68-XX) 28 Dynamical systems and ergodic theory (37-XX) 24 Numerical analysis (65-XX) 19 Game theory, economics, finance, and other social and behavioral sciences (91-XX) 15 History and biography (01-XX) 14 Global analysis, analysis on manifolds (58-XX) 14 Statistics (62-XX) 13 Functions of a complex variable (30-XX) 13 Manifolds and cell complexes (57-XX) 9 General and overarching topics; collections (00-XX) 9 Operations research, mathematical programming (90-XX) 9 Biology and other natural sciences (92-XX) 8 Field theory and polynomials (12-XX) 8 Ordinary differential equations (34-XX) 8 Approximations and expansions (41-XX) 5 Mathematical logic and foundations (03-XX) 5 Mechanics of particles and systems (70-XX) 4 Partial differential equations (35-XX) 4 Probability theory and stochastic processes (60-XX) 4 Information and communication theory, circuits (94-XX) 3 Number theory (11-XX) 3 Real functions (26-XX) 3 Harmonic analysis on Euclidean spaces (42-XX) 2 Functional analysis (46-XX) 2 Algebraic topology (55-XX) 1 Algebraic geometry (14-XX) 1 Operator theory (47-XX) 1 Convex and discrete geometry (52-XX) 1 Systems theory; control (93-XX)
#### Citations contained in zbMATH Open
136 Publications have been cited 8,389 times in 6,188 Documents Cited by Year
Differentiable dynamical systems. With an appendix to the first part of the paper: “Anosov diffeomorphisms” by John Mather. Zbl 0202.55202
Smale, S.
1967
Differential equations, dynamical systems, and linear algebra. Zbl 0309.34001
Hirsch, Morris W.; Smale, Stephen
1974
Emergent behavior in flocks. Zbl 1366.91116
Cucker, Felipe; Smale, Steve
2007
On the mathematical foundations of learning. Zbl 0983.68162
Cucker, Felipe; Smale, Steve
2002
Mathematical problems for the next century. Zbl 0947.01011
Smale, Steve
1998
On a theory of computation and complexity over the real numbers: NP- completeness, recursive functions and universal machines. Zbl 0681.03020
Blum, Lenore; Shub, Mike; Smale, Steve
1989
Complexity and real computation: A manifesto. Zbl 0872.68036
Blum, Lenore; Cucker, Felipe; Shub, Mike; Smale, Steve
1996
An infinite dimensional version of Sard’s theorem. Zbl 0143.35301
Smale, S.
1965
Learning theory estimates via integral operators and their approximations. Zbl 1127.68088
Smale, Steve; Zhou, Ding-Xuan
2007
Topology and mechanics. II: The planar $$n$$-body problem. Zbl 0203.26102
Smale, S.
1970
The fundamental theorem of algebra and complexity theory. Zbl 0456.12012
Smale, Steve
1981
Diffeomorphisms with many periodic points. Zbl 0142.41103
Smale, S.
1965
Differential equations, dynamical systems, and an introduction to chaos. 2nd ed. Zbl 1135.37002
Hirsch, Morris W.; Smale, Stephen; Devaney, Robert L.
2004
On the mathematics of emergence. Zbl 1166.92323
Cucker, Felipe; Smale, Steve
2007
Topology and mechanics. I. Zbl 0202.23201
Smale, S.
1970
Generalized Poincaré’s conjecture in dimensions greater than four. Zbl 0099.39202
Smale, Stephen
1961
Structural stability theorems. Zbl 0214.50702
Palis, J.; Smale, S.
1970
A convergent process of price adjustment and global Newton methods. Zbl 0354.90018
Smale, Steve
1976
On the efficiency of algorithms of analysis. Zbl 0592.65032
Smale, Steve
1985
Finding the homology of submanifolds with high confidence from random samples. Zbl 1148.68048
Niyogi, Partha; Smale, Stephen; Weinberger, Shmuel
2008
Complexity of Bezout’s theorem. I: Geometric aspects. Zbl 0821.65035
Shub, Michael; Smale, Steve
1993
Shannon sampling and function reconstruction from point values. Zbl 1107.94007
Smale, Steve; Zhou, Ding-Xuan
2004
On the structure of manifolds. Zbl 0109.41103
Smale, S.
1962
A generalized Morse theory. Zbl 0119.09201
Palais, R. S.; Smale, S.
1964
Diffeomorphisms of the 2-sphere. Zbl 0118.39103
Smale, S.
1959
On gradient dynamical systems. Zbl 0136.43702
Smale, S.
1961
Estimating the approximation error in learning theory. Zbl 1079.68089
Smale, Steve; Zhou, Ding-Xuan
2003
The classification of immersions of spheres in Euclidean spaces. Zbl 0089.18201
Smale, Stephen
1959
Complexity of Bezout’s theorem. II: Volumes and probabilities. Zbl 0851.65031
Shub, M.; Smale, S.
1993
Shannon sampling. II: Connections to learning theory. Zbl 1107.94008
Smale, Steve; Zhou, Ding-Xuan
2005
Best choices for regularization parameters in learning theory: on the bias-variance problem. Zbl 1057.68085
Cucker, Felipe; Smale, Steve
2002
Newton’s method estimates from data at one point. Zbl 0613.65058
Smale, Steve
1986
On the differential equations of species in competition. Zbl 0344.92009
Smale, S.
1976
Complexity of Bezout’s theorem. IV: Probability of success; extensions. Zbl 0843.65035
Shub, Michael; Smale, Steve
1996
Differential equations, dynamical systems, and an introduction to chaos. 3rd ed. Zbl 1239.37001
Hirsch, Morris W.; Smale, Stephen; Devaney, Robert L.
2013
Online learning with Markov sampling. Zbl 1170.68022
Smale, Steve; Zhou, Ding-Xuan
2009
Complexity of Bezout’s theorem. III: Condition number and packing. Zbl 0846.65018
Shub, Michael; Smale, Steve
1993
Morse inequalities for a dynamical system. Zbl 0100.29701
Smale, Stephen
1960
Mathematical problems for the next century. Zbl 1031.00005
Smale, Steve
2000
On the structure of 5-manifolds. Zbl 0101.16103
Smale, Stephen
1962
Complexity of Bezout’s theorem. V: Polynomial time. Zbl 0846.65022
Shub, M.; Smale, S.
1994
Complexity and real computation. Foreword by Richard M. Karp. Zbl 0948.68068
Blum, Leonore; Cucker, Felipe; Shub, Michael; Smale, Steve
1997
The mathematics of learning: dealing with data. Zbl 1083.68100
Poggio, Tomaso; Smale, Steve
2003
On the Morse index theorem. Zbl 0166.36102
Smale, S.
1965
On the average number of steps of the simplex method of linear programming. Zbl 0526.90060
Smale, Steve
1983
The mathematics of time. Essays on dynamical systems, economic processes, and related topics. Zbl 0451.58001
Smale, Steve
1980
Global analysis and economics. II: Extension of a theorem of Debreu. Zbl 0316.90006
Smale, S.
1974
Stable manifolds for differential equations and diffeomorphisms. Zbl 0113.29702
Smale, S.
1963
Morse theory and a non-linear generalization of the Dirichlet problem. Zbl 0131.32305
Smale, S.
1964
Complexity theory and numerical analysis. Zbl 0883.65125
Smale, Steve
1997
A Vietoris mapping theorem for homotopy. Zbl 0089.39003
Smale, Stephen
1957
On algorithms for solving f(x)=0. Zbl 0408.65032
Hirsch, Morris W.; Smale, Stephen
1979
Global analysis and economics. VI: Geometric analysis of Pareto optima and price equilibria under classical hypotheses. Zbl 0348.90017
Smale, S.
1976
Global analysis and economics. V: Pareto theory with constraints. Zbl 0357.90010
Smale, S.
1974
Structurally stable systems are not dense. Zbl 0149.20001
Smale, S.
1966
The prisoner’s dilemma and dynamical systems associated to non- cooperative games. Zbl 0463.90099
Smale, Steve
1980
Global analysis and economics. I: Pareto optimum and a generalization of Morse theory. Zbl 0269.58009
Smale, Steve
1973
On the mathematical foundations of electrical circuit theory. Zbl 0286.34071
Smale, S.
1972
Algorithms for solving equations. Zbl 0665.65058
Smale, Steve
1987
Computational complexity: On the geometry of polynomials and a theory of cost. II. Zbl 0625.65036
Shub, M.; Smale, S.
1986
A topological view of unsupervised learning from noisy data. Zbl 1230.62085
Niyogi, P.; Smale, S.; Weinberger, S.
2011
Online learning algorithms. Zbl 1119.68098
Smale, Steve; Yao, Yuan
2006
Dynamics retrospective: Great problems, attempts that failed. Zbl 0745.58018
Smale, Steve
1991
On the geometry of polynomials and a theory of cost. I. Zbl 0603.65027
Shub, Mike; Smale, Steve
1985
Global analysis and economics. III: Pareto Optima and price equilibria. Zbl 0316.90007
Smale, S.
1974
Nongenericity of $$\Omega$$-stability. Zbl 0215.25102
Abraham, R.; Smale, S.
1970
On the topology of algorithms. I. Zbl 0639.68042
Smale, Steve
1987
On the existence of generally convergent algorithms. Zbl 0595.65048
Shub, Michael; Smale, Steve
1986
Global analysis and economics. IV: Finiteness and stability of equilibria with general consumption sets and production. Zbl 0316.90008
Smale, S.
1974
Notes on differentiable dynamical systems. Zbl 0205.54201
Smale, S.
1970
Regular curves on Riemannian manifolds. Zbl 0081.38103
Smale, Stephen
1958
A mathematical model of two cells via Turing’s equation. Zbl 0333.92002
Smale, S.
1974
A classification of immersions of the two-sphere. Zbl 0089.18102
Smale, Stephen
1959
Geometry on probability spaces. Zbl 1187.68270
Smale, Steve; Zhou, Ding-Xuan
2009
On the immersion of manifolds in Euclidean space. Zbl 0097.38805
Lashof, R.; Smale, S.
1958
Exchange processes with price adjustment. Zbl 0366.90013
Smale, Stephen
1976
Complexity estimates depending on condition and round-off error. Zbl 1065.68533
Cucker, Felipe; Smale, Steve
1999
Modeling language evolution. Zbl 1083.68131
Cucker, Felipe; Smale, Steve; Zhou, Ding-Xuan
2004
The qualitative analysis of a difference equation of population growth. Zbl 0342.92014
Smale, S.; Williams, R. F.
1976
Finding a horseshoe on the beaches of Rio. Zbl 0983.37001
Smale, Steve
1998
On the intractability of Hilbert’s Nullstellensatz and an algebraic version of “$$NP\neq P$$?”. Zbl 0882.03040
Shub, Michael; Smale, Steve
1995
The $$\Omega$$-stability theorem. Zbl 0205.54104
Smale, S.
1970
Global analysis and economics. Zbl 0477.90014
Smale, Steve
1981
Separation of complexity classes in Koiran’s weak model. Zbl 0819.68053
Cucker, F.; Shub, M.; Smale, S.
1994
Some remarks on the foundations of numerical analysis. Zbl 0703.65003
Smale, Steve
1990
Smooth solutions of the heat and wave equations. Zbl 0439.35017
Smale, Stephen
1980
Beyond hyperbolicity. Zbl 0247.58008
Shub, M.; Smale, S.
1972
The generalized Poincaré conjecture in higher dimensions. Zbl 0099.39201
Smale, Stephen
1960
A polynomial time algorithm for diophantine equations in one variable. Zbl 0920.11085
Cucker, Felipe; Koiran, Pascal; Smale, Steve
1999
Algebraic settings for the problem ”P$$\neq$$NP?”. Zbl 0856.68068
Blum, Lenore; Cucker, Felipe; Shub, Mike; Smale, Steve
1996
On the problem of reviving the ergodic hypothesis of Boltzmann and Birkhoff. Zbl 0486.58014
Smale, S.
1980
The problem of the average speed of the simplex method. Zbl 0552.90059
Smale, S.
1983
Global analysis and economics. I: Pareto optimum and a generalisation of Morse theory. Zbl 0267.58008
Smale, S.
1972
Self-intersections of immersed manifolds. Zbl 0093.37501
Lashof, R. K.; Smale, S.
1959
Hodge theory on metric spaces. Appendix by Anthony W. Baker. Zbl 1366.58001
Bartholdi, Laurent; Schick, Thomas; Smale, Nat; Smale, Steve
2012
On a theory of computation over the real numbers; NP completeness, recursive functions and universal machines. Zbl 0691.68034
Blum, L.; Shub, M.; Smale, S.
1990
Optimizing several functions. Zbl 0349.90086
Smale, Stephen
1975
Differentiable and combinatorial structures on manifolds. Zbl 0111.18902
Smale, Stephen
1961
Problems on the nature of relative equilibria in celestial mechanics. Zbl 0215.52602
Smale, S.
1971
Stable manifolds for differential equations and diffeomorphisms. Zbl 0202.55201
Smale, S.
1962
Mathematics of the genome. Zbl 1380.37148
Rajapakse, Indika; Smale, Steve
2017
The pitchfork bifurcation. Zbl 1373.34058
Rajapakse, Indika; Smale, Steve
2017
Emergence of function from coordinated cells in a tissue. Zbl 1404.92067
Rajapakse, Indika; Smale, Stephen
2017
Introduction to the peptide binding problem of computational immunology: new results. Zbl 1329.92096
Shen, Wen-Jun; Wong, Hau-San; Xiao, Quan-Wu; Guo, Xin; Smale, Stephen
2014
Differential equations, dynamical systems, and an introduction to chaos. 3rd ed. Zbl 1239.37001
Hirsch, Morris W.; Smale, Stephen; Devaney, Robert L.
2013
Hodge theory on metric spaces. Appendix by Anthony W. Baker. Zbl 1366.58001
Bartholdi, Laurent; Schick, Thomas; Smale, Nat; Smale, Steve
2012
Abstract and classical Hodge-de Rham theory. Zbl 1243.58003
Smale, Nat; Smale, Steve
2012
A topological view of unsupervised learning from noisy data. Zbl 1230.62085
Niyogi, P.; Smale, S.; Weinberger, S.
2011
Mathematics of the neural response. Zbl 1185.68813
Smale, S.; Rosasco, L.; Bouvrie, J.; Caponnetto, A.; Poggio, T.
2010
Online learning with Markov sampling. Zbl 1170.68022
Smale, Steve; Zhou, Ding-Xuan
2009
Geometry on probability spaces. Zbl 1187.68270
Smale, Steve; Zhou, Ding-Xuan
2009
Finding the homology of submanifolds with high confidence from random samples. Zbl 1177.62003
Niyogi, Partha; Smale, Stephen; Weinberger, Shmuel
2009
Finding the homology of submanifolds with high confidence from random samples. Zbl 1148.68048
Niyogi, Partha; Smale, Stephen; Weinberger, Shmuel
2008
Learning theory and approximation. Abstracts from the workshop held June 29 – July 5, 2008. Zbl 1177.68114
Jetter, Kurt (ed.); Smale, Steve (ed.); Zhou, Ding-Xuan (ed.)
2008
Emergent behavior in flocks. Zbl 1366.91116
Cucker, Felipe; Smale, Steve
2007
Learning theory estimates via integral operators and their approximations. Zbl 1127.68088
Smale, Steve; Zhou, Ding-Xuan
2007
On the mathematics of emergence. Zbl 1166.92323
Cucker, Felipe; Smale, Steve
2007
Risk bounds for random regression graphs. Zbl 1368.68278
Caponnetto, A.; Smale, S.
2007
Online learning algorithms. Zbl 1119.68098
Smale, Steve; Yao, Yuan
2006
Shannon sampling. II: Connections to learning theory. Zbl 1107.94008
Smale, Steve; Zhou, Ding-Xuan
2005
On problems of computational complexity. Zbl 1147.68527
Smale, Stephen
2005
Differential equations, dynamical systems, and an introduction to chaos. 2nd ed. Zbl 1135.37002
Hirsch, Morris W.; Smale, Stephen; Devaney, Robert L.
2004
Shannon sampling and function reconstruction from point values. Zbl 1107.94007
Smale, Steve; Zhou, Ding-Xuan
2004
Modeling language evolution. Zbl 1083.68131
Cucker, Felipe; Smale, Steve; Zhou, Ding-Xuan
2004
Estimating the approximation error in learning theory. Zbl 1079.68089
Smale, Steve; Zhou, Ding-Xuan
2003
The mathematics of learning: dealing with data. Zbl 1083.68100
Poggio, Tomaso; Smale, Steve
2003
On the mathematical foundations of learning. Zbl 0983.68162
Cucker, Felipe; Smale, Steve
2002
Best choices for regularization parameters in learning theory: on the bias-variance problem. Zbl 1057.68085
Cucker, Felipe; Smale, Steve
2002
Mathematical problems for the next century. Zbl 1031.00005
Smale, Steve
2000
Mathematical problems of the next century. Zbl 1077.01502
Smale, S.
2000
The collected papers of Stephen Smale. Vols. 1-3. Edited by F. Cucker and R. Wong. Zbl 0995.01005
Smale, Stephen
2000
Mathematical problems for the next century. Zbl 1040.01006
Smale, Steve
2000
Complexity estimates depending on condition and round-off error. Zbl 1065.68533
Cucker, Felipe; Smale, Steve
1999
A polynomial time algorithm for diophantine equations in one variable. Zbl 0920.11085
Cucker, Felipe; Koiran, Pascal; Smale, Steve
1999
Mathematical problems for the next century. Zbl 0947.01011
Smale, Steve
1998
Finding a horseshoe on the beaches of Rio. Zbl 0983.37001
Smale, Steve
1998
Some lower bounds for the complexity of continuation methods. Zbl 0918.65038
Dedieu, Jean-Pierre; Smale, Steve
1998
The work of Curtis T. McMullen. Zbl 1288.01063
Smale, Steven
1998
Complexity and real computation. Foreword by Richard M. Karp. Zbl 0948.68068
Blum, Leonore; Cucker, Felipe; Shub, Michael; Smale, Steve
1997
Complexity theory and numerical analysis. Zbl 0883.65125
Smale, Steve
1997
Complexity and real computation: A manifesto. Zbl 0872.68036
Blum, Lenore; Cucker, Felipe; Shub, Mike; Smale, Steve
1996
Complexity of Bezout’s theorem. IV: Probability of success; extensions. Zbl 0843.65035
Shub, Michael; Smale, Steve
1996
Algebraic settings for the problem ”P$$\neq$$NP?”. Zbl 0856.68068
Blum, Lenore; Cucker, Felipe; Shub, Mike; Smale, Steve
1996
On the intractability of Hilbert’s Nullstellensatz and an algebraic version of “$$NP\neq P$$?”. Zbl 0882.03040
Shub, Michael; Smale, Steve
1995
Complexity of Bezout’s theorem. V: Polynomial time. Zbl 0846.65022
Shub, M.; Smale, S.
1994
Separation of complexity classes in Koiran’s weak model. Zbl 0819.68053
Cucker, F.; Shub, M.; Smale, S.
1994
Complexity of Bezout’s theorem. I: Geometric aspects. Zbl 0821.65035
Shub, Michael; Smale, Steve
1993
Complexity of Bezout’s theorem. II: Volumes and probabilities. Zbl 0851.65031
Shub, M.; Smale, S.
1993
Complexity of Bezout’s theorem. III: Condition number and packing. Zbl 0846.65018
Shub, Michael; Smale, Steve
1993
The Gödel incompleteness theorem and decidability over a ring. Zbl 0793.03066
Blum, Lenore; Smale, Steve
1993
Dynamics retrospective: Great problems, attempts that failed. Zbl 0745.58018
Smale, Steve
1991
Some remarks on the foundations of numerical analysis. Zbl 0703.65003
Smale, Steve
1990
On a theory of computation over the real numbers; NP completeness, recursive functions and universal machines. Zbl 0691.68034
Blum, L.; Shub, M.; Smale, S.
1990
The story of the higher dimensional Poincaré conjecture (what actually happened on the beaches of Rio). Zbl 0703.57001
Smale, Steve
1990
On a theory of computation and complexity over the real numbers: NP- completeness, recursive functions and universal machines. Zbl 0681.03020
Blum, Lenore; Shub, Mike; Smale, Steve
1989
Algorithms for solving equations. Zbl 0665.65058
Smale, Steve
1987
On the topology of algorithms. I. Zbl 0639.68042
Smale, Steve
1987
Newton’s method estimates from data at one point. Zbl 0613.65058
Smale, Steve
1986
Computational complexity: On the geometry of polynomials and a theory of cost. II. Zbl 0625.65036
Shub, M.; Smale, S.
1986
On the existence of generally convergent algorithms. Zbl 0595.65048
Shub, Michael; Smale, Steve
1986
On the efficiency of algorithms of analysis. Zbl 0592.65032
Smale, Steve
1985
On the geometry of polynomials and a theory of cost. I. Zbl 0603.65027
Shub, Mike; Smale, Steve
1985
On the average number of steps of the simplex method of linear programming. Zbl 0526.90060
Smale, Steve
1983
The problem of the average speed of the simplex method. Zbl 0552.90059
Smale, S.
1983
On the average cost of solving polynomial equations. Zbl 0529.41008
Shub, Mike; Smale, Steve
1983
The fundamental theorem of algebra and complexity theory. Zbl 0456.12012
Smale, Steve
1981
Global analysis and economics. Zbl 0477.90014
Smale, Steve
1981
The mathematics of time. Essays on dynamical systems, economic processes, and related topics. Zbl 0451.58001
Smale, Steve
1980
The prisoner’s dilemma and dynamical systems associated to non- cooperative games. Zbl 0463.90099
Smale, Steve
1980
Smooth solutions of the heat and wave equations. Zbl 0439.35017
Smale, Stephen
1980
On the problem of reviving the ergodic hypothesis of Boltzmann and Birkhoff. Zbl 0486.58014
Smale, S.
1980
On algorithms for solving f(x)=0. Zbl 0408.65032
Hirsch, Morris W.; Smale, Stephen
1979
On comparative statics and bifurcation in economic equilibrium theory. Zbl 0437.90026
Smale, Steve
1979
An approach to the analysis of dynamic processes in economic systems. Zbl 0387.90031
Smale, Steve
1978
Convergent process of price adjustment and global Newton methods. Zbl 0384.34025
Smale, Steve
1977
Dynamical systems and turbulence. Zbl 0362.58012
Smale, Steve
1977
A convergent process of price adjustment and global Newton methods. Zbl 0354.90018
Smale, Steve
1976
On the differential equations of species in competition. Zbl 0344.92009
Smale, S.
1976
Global analysis and economics. VI: Geometric analysis of Pareto optima and price equilibria under classical hypotheses. Zbl 0348.90017
Smale, S.
1976
Exchange processes with price adjustment. Zbl 0366.90013
Smale, Stephen
1976
The qualitative analysis of a difference equation of population growth. Zbl 0342.92014
Smale, S.; Williams, R. F.
1976
Optimizing several functions. Zbl 0349.90086
Smale, Stephen
1975
Sufficient conditions for an optimum. Zbl 0314.58007
Smale, S.
1975
Global analysis and economics. Pareto optimum and a generalization of Morse theory. Zbl 0312.90007
Smale, Steve
1975
Differential equations, dynamical systems, and linear algebra. Zbl 0309.34001
Hirsch, Morris W.; Smale, Stephen
1974
Global analysis and economics. II: Extension of a theorem of Debreu. Zbl 0316.90006
Smale, S.
1974
Global analysis and economics. V: Pareto theory with constraints. Zbl 0357.90010
Smale, S.
1974
Global analysis and economics. III: Pareto Optima and price equilibria. Zbl 0316.90007
Smale, S.
1974
Global analysis and economics. IV: Finiteness and stability of equilibria with general consumption sets and production. Zbl 0316.90008
Smale, S.
1974
A mathematical model of two cells via Turing’s equation. Zbl 0333.92002
Smale, S.
1974
Global analysis and economics. I: Pareto optimum and a generalization of Morse theory. Zbl 0269.58009
Smale, Steve
1973
Stability and isotopy in discrete dynamical systems. Zbl 0284.58013
Smale, Steve
1973
On the mathematical foundations of electrical circuit theory. Zbl 0286.34071
Smale, S.
1972
Beyond hyperbolicity. Zbl 0247.58008
Shub, M.; Smale, S.
1972
Global analysis and economics. I: Pareto optimum and a generalisation of Morse theory. Zbl 0267.58008
Smale, S.
1972
Topology and mechanics. Zbl 0233.57018
Smale, S.
1972
Problems on the nature of relative equilibria in celestial mechanics. Zbl 0215.52602
Smale, S.
1971
Topology and mechanics. II: The planar $$n$$-body problem. Zbl 0203.26102
Smale, S.
1970
Topology and mechanics. I. Zbl 0202.23201
Smale, S.
1970
Structural stability theorems. Zbl 0214.50702
Palis, J.; Smale, S.
1970
...and 36 more Documents
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#### Cited by 6,990 Authors
70 Ha, Seung-Yeal 51 Llibre, Jaume 49 Grines, Vyacheslav Zigmundovich 49 Zhou, Dingxuan 44 Cucker, Felipe 41 Smale, Steve 39 Pochinka, Olga Vital’evna 34 Shub, Michael 26 Zhuzhoma, Evgeniĭ Viktorovich 25 Choi, Young-Pil 24 Medvedev, Vladislav Sergeevich 23 Carrillo de la Plata, José Antonio 23 Marsden, Jerrold Eldon 23 Sun, Hongwei 22 Beltrán, Carlos 22 Chen, Dirong 22 Yu, Pei 21 Koiran, Pascal 21 Meer, Klaus 20 Pardo, Luis Miguel 20 Petković, Miodrag S. 19 Bürgisser, Peter 19 Han, Maoan 19 Hirsch, Morris W. 19 Sheng, Baohuai 18 Mello, Luis Fernando O. 18 Xiang, Dao-Hong 17 Degond, Pierre 17 Holmes, Philip J. 17 Pillonetto, Gianluigi 17 Ruelle, David Pierre 16 Argyros, Ioannis Konstantinos 16 Bonatti, Christian 16 Kim, Jeongho 16 Laudenbach, François 15 Guo, Zheng-Chu 14 Kuznetsov, Sergey P. 14 Li, Chong 14 Li, Luoqing 14 Wu, Qiang 14 Xu, Zongben 13 Chen, Guanrong 13 Chen, Hong 13 Fernandes, Antonio Carlos 13 Jørgensen, Palle E. T. 13 Rosasco, Lorenzo A. 13 Shi, Lei 13 Tong, Hongzhi 13 Yorke, James Alan 13 Zhang, Xiongtao 12 Basu, Saugata 12 Dedieu, Jean-Pierre 12 Dong, Jiu-Gang 12 Fornasier, Massimo 12 Hu, Ting 12 Li, Jibin 12 Malajovich, Gregorio 12 Palis, Jacob jun. 12 Sanguineti, Marcello 11 Chazal, Frédéric 11 Devaney, Robert L. 11 Ferreira, Orizon Pereira 11 Gutiérrez, José Manuel 11 Kim, Doheon 11 Li, Zhuchun 11 Pérez-Chavela, Ernesto 11 Pugh, Charles Chapman 11 Temam, Roger Meyer 10 Armentano, Diego 10 Bellomo, Nicola 10 Block, Louis Stuart 10 Bowen, Rufus 10 Crovisier, Sylvain 10 Gnecco, Giorgio 10 Guckenheimer, John M. 10 Gurevich, Elena Ya. 10 Kim, Dohyun 10 Pan, Victor Yakovlevich 10 Rančić, Lidija Z. 10 Robinson, Clark 10 Santoprete, Manuele 10 Wang, Qiudong 10 Xian, Jun 10 Zhang, Haizhang 10 Zou, Bin 9 Bournez, Olivier 9 Campagnolo, Manuel Lameiras 9 Cao, Feilong 9 De Vito, Ernesto 9 Diacu, Florin Nicolae 9 Fiedler, Bernold 9 Graça, Daniel Silva 9 Lv, Shaogao 9 Malinowska, Agnieszka Barbara 9 Petković, Ljiljana D. 9 Rojas, J. Maurice 9 Shamolin, Maksim Vladimirovich 9 Straughan, Brian 9 Tadmor, Eitan 9 Takens, Floris ...and 6,890 more Authors
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#### Cited in 666 Serials
202 Journal of Differential Equations 179 Transactions of the American Mathematical Society 160 Journal of Complexity 121 Journal of Mathematical Analysis and Applications 113 Theoretical Computer Science 111 Physica D 108 Proceedings of the American Mathematical Society 106 International Journal of Bifurcation and Chaos in Applied Sciences and Engineering 92 Journal of Mathematical Economics 80 Applied Mathematics and Computation 79 Ergodic Theory and Dynamical Systems 79 Bulletin of the American Mathematical Society 75 Topology and its Applications 66 Inventiones Mathematicae 64 Communications in Mathematical Physics 63 M$$^3$$AS. Mathematical Models & Methods in Applied Sciences 58 Chaos 58 Foundations of Computational Mathematics 57 Chaos, Solitons and Fractals 57 Bulletin of the American Mathematical Society. New Series 55 Journal of Computational and Applied Mathematics 53 Advances in Mathematics 51 Journal of Mathematical Sciences (New York) 48 Mathematische Zeitschrift 45 Nonlinear Analysis. Theory, Methods & Applications. Series A: Theory and Methods 44 Automatica 44 Journal of Economic Theory 42 Journal of Statistical Physics 40 Computers & Mathematics with Applications 39 Journal of Mathematical Physics 39 Mathematische Annalen 38 Archive for Rational Mechanics and Analysis 37 Mathematical Notes 37 Journal of Dynamics and Differential Equations 37 Nonlinear Analysis. Theory, Methods & Applications 35 Journal of Mathematical Biology 35 Linear Algebra and its Applications 35 Analysis and Applications (Singapore) 34 Journal of Symbolic Computation 33 Neural Computation 33 Celestial Mechanics and Dynamical Astronomy 33 Discrete and Continuous Dynamical Systems 31 Journal of Optimization Theory and Applications 30 Discrete & Computational Geometry 30 Applied and Computational Harmonic Analysis 28 Communications in Nonlinear Science and Numerical Simulation 27 Mathematics of Computation 27 Bulletin of Mathematical Biology 27 Annales de l’Institut Henri Poincaré. Analyse Non Linéaire 26 Journal of Geometry and Physics 26 Abstract and Applied Analysis 26 Geometry & Topology 26 Qualitative Theory of Dynamical Systems 25 Publications Mathématiques 25 Journal of Functional Analysis 25 Journal of Economic Dynamics & Control 25 Advances in Computational Mathematics 24 Mathematical Biosciences 24 Applied Mathematics Letters 24 Regular and Chaotic Dynamics 24 International Journal of Wavelets, Multiresolution and Information Processing 24 Proceedings of the Steklov Institute of Mathematics 23 Israel Journal of Mathematics 23 Journal of the Franklin Institute 23 Systems & Control Letters 23 Nonlinear Analysis. Real World Applications 22 Duke Mathematical Journal 22 Mathematical Programming. Series A. Series B 21 Nonlinearity 21 Annales Scientifiques de l’École Normale Supérieure. Quatrième Série 21 Journal of Approximation Theory 21 Mathematical Programming 21 Acta Applicandae Mathematicae 21 Celestial Mechanics 21 SIAM Journal on Applied Dynamical Systems 20 Annales de l’Institut Fourier 20 Geometriae Dedicata 20 Journal of Nonlinear Science 20 Journal of Difference Equations and Applications 20 Nonlinear Dynamics 19 The Annals of Statistics 17 Neural Networks 17 Algebraic & Geometric Topology 17 Journal of Theoretical Biology 16 Journal of Pure and Applied Algebra 16 Mathematical Problems in Engineering 16 Differential Equations 16 Journal of Fixed Point Theory and Applications 16 Kinetic and Related Models 16 Science China. Mathematics 15 Computer Methods in Applied Mechanics and Engineering 15 General Relativity and Gravitation 15 Physics Letters. A 15 Annali di Matematica Pura ed Applicata. Serie Quarta 15 Annals of Global Analysis and Geometry 15 Constructive Approximation 15 Journal of the American Mathematical Society 15 Mathematical and Computer Modelling 15 Economic Theory 14 ZAMP. Zeitschrift für angewandte Mathematik und Physik ...and 566 more Serials
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#### Cited in 63 Fields
1,734 Dynamical systems and ergodic theory (37-XX) 914 Computer science (68-XX) 811 Ordinary differential equations (34-XX) 677 Numerical analysis (65-XX) 525 Manifolds and cell complexes (57-XX) 461 Biology and other natural sciences (92-XX) 448 Game theory, economics, finance, and other social and behavioral sciences (91-XX) 446 Global analysis, analysis on manifolds (58-XX) 416 Partial differential equations (35-XX) 379 Differential geometry (53-XX) 379 Mechanics of particles and systems (70-XX) 331 Operations research, mathematical programming (90-XX) 321 Statistics (62-XX) 301 Systems theory; control (93-XX) 241 Probability theory and stochastic processes (60-XX) 205 Algebraic topology (55-XX) 188 Operator theory (47-XX) 175 Calculus of variations and optimal control; optimization (49-XX) 174 General topology (54-XX) 160 Algebraic geometry (14-XX) 157 Statistical mechanics, structure of matter (82-XX) 154 Functions of a complex variable (30-XX) 152 Mathematical logic and foundations (03-XX) 150 Functional analysis (46-XX) 137 Information and communication theory, circuits (94-XX) 136 Fluid mechanics (76-XX) 99 Linear and multilinear algebra; matrix theory (15-XX) 97 Several complex variables and analytic spaces (32-XX) 95 Real functions (26-XX) 94 Field theory and polynomials (12-XX) 90 Measure and integration (28-XX) 89 Approximations and expansions (41-XX) 87 Combinatorics (05-XX) 79 Quantum theory (81-XX) 63 Number theory (11-XX) 60 Harmonic analysis on Euclidean spaces (42-XX) 58 Difference and functional equations (39-XX) 57 Convex and discrete geometry (52-XX) 55 History and biography (01-XX) 55 Mechanics of deformable solids (74-XX) 42 Commutative algebra (13-XX) 42 Relativity and gravitational theory (83-XX) 41 Group theory and generalizations (20-XX) 38 Topological groups, Lie groups (22-XX) 34 General and overarching topics; collections (00-XX) 33 Integral equations (45-XX) 25 Potential theory (31-XX) 17 Optics, electromagnetic theory (78-XX) 17 Geophysics (86-XX) 16 Nonassociative rings and algebras (17-XX) 14 Geometry (51-XX) 13 $$K$$-theory (19-XX) 12 Category theory; homological algebra (18-XX) 12 Special functions (33-XX) 12 Classical thermodynamics, heat transfer (80-XX) 11 Astronomy and astrophysics (85-XX) 10 Abstract harmonic analysis (43-XX) 8 Order, lattices, ordered algebraic structures (06-XX) 6 Associative rings and algebras (16-XX) 6 Integral transforms, operational calculus (44-XX) 3 Mathematics education (97-XX) 1 General algebraic systems (08-XX) 1 Sequences, series, summability (40-XX)
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https://phys.libretexts.org/Courses/Joliet_Junior_College/Physics_201_-_Fall_2019/Book%3A_Physics_(Boundless)/07%3A_Work_and_Energy/7.13%3A_Prelude_to_Potential_Energy_and_Conservation_of_Energy
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$$\require{cancel}$$
# 7.13: Prelude to Potential Energy and Conservation of Energy
In George Rhoads’ rolling ball sculpture, the principle of conservation of energy governs the changes in the ball’s kinetic energy and relates them to changes and transfers for other types of energy associated with the ball’s interactions. In this chapter, we introduce the important concept of potential energy. This will enable us to formulate the law of conservation of mechanical energy and to apply it to simple systems, making solving problems easier. In the final section on sources of energy, we will consider energy transfers and the general law of conservation of energy. Throughout this book, the law of conservation of energy will be applied in increasingly more detail, as you encounter more complex and varied systems, and other forms of energy.
## Contributors and Attributions
• Samuel J. Ling (Truman State University), Jeff Sanny (Loyola Marymount University), and Bill Moebs with many contributing authors. This work is licensed by OpenStax University Physics under a Creative Commons Attribution License (by 4.0).
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| 2022-01-23T21:18:45 |
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https://tjyj.stats.gov.cn/CN/Y2021/V38/I6/30
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• •
### 中国产业部门隐含碳排放效率研究——基于三阶段DEA模型与非竞争型I-O模型的实证分析
• 出版日期:2021-06-25 发布日期:2021-06-25
### Study on the Carbon Emissions Efficiency Embodied in China’s Industrial Sector—Empirical Analysis Based on Three-stage DEA Model and Non-competitive I-O Model
Hu Jianbo Yan Shuo Han Jun
• Online:2021-06-25 Published:2021-06-25
Abstract: Based on China’ s Input-output Tables ( extended) 2002 - 2017, this paper first applies the non-competitive input-output model to calculate the carbon emissions embodied in each industrial sector in China, introduces them into the carbon emissions efficiency model, and then uses the three-stage DEA model to eliminate the external environment and random interference factors, so as to obtain a more accurate and objective carbon emissions efficiency level embodied in various industrial sectors. The results show that the carbon emissions efficiency embodied in China’ s overall industrial sector is relatively low, and the levels of efficiency between industrial sectors are significantly different. The clustering analysis of the yearly average efficiency of carbon emissions embodied in each industrial sector in the third stage indicates that agriculture, oil and gas, wholesale and retail, catering and other services have high efficiency, electrical machinery and equipment manufacturing, communications equipment and computer and other electronic equipment manufacturing, electric power and heat production and supply, gas production and supply, coal mining have medium efficiency, while resource-dependent and less innovative industries such as textile, clothing, footwear, hats, leather, feather and their products, wood processing and furniture manufacturing, water production and supply, construction, transportation, storage and postal industries have low efficiency. The external environment has a significant impact on the carbon emissions efficiency embodied in various industrial sectors in three ways, namely “ cross type”, “ overlap type” and “ parallel type”. The “ cross type” is mainly in the manufacturing industry, the impact of external environment on its carbon emissions efficiency firstly improving and then suppressing. The “overlap type” is mainly in the agriculture and services industry, and the external environment has little impact on their carbon emissions efficiency. “Parallel type ” is mainly in resource-based industry, and the impact of the external environment on its carbon emissions efficiency depends on specific industries.
| 2022-08-09T16:43:29 |
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https://zbmath.org/authors/?q=ai%3Akrantz.steven-george
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## Krantz, Steven George
Compute Distance To:
Author ID: krantz.steven-george Published as: Krantz, Steven G.; Krantz, S. G.; Krantz, Steven; Krantz, Steven George Homepage: https://www.math.wustl.edu/~sk/ External Links: MGP · ORCID · Wikidata · dblp · GND · IdRef
Documents Indexed: 294 Publications since 1976, including 70 Books 17 Contributions as Editor · 2 Further Contributions Reviewing Activity: 195 Reviews Co-Authors: 102 Co-Authors with 148 Joint Publications 3,483 Co-Co-Authors
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### Co-Authors
163 single-authored 19 Greene, Robert Everist 19 Kim, Kang-Tae 13 Li, Songying 13 Peloso, Marco Maria 12 Parks, Harold R. 11 Isaev, Alexander 7 Ma, Daowei 4 Chang, Der-Chen E. 4 Fontana, Luigi 4 Fu, Siqi 3 Bedford, Eric 3 Blank, Brian E. 3 Chen, Goong 3 Cima, Joseph A. 3 Daghighi, Abtin 3 D’Angelo, John P. 3 Huang, Xiaojun 3 Osserman, Robert 3 Rochberg, Richard 2 Alladi, Krishnaswami 2 Aron, Richard Martin 2 Bott, Raoul Harry 2 Dao, Nguyen Anh 2 Douglas, Ronald George 2 Earle, Clifford J. 2 Fridman, Buma L. 2 Gavosto, Estela Ana 2 Hejhal, Dennis A. 2 Jørgensen, Troels 2 Jorgenson, Jay Alan 2 Kahane, Jean-Pierre 2 Marden, Albert 2 Munao, Simone 2 Nathanson, Melvyn Bernard 2 Parsons, Torrence D. 2 Rao, Arni S. R. Srinivasa 2 Sawyer, Eric T. 2 Stein, Elias Menachem 2 Stoppato, Caterina 2 Treil, Sergei 2 Wójcicki, Paweł M. 1 Agarwal, Ravi P. 1 Aladro, Gerardo 1 Alon, Noga M. 1 Atiyah, Michael Francis 1 Bar-Natan, Dror 1 Beckner, William 1 Bell, Steven R. 1 Bland, John S. 1 Brown, Johnny E. 1 Burns, Daniel M. jun. 1 Byun, Jisoo 1 Casazza, Peter George 1 Cattaneo, Alberto Sergio 1 Chen, Zhenhua 1 Chuaqui, Martin 1 Coates, John H. 1 Coleman, Matthew P. 1 Dafni, Galia 1 Di Biase, Fausto 1 Duesberg, Peter 1 Duncan, John 1 Erdős, Pál 1 Ewing, John Harwood 1 Fan, Dashan 1 Fefferman, Charles Louis 1 Ferguson, Tim 1 Fornæss, John Erik 1 Garcia, Stephan Ramon 1 Gaussier, Hervé 1 Gehring, Frederick William 1 Gerver, Joseph L. 1 Godsil, Christopher David 1 Goldberg, Lisa A. 1 Goldfeld, Dorian Morris 1 Goldston, Daniel Alan 1 Goodwillie, Thomas Gehret 1 Graham, Ian R. 1 Graham, Ronald Lewis 1 Greenberg, Marvin Jay 1 Hintikka, Eric A. 1 Hirzebruch, Friedrich 1 Howe, Roger Evans 1 Ionescu, Alexandru D. 1 Jackson, Allyn 1 Jeffrey, Lisa Claire 1 Jenkins, James Allister 1 Jenkis, James 1 Jensen, Gary R. 1 Jewell, Nicholas P. 1 Kaiser, Klaus Hermann 1 Kearn, Vickie 1 Kenig, Carlos Eduardo 1 Khavinson, Dima 1 Knapp, Anthony William 1 Kobayashi, Shoshichi 1 Kra, Irwin 1 Kramer, Jürg 1 Kuperberg, Gregory John 1 Lachaud, Gilles ...and 74 more Co-Authors
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### Serials
18 Complex Variables and Elliptic Equations 14 Journal of Mathematical Analysis and Applications 13 Textbooks in Mathematics 12 Notices of the American Mathematical Society 11 Rocky Mountain Journal of Mathematics 10 American Mathematical Monthly 8 The Journal of Geometric Analysis 7 Illinois Journal of Mathematics 7 Real Analysis Exchange 7 Complex Variables. Theory and Application 6 Michigan Mathematical Journal 6 Complex Analysis and Operator Theory 5 Duke Mathematical Journal 5 Indiana University Mathematics Journal 5 Manuscripta Mathematica 5 Expositiones Mathematicae 4 Journal of the Korean Mathematical Society 4 Pacific Journal of Mathematics 4 Proceedings of the American Mathematical Society 4 Transactions of the American Mathematical Society 4 The Dolciani Mathematical Expositions 3 Journal of Functional Analysis 3 Mathematische Annalen 3 Nonlinear Analysis. Theory, Methods & Applications. Series A: Theory and Methods 3 Bulletin of the Korean Mathematical Society 3 Mathematical Research Letters 3 The Carus Mathematical Monographs 3 Contemporary Mathematics 3 Proceedings of Symposia in Pure Mathematics 2 Houston Journal of Mathematics 2 Mathematics Magazine 2 Advances in Mathematics 2 International Journal of Mathematics and Mathematical Sciences 2 Journal of Differential Equations 2 Journal für die Reine und Angewandte Mathematik 2 Mathematische Zeitschrift 2 Bulletin of the American Mathematical Society. New Series 2 Graduate Studies in Mathematics 2 Cornerstones 1 Journal d’Analyse Mathématique 1 Studia Mathematica 1 The Mathematical Intelligencer 1 Acta Mathematica Vietnamica 1 Annales de l’Institut Fourier 1 Canadian Journal of Mathematics 1 Canadian Mathematical Bulletin 1 Colloquium Mathematicum 1 Commentarii Mathematici Helvetici 1 Integral Equations and Operator Theory 1 Mathematica Scandinavica 1 Memoirs of the American Mathematical Society 1 Nagoya Mathematical Journal 1 Quaestiones Mathematicae 1 European Journal of Combinatorics 1 Journal of Symbolic Computation 1 Journal of the American Mathematical Society 1 Bulletin of the Allahabad Mathematical Society 1 Communications in Partial Differential Equations 1 SIAM Journal on Applied Mathematics 1 Experimental Mathematics 1 Electronic Research Announcements of the American Mathematical Society 1 The Journal of Fourier Analysis and Applications 1 The Asian Journal of Mathematics 1 Missouri Journal of Mathematical Sciences 1 Annali della Scuola Normale Superiore di Pisa. Classe di Scienze. Serie V 1 Bulletin of the American Mathematical Society 1 Basler Lehrbücher 1 Fields Institute Communications 1 Graduate Texts in Mathematics 1 Lecture Notes in Mathematics 1 Mathematical Sciences Research Institute Publications 1 Progress in Mathematics 1 Regional Conference Series in Mathematics 1 Leituras em Matemática 1 Electronic Research Announcements in Mathematical Sciences 1 Synthesis Lectures on Mathematics and Statistics 1 Journal of Theoretical Biology 1 International Journal of Analysis and Applications 1 Complex Analysis and its Synergies 1 Modern Birkhäuser Classics 1 Applied and Numerical Harmonic Analysis 1 Springer Monographs in Mathematics 1 Contemporary Mathematicians 1 Birkhäuser Advanced Texts. Basler Lehrbücher 1 MAA Textbooks 1 Pure and Applied Mathematics. A Wiley-Interscience Series of Texts, Monographs and Tracts 1 MAA Spectrum
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### Fields
172 Several complex variables and analytic spaces (32-XX) 53 Functions of a complex variable (30-XX) 39 General and overarching topics; collections (00-XX) 30 Partial differential equations (35-XX) 28 History and biography (01-XX) 26 Real functions (26-XX) 24 Functional analysis (46-XX) 18 Harmonic analysis on Euclidean spaces (42-XX) 14 Operator theory (47-XX) 12 Global analysis, analysis on manifolds (58-XX) 10 Potential theory (31-XX) 8 Mathematics education (97-XX) 6 Mathematical logic and foundations (03-XX) 6 Differential geometry (53-XX) 5 Abstract harmonic analysis (43-XX) 5 General topology (54-XX) 4 Measure and integration (28-XX) 4 Ordinary differential equations (34-XX) 4 Integral equations (45-XX) 4 Convex and discrete geometry (52-XX) 4 Manifolds and cell complexes (57-XX) 4 Computer science (68-XX) 3 Geometry (51-XX) 2 Combinatorics (05-XX) 2 Number theory (11-XX) 2 Algebraic geometry (14-XX) 2 Topological groups, Lie groups (22-XX) 2 Dynamical systems and ergodic theory (37-XX) 2 Approximations and expansions (41-XX) 2 Algebraic topology (55-XX) 2 Mechanics of deformable solids (74-XX) 2 Biology and other natural sciences (92-XX) 1 Order, lattices, ordered algebraic structures (06-XX) 1 Field theory and polynomials (12-XX) 1 Group theory and generalizations (20-XX) 1 Difference and functional equations (39-XX) 1 Sequences, series, summability (40-XX) 1 Integral transforms, operational calculus (44-XX) 1 Calculus of variations and optimal control; optimization (49-XX) 1 Probability theory and stochastic processes (60-XX) 1 Numerical analysis (65-XX) 1 Mechanics of particles and systems (70-XX) 1 Operations research, mathematical programming (90-XX) 1 Systems theory; control (93-XX)
### Citations contained in zbMATH Open
206 Publications have been cited 2,741 times in 2,068 Documents Cited by Year
Function theory of several complex variables. Zbl 0471.32008
Krantz, Steven G.
1982
A primer of real analytic functions. 2nd ed. Zbl 1015.26030
Krantz, Steven G.; Parks, Harold R.
2002
Function theory of several complex variables. Reprint of the 1992 2nd ed. with corrections. Zbl 1087.32001
Krantz, Steven G.
2001
Function theory of several complex variables. 2. ed. Zbl 0776.32001
Krantz, Steven G.
1992
The implicit function theorem. History, theory, and applications. Zbl 1012.58003
Krantz, Steven G.; Parks, Harold R.
2002
Rigidity of holomorphic mappings and a new Schwarz lemma at the boundary. Zbl 0807.32008
Burns, Daniel M.; Krantz, Steven G.
1994
A primer of real analytic functions. Zbl 0767.26001
Krantz, Steven; Parks, Harold R.
1992
$$H^ p$$ theory on a smooth domain in $$\mathbb{R}^ N$$ and elliptic boundary value problems. Zbl 0804.35027
Chang, Der-Chen; Krantz, Steven G.; Stein, Elias M.
1993
Deformation of complex structures, estimates for the (partial d) equation, and stability of the Bergman kernel. Zbl 0504.32016
Greene, Robert E.; Krantz, Steven G.
1982
On the iterated logarithmic Bloch space on the unit ball. Zbl 1221.47056
Krantz, Steven G.; Stević, Stevo
2009
Geometric integration theory. Zbl 1149.28001
Krantz, Steven G.; Parks, Harold R.
2008
Distance to $$C^k$$ hypersurfaces. Zbl 0431.57009
Krantz, Steven G.; Parks, Harold R.
1981
Domains with non-compact automorphism group: a survey. Zbl 1040.32019
Isaev, A. V.; Krantz, S. G.
1999
Boundedness and compactness of integral operators on spaces of homogeneous type and applications. I. Zbl 0990.47042
Krantz, Steven G.; Li, Song-Ying
2001
Lipschitz spaces, smoothness of functions, and approximation theory. Zbl 0518.46018
Krantz, Steven G.
1983
Boundedness and compactness of integral operators on spaces of homogeneous type and applications. II. Zbl 0990.47043
Krantz, Steven G.; Li, Song-Ying
2001
The geometry of domains in space. Zbl 0929.26001
Krantz, Steven G.; Parks, Harold R.
1999
Optimal Lipschitz and $$L^p$$ regularity for the equation $$\overline\partial u=f$$ on strongly pseudo-convex domains. Zbl 0303.35059
Krantz, S. G.
1976
Handbook of complex variables. Zbl 0946.30001
Krantz, Steven G.
1999
Geometric function theory. Explorations in complex analysis. Zbl 1086.30001
Krantz, Steven G.
2006
The Schwarz lemma at the boundary. Zbl 1227.30023
Krantz, Steven G.
2011
Function theory of one complex variable. 3rd ed. Zbl 1114.30001
Greene, Robert E.; Krantz, Steven G.
2006
The Lindelöf principle and normal functions of several complex variables. Zbl 0522.32003
Cima, Joseph A.; Krantz, Steven G.
1983
The Bergman kernel and projection on non-smooth worm domains. Zbl 1161.32016
Krantz, Steven G.; Peloso, Marco M.
2008
A criterion for normality in $$\mathbb{C}^ n$$. Zbl 0749.32001
1991
The implicit function theorem. History, theory, and applications. Reprint of the 2003 hardback edition. Zbl 1269.58003
Krantz, Steven G.; Parks, Harold R.
2013
The automorphism groups of strongly pseudoconvex domains. Zbl 0531.32016
Greene, Robert E.; Krantz, Steven G.
1982
On a problem of Moser. Zbl 0846.32010
Huang, Xiaojun; Krantz, Steven G.
1995
Duality theorems for Hardy and Bergman spaces on convex domains of finite type in $${\mathbb{C}}^ n$$. Zbl 0835.32004
Krantz, Steven G.; Li, Song-Ying
1995
On the automorphism groups of hyperbolic manifolds. Zbl 0974.32018
Isaev, Alexander V.; Krantz, Steven G.
2001
The geometry of complex domains. Zbl 1239.32011
Greene, Robert E.; Kim, Kang-Tae; Krantz, Steven G.
2011
Bloch functions on strongly pseudoconvex domains. Zbl 0628.32006
Krantz, Steven G.; Ma, Daowei
1988
Compactness of the $$\bar \partial$$-Neumann operator. Zbl 0736.35071
Krantz, Steven G.
1988
Complex scaling and domains with non-compact automorphism group. Zbl 1065.32014
Kim, Kang-Tae; Krantz, Steven G.
2001
Analysis, designs, and behaviour of dissipative joints for coupled beams. Zbl 0685.73046
Chen, G.; Krantz, S. G.; Russel, D. L.; Wayne, C. E.; West, H. H.; Coleman, M. P.
1989
Geometric analysis of the Bergman kernel and metric. Zbl 1281.32004
Krantz, Steven G.
2013
On decomposition theorems for Hardy spaces on domains in $$\mathbb{C}^ n$$ and applications. Zbl 0886.32003
Krantz, Steven G.; Li, Song-Ying
1995
Fractional integration on Hardy spaces. Zbl 0504.47034
Krantz, Steven G.
1982
Techniques for studying automorphisms of weakly pseudoconvex domains. Zbl 0779.32017
Greene, Robert E.; Krantz, Steven G.
1993
Smoothness to the boundary of conformal maps. Zbl 0626.30005
Bell, Steven R.; Krantz, Steven G.
1987
A panorama of harmonic analysis. Zbl 0947.42001
Krantz, Steven G.
1999
Characterization of complex manifolds by the isotropy subgroups of their automorphism groups. Zbl 0622.32020
Greene, Robert E.; Krantz, Steven G.
1985
Hardy spaces and elliptic boundary value problems. Zbl 0765.42014
Chang, Der-Chen; Krantz, Steven G.; Stein, Elias M.
1992
A note on the Wong-Rosay theorem in complex manifolds. Zbl 1044.32019
Gaussier, Hervé; Kim, Kang-Tae; Krantz, Steven G.
2002
Invariant metrics and the boundary behavior of holomorphic functions on domains in $${\mathbb{C}}^ n$$. Zbl 0728.32002
Krantz, Steven G.
1991
A unique continuation problem for holomorphic mappings. Zbl 0781.32018
Huang, Xiaojun; Krantz, Steven G.
1993
Invariants of Bergman geometry and the automorphism groups of domains in $${\mathbb{C}^n}$$. Zbl 0997.32012
Greene, R. E.; Krantz, S. G.
1991
Geometric Lipschitz spaces and applications to complex function theory and nilpotent groups. Zbl 0428.41004
Krantz, Steven G.
1979
Analysis and geometry on worm domains. Zbl 1147.32020
Krantz, Steven G.; Peloso, Marco M.
2008
Intrinsic Lipschitz classes on manifolds with applications to complex function theory and estimates for the $$\overline\partial$$ and $$\overline\partial_b$$ equations. Zbl 0382.32012
Krantz, Steven G.
1978
Explorations in harmonic analysis. With applications to complex function theory and the Heisenberg group. Zbl 1171.43001
Krantz, Steven G.
2009
Biholomorphic self-maps of domains. Zbl 0625.32024
Greene, Robert E.; Krantz, Steven G.
1987
Holomorphic functions of bounded mean oscillation and mapping properties of the Szegö projection. Zbl 0456.32004
Krantz, Steven G.
1980
Area integral characterizations of functions in Hardy spaces on domains in $$\mathbb{C}^ n$$. Zbl 0887.32002
Krantz, Steven G.; Li, Song-Ying
1997
Normal families and the semicontinuity of isometry and automorphism groups. Zbl 0584.58014
Greene, Robert E.; Krantz, Steven G.
1985
The boundary behavior of the Kobayashi metric. Zbl 0760.32010
Krantz, Steven G.
1992
A note on Hardy spaces and functions of bounded mean oscillation on domains in $$\mathbb{C}^ n$$. Zbl 0802.32013
Krantz, Steven G.; Li, Song-Ying
1994
Partial differential equations and complex analysis. Zbl 0852.35001
Krantz, Steven George; Gavosto, Estela A.; Peloso, Marco M.
1992
A Hopf lemma for holomorphic functions and applications. Zbl 0837.30019
Huang, Xiaojun; Krantz, S. G.; Ma, D.; Pan, Y.
1995
Stability of the Caratheodory and Kobayashi metrics and applications to biholomorphic mappings. Zbl 0533.32011
Greene, Robert E.; Krantz, Steven G.
1984
Complex analysis: the geometric viewpoint. Zbl 0743.30002
Krantz, Steven G.
1990
Geometric analysis and function spaces. Expository lectures from the NSF- CBMS regional conference held at George Mason University, Fairfax, VA (USA), May 26-31, 1992. Zbl 0783.32001
Krantz, Steven G.
1993
Optimal $$L^ p$$ estimates for the $$\bar \partial$$-equation on complex ellipsoids in $$\mathbb{C}^ n$$. Zbl 0789.32011
Chen, Zhenhua; Krantz, Steven G.; Ma, Daowei
1993
Stability properties of the Bergman kernel and curvature properties of bounded domains. Zbl 0483.32014
Greene, R. E.; Krantz, Steven G.
1981
On the Bergman invariant and curvatures of the Bergman metric. Zbl 0855.32008
Krantz, Steven G.; Yu, Jiye
1996
Lipschitz spaces on stratified groups. Zbl 0529.22006
Krantz, Steven
1982
Reinhardt domains with non-compact automorphism groups. Zbl 0866.32001
Fu, Siqi; Isaev, A. V.; Krantz, Steven G.
1996
On fixed points and determining sets for holomorphic automorphisms. Zbl 1026.32042
Fridman, B. L.; Kim, K. T.; Krantz, S. G.; Ma, D.
2002
Calculation and estimation of the Poisson kernel. Zbl 1060.31004
Krantz, Steven G.
2005
On the vector sum of two convex sets in space. Zbl 0728.52003
Krantz, Steven G.; Parks, Harold R.
1991
Structure and interpolation theorems for certain Lipschitz spaces and estimates for the $$\overline\partial$$ equation. Zbl 0357.46037
Krantz, Steven G.
1976
The Kobayashi metric of a complex ellipsoid in $$\mathbb{C}^ 2$$. Zbl 0783.32012
Blank, Brian E.; Fan, Dashan; Klein, David; Krantz, Steven G.; Ma, Daowei; Pang, Myung-Yull
1992
Analysis on the Heisenberg group and estimates for functions in Hardy classes of several complex variables. Zbl 0401.43004
Krantz, Steven G.
1979
Characterization of the Hilbert ball by its automorphism group. Zbl 1007.32002
Kim, Kang-Tae; Krantz, Steven G.
2002
Bergman kernel and projection on the unbounded Diederich-Fornaess worm domain. Zbl 1377.32003
Krantz, Steven G.; Peloso, Marco M.; Stoppato, Caterina
2016
Complex analysis: the geometric viewpoint. 2nd ed. Zbl 1051.30001
Krantz, Steven G.
2004
Complex scaling and geometric analysis of several variables. Zbl 1156.32001
Kim, Kang-Tae; Krantz, Steven G.
2008
Characterizations of certain weakly pseudoconvex domains with non-compact automorphism groups. Zbl 0626.32023
Greene, Robert E.; Krantz, Steven G.
1987
On the boundary orbit accumulation set for a domain with noncompact automorphism group. Zbl 0879.32016
Isaev, A. V.; Krantz, S. G.
1996
Antisocial subcovers of self-centered coverings. Zbl 0631.52013
Krantz, Steven G.; Parsons, T. D.
1986
Nonlinear conditions for differentiability of functions. Zbl 0632.58008
Duncan, John; Krantz, Steven G.; Parks, Harold R.
1985
Characterization of smooth domains in C by their biholomorphic self-maps. Zbl 0524.30007
Krantz, Steven G.
1983
Harmonic and complex analysis in several variables. Zbl 1414.32001
Krantz, Steven G.
2017
Some new results on domains in complex space with non-compact automorphism group. Zbl 1035.32019
Kim, Kang-Tae; Krantz, Steven G.
2003
A guide to complex variables. Zbl 1147.30001
Krantz, Steven G.
2008
Toeplitz operators and related function algebras on certain pseudo-convex domains. Zbl 0371.47029
Jewell, Nicholas P.; Krantz, Steven G.
1979
Function theory of one complex variable. 2nd ed. Zbl 0988.30001
Greene, Robert E.; Krantz, Steven G.
2002
A reflection principle for proper holomorphic mappings of strongly pseudoconvex domains and applications. Zbl 0518.32009
Cima, Joseph A.; Krantz, Steven G.; Suffridge, Ted J.
1984
Fatou theorems on domains in $${\mathbb{C}}^ n$$. Zbl 0614.32007
Krantz, Steven G.
1987
Asymptotic eigenfrequency distributions for the $$N$$-beam Euler-Bernoulli coupled beam equation with dissipative joints. Zbl 0746.35025
Krantz, Steven G.; Paulsen, William H.
1991
On the dimensions of the automorphism groups of hyperbolic Reinhardt domains. Zbl 0968.32001
Gifford, J. A.; Isaev, A. V.; Krantz, S. G.
2000
Characterizations of various domains of holomorphy via $$\overline\partial$$ estimates and applications to a problem of Kohn. Zbl 0394.32009
Krantz, Steven G.
1979
Boundary values and estimates for holomorphic functions of several complex variables. Zbl 0431.32004
Krantz, Steven G.
1980
A matter of gravity. Zbl 1045.51007
Krantz, Steven G.
2003
Geometric characterizations of centroids of simplices. Zbl 1089.52009
Krantz, Steven G.; McCarthy, John E.; Parks, Harold R.
2006
Function theory of one complex variable. Zbl 0880.30003
Greene, Robert E.; Krantz, Steven G.
1997
Analysis of some function spaces associated to Hankel operators. Zbl 0878.47012
Krantz, Steven G.; Li, Song-Ying; Rochberg, Richard
1997
Finite type conditions on Reinhardt domains. Zbl 0955.32028
Fu, Siqi; Isaev, Alexander V.; Krantz, Steven G.
1996
The effect of boundary geometry on Hankel operators belonging to the trace ideals of Bergman spaces. Zbl 0903.47019
Krantz, Steven G.; Li, Song-Ying; Rochberg, Richard
1997
A Kobayashi metric version of Bun Wong’s theorem. Zbl 1172.32002
Kim, Kang-Tae; Krantz, Steven G.
2009
Lorentz boundedness and compactness characterization of integral commutators on spaces of homogeneous type. Zbl 1457.42027
Dao, Nguyen Anh; Krantz, Steven G.
2021
True epidemic growth construction through harmonic analysis. Zbl 1437.92124
Krantz, Steven G.; Polyakov, Peter; Rao, Arni S. R. Srinivasa
2020
Differential equations. A modern approach with wavelets. Zbl 1454.34001
Krantz, Steven G.
2020
$$L^p$$ regularity of the Bergman projection on domains covered by the polydisc. Zbl 1457.32003
Chen, Liwei; Krantz, Steven G.; Yuan, Yuan
2020
Applications of Bergman representative coordinates. Zbl 1442.32003
Krantz, Steven G.
2020
The Besicovitch covering lemma and maximal functions. Zbl 1418.42030
Krantz, Steven G.
2019
The Fefferman-Szegő metric and applications. Zbl 1417.32014
Krantz, Steven G.
2019
Complex variables. A physical approach with applications. 2nd edition. Zbl 1410.30001
Krantz, Steven G.
2019
Canonical kernels versus constructible kernels. Zbl 1429.30016
Krantz, Steven G.
2019
Geometric analysis on the Diederich-Fornæss index. Zbl 1400.32018
Krantz, Steven George; Liu, Bingyuan; Peloso, Marco Maria
2018
On a theorem of F. Forelli and a result of Hartogs. Zbl 1387.32003
Krantz, Steven G.
2018
Uniqueness properties of Hardy space functions. Zbl 1393.32003
Krantz, Steven G.
2018
Semicontinuity of automorphism groups: the converse direction. Zbl 1398.32030
Krantz, Steven G.
2018
Harmonic and complex analysis in several variables. Zbl 1414.32001
Krantz, Steven G.
2017
The weighted Bergman kernel and the Green’s function. Zbl 1361.30096
Krantz, Steven; Wójcicki, Paweł M.
2017
A primer of mathematical writing. Being a disquisition on having your ideas recorded, typeset, published, read, and appreciated. 2nd edition. Zbl 1390.00064
Krantz, Steven G.
2017
Bergman kernel and projection on the unbounded Diederich-Fornaess worm domain. Zbl 1377.32003
Krantz, Steven G.; Peloso, Marco M.; Stoppato, Caterina
2016
The Greene-Krantz conjecture in dimension two. Zbl 1405.32026
Krantz, Steven G.
2016
Local maximum modulus property for polyanalytic functions. Zbl 1332.30070
Daghighi, Abtin; Krantz, Steven G.
2016
Erratum: A note on a conjecture concerning boundary uniqueness. Zbl 1403.30014
Daghighi, Abtin; Krantz, Steven
2016
Smoothness to the boundary of biholomoprhic mappings: an overview. Zbl 1345.32016
Krantz, Steven G.
2015
Convex analysis. Zbl 1310.26001
Krantz, Steven G.
2015
Reflections on Paul Erdős on his birth centenary. Zbl 1338.01020
Lóvasz, László; Sós, Vera T.; Graham, Ronald L.; Spencer, Joel; Kahane, Jean-Pierre; Nathanson, Melvyn B.
2015
A note on a conjecture concerning boundary uniqueness. Zbl 1319.30027
Daghighi, Abtin; Krantz, Steven G.
2015
A direct connection between the Bergman and Szegő projections. Zbl 1297.32005
Krantz, Steven G.
2014
The Corona problem. Connections between operator theory, function theory, and geometry. Selected papers based on the workshop, Toronto, Canada, June 2012. Zbl 1297.30004
2014
The impact of the theorem of Bun Wong and Rosay. Zbl 1290.32019
Krantz, Steven G.
2014
The Corona problem in several complex variables. Zbl 1317.32004
Krantz, Steven G.
2014
Real analysis and foundations. 3rd ed. Zbl 1278.26001
Krantz, Steven G.
2014
The implicit function theorem. History, theory, and applications. Reprint of the 2003 hardback edition. Zbl 1269.58003
Krantz, Steven G.; Parks, Harold R.
2013
Geometric analysis of the Bergman kernel and metric. Zbl 1281.32004
Krantz, Steven G.
2013
Semicontinuity of automorphism groups of strongly pseudoconvex domains: the low differentiability case. Zbl 1271.32021
Greene, Robert E.; Kim, Kang-Tae; Krantz, Steven G.; Seo, Aeryeong
2013
The Carathéodory and Kobayashi/Royden metrics by way of dual extremal problems. Zbl 1277.32014
Royden, Halsey; Wong, Pit-Mann; Krantz, Steven G.
2013
The automorphism groups of domains in complex space: a survey. Zbl 1274.32001
Krantz, Steven G.
2013
A guide to functional analysis. Zbl 1271.46001
Krantz, Steven G.
2013
On limits of sequences of holomorphic functions. Zbl 1294.30011
Krantz, Steven G.
2013
The Kobayashi metric, extremal discs, and biholomorphic mappings. Zbl 1246.32012
Krantz, Steven G.
2012
The automorphism group of a domain with an exponentially flat boundary point. Zbl 1227.32031
Krantz, Steven G.
2012
Geometric properties of boundary orbit accumulation points. Zbl 1247.32020
Krantz, Steven G.
2012
The Schwarz lemma at the boundary. Zbl 1227.30023
Krantz, Steven G.
2011
The geometry of complex domains. Zbl 1239.32011
Greene, Robert E.; Kim, Kang-Tae; Krantz, Steven G.
2011
Convergence of automorphisms and semicontinuity of automorphism groups. Zbl 1271.32018
Krantz, Steven G.
2011
The proof is in the pudding. The changing nature of mathematical proof. Zbl 1318.00005
Krantz, Steven G.
2011
Boundary decomposition of the Bergman kernel. Zbl 1226.30006
Krantz, Steven G.
2011
Convexity in real analysis. Zbl 1246.26010
Krantz, Steven G.
2011
On a construction of L. Hua for positive reproducing kernels. Zbl 1197.32002
Krantz, Steven G.
2010
Essentials of topology with applications. Zbl 1178.54001
Krantz, Steven G.
2010
Normed domains of holomorphy. Zbl 1196.32009
Krantz, Steven G.
2010
The corona problem with two pieces of data. Zbl 1204.32004
Krantz, Steven G.
2010
On the iterated logarithmic Bloch space on the unit ball. Zbl 1221.47056
Krantz, Steven G.; Stević, Stevo
2009
Explorations in harmonic analysis. With applications to complex function theory and the Heisenberg group. Zbl 1171.43001
Krantz, Steven G.
2009
A Kobayashi metric version of Bun Wong’s theorem. Zbl 1172.32002
Kim, Kang-Tae; Krantz, Steven G.
2009
An ontology of directional regularity implying joint regularity. Zbl 1186.26008
Krantz, Steven G.
2009
A guide to topology. Zbl 1170.54001
Krantz, Steven G.
2009
Geometric integration theory. Zbl 1149.28001
Krantz, Steven G.; Parks, Harold R.
2008
The Bergman kernel and projection on non-smooth worm domains. Zbl 1161.32016
Krantz, Steven G.; Peloso, Marco M.
2008
Analysis and geometry on worm domains. Zbl 1147.32020
Krantz, Steven G.; Peloso, Marco M.
2008
Complex scaling and geometric analysis of several variables. Zbl 1156.32001
Kim, Kang-Tae; Krantz, Steven G.
2008
A guide to complex variables. Zbl 1147.30001
Krantz, Steven G.
2008
New results on the Bergman kernel of the worm domain in complex space. Zbl 1140.32310
Krantz, Steven G.; Peloso, Marco M.
2008
The Carathéodory and Kobayashi metrics and applications in complex analyis. Zbl 1177.30060
Krantz, Steven G.
2008
Pseudoconvexity, analytic discs and invariant metrics. Zbl 1162.32007
Krantz, Steven G.
2008
A tale of three kernels. Zbl 1157.32005
Krantz, Steven G.
2008
The Hartogs extension phenomenon redux. Zbl 1140.32007
Krantz, Steven G.
2008
On functions in $$p$$-adic $$BMO$$ and the distribution of prime integers. Zbl 1119.46029
Krantz, Steven G.
2007
The Carathéodory-Cartan-Kaup-Wu theorem on an infinite-dimensional Hilbert space. Zbl 1143.46024
Cima, Joseph A.; Graham, Ian; Kim, Kang Tae; Krantz, Steven G.
2007
The Lindelöf principle in several complex variables. Zbl 1109.32006
Krantz, Steven G.
2007
The boundary behavior of holomorphic functions: global and local results. Zbl 1141.32002
Krantz, Steven G.
2007
A tribute to Professor william f. ames on his 80th birthday. Zbl 1151.01322
Agarwal, Ravi P.; Krantz, Steven G.
2007
How to write your first paper. Zbl 1145.00301
Krantz, Steven G.
2007
Geometric function theory. Explorations in complex analysis. Zbl 1086.30001
Krantz, Steven G.
2006
Function theory of one complex variable. 3rd ed. Zbl 1114.30001
Greene, Robert E.; Krantz, Steven G.
2006
Geometric characterizations of centroids of simplices. Zbl 1089.52009
Krantz, Steven G.; McCarthy, John E.; Parks, Harold R.
2006
On determining sets for holomorphic automorphisms. Zbl 1144.32012
Fridman, B. L.; Kim, K.-T.; Krantz, S. G.; Ma, D.
2006
Calculus. Multivariable. Zbl 1098.26002
Blank, Brian E.; Krantz, Steven G.
2006
Calculation and estimation of the Poisson kernel. Zbl 1060.31004
Krantz, Steven G.
2005
Analytic polyhedra in $$\mathbb C^2$$ with a non-compact automorphism group. Zbl 1062.32020
Kim, Kang-Tae; Krantz, Steven G.; Spiro, Andrea F.
2005
Real analysis and foundations. 2nd ed. Zbl 1056.26001
Krantz, Steven G.
2005
The automorphism groups of domains. Zbl 1138.32302
Kim, Kang-Tae; Krantz, Steven G.
2005
Two results on uniqueness of conformal mappings. Zbl 1083.30010
Krantz, Steven G.
2005
Mathematical publishing. A guidebook. Zbl 1084.00004
Krantz, Steven G.
2005
Mathematical apocrypha redux. More stories and anecdotes of mathematicians and the mathematical. Zbl 1082.00002
Krantz, Steven G.
2005
Complex analysis: the geometric viewpoint. 2nd ed. Zbl 1051.30001
Krantz, Steven G.
2004
Creating more convergent series. Zbl 1044.40001
Krantz, Steven G.; McNeal, Jeffery D.
2004
Some new results on domains in complex space with non-compact automorphism group. Zbl 1035.32019
Kim, Kang-Tae; Krantz, Steven G.
2003
A matter of gravity. Zbl 1045.51007
Krantz, Steven G.
2003
Normal families of holomorphic functions and mappings on a Banach space. Zbl 1069.46026
Kim, Kang-Tae; Krantz, Steven G.
2003
Determining sets and fixed points for holomorphic endomorphisms. Zbl 1053.32010
Kim, Kang-Tae; Krantz, Steven G.
2003
The Bergman metric invariants and their boundary behavior. Zbl 1048.32002
Kim, Kang-Tae; Krantz, Steven G.
2003
A primer of real analytic functions. 2nd ed. Zbl 1015.26030
Krantz, Steven G.; Parks, Harold R.
2002
The implicit function theorem. History, theory, and applications. Zbl 1012.58003
Krantz, Steven G.; Parks, Harold R.
2002
A note on the Wong-Rosay theorem in complex manifolds. Zbl 1044.32019
Gaussier, Hervé; Kim, Kang-Tae; Krantz, Steven G.
2002
On fixed points and determining sets for holomorphic automorphisms. Zbl 1026.32042
Fridman, B. L.; Kim, K. T.; Krantz, S. G.; Ma, D.
2002
Characterization of the Hilbert ball by its automorphism group. Zbl 1007.32002
Kim, Kang-Tae; Krantz, Steven G.
2002
Function theory of one complex variable. 2nd ed. Zbl 0988.30001
Greene, Robert E.; Krantz, Steven G.
2002
Determination of a domain in complex space by its automorphism group. Zbl 1030.32018
Krantz, Steven G.
2002
A smoothly bounded domain in a complex surface with a compact quotient. Zbl 1028.32010
Cheung, Wing Sum; Fu, Siqi; Krantz, Steven G.; Wong, Bun
2002
Function theory of several complex variables. Reprint of the 1992 2nd ed. with corrections. Zbl 1087.32001
Krantz, Steven G.
2001
Boundedness and compactness of integral operators on spaces of homogeneous type and applications. I. Zbl 0990.47042
Krantz, Steven G.; Li, Song-Ying
2001
Boundedness and compactness of integral operators on spaces of homogeneous type and applications. II. Zbl 0990.47043
Krantz, Steven G.; Li, Song-Ying
2001
...and 106 more Documents
all top 5
### Cited by 2,385 Authors
94 Krantz, Steven George 27 Kim, Kang-Tae 22 Stević, Stevo 18 Örnek, Bülent Nafi 15 Liu, Taishun 14 Yang, Dachun 13 Tu, Zhenhan 12 Chang, Der-Chen E. 12 Isaev, Alexander 12 Li, Songying 12 Shoikhet, David 11 de la Llave, Rafael 11 Duong, Xuan Thinh 11 Huang, Xiaojun 11 Peloso, Marco Maria 10 Byun, Jisoo 10 Dovbush, Peter V. 10 Ha, Ly Kim 10 Ninh Văn Thu 10 Tang, Xiaomin 9 Fridman, Buma L. 9 Gaussier, Hervé 9 Lebl, Jiří 9 Lee, Kang-Hyurk 9 Ma, Daowei 9 Verma, Kaushal 9 Yang, Dongyong 9 Zimmer, Andrew M. 8 Chen, Shaolin 8 McNeal, Jeffery D. 8 Noell, Alan V. 8 Yang, Sibei 8 Zeytuncu, Yunus Ergýn 7 Brackx, Fred F. 7 Chakrabarti, Debraj 7 Choe, Boo Rim 7 De Schepper, Hennie 7 Fornæss, John Erik 7 Fu, Siqi 7 Greene, Robert Everist 7 Harrington, Phillip S. 7 Lanzani, Loredana 7 Liu, Bingyuan 7 Peralta-Salas, Daniel 7 Seshadri, Harish 7 Stein, Elias Menachem 7 Straube, Emil J. 7 Wu, Huoxiong 7 Yamamori, Atsushi 7 Yan, Lixin 6 Agler, Jim 6 Berhanu, Shiferaw 6 Bernal-Gonzàlez, Luis 6 Boas, Harold P. 6 Bracci, Filippo 6 Čučković, Željko 6 Guo, Kunyu 6 Li, Songxiao 6 Mitrea, Marius 6 Nestoridis, Vassili 6 Nicolay, Samuel 6 Pan, Yifei 6 Ravisankar, Sivaguru 6 Şahutoğlu, Sönmez 6 Shamoyan, Romi F. 6 Wang, Jianfei 6 Wick, Brett D. 6 Zhang, Liyou 5 Akyel, Tuğba 5 Alpay, Daniel Aron 5 Cao, Jun 5 Chen, Bo-Yong 5 Chen, Dazhao 5 Cho, Hong Rae 5 Cho, Sanghyun 5 Ding, Yong 5 Elin, Mark 5 Engliš, Miroslav 5 Gong, Sheng 5 Haslinger, Friedrich 5 Hu, Zhangjian 5 Kim, Hyeseon 5 Klep, Igor 5 Lee, Young Joo 5 Li, Ji 5 Liu, Yongmin 5 Monguzzi, Alessandro 5 Nikolov, Nikolai Marinov 5 Popescu, Gelu 5 Ren, Guangbin 5 Shapiro, Michael V. 5 Sommen, Franciscus 5 Ungar, Abraham Albert 5 Yin, Wanke 5 Yu, Yanyan 5 Zhang, Shuo 5 Zheng, Dechao 5 Zhou, Xiangyu 4 Auscher, Pascal 4 Bandtlow, Oscar F. ...and 2,285 more Authors
all top 5
### Cited in 437 Serials
157 Journal of Mathematical Analysis and Applications 125 The Journal of Geometric Analysis 74 Proceedings of the American Mathematical Society 59 Transactions of the American Mathematical Society 53 Journal of Functional Analysis 49 Complex Variables and Elliptic Equations 48 Mathematische Annalen 47 Advances in Mathematics 36 Mathematische Zeitschrift 34 Complex Analysis and Operator Theory 29 Applied Mathematics and Computation 27 Journal of Differential Equations 21 Duke Mathematical Journal 21 Integral Equations and Operator Theory 19 Journal d’Analyse Mathématique 18 Annales de l’Institut Fourier 18 Science China. Mathematics 17 Rocky Mountain Journal of Mathematics 15 Michigan Mathematical Journal 15 Nonlinear Analysis. Theory, Methods & Applications. Series A: Theory and Methods 15 Linear Algebra and its Applications 15 Journal of Inequalities and Applications 14 Annali di Matematica Pura ed Applicata. Serie Quarta 13 Journal of Approximation Theory 13 Manuscripta Mathematica 13 Monatshefte für Mathematik 13 Science in China. Series A 13 International Journal of Mathematics 12 Communications in Mathematical Physics 12 Annali della Scuola Normale Superiore di Pisa. Classe di Scienze. Serie IV 12 Communications in Partial Differential Equations 12 Comptes Rendus. Mathématique. Académie des Sciences, Paris 11 Archiv der Mathematik 11 Bulletin of the American Mathematical Society. New Series 10 Israel Journal of Mathematics 10 Automatica 10 Inventiones Mathematicae 10 SIAM Journal on Mathematical Analysis 10 Annales de la Faculté des Sciences de Toulouse. Mathématiques. Série VI 10 Potential Analysis 10 European Series in Applied and Industrial Mathematics (ESAIM): Control, Optimization and Calculus of Variations 10 Acta Mathematica Sinica. English Series 10 Computational Methods and Function Theory 9 Results in Mathematics 9 Bulletin des Sciences Mathématiques 9 Analysis and Mathematical Physics 9 Journal of Function Spaces 8 Mathematische Nachrichten 8 Tohoku Mathematical Journal. Second Series 8 Systems & Control Letters 8 Annals of Global Analysis and Geometry 8 Journal de Mathématiques Pures et Appliquées. Neuvième Série 8 Indagationes Mathematicae. New Series 8 Calculus of Variations and Partial Differential Equations 8 Advances in Applied Clifford Algebras 8 The Journal of Fourier Analysis and Applications 8 Complex Analysis and its Synergies 7 Archive for Rational Mechanics and Analysis 7 Computers & Mathematics with Applications 7 Journal of Statistical Physics 7 Mathematical Notes 7 Nagoya Mathematical Journal 7 Revista Matemática Iberoamericana 7 Geometric and Functional Analysis. GAFA 7 Journal of Mathematical Sciences (New York) 7 Filomat 6 Bulletin of the Australian Mathematical Society 6 Mathematical Methods in the Applied Sciences 6 Collectanea Mathematica 6 Journal of Computational and Applied Mathematics 6 Physica D 6 Journal of the American Mathematical Society 6 Forum Mathematicum 6 Expositiones Mathematicae 6 Abstract and Applied Analysis 5 Arkiv för Matematik 5 Chaos, Solitons and Fractals 5 Indiana University Mathematics Journal 5 Kodai Mathematical Journal 5 Memoirs of the American Mathematical Society 5 Pacific Journal of Mathematics 5 Proceedings of the Edinburgh Mathematical Society. Series II 5 Chinese Annals of Mathematics. Series B 5 Constructive Approximation 5 Annales Academiae Scientiarum Fennicae. Mathematica 5 Communications of the Korean Mathematical Society 5 Mediterranean Journal of Mathematics 5 Revista de la Real Academia de Ciencias Exactas, Físicas y Naturales. Serie A: Matemáticas. RACSAM 4 Applicable Analysis 4 Journal of Mathematical Physics 4 Acta Mathematica Vietnamica 4 Annales Polonici Mathematici 4 Czechoslovak Mathematical Journal 4 Illinois Journal of Mathematics 4 Journal of Economic Theory 4 Journal of the Korean Mathematical Society 4 Topology and its Applications 4 Bulletin of the Korean Mathematical Society 4 Probability Theory and Related Fields 4 Journal of Complexity ...and 337 more Serials
all top 5
### Cited in 59 Fields
883 Several complex variables and analytic spaces (32-XX) 322 Functions of a complex variable (30-XX) 308 Operator theory (47-XX) 285 Partial differential equations (35-XX) 240 Functional analysis (46-XX) 191 Harmonic analysis on Euclidean spaces (42-XX) 128 Differential geometry (53-XX) 94 Global analysis, analysis on manifolds (58-XX) 80 Dynamical systems and ergodic theory (37-XX) 76 Numerical analysis (65-XX) 75 Real functions (26-XX) 75 Potential theory (31-XX) 72 Probability theory and stochastic processes (60-XX) 64 Ordinary differential equations (34-XX) 51 Calculus of variations and optimal control; optimization (49-XX) 51 Systems theory; control (93-XX) 45 Approximations and expansions (41-XX) 40 Convex and discrete geometry (52-XX) 36 Algebraic geometry (14-XX) 36 Linear and multilinear algebra; matrix theory (15-XX) 36 Fluid mechanics (76-XX) 33 Operations research, mathematical programming (90-XX) 32 Mechanics of deformable solids (74-XX) 31 Measure and integration (28-XX) 30 Combinatorics (05-XX) 30 Quantum theory (81-XX) 29 Statistics (62-XX) 29 Statistical mechanics, structure of matter (82-XX) 26 Topological groups, Lie groups (22-XX) 26 Game theory, economics, finance, and other social and behavioral sciences (91-XX) 25 Number theory (11-XX) 25 Computer science (68-XX) 22 Biology and other natural sciences (92-XX) 21 Abstract harmonic analysis (43-XX) 20 Mathematical logic and foundations (03-XX) 20 Manifolds and cell complexes (57-XX) 19 Special functions (33-XX) 18 Integral equations (45-XX) 17 Difference and functional equations (39-XX) 17 General topology (54-XX) 16 Mechanics of particles and systems (70-XX) 15 Geometry (51-XX) 13 Group theory and generalizations (20-XX) 11 Information and communication theory, circuits (94-XX) 10 Relativity and gravitational theory (83-XX) 9 History and biography (01-XX) 8 Integral transforms, operational calculus (44-XX) 5 Field theory and polynomials (12-XX) 5 Optics, electromagnetic theory (78-XX) 3 General and overarching topics; collections (00-XX) 3 Commutative algebra (13-XX) 3 Associative rings and algebras (16-XX) 3 Geophysics (86-XX) 3 Mathematics education (97-XX) 2 Nonassociative rings and algebras (17-XX) 2 Category theory; homological algebra (18-XX) 2 Sequences, series, summability (40-XX) 1 $$K$$-theory (19-XX) 1 Astronomy and astrophysics (85-XX)
### Wikidata Timeline
The data are displayed as stored in Wikidata under a Creative Commons CC0 License. Updates and corrections should be made in Wikidata.
| 2022-05-18T03:30:38 |
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|
https://www.ncbj.gov.pl/en/seminaria-konwersatoria/theoretical-physics-division-seminar?page=3
|
# Theoretical Physics Division seminar
• ## POSSIBLE UNITARITY OF BLACK HOLE EVAPORATION
In the framework of finite-dimensional Fock space models, for a fixed given mean number of particles $\bar{n}_{k}$, blackbody-like or another, it is shown that there are, in the space $S$ of all pure states, a multi-dimensional subspace $s_{\bar{n}_{k}}$ of initial pure states and a corresponding multi-dimensional subspace $S_{\bar{n}_{k}}$ of final pure states yielding $\bar{n}_{k}$, which are mutually related by a unitary transformation.
• ## High-energy QCD: towards precision
In this talk, I will discuss some recent and ongoing theoretical progresses concerning Quantum Chromodynamics in the regime of high-energy scattering, or equivalently low Bjorken x, in which the nonlinearity of the gluon field dynamics is essential. I will focus mostly on advances in higher order computations, aiming at a precise description of this nonlinear regime.
You're welcome,
• English translation unavailable for Evolution equations for medium-induced QCD cascades and their solutions.
• English translation unavailable for Probing BFKL effects with forward Drell-Yan production.
• English translation unavailable for ,,Dynamics of a quantum phase transition: Kibble-Zurek scaling hypothesis''.
• English translation unavailable for Singularity avoidance for collapsing quantum dust in the Lemaître-Tolman-Bondi model.
• English translation unavailable for Pseudo Nambu-Goldstone Dark Matter.
• English translation unavailable for Co to znaczy skwantować układ klasyczny: uwagi i przestrogi.
• English translation unavailable for Beginners view on resurgence.
| 2023-04-02T00:28:23 |
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|
https://math.wikia.org/wiki/Pythagorean_theorem/Proof
|
1,183 Pages
Theorem
, where are the sides of a right triangle, is the hypotenuse, and are the legs.
Theorem. '
Prerequisites:
Formula for area of triangle
Additive nature of area
Proof.
Construct a square of arbitrary side length . Construct a second square, larger than the first, and place it such that each side is tangent to exactly one vertex of the first square, forming four congruent right triangles such that is the length of the hypotenuse. Let represent the length of one leg of a triangle and let represent the length of the second leg. Since area is additive in nature, the area of the larger square is equivalent to the sum of the area of the smaller square and the area of the triangles:
Community content is available under CC-BY-SA unless otherwise noted.
| 2020-12-05T06:00:41 |
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https://docs.nersc.gov/tutorials/playbooks/compiling/
|
# Compiling a code on NERSC resources¶
## Purpose¶
This playbook will guide you through the steps to compile a code on NERSC's Perlmutter supercomputer.
### Overview of process¶
From the perspective of a person compiling code, there are three phases in the code compilation process.
First, we will set up the environment to prepare it to compile the code, by figuring out the dependencies and other requirements, and then customizing the build settings to enable this.
Second, we will build the application by compiling human-readable code into machine-readable object files, and linking object files and libraries into a binary.
Finally, we will install the code in the appropriate location, where you can access it and run it within a job (batch or interactive).
#### How code is compiled (from a technical perspective)¶
Compiling a code is a multistep process. First, the compiler translates human-readable code into machine-readable object files. To do this, it may need additional inputs, called "include" or "header" files. The location of these files, if they are not included in the compiler's default search directories, must be provided to the compiler and are denoted with a -I flag on the compile line (e.g., -I /path/to/include). The products of this compilation process, called object files, are usually named with a .o suffix. They may be linked together into a library file in an intermediate step.
The final step is to combine object files and library files into the final executable. This step is known as linking. During this process, the linker makes sure that all variables and functions or subroutines that are used in the code are defined. It searches for the required libraries in default directories and directories provided by the user with the -L flag (e.g., -L /path/to/libs). The names of required libraries beyond the defaults are denoted by -lname (for a library file with the actual name libname.a or libname.so).
An executable may be statically linked or dynamically linked. A statically linked executable is self-contained; all object files and library files are bundled together into a single large file. During link time, the linker searches for library files terminating in .a to include in the executable. On the other hand, a dynamically linked executable is generally smaller and contains a list of directories where the shared-object libraries (generally terminating in a .so suffix) reside. When the dynamically linked executable is invoked, it loads the necessary libraries at runtime.
## Steps¶
1. Determine dependencies and requirements.
4. Set up build configuration.
5. Build and install the code.
## Detailed instructions¶
### Step 1: Determine dependencies and requirements¶
Look at the documentation for the code you want to compile. There may be documentation available online, or else there could be a file included in the package called README or INSTALL or something similar. This is a crucial first step -- usually the developers will explain how to compile the code. Even if it doesn't make much sense at first, reading the instructions and following that by reading this playbook should help to clarify matters.
Something important to examine is the code's dependency (if any) on other software. Does the code have any dependencies on other libraries? Does it use MPI for parallelization? Does it use any I/O libraries? Does it use numerical libraries? Does it require BLAS subroutines?
If your code uses MPI, then you will use the ftn, cc, and/or CC compiler wrappers for code written in Fortran, C, or C++ (respectively) when compiling.
NERSC may have other common dependencies available through its module system. Use module spider <example> to search for a package called <example>. If you find one you're looking for, make a note of it, as in the third step, we will load that module.
BLAS subroutines are available in the Cray libsci module and will be linked into the final executable automatically if you are using the compiler wrappers.
If you cannot find a particular package, you may need to compile it yourself. In this case, repeat this step focused on that dependency.
Download the packages that you need to install the code. Common commands for accessing code from a public repository include
• wget https://url.for.code/path/to/code/code-version.tar.gz (for a code that provides tar files as releases)
• git clone https://github.com/project/code.git (for a code with a repository on Github that can be cloned)
• scp [email protected]:mydir/myfile.tar.gz ./mydir (for copying a gzipped tar file from another.cluster to the directory mydir, invoking this command from a NERSC machine. You'll need to authenticate to the other cluster.)
If the code you've downloaded is a tar file or a zip file, you'll need to expand it. The following table provides useful commands for this.
File Suffix Example Command
.tar tar -xvf file.tar
.tar.gz. tar -xvzf file.tar.gz
.tgz tar -xvzf file.tgz
.zip gunzip file.zip
Make sure your source code ends up in an appropriate location. You can download a tar file, cd to the directory where you want the source code, and then invoke the command to expand the downloaded file (be sure to provide the path to the downloaded file in your command!). Many users store source code in their home directory or in their project CFS directory. If you download it to scratch, it could be purged from the system!
In Step 1, we determined which modules would be relevant and useful for this code. At this point, we now load the modules. Note that some modules may require prerequisite modules to be loaded.
### Step 4: Set up build configuration¶
There are many different build systems that are used to compile. The most common ones are Makefiles, Autoconf, and CMake.
#### Makefiles¶
A makefile orchestrates the compilation of object files and their linking into libraries or executables. For some applications, makefiles are provided that need to be customized for the platform. For tips on customizing makefiles, see the section on editing makefiles in the NERSC build tools documentation.
#### Autoconf¶
This is the canonical method for building code, and often the simplest. An automated script called configure sets up the configuration of makefiles.
The configure script takes options, which set variables in the makefile. For more information about configure as applied in the NERSC environment, please see the NERSC Autoconf Documentation
The configuration process could fail if settings are not quite right. Look for error outputs and adjust configuration settings accordingly. Reinvoking configure overwrites any previous settings.
#### CMake¶
CMake is similar to Autotools in the sense that it is an automation that sets up the configuration of Makefiles. But, it is a much more powerful tool that can do much more complex processes. For a typical user, we can ignore most of its features and focus on a minimum set.
CMake can sometimes have trouble finding the Cray compiler wrappers, so we recommend invoking it in the following way:
CC=$(which cc) CXX=$(which CC) FC=\$(which ftn) <cmake command>
### Step 5: Build and install the code¶
For most codes that used makefiles or autoconf, simply typing make on the command line begins the build process. We recommend keeping a record of what took place during the compilation (especially handy when there's been a build error!) by redirecting the output of the make command to a file.
make > make.log &
(The optional ampersand backgrounds the process, which is handy if you want to do something else in the shell while you wait for your code to compile.) If you want to watch the text scroll by as it happens, use the tee command to send the make output to both a file and the screen:
make | tee make.log
If there are issues in the compilation, you can generally wipe the slate clean by invoking make clean, which removes object files that were compiled, then start over.
For CMake, the command could instead be cmake --build . (or something similar) and as the compilation progresses a percent progress is reported.
After our executable has been successfully compiled, it can be installed with the make install command. (Check your instructions -- this step is not always required.) The most common error in this phase occurs when the install directory has not been set properly. Build systems often default to a system-level installation directory, which is not accessible to NERSC users. Correcting the installation directory (often called prefix in the case of autobuild) in the configuration stage will solve this problem.
## Troubleshooting¶
Even the most experienced NERSC staff encounter errors as they proceed to build a new piece of software the first time. Sometimes instructions are incomplete, or the uniqueness of the system environment results in a unique situation. Fortunately, error messages from build tools and compilers are often helpful.
Because build errors are common, you can often find out how to solve your problem by using your favorite search engine to browse for matches to key words in your error message. And of course, you can submit a ticket for any issue that has you truly stumped.
| 2023-03-20T15:53:46 |
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|
https://bomberosbogota.gov.co/calendario/ano/2021?mini=2022-01
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| 2022-01-19T17:24:06 |
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|
https://par.nsf.gov/biblio/10296795-mixing-uncertainties-low-metallicity-agb-stars-impact-stellar-structure-nucleosynthesis
|
Mixing Uncertainties in Low-Metallicity AGB Stars: The Impact on Stellar Structure and Nucleosynthesis
The slow neutron-capture process (s-process) efficiency in low-mass AGB stars (1.5 < M/M⊙ < 3) critically depends on how mixing processes in stellar interiors are handled, which is still affected by considerable uncertainties. In this work, we compute the evolution and nucleosynthesis of low-mass AGB stars at low metallicities using the MESA stellar evolution code. The combined data set includes models with initial masses Mini/M⊙=2 and 3 for initial metallicities Z=0.001 and 0.002. The nucleosynthesis was calculated for all relevant isotopes by post-processing with the NuGrid mppnp code. Using these models, we show the impact of the uncertainties affecting the main mixing processes on heavy element nucleosynthesis, such as convection and mixing at convective boundaries. We finally compare our theoretical predictions with observed surface abundances on low-metallicity stars. We find that mixing at the interface between the He-intershell and the CO-core has a critical impact on the s-process at low metallicities, and its importance is comparable to convective boundary mixing processes under the convective envelope, which determine the formation and size of the 13C-pocket. Additionally, our results indicate that models with very low to no mixing below the He-intershell during thermal pulses, and with a 13C-pocket size of at least more »
Authors:
; ; ; ;
Award ID(s):
Publication Date:
NSF-PAR ID:
10296795
Journal Name:
Universe
Volume:
7
Issue:
2
Page Range or eLocation-ID:
25
ISSN:
2218-1997
1. ABSTRACT In this work, we investigate the impact of uncertainties due to convective boundary mixing (CBM), commonly called ‘overshoot’, namely the boundary location and the amount of mixing at the convective boundary, on stellar structure and evolution. For this we calculated two grids of stellar evolution models with the MESA code, each with the Ledoux and the Schwarzschild boundary criterion, and vary the amount of CBM. We calculate each grid with the initial masses of 15, 20, and $25\, \rm {M}_\odot$. We present the stellar structure of the models during the hydrogen and helium burning phases. In the latter, we examine the impact on the nucleosynthesis. We find a broadening of the main sequence with more CBM, which is more in agreement with observations. Furthermore, during the core hydrogen burning phase there is a convergence of the convective boundary location due to CBM. The uncertainties of the intermediate convective zone remove this convergence. The behaviour of this convective zone strongly affects the surface evolution of the model, i.e. how fast it evolves redwards. The amount of CBM impacts the size of the convective cores and the nucleosynthesis, e.g. the 12C to 16O ratio and the weak s-process. Lastly, we determinemore »
3. ABSTRACT We have modelled the multicycle evolution of rapidly accreting CO white dwarfs (RAWDs) with stable H burning intermittent with strong He-shell flashes on their surfaces for 0.7 ≤ MRAWD/M⊙ ≤ 0.75 and [Fe/H] ranging from 0 to −2.6. We have also computed the i-process nucleosynthesis yields for these models. The i process occurs when convection driven by the He-shell flash ingests protons from the accreted H-rich surface layer, which results in maximum neutron densities Nn, max ≈ 1013–1015 cm−3. The H-ingestion rate and the convective boundary mixing (CBM) parameter ftop adopted in the one-dimensional nucleosynthesis and stellar evolution models are constrained through three-dimensional (3D) hydrodynamic simulations. The mass ingestion rate and, for the first time, the scaling laws for the CBM parameter ftop have been determined from 3D hydrodynamic simulations. We confirm our previous result that the high-metallicity RAWDs have a low mass retention efficiency ($\eta \lesssim 10{{\ \rm per\ cent}}$). A new result is that RAWDs with [Fe/H] $\lesssim -2$ have $\eta \gtrsim 20{{\ \rm per\ cent}}$; therefore, their masses may reach the Chandrasekhar limit and they may eventually explode as SNeIa. This result and the good fits of the i-process yields from the metal-poor RAWDs to the observed chemicalmore »
| 2022-11-27T06:29:19 |
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|
http://dlmf.nist.gov/8.2
|
# §8.2 Definitions and Basic Properties
## §8.2(i) Definitions
The general values of the incomplete gamma functions $\mathop{\gamma\/}\nolimits\!\left(a,z\right)$ and $\mathop{\Gamma\/}\nolimits\!\left(a,z\right)$ are defined by
8.2.1 $\displaystyle\mathop{\gamma\/}\nolimits\!\left(a,z\right)$ $\displaystyle=\int_{0}^{z}t^{a-1}e^{-t}dt,$ $\realpart{a}>0$, Defines: $\mathop{\gamma\/}\nolimits\!\left(a,z\right)$: incomplete gamma function Symbols: $dx$: differential of $x$, $e$: base of exponential function, $\int$: integral, $\realpart{}$: real part, $z$: complex variable and $a$: parameter Referenced by: §8.2(iii), §8.6(i), §8.6(ii) Permalink: http://dlmf.nist.gov/8.2.E1 Encodings: TeX, pMML, png 8.2.2 $\displaystyle\mathop{\Gamma\/}\nolimits\!\left(a,z\right)$ $\displaystyle=\int_{z}^{\infty}t^{a-1}e^{-t}dt,$ Defines: $\mathop{\Gamma\/}\nolimits\!\left(a,z\right)$: incomplete gamma function Symbols: $dx$: differential of $x$, $e$: base of exponential function, $\int$: integral, $z$: complex variable and $a$: parameter A&S Ref: 6.5.3 Referenced by: §8.2(i), §8.2(iii), §8.21(iii), §8.6(i) Permalink: http://dlmf.nist.gov/8.2.E2 Encodings: TeX, pMML, png
without restrictions on the integration paths. However, when the integration paths do not cross the negative real axis, and in the case of (8.2.2) exclude the origin, $\mathop{\gamma\/}\nolimits\!\left(a,z\right)$ and $\mathop{\Gamma\/}\nolimits\!\left(a,z\right)$ take their principal values; compare §4.2(i). Except where indicated otherwise in the DLMF these principal values are assumed. For example,
8.2.3 $\mathop{\gamma\/}\nolimits\!\left(a,z\right)+\mathop{\Gamma\/}\nolimits\!\left% (a,z\right)=\mathop{\Gamma\/}\nolimits\!\left(a\right),$ $a\neq 0,-1,-2,\dots$.
Normalized functions are:
8.2.4 $\displaystyle\mathop{P\/}\nolimits\!\left(a,z\right)$ $\displaystyle=\frac{\mathop{\gamma\/}\nolimits\!\left(a,z\right)}{\mathop{% \Gamma\/}\nolimits\!\left(a\right)},$ $\displaystyle\mathop{Q\/}\nolimits\!\left(a,z\right)$ $\displaystyle=\frac{\mathop{\Gamma\/}\nolimits\!\left(a,z\right)}{\mathop{% \Gamma\/}\nolimits\!\left(a\right)},$ Defines: $\mathop{P\/}\nolimits\!\left(a,z\right)$: normalized incomplete gamma function and $\mathop{Q\/}\nolimits\!\left(a,z\right)$: normalized incomplete gamma function Symbols: $\mathop{\Gamma\/}\nolimits\!\left(z\right)$: gamma function, $\mathop{\Gamma\/}\nolimits\!\left(a,z\right)$: incomplete gamma function, $\mathop{\gamma\/}\nolimits\!\left(a,z\right)$: incomplete gamma function, $z$: complex variable and $a$: parameter A&S Ref: 6.5.1 (The function $\mathop{Q\/}\nolimits\!\left(a,z\right)$ is not defined in AMS 55.) Referenced by: §8.11(v) Permalink: http://dlmf.nist.gov/8.2.E4 Encodings: TeX, TeX, pMML, pMML, png, png
8.2.5 $\mathop{P\/}\nolimits\!\left(a,z\right)+\mathop{Q\/}\nolimits\!\left(a,z\right% )=1.$
8.2.6 $\mathop{\gamma^{*}\/}\nolimits\!\left(a,z\right)=z^{-a}\mathop{P\/}\nolimits\!% \left(a,z\right)=\frac{z^{-a}}{\mathop{\Gamma\/}\nolimits\!\left(a\right)}% \mathop{\gamma\/}\nolimits\!\left(a,z\right).$ Defines: $\mathop{\gamma^{*}\/}\nolimits\!\left(a,z\right)$: incomplete gamma function Symbols: $\mathop{\Gamma\/}\nolimits\!\left(z\right)$: gamma function, $\mathop{\gamma\/}\nolimits\!\left(a,z\right)$: incomplete gamma function, $\mathop{P\/}\nolimits\!\left(a,z\right)$: normalized incomplete gamma function, $z$: complex variable and $a$: parameter A&S Ref: 6.5.4 Referenced by: §8.2(iii), §8.6(i) Permalink: http://dlmf.nist.gov/8.2.E6 Encodings: TeX, pMML, png
8.2.7 $\mathop{\gamma^{*}\/}\nolimits\!\left(a,z\right)=\frac{1}{\mathop{\Gamma\/}% \nolimits\!\left(a\right)}\int_{0}^{1}t^{a-1}e^{-zt}dt,$ $\realpart{a}>0$.
## §8.2(ii) Analytic Continuation
In this subsection the functions $\mathop{\gamma\/}\nolimits$ and $\mathop{\Gamma\/}\nolimits$ have their general values.
The function $\mathop{\gamma^{*}\/}\nolimits\!\left(a,z\right)$ is entire in $z$ and $a$. When $z\neq 0$, $\mathop{\Gamma\/}\nolimits\!\left(a,z\right)$ is an entire function of $a$, and $\mathop{\gamma\/}\nolimits\!\left(a,z\right)$ is meromorphic with simple poles at $a=-n$, $n=0,1,2,\dots$, with residue $(-1)^{n}/n!$.
For $m\in\Integer$,
8.2.8 $\displaystyle\mathop{\gamma\/}\nolimits\!\left(a,ze^{2\pi mi}\right)$ $\displaystyle=e^{2\pi mia}\mathop{\gamma\/}\nolimits\!\left(a,z\right),$ $a\neq 0,-1,-2,\dots$, 8.2.9 $\displaystyle\mathop{\Gamma\/}\nolimits\!\left(a,ze^{2\pi mi}\right)$ $\displaystyle=e^{2\pi mia}\mathop{\Gamma\/}\nolimits\!\left(a,z\right)+(1-e^{2% \pi mia})\mathop{\Gamma\/}\nolimits\!\left(a\right).$
(8.2.9) also holds when $a$ is zero or a negative integer, provided that the right-hand side is replaced by its limiting value. For example, in the case $m=-1$ we have
8.2.10 $e^{-\pi ia}\mathop{\Gamma\/}\nolimits\!\left(a,ze^{\pi i}\right)-e^{\pi ia}% \mathop{\Gamma\/}\nolimits\!\left(a,ze^{-\pi i}\right)=-\frac{2\pi i}{\mathop{% \Gamma\/}\nolimits\!\left(1-a\right)},$
without restriction on $a$.
Lastly,
8.2.11 $\mathop{\Gamma\/}\nolimits\!\left(a,ze^{\pm\pi i}\right)=\mathop{\Gamma\/}% \nolimits\!\left(a\right)(1-z^{a}e^{\pm\pi ia}\mathop{\gamma^{*}\/}\nolimits\!% \left(a,-z\right)).$
## §8.2(iii) Differential Equations
If $w=\mathop{\gamma\/}\nolimits\!\left(a,z\right)$ or $\mathop{\Gamma\/}\nolimits\!\left(a,z\right)$, then
8.2.12 $\frac{{d}^{2}w}{{dz}^{2}}+\left(1+\frac{1-a}{z}\right)\frac{dw}{dz}=0.$
If $w=e^{z}z^{1-a}\mathop{\Gamma\/}\nolimits\!\left(a,z\right)$, then
8.2.13 $\frac{{d}^{2}w}{{dz}^{2}}-\left(1+\frac{1-a}{z}\right)\frac{dw}{dz}+\frac{1-a}% {z^{2}}w=0.$
Also,
8.2.14 $z\frac{{d}^{2}\mathop{\gamma^{*}\/}\nolimits}{{dz}^{2}}+(a+1+z)\frac{d\mathop{% \gamma^{*}\/}\nolimits}{dz}+a\mathop{\gamma^{*}\/}\nolimits=0.$
| 2015-09-03T23:25:40 |
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|
https://publications.drdo.gov.in/ojs/index.php/dsj/article/download/4673/4550
|
Modeling of Cooling and Solidification of TNT based Cast High Explosive Charges
Cast trinitrotoluene (TNT) based high explosive charges suffer from different defects such as cracks, voids, etc. One of the quality control measures is to cool the castings gradually, so that the entire charge solidifies without a large temperature gradient from core to the periphery of the cast charge. The fact that the solidification of high explosive casting starts from the periphery (cooler side) and travels towards the center enables us to predict the solidification profile of TNT based explosive castings. Growth of solidification thickness and cooling temperature profiles of TNT based cast high explosive charges are predicted as functions of time and space using unsteady state heat transfer principles, associated with heat balance at solid to liquid interface as a moving boundary of solidification. This will enable adoption of proper quality control during solidification of the molten TNT to eliminate inherent drawbacks of cast high explosive charges. The solidification profiles of TNT based cast charges under controlled and natural conditions are predicted and the model is validated against 145 mm diameter TNT cast charge which is found to be in broad agreement with experiments.
C Specific heat of TNT
hsf Latent heat of fusion of TNT
k Thermal conductivity of TNT
ρ Density
r Reference radius at any time
T0 Initial temperature
Tf Fusion (melting) temperature of TNT
Tw Wall temperature
δ Solidification thickness
ά (= k/ρ C) Thermal diffusivity
l Liquid
sv Solid
B Polynomial constant (B=1 at r=0 & Tl = T0)
φ Dimensionless temperature parameter
S Dimensionless sub cooling parameter
Dimensionless numbers
$\delta +=\frac{\delta }{R}$
t+ = ά.t/R2
a+ = ά1/ άs
The two main high explosive loading techniques in military ammunition are pressing and casting. All high caliber bombs, warheads, etc., are filled by casting method in general, with trinitrotoluene (TNT) as casting medium. Some of the serious defects of TNT casting are the shrinkage that occurs as the filling solidifies, formation of voids and pores due to entrapped air, dissolved gases, and improper feeding of casting material1. The casting solidifies from outside and the consequent shrinkage is that of an isolated mass at the center of the casting2. The shrinkage takes place in the axial direction. Improper control of specific transport mechanisms will lead to cracking of charge due to excessive thermal stresses. It is also seen that in homogeneous crystal growth takes place as the casting solidifies3. These deficiencies in the casting of high explosive will not only alter the detonation profile but may also lead to accidental and premature explosion in dynamic conditions. As such an explosive charge is required to withstand a dynamic load of 200 MPa4.
Entrapped air can be removed by mechanical means such as hot probing, vibration, etc. But this may not compensate for the shrinkage. In the casting, shrinkage can be minimized by carefully cooling the charge under controlled conditions5. Crystal size can also be controlled by varying the rate of heat transfer6, especially towards its softening temperature of around 80 °C. As casting is a heat transfer problem with phase change7, prediction of solid-liquid interface position is important for the filling of explosives in shells and moulds as it helps in optimizing the filling conditions.
Plastic bonded explosives (PBXs) are replacing the TNT based explosives to overcome these deficiencies, especially for underwater weapons8. However, bulk production facilities are not yet fully established for PBXs. Filling of PBXs in warheads is expensive and time consuming. In view of this fact, TNT based charges are still being manufactured around the world for military applications. Hence, the present study is of practical importance. In the present study, growth rate of solidification thickness (or solidification period) and cooling rates are computed. The predicted profiles and the experimental results are compared. A 145 mm caliber TNT based charge, when allowed to solidify under controlled conditions is seen to give better quality explosive charge in terms of explosive loading, increased density and reduced porosity. This results in better explosive parameters.
The physical model of solidification problem is shown in Fig. 1. At time zero, the vertical cylindrical mould of radius R is filled with the molten explosive. Cooling is provided on the outer surface of the mould so that the temperature of the mould wall remains constant at ${T}_{w}$ . Solidification, commencing at the inner side of wall of the mould extends towards the central core of the explosive. For t > 0, the solidified thickness is δ. The heat flow in the liquid $\left(0\le r\le R-\delta \right)$ and solid $\left(R-\delta \le r\le R\right)$ regions of the explosive are governed by the equation of unsteady state heat conduction as9.
${\rho }_{l}{C}_{l}\frac{d{T}_{l}}{dt}\text{\hspace{0.17em}}=\frac{{k}_{l}}{r}\text{\hspace{0.17em}}\frac{d}{dr}\left[r\frac{d{T}_{l}}{dr}\right]$ $for\text{\hspace{0.17em}}\text{\hspace{0.17em}}0\le r\le \left(R-\delta \right)$ (1a)
${\rho }_{s}{C}_{s}\frac{d{T}_{s}}{dt}=\frac{{k}_{s}}{r}\frac{d}{dr}\left[r\frac{d{T}_{s}}{dr}\right]$ $for\text{\hspace{0.17em}}\text{\hspace{0.17em}}\left(R-\delta \right)\le r\le R$ (1b)
2.1Initial Condition
Initially, the explosive contained in the mould is in the molten state at a uniform temperature ${T}_{l}={T}_{o}$
Thus, at $t=0,{T}_{l}={T}_{o}\text{\hspace{0.17em}}\text{\hspace{0.17em}}for\text{\hspace{0.17em}}\text{\hspace{0.17em}}0\le r\le R$ (2)
2.2 Boundary Conditions
At any instance of time, the temperature is maximum at the axis of the cylindrical charge, i.e., at r=0. This fact, by virtue of symmetry at r=0, can be mathematically represented as.
At r = 0, $\frac{d{T}_{1}}{dr}=0$ (3)
Pressure within the mould is constant. Hence, the temperature at the liquid- solid interface remains constant at Tf where Tf is the phase change temperature of TNT.
At $r=R-\delta ,\text{\hspace{0.17em}}{T}_{l}={T}_{s}={T}_{f,\text{\hspace{0.17em}}}$ where ${T}_{f}$ is constant (4) The above condition is presumed, as constant temperature is maintained at the wall.
At r = R, T = Tw, where Tw is constant (5)
2.3 Heat Balance at the Liquid–solid Interface
T1, the temperature within the liquid phase is higher than the phase change temperature Tf of TNT. Thus, the sensible and latent heats liberated at r = R-δ, the liquid–solid interface are conducted through the solid phase to the coolant at r=R. The resulting equation of heat balance is given below10.
${k}_{s}\frac{d{T}_{s}}{dr}|\begin{array}{l}\\ r=R-\delta \end{array}={k}_{l}\frac{d{T}_{l}}{dr}|\begin{array}{l}\\ r=R-\delta \end{array}-{\rho }_{{}_{S}}{h}_{sf}\frac{d\delta }{dt}$ (6)
El-Genk and Cronenberg11 demonstrated that the problem of unsteady state heat conduction with moving boundary can become one of continuous growth, or asymptotic growth, or growth-and-decay depending on the boundary conditions imposed. Because of the adiabatic condition of heat flow at the center, i.e., at r=0, continuous growth of the solid crust takes place in the present case. integral method is used to solve Eqn. (1) for liquid phase. In this method, the equation in liquid phase is integrated with respect to r in the appropriate range of r, i.e., r=0 to (R-δ). The resulting equation is given below.
${\rho }_{l}{C}_{l}\frac{d}{dt}\underset{0}{\overset{\left(R-\delta \right)}{\int }}r\left({T}_{l}-{T}_{f}\right)dr={k}_{l}\left(R-\delta \right)\frac{d{T}_{l}}{dr}|\begin{array}{l}\\ r=R-\delta \end{array}$ (7)
Temperature profiles are assumed for use in and evaluation of Eqns. (6) and (7). These profiles are for $0\le r\le \left(R-\delta \right)$
$\frac{{T}_{l}-{T}_{f}}{{T}_{o}-{T}_{f}}=B\left[1-{\left[\frac{r}{R-\delta }\right]}^{2}\right]$ (8)
and for $\left(R-\delta \right)\le r\le R:$
$\frac{{T}_{f}-{T}_{s}}{{T}_{f}-{T}_{w}}=\left[\frac{r-R+\delta }{\delta }\right]$ (9)
Temperature profiles given by Eqns. (8) and (9) are obtained subject to the boundary conditions Eqns. (3) - (5).
Equations (6) and (7) are evaluated using Eqns. (8) and (9) to yield differential equations:
$\frac{d{\delta }^{+}}{d{t}^{+}}=S\left[\frac{1-{\delta }^{+}\left(1-2B\phi \right)}{{\delta }^{+}\left(1-{\delta }^{+}\right)}\right]$ (10)
$\frac{dB}{d{t}^{+}}=\frac{2B\left[S\left(1-{\delta }^{+}\left(1-2B\phi \right)\right)-4{\alpha }^{+}{\delta }^{+}\right]}{{\delta }^{+}{\left(1-{\delta }^{+}\right)}^{2}}$ (11)
where $\phi =\frac{{k}_{l}\left({T}_{o}-{T}_{f}\right)}{{k}_{s}\left({T}_{f}-{T}_{w}\right)}and\text{\hspace{0.17em}}\text{\hspace{0.17em}}\text{\hspace{0.17em}}S=\frac{{C}_{s}\left({T}_{f}-{T}_{w}\right)}{{h}_{sf}}$
${\delta }^{+}=\frac{\delta }{R}\text{\hspace{0.17em}}\text{\hspace{0.17em}}and\text{\hspace{0.17em}}\text{\hspace{0.17em}}{t}^{+}=\text{\hspace{0.17em}}{\alpha }_{s}\text{\hspace{0.17em}}\frac{t}{{R}^{2}};\text{\hspace{0.17em}}\text{\hspace{0.17em}}{\alpha }_{s}=\text{\hspace{0.17em}}\frac{{k}_{s}}{\left({\rho }_{s}{C}_{s}\right)};\text{\hspace{0.17em}}\text{\hspace{0.17em}}\alpha +=\frac{{a}_{l}}{{a}_{s}}$ where φ and S are the dimensionless temperature parameter and sub cooling parameter respectively. Equations (10) and (11) are simultaneously solved for δ+ and B by fourth-order Runge-Kutta method with the initial conditions that at t+ =0, δ+ =0 and B=1 The values of parameters φ and s given below are calculated from above relations for T0=90°C and Tw=18°C using approximated thermo-physical properties of TNT12 which are summarized in Table 1.
Table 1.Thermo-physical properties of TNT.
TNT (Special Grade) manufactured in one of the Indian Ordnance Factories was used in the experiments. Melting point, purity and theoretical density of TNT are 80.6 °C, 99.799 % (JSS 1376-02:2004 (Rev. 03)) and 1.654 g/cc respectively, and are assumed to be constant for simplicity. Thermal conductivity of TNT is very poor as compared to stainless steel or even as compared to water.
Before conducting the experiments, solid TNT was melt in a jacketed anchor blade mixer and poured into a preheated jacketed stainless steel mould of 145 mm diameter and 350 mm height. The initial temperature of the mould was kept uniform and only liquid phase was allowed to exist. Explosive charge of diameter 145 mm and height 270 mm is realized from this set up. The upper portion, up to about 60 mm of the solidified charge was of very poor quality with pores, uneven finish and piping. This part of the charge was removed by machining. The final charge was of dimensions ϕ 145 x 190 mm (height). The experimental arrangement is shown in Fig. 2. The test conditions are reflected. In Fig. 3. Symmetry enables the solution to be carried out only for a representative half of the charge which is shown in Fig. 3.
The temperature of the charge was monitored and controlled through six PT-100 temperature sensors inserted to a depth of 65 mm at six different equi-spaced radial points along the diameter of the charge and connected to the master controller.
Radial points are chosen as the length to diameter ratio is more than 1.5. This is also because of the reason that the interior quality of the charge is established by testing the mould product by dissection for density equality, blowholes, cracks and shrink holes radially13. The rate of cooling was controlled by an indigenously developed 8085 microprocessor based control system which regulated the flow of hot water/steam or compressed air through a set of solenoid valves either to heat or cool respectively. The maximum scatter of temperature observed during the cooling process was about 4°C (±2%). The central core temperature was considered for generation of experimental temperature profile. The predicted and experimental solidification profiles are compared in Fig. 4. Cooling trends of charge at the top of the charge (30 mm) are monitored, both under natural and controlled conditions were monitored and plotted in Fig. 5.
Different solidification periods were computed by varying Tw in the model in order to study the effect of wall temperature. The same is shown in Fig. 6.
The cast charges cooled under different conditions were cut into smaller discs and the densities were determined by using Archimedes’s principle. The density values along with the porosity values (with < 1% variation) are furnished in Table 2. Porosities in the specimen samples were calculated using the formula.
In the solid, the temperature decreases due to the growth of frozen layer, while in the liquid, the distributions change relatively little during the course of the solidification. The temperature gradient in the solid near the interface initially is much greater and then decreases at later times and finally approaches the temperature gradient in the liquid phase. As the casting solidifies from periphery to the core, the thickness of solid TNT grows towards the center. Initially, solidification of TNT is expected to be faster than at later stages in view of its poor conductivity. Therefore, solidification (the motion of the solid-liquid interface) slows down and finally sieges, when equilibrium temperature is attained1. This can be very clearly seen from Fig. 4, where initially solidification rate is relatively fast and slowed down as time lapsed. The deviation that is seen between the predicated and experimental profiles may be due to the uncertainties in the approximated thermo-physical properties and experimental conditions.
From the temperature profiles under plant (natural cooling) and laboratory (controlled cooling) conditions as can be seen from Fig. 5, it indicates that in the former case solidification is complete in about 4 h and 30 min and the temperature falls to 50 °C in about 7 h indicating that the process of solidification takes place between 50 °C and 60 °C14. This only resulted in poor quality charge. Whereas, in controlled cooling where the outside temperature was maintained, the charge took about 13 h to completely come to uniform phase change temperature along the diameter. This period is arrived at from Fig. 4, where the charge took this time to solidify. Then the liquid phase quickly solidified simultaneously throughout the diameter without leaving any voids. This yielded good quality charge without cracks and voids. Cooling the charge at lower Tw reduces the solidification time due to higher temperature gradient. However, this results in large amount of porosity in the charge, since only little time is available for the molten TNT to fill the pores caused by occluded air. As a result a very inferior quality charge is obtained15,16. At the same time if the Tw is high, solidification time is appreciably high as can be seen from Fig. 6, while not bringing about any significant change in the charge quality. Under natural cooling conditions, density of solid TNT achieved is 1.55 g/cc while under controlled (Tw around 50°C) conditions, density increases to 1.60 g/cc. It is known that every 0.01 g/cc density variation brings in about 2 % variation in explosive energy17. Thus, 0.05 g/cc increase in density by adopting controlled cooling will better the explosive energy by 10 %. Reduction of porosity from 2 % to 0.5 %, would result in an improvement of VOD, detonation pressure and Shaped charge jet velocity by 1.2 %, 4.5 %, and 1.7 % respectively18.
Table 2.Charge analysis.
The model predicts the solidification time and temperature profile of cast explosives more or less accurately. The predicted profile of cooling is in good agreement with experimental profile. By predicting the solidification time, the density of the charge and the porosity can be estimated and thus corrective measures can be exercises by optimizing the plant conditions.
It can be concluded that for an explosive of 145 mm caliber, the optimum cooling temperature is about 50 °C and the solidification time is around 14 h at 50 °C for obtaining higher charge density, which in turn boosts the explosive parameters like velocity of detonation, detonation pressure, etc.
The authors express their gratitude to Dr Haridwar Singh, Director (Retd.), Shri J. S. Gharia, Sc ‘G’ (Retd.), HEMRL, Pune for giving permission to carry out the experimental work. The authors express their gratitude to Shri C.D. Malleswar, Director, NSTL, Visakhapatnam for according permission and for his encouragement to publish this paper.
1. Li, S.; Mine, K.; Sanakanishi, S. & Anzai, K. Quantitative prediction method for shrinkage porosity considering molten metal supply by pressure in squeeze casting. Material Transaction, 2007, 48 (8), 2186-93.
2. Gonzalez, M.; Goldschmit, M.B.; Assanelli, A.P.; Berdaguer, E.F. & Dvorkin, E.N. Modeling of the solidification process in a continuous casting installation for steel slabs. Metall. Mater. Trans. B, 2003, 34B, 455-73.
3. Mudryy, R. & Nastec, L. Computational multi phase modeling of cast energetic materials. EPD Congress 2013, TMS, Multi Structure Evolution II, John Wiley Publications, 2013. 31-38.
4. Li, W.; Yan, H.; Zhang, Q. & Ji, Y.H. Compression process of pores inside explosive charge in a warhead under launching load. Def. Sci. J., 2010, 60(3), 244-50.
5. Agrawal, J.P. High energy materials, processing of explosives. Wiley VCH Publication, 2010, p. 164.
6. Fleming, Merton C. Solidification processing. McGraw Hill Book co., New York, 1974.
7. Sun, D. & Garimella, S.V. Numerical and experimental investigation of solidification shrinkage. Numer. Heat Trans. A-Appl., 2007, 52 (2), 145-62.
8. Kumar, A.S.; Rao, V.B.; Sinha, R.K. & Rao, A.S. Evaluation of plastic bonded explosive (PBX) formulations based on RDX, aluminum, and HTPB for underwater applications. Propell. Explos. Pyrot., 2010, 35(4), 359–64.
9. Bird, R.B.; Stuward, W.E. & Lightfoot E.N. Transport phenomena. John Wiley, New York, 1960.
10. Carslaw, S. & Jaeger, J. Conduction of heat in solids. Ed. 2. Oxford University Press, London, 1973.
11. El-Genk, M.S. & Cronenberg, A.W. Stefan-like problem in finite geometry. AIChE Symposium Series, 75, 1979, 69-80.
12. Srihakulung, O. & Soongsumal, Y. Improving TNT curing process by using Infrared camera. World Academy of Science, Engineering and Technology, 2011, 5, 803-05.
13. Zhang, W.; Tian, Y.; Zhou, H.; Yang, Z.; Luo, G. & Zong, H. Process monitoring of cast explosive solidification molding by on-line multichannel ultrasonic measurement. Paper presented at 17th World Conference on Nondestructive Testing, Shanghai, China, Oct. 2008, 25-28.
14. Engineering design handbook, warhead general (U), 1964, AMCP 706-290, 125
15. Chen, Chun-Ye & Shiuan, Jonq-Hwa. Numerical simulation of casting explosives in shell. Propell. Explos. Pyrot., 1992, 17 (1), 20-26.
16. Sun, D.; Garimella, S.V.; Singh, S. & Naik, N. Numerical and experimental investigation of the melt casting of explosives. Propell. Explos. Pyrot., 2005, 30(5), 369–80.
17. Murphy, M.J. The effects of gradients in HMX/TNT content and porosity on shaped charge jet characteristics.In Proceedings of the 11th Symposium (International) on Ballistics, 1989, 189-197.
18. Gharia, J.S.; Kumar, A.S.; Raghavendra, L.N. & Vadali, S.R. Effect of density gradient and porosity on HMX/TNT pressure cast shaped charge performance. Propell. Explos. Pyrot., 1996, 21(1), 36-39.
Dr A. Srinivas Kumar Dr A. Srinivas Kumar obtained his PhD (Chemical Engineering) from College of Engineering (A), Andhra University, Visakhapatnam. He is currently working as Scientist ‘G’ at NSTL, Visakhapatnam. His fields of specialisation are: High explosives and high energy batteries. He has 16 Papers published in International and National Journals. Dr Dharma Rao Vedula Dr Dharma Rao Vedula is working as a professor in GVP College of Engineering (A) in the Department of Mechanical Engineering following his retirement in the year 2011 from Andhra University College of Engineering (A) in the Department of Chemical Engineering. He guided 10 PhD students and Published 47 Research papers in refereed International Journals. He participated as Collaborative Researcher with University of Miami, USA.
| 2019-10-23T12:56:50 |
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# Quantification of Potential Inequities in Breast Cancer Incidence in New Mexico Through Bayesian Disease Mapping
#### David Zahrieh, PhD1; Michael A. Golafshar, MS2; Samir H. Patel, MD3; Todd A. DeWees, PhD2,3 (View author affiliations)
Suggested citation for this article: Zahrieh D, Golafshar MA, Patel SH, DeWees TA. Quantification of Potential Inequities in Breast Cancer Incidence in New Mexico Through Bayesian Disease Mapping. Prev Chronic Dis 2021;18:200468. DOI: http://dx.doi.org/10.5888/pcd18.200468external icon.
PEER REVIEWED
Summary
What is already known on this topic?
Breast cancer incidence among non-Hispanic American Indian and Alaska Native (AI/AN) women has been quantified in large geographic regions of the United States, showing substantial regional variation in incidence inequities among non-Hispanic AI/AN populations.
What is added by this report?
We found substantial evidence in New Mexico of an overall reduction in breast cancer incidence among at-risk non-Hispanic AI/AN women compared with non-Hispanic White women in certain counties in the state.
What are the implications for public health practice?
Our findings can facilitate targeted statewide and county-level cancer control interventions to mitigate such disparities.
## Abstract
Introduction
The incidence of breast cancer among non-Hispanic American Indian and Alaska Native (AI/AN) women varies across the United States. We applied county-level Bayesian disease mapping to quantify potential inequities in 10-year breast cancer incidence in New Mexico to better inform health equity initiatives among its non-Hispanic at-risk AI/AN population.
Methods
We used data from the Surveillance, Epidemiology, and End Results (SEER) program from 2005 through 2014 to identify new cases of breast cancer in New Mexico’s 33 counties. To account for spatial variation, a county-level Area Deprivation Index, and the small area estimation problem inherent in these data, we borrowed strength globally and locally by applying Bayesian disease mapping to the counts of age-adjusted county-level breast cancer incidence. We quantified the disparity effect, as measured by the age-adjusted rate ratio, comparing the incidence of breast cancer between at-risk non-Hispanic AI/AN and non-Hispanic White women and assessed whether the ratio differed among counties.
Results
Accounting for over-dispersion and spatial correlation among the 33 counties and a county-level Area Deprivation Index, the posterior mean of the overall age-adjusted rate ratio was 0.384 (95% credible interval, 0.253–0.546). The age-adjusted rate of breast cancer in non-Hispanic AI/AN women was 0.38 times the corresponding age-adjusted rate for non-Hispanic White women; however, a significant reduction in breast cancer incidence was observed in 16 of the 33 counties.
Conclusion
The application of Bayesian disease mapping to these data provided substantial evidence of an overall disparity in breast cancer incidence between at-risk non-Hispanic AI/AN and non-Hispanic White women in New Mexico, which was more marked than previously reported and limited to certain counties. Targeted statewide and county-level health-equity initiatives may lead to a reduction in these disparities.
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## Introduction
In the past 2 decades, substantial progress has been made in the United States in reducing breast cancer death rates for non-Hispanic White women; however, this reduction has not been shared by non-Hispanic American Indian and Alaska Native (AI/AN) women (1). The corresponding mortality-to-incidence ratio is higher for non-Hispanic AI/AN women than for non-Hispanic White women (1). This inequity has persisted despite breast cancer being amenable to screening and treatment. A possible contributor to the higher mortality-to-incidence ratio may be a lower prevalence of mammography use among non-Hispanic AI/AN women compared with non-Hispanic White women (2). Mammography can detect breast cancer in its early stages when it may respond better to treatment (3). Although use of mammography has recently increased among non-Hispanic AI/AN women, its use remains below Healthy People 2020 targets and lower than among other racial/ethnic subgroups (4).
An important indicator of health status in the non-Hispanic AI/AN population is breast cancer incidence. This incidence has primarily been quantified in large geographic regions of the United States (1,5,6). The less favorable regional-level breast cancer incidence rates reported among non-Hispanic AI/AN versus non-Hispanic White women in the southwestern region of the United States underscore the need to continue to quantify potential inequities in breast cancer outcomes, and at a more granular county level, to facilitate targeted cancer control interventions to mitigate such disparities.
Our aim was to quantify potential disparities in breast cancer incidence between non-Hispanic AI/AN women and non-Hispanic White women in New Mexico overall and in each of its 33 counties during our 10-year study period, 2005 through 2014. New Mexico has 23 federally recognized tribes and, based on 2015 estimates, AI/ANs make up nearly 10.5% of the state’s population (7). Because we were interested in obtaining precise local estimates of breast cancer incidence among each racial/ethnic group at the county level as well as assessing broad trends across the state, we used Bayesian disease mapping, which can be implemented to account for spatial variation. It can also account for county-level covariates when quantifying such potential inequities and can address the small area estimation problem inherent in these data by borrowing strength globally and locally across the state (8).
By using Surveillance, Epidemiology, and End Results (SEER) (9) program data from 2005 through 2014, we applied Bayesian disease mapping to address 3 study-specific questions to quantify potential inequities in 10-year breast cancer incidence in New Mexico:
1. Is the overall incidence of breast cancer among at-risk non-Hispanic AI/AN women excessively low compared with non-Hispanic White women?
2. Does the rate ratio, comparing the incidence of breast cancer between at-risk non-Hispanic AI/AN women and non-Hispanic White women, differ among New Mexico counties?
3. Do some counties in New Mexico have a lower breast cancer incidence among at-risk AI/AN women than would be expected?
Research into these questions can contribute to planning public health services and interventions in New Mexico that may lead to reducing disparities in breast cancer outcomes among non-Hispanic AI/AN at-risk women.
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## Methods
### Data preparation
Data were limited to AI/AN and White women of non-Hispanic origin who were aged 15 years or older (Figure 1). From the data on the 38,997 women in the SEER registry who received a diagnosis of breast cancer, 13,135 were diagnosed from 2005 through 2014. County of residence was known for 12,974 of these women, of whom 8,794 were of non-Hispanic origin. After excluding other racial/ethnic groups (109 Asian or Pacific Islander, 164 Black, and 60 unknown race), our population surveillance data consisted of 8,461 women with breast cancer (567 non-Hispanic AI/AN women, 7,894 non-Hispanic White women) diagnosed from 2005 through 2014 across the 33 counties. Data on the number of women at risk were obtained from US Census Bureau data for 2010, the midpoint of our study period, and retrieved in 5-year age intervals (eg, 15–19 y). Although the risk of breast cancer for women aged 15 to 17 is low, to avoid excluding at-risk women aged 18 and 19, we retrieved the number at risk in the 15 to 19 age interval in addition to all higher 5-year age intervals. Therefore, we considered 443,814 non-Hispanic AI/AN and non-Hispanic White women aged 15 years or older at risk for breast cancer. These data were extended to include county-level Area Deprivation Index (ADI) scores developed by Mayo Clinic researchers (10), which were measured from 17 indicators that served as a surrogate for income, employment, housing, and education.
### Statistical analysis
To address questions on disparate incidence, we applied a single Bayesian Poisson hierarchical model to model the county-level, age-adjusted number of women with breast cancer defined as
where yiar denotes the number of women with breast cancer in county i, age group a, racial group r, and πa denotes the proportion of the 2010 US female population aged 15 years or older in age group a. Here, i ranges from 1 to 33; a ∈ {15 − 19, 20 − 24, …, 80 – 84, 85+} and r = 0 (non-Hispanic White population) or r = 1 (non-Hispanic AI/AN population). Also, let nir denote the population size at risk in the ith county for the rth racial group. Then, the hierarchical model proposed to address our study-specific questions can be expressed as
log (λir) = β0 + β1x1 + β2x2 + β3x1x2 + θir + ϕir
with x1 denoting an indicator variable, which takes the value 1 if r = 1 (non-Hispanic AI/AN population) and zero if r = 0 (non-Hispanic White population), and x2 denoting an indicator variable, which takes the value 1 if county-level ADI is in the lower 20th percentile and zero otherwise.
The inclusion of the interaction term permitted the disparity effect to be different at each level of the county-level variable x2. The prior distribution for each parameter β1, β2, and β3 was set to a normal distribution with mean 0 and variance 1,000, while a flat prior was assumed for β0. The θir captured region-wide heterogeneity via an ordinary, exchangeable normal prior,
θir~ N(0,τh),
where τh is a variance term. These random effects captured extra-Poisson variability (or over-dispersion) in the log-relative risks that varied globally (ie, over the entire state). Finally, the random effects ϕir are the parameters that make this a spatial model by capturing regional clustering. That is, they modeled extra-Poisson variability in the log-relative risks that varied locally, so that nearby counties would have more similar rates. Spatial association was defined through a neighborhood structure where 1 county was related to other counties that shared a common border and determined by an adjacency matrix. To specify the spatial association, we assumed a race-specific improper conditional autoregressive (CAR) (11) specification for ϕ.r such that for each racial group r we have
ϕ.r =0~CAR(τb; r= 0) and ϕ.r = 1~ CAR(τc; r = 1)
The variance parameters τh, τb, and τc were given standard deviation uniform prior distributions in the range of 0 to 100 (12). The inclusion of both spatially uncorrelated (θ) and spatially correlated (ϕ) heterogeneity effects also addressed the small area estimation problem by borrowing strength globally and locally, respectively.
We used Markov chain Monte Carlo (MCMC) sampling to estimate posterior quantiles for the proposed Bayesian Poisson hierarchical model; R (R Foundation) and OpenBUGS (13) were used to fit the proposed hierarchical model. Estimated posterior quantiles were based on 3 chains, including a burn-in period for each chain. A long run of the sampler was required because of high levels of autocorrelation; therefore, samples were thinned by using only every fiftieth step in the sampler as a strategy for dealing with the otherwise overwhelming amounts of MCMC output (14). Consequently, posterior distributions were based on 60,000 samples, or 20,000 per chain. The deviance information criterion (DIC) was used to assess model adequacy (15). In our application, a difference in DIC greater than 2 was used to ascertain if the DIC was exhibiting a preference.
To answer our first question, we reported and interpreted the estimated posterior mean and 95% credible interval for the overall rate ratio defined as the ratio of the statewide average rates in each racial category (non-Hispanic AI/AN vs non-Hispanic White), or $λ-∙1λ-∙0$, where and . To answer the second question, we present the estimated posterior means and corresponding 95% credible intervals for each county-level rate ratio (non-Hispanic AI/AN vs non-Hispanic White women), defined as $λi1λi0$ for the ith county. Finally, within the non-Hispanic AI/AN population, we reported and interpreted the estimated posterior mean and 95% credible interval for each county-level rate ratio (ie, the non-Hispanic AI/AN county-level rate vs the statewide average rate within non-Hispanic AI/AN), or $λi1λ-∙1$ , to answer our last question.
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## Results
Of the 443,814 at-risk women in our 2010 sample, 75,048 (16.9%) were non-Hispanic AI/AN. For each of the 33 New Mexico counties in New Mexico, we calculated the county-level ADI based on 2012 socioeconomic data according to the lower 20%, middle 60%, and upper 20% (Figure 2). The 20th and 80th percentile ADI were 101.6 and 120.8, respectively, and the median ADI was 110.2 (range, 39.2–149.8); higher values correspond to increased socioeconomic disadvantage.
In the estimated posterior quantities from fitting the proposed model (Table 1), the expected [standard deviation] estimate of the standard deviation associated with the spatially correlated heterogeneity effects suggested strong spatial patterning in the non-Hispanic AI/AN population (√τc: 0.567 [0.499]), whereas this was not the case in the non-Hispanic White population (√τb: 0.143 [0.110]). We mapped the sum of the posterior averages of the county-specific random effects ϕ and θ that were exponentiated within the non-Hispanic White population and the corresponding non-Hispanic AI/AN population (Figure 3). Interpreting the excess variability observed in the data in this fashion isolates the upper half of the state as an area of generally increased risk of breast cancer diagnosis in both maps, but those northern areas of increased risk are largely concentrated in the north-central regions in the non-Hispanic White population; furthermore, the northern areas of elevated risk of breast cancer diagnosis are more pronounced in the non-Hispanic AI/AN population. Although the areas of low risk of breast cancer diagnosis in the non-Hispanic AI/AN population are seen across the lower half of the state, the regions of low risk within the non-Hispanic White population are confined to the southeastern portion of the state.
The posterior mean of the overall, age-adjusted rate ratio was 0.384 (95% credible interval, 0.253–0.546). These data provide evidence of a significant overall disparity effect across New Mexico. The estimated rate of breast cancer in non-Hispanic AI/AN women was approximately 0.38 times the corresponding age-adjusted rate for non-Hispanic White women. Making allowance for the unobserved confounders θ and ϕ as well as allowing the disparity effect to be different across the 2 levels of the county-level ADI variable, we calculated the posterior mean for the age-adjusted rate ratio for each county on the basis of the proposed model (Table 2). For 16 of the 33 counties, the 95% credible intervals for the age-adjusted rate ratios were less than 1, while for the remaining 17 counties the 95% credible intervals included the null value of 1. It is worth noting that the 7 smallest posterior means for the age-adjusted rate ratios coincided with the 7 counties in the lowest 20th percentile for ADI. We also estimated posterior mean and 95% credible interval for each county-level rate ratio in the non-Hispanic AI/AN population. Compared with the average rate of breast cancer incidence in the non-Hispanic AI/AN population, the relative risk of breast cancer was largely constant across all counties, and all 95% credible intervals for the age-adjusted rate ratios were wide and included 1. Because the results depended on prior specifications, we examined sensitivity to prior specification. On the basis of these sensitivity analyses, our conclusions remained unchanged.
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## Discussion
We focused on quantifying potential inequities in 10-year breast cancer incidence in New Mexico and in each county to better inform health equity initiatives for non-Hispanic AI/AN women at risk for breast cancer. We used the age-adjusted rate ratio, comparing the incidence of breast cancer between at-risk non-Hispanic AI/AN and non-Hispanic White women, to quantify the disparity effect and based it on county-level age-adjusted counts of observed breast cancer cases diagnosed from 2005 through 2014 in New Mexico. Although traditional methods that calculate age-adjusted standardized incidence ratios are appropriate for large geographic areas, they are often unsuitable when the goal is to quantify local risk in small geographic areas, such as counties, while adjusting for potentially relevant covariate information; the local sample sizes in each county were too small to obtain reliable estimates with the desired levels of statistical precision by using traditional methods (16). To obtain a reliable estimate of the disparity effect in each county and overall, we applied Bayesian disease mapping to these population surveillance data. Bayesian disease mapping is a model-based approach that offered a means to improve county-level incidence estimates by borrowing more information from neighboring counties than from counties farther away, thereby smoothing extreme rates based on small local sample sizes toward local, neighboring values. Furthermore, this modeling-based approach accounted for the number of women at risk as well as a county-level ADI.
We found evidence of a substantial overall disparity effect across New Mexico. The age-adjusted rate of breast cancer among non-Hispanic AI/AN women was approximately 0.38 times the corresponding age-adjusted rate for non-Hispanic White women. The lower and upper limits of the corresponding 95% credible interval were 0.253 and 0.547, respectively. This overall finding appears in keeping with previous studies (1,5). By using age-adjusted breast cancer incidence rates in the southwest region for 2010 through 2015, Melkonian and colleagues in 2019 reported a corresponding age-adjusted rate ratio of 0.57 (5). Before that, White and colleagues in 2014 reported an age-adjusted rate ratio in the Southwest region of 0.49 during their study period, 1999–2009 (1).
Although previous studies have shown substantially lower breast cancer incidence rates among non-Hispanic AI/AN than non-Hispanic White women, there were regional differences in the age-adjusted rate ratios (1,5,17). In these epidemiologic studies, aggregated data over large geographic regions of the United States were used to quantify the age-adjusted rate ratios of breast cancer in each region. The southwest region comprises 5 states: Arizona, Colorado, Utah, Nevada, and New Mexico. Because activities such as health education, health statistics, and public health services are commonly implemented at the state rather than the regional level, we selected New Mexico for our study. Our findings can be directly accessible to New Mexico state health authorities to evaluate such disparities in their state and act to address them. Furthermore, federal funding for public health infrastructure such as mammography centers is commonly awarded at the state level so that knowing the state-level breast cancer burden in the non-Hispanic AI/AN population could facilitate targeted requests for federal and state funding. In our study, we observed a significant reduction in the age-adjusted breast cancer incidence rate in 16 of 33 New Mexico counties; 17 counties had no significant reduction.
Our application of Bayesian disease mapping to these population surveillance data from New Mexico provided substantial evidence of a significant overall reduction in the breast cancer incidence rate in at-risk non-Hispanic AI/AN women compared with non-Hispanic White women, which was more marked than previous reports. Targeted statewide health equity initiatives may reduce disparities in breast cancer incidence among non-Hispanic AI/AN women at risk for breast cancer, whereas targeted county-level initiatives may directly reduce disparities in breast cancer incidence.
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## Acknowledgments
This article was supported with data generated by Mayo Clinic researchers. Research reported in this article was supported in part by the Mayo Clinic Office of Health Disparities Research Pilot Grant. Additionally, our work was partially supported by the National Institutes of Health Grant: U10CA180882 (Alliance for Clinical Trials in Oncology Statistics and Data Management Grant), and P30CA15083 (Mayo Clinic Comprehensive Cancer Center Grant). The authors have no conflicts of interest to report. No copyrighted material was used in this article.
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## Author Information
Corresponding Author: David Zahrieh, PhD, Mayo Clinic, Department of Quantitative Health Sciences, 200 First St SW, Rochester, MN 55905. Telephone: 507-293-2688. Email: [email protected].
Author Affiliations: 1Department of Health Sciences Research, Mayo Clinic, Rochester, Minnesota. 2Department of Health Sciences Research, Mayo Clinic, Scottsdale, Arizona. 3Department of Radiation Oncology, Mayo Clinic, Phoenix, Arizona.
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## References
1. White MC, Espey DK, Swan J, Wiggins CL, Eheman C, Kaur JS. Disparities in cancer mortality and incidence among American Indians and Alaska Natives in the United States. Am J Public Health 2014;104(Suppl 3):S377–87. CrossRefexternal icon PubMedexternal icon
2. Cobb N, Espey D, King J. Health behaviors and risk factors among American Indians and Alaska Natives, 2000–2010. Am J Public Health 2014;104(Suppl 3):S481–9. CrossRefexternal icon PubMedexternal icon
3. Mandelblatt JS, Cronin KA, Bailey S, Berry DA, de Koning HJ, Draisma G, et al. ; Breast Cancer Working Group of the Cancer Intervention and Surveillance Modeling Network. Effects of mammography screening under different screening schedules: model estimates of potential benefits and harms. Ann Intern Med 2009;151(10):738–47. CrossRefexternal icon PubMedexternal icon
4. White A, Thompson TD, White MC, Sabatino SA, de Moor J, Doria-Rose PV, et al. Cancer screening test use—United States 2015. MMWR Morb Mortal Wkly Rep 2017;66(8):201–6. CrossRefexternal icon PubMedexternal icon
5. Melkonian SC, Jim MA, Haverkamp D, Wiggins CL, McCollum J, White MC, et al. Disparities in cancer incidence and trends among American Indians and Alaska Natives in the United States, 2010–2015. Cancer Epidemiol Biomarkers Prev 2019;28(10):1604–11. CrossRefexternal icon PubMedexternal icon
6. Espey D, Paisano R, Cobb N. Regional patterns and trends in cancer mortality among American Indians and Alaska Natives, 1990–2001. Cancer 2005;103(5):1045–53. CrossRefexternal icon PubMedexternal icon
7. New Mexico Economic Development Department. Tribal profiles: Native American population. https://gonm.biz/site-selection/tribal-profiles/. Accessed Nov 7, 2020.
8. Gelfand A, Diggle P, Fuentes M, Guttorp P. Handbook of spatial statistics. Boca Raton (FL): CRC Press; 2010.
9. Hankey BF, Ries LA, Edwards BK. The Surveillance, Epidemiology, and End Results program: a national resource. Cancer Epidemiol Biomarkers Prev 1999;8(12):1117–21. PubMedexternal icon
10. Kurani S, McCoy RG, Inselman J, Jeffery MM, Chawla S, Finney Rutten LJ, et al. Place, poverty and prescriptions: a cross-sectional study using Area Deprivation Index to assess opioid use and drug-poisoning mortality in the USA from 2012 to 2017. BMJ Open 2020;10(5):e035376. CrossRefexternal icon PubMedexternal icon
11. Besag J, Mollie A. Bayesian image restoration, with two applications in spatial statistics. Ann Inst Stat Math 1991;43:1–59. CrossRefexternal icon
12. Gelman A. Prior distributions for variance parameters in hierarchical models. Bayesian Anal 2006;1(3):515–34. CrossRefexternal icon
13. Lunn D, Spiegelhalter D, Thomas A, Best N. The BUGS project: evolution, critique and future directions. Stat Med 2009;28(25):3049–67. CrossRefexternal icon PubMedexternal icon
14. Jackman S. Bayesian analysis for the social sciences. New York (NY): John Wiley & Sons, Ltd; 2009.
15. Spiegelhalter DJ, Best NG, Carlin BP, van der Linde A. Bayesian measures of model complexity and fit. J R Stat Soc 2002;64(4):583–639. CrossRefexternal icon
16. Waller LA, Carlin BP. Disease mapping. In Chapman Hall CRC handbook of modern statistical methods. London (UK): Taylor and Francis; 2010, p. 217–43.
17. Wiggins CL, Espey DK, Wingo PA, Kaur JS, Wilson RT, Swan J, et al. Cancer among American Indians and Alaska Natives in the United States, 1999–2004. Cancer 2008;113(5 Suppl):1142–52. CrossRefexternal icon PubMedexternal icon
18. Becker SA, Affonso DD, Beard MBH. Talking circles: Northern Plains tribes American Indian women’s views of cancer as a health issue. Public Health Nurs 2006;23(1):27–36. CrossRefexternal icon PubMedexternal icon
19. Daley CM, Kraemer-Diaz A, James AS, Monteau D, Joseph S, Pacheco J, et al. Breast cancer screening beliefs and behaviors among American Indian women in Kansas and Missouri: a qualitative inquiry. J Cancer Educ 2012;27(1 Suppl):S32–40. CrossRefexternal icon PubMedexternal icon
20. Watson-Johnson LC, DeGroff A, Steele CB, Revels M, Smith JL, Justen E, et al. Mammography adherence: a qualitative study. J Womens Health (Larchmt) 2011;20(12):1887–94. CrossRefexternal icon PubMedexternal icon
21. Ndikum-Moffor FM, Braiuca S, Daley CM, Gajewski BJ, Engelman KK. Assessment of mammography experiences and satisfaction among American Indian/Alaska Native women. Womens Health Issues 2013;23(6):e395–402. CrossRefexternal icon PubMedexternal icon
22. Vang S, Margolies LR, Jandorf L. Mobile mammography participation among medically underserved women: a systematic review. Prev Chronic Dis 2018;15:E140. CrossRefexternal icon PubMedexternal icon
23. Roen EL, Roubidoux MA, Joe AI, Russell TR, Soliman AS. Adherence to screening mammography among American Indian women of the Northern Plains. Breast Cancer Res Treat 2013;139(3):897–905. CrossRefexternal icon PubMedexternal icon
24. Paskett E, Tatum C, Rushing J, Michielutte R, Bell R, Long Foley K, et al. Randomized trial of an intervention to improve mammography utilization among a triracial rural population of women. J Natl Cancer Inst 2006;98(17):1226–37. CrossRefexternal icon PubMedexternal icon
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## Tables
Table 1. Estimated Posterior Quantities From Fitting the Proposed Model, New Mexico Breast Cancer Incidence Study, 2005–2014a
Description of Explanatory Variable Parameter Mean (SD) 95% Credible Interval
Intercept β0 −7.009 (0.090) (−7.189 to −6.836)
x1 non-Hispanic AI/AN vs non-Hispanic White β1 −0.937 (0.360) (−1.763 to −0.346)
x2 ADI in lower 20th percentile vs otherwise β2 0.229 (0.132) (−0.035 to 0.486)
2-Way interaction (x1 × x2) β3 −0.303 (0.551) (−1.373 to 0.812)
Random effects
Spatial component: non-Hispanic White √τb 0.143 (0.110) (0.003 to 0.411)
Spatial component: non-Hispanic AI/AN √τc 0.567 (0.499) (0.029 to 1.859)
Dispersion parameter √τh 0.070 (0.054) (0.004 to 0.205)
Overall rate ratio (non-Hispanic AI/AN vs non-Hispanic White),
$λ-∙1/λ-∙0$
0.384 (0.075) (0.253 to 0.546)
Abbreviations: ADI, Area Deprivation Index; AI/AN, American Indian/Alaska Native.
a Estimates of posterior quantities were obtained from Markov chain Monte Carlo sampling. The 20th percentile for the ADI was 101.6; higher values correspond to increased socioeconomic disadvantage. The overall rate ratio was defined as the ratio of the average rates within each racial category (non-Hispanic AI/AN vs non-Hispanic white), or $λ-∙1λ-∙0$ , where and and i = 1, …, 33 corresponding to the 33 counties in New Mexico. The deviance information criterion was 160.9.
Table 2. County-Specific Posterior Means and 95% Credible Intervals for the Rate Ratios, New Mexico Breast Cancer Incidence Study, 2005–2014a
County ADI Quintilesb Non-Hispanic AI/AN vs Non-Hispanic White Women, Posterior Mean Rate Ratio (95% Credible Interval) Non-Hispanic AI/AN Population, Posterior Mean Rate Ratio (95% Credible Interval)
Bernalillo Q1 0.311 (0.121–0.600) 0.883 (0.387–1.527)
Catron Q1 0.346 (0.066–0.927) 0.964 (0.204–2.428)
Chaves Q2–Q4 0.446 (0.092–0.991) 0.963 (0.211–1.968)
Cibola Q5 0.440 (0.175–0.834) 0.994 (0.459–1.637)
Colfax Q2–Q4 0.488 (0.109–1.284) 1.121 (0.278–2.785)
Curry Q2–Q4 0.490 (0.064–1.348) 1.051 (0.149–2.772)
De Baca Q2–Q4 0.460 (0.095–1.073) 0.998 (0.228–2.123)
Dona Ana Q2–Q4 0.407 (0.066–0.910) 0.915 (0.160–1.889)
Eddy Q1 0.372 (0.058–1.061) 0.954 (0.160–2.556)
Grant Q2–Q4 0.432 (0.067–1.062) 0.975 (0.162–2.225)
Guadalupe Q2–Q4 0.456 (0.108–1.037) 1.009 (0.261–2.094)
Harding Q2–Q4 0.477 (0.112–1.162) 1.075 (0.282–2.455)
Hidalgo Q5 0.492 (0.048–1.436) 1.075 (0.114–2.979)
Lea Q2–Q4 0.480 (0.069–1.215) 0.994 (0.153–2.346)
Lincoln Q1 0.335 (0.081–0.822) 0.920 (0.242–2.049)
Los Alamos Q1 0.370 (0.080–1.072) 1.093 (0.264–3.024)
Luna Q5 0.432 (0.063–1.058) 0.967 (0.154–2.196)
McKinley Q5 0.462 (0.228–0.808) 1.041 (0.662–1.471)
Mora Q2–Q4 0.460 (0.132–1.044) 1.066 (0.346–2.254)
Otero Q2–Q4 0.437 (0.112–0.930) 0.973 (0.273–1.915)
Quay Q2–Q4 0.455 (0.109–1.026) 1.008 (0.264–2.093)
Rio Arriba Q2–Q4 0.416 (0.131–0.816) 0.969 (0.341–1.677)
Roosevelt Q2–Q4 0.463 (0.085–1.087) 0.986 (0.198–2.141)
San Juan Q2–Q4 0.478 (0.250–0.820) 1.063 (0.696–1.519)
San Miguel Q5 0.465 (0.132–1.078) 1.068 (0.338–2.290)
Sandoval Q1 0.339 (0.120–0.715) 0.965 (0.387–1.849)
Santa Fe Q1 0.326 (0.106–0.737) 0.987 (0.363–2.071)
Sierra Q2–Q4 0.419 (0.092–0.903) 0.940 (0.222–1.825)
Socorro Q5 0.422 (0.106–0.860) 0.936 (0.260–1.680)
Taos Q2–Q4 0.492 (0.139–1.296) 1.180 (0.378–2.964)
Torrance Q2–Q4 0.432 (0.123–0.889) 0.975 (0.305–1.812)
Union Q2–Q4 0.499 (0.092–1.341) 1.124 (0.225–2.876)
Valencia Q2–Q4 0.421 (0.100–0.882) 0.946 (0.247–1.772)
Abbreviation: ADI, area deprivation index; AI/AN, American Indian/Alaska Native; Q, quintile.
a The overall rate ratio (95% credible interval) comparing non-Hispanic AI/AN vs non-Hispanic white was 0.384 (0.253–0.546).
b The ADI for 2012; higher values correspond to increased socioeconomic disadvantage.
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Page last reviewed: March 11, 2021
| 2023-03-29T06:24:57 |
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|
https://tjyj.stats.gov.cn/CN/10.19343/j.cnki.11-1302/c.2019.01.009
|
• •
零膨胀计数数据的联合建模及变量选择
• 出版日期:2019-01-25 发布日期:2019-01-16
Joint Modeling and Variable Selection from Zero-Inflated Count Data
Hu Yanan & Tian Maozai
• Online:2019-01-25 Published:2019-01-16
Abstract: Zero-inflated count data damage the mean-variance relation in Poisson distribution, which can be explained by the mixture distribution composed pro rata of data subject to Poisson distribution and zero-valued observations (degradation distribution). This paper studies the joint modeling and variable selection from zero-inflated count data based on the adaptive elastic-net technique. As to the zero-inflated Poisson distribution, some latent variables are induced into constructing a complete likelihood of the regression model, consisted of two components (zero-inflated and Poisson). Taking the possible collinearity and sparsity of covariates into account, the objective function is obtained by adding the adaptive elastic-net penalty to the likelihood function. Then the sparse estimator of the regression coefficient is achieved by using the EM algorithm to optimize the objective function. The Bayesian information criterion (BIC) is employed to determine the optimal tuning parameter. This paper also presents the performance of the proposed estimator with large sample properties through a theoretical demonstration and simulation study, and then applied to the practical issues with the real data.
| 2022-11-28T15:46:18 |
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http://trove.nla.gov.au/work/125056?q&versionId=133053
|
# English, Article edition: ON THE PROPERTIES OF A GENERALIZED CLASS OF T-NORMS IN INTERVAL-VALUED FUZZY LOGICS BART VAN GASSE; CHRIS CORNELIS; GLAD DESCHRIJVER; ...
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Bookmark: http://trove.nla.gov.au/version/133053
Physical Description
• article
Language
• English
### Edition details
Title
• ON THE PROPERTIES OF A GENERALIZED CLASS OF T-NORMS IN INTERVAL-VALUED FUZZY LOGICS
Author
• BART VAN GASSE
• CHRIS CORNELIS
• ETIENNE E. KERRE
Physical Description
• article
Notes
• Since it does not generate any MTL-algebra (prelinear residuated lattice), the lattice $\mathcal{L}^I$ of closed subintervals of [0, 1] falls outside the mainstream of research on formal fuzzy logics. However, due to the intimate connection between logical connectives on $\mathcal{L}^I$ and those on [0, 1], many relevant logical properties can still be maintained, sometimes in a slightly weaker form. In this paper, we focus on a broad class of parametrized t-norms on $\mathcal{L}^I$. We derive their corresponding residual implicators, and examine commonly imposed logical properties. Importantly, we formally establish one-to-one correspondences between â¨-definability (respectively, weak divisibility) for t-norms of this class and strong â¨-definability (resp., divisibility) for their counterparts on [0, 1].
• Formal fuzzy logic, interval-valued fuzzy sets, triangular norms, residuated lattices
• RePEc:wsi:nmncxx:v:02:y:2006:i:01:p:29-41
Language
• English
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| 2017-02-25T05:19:00 |
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https://www.anl.gov/argonne-scientific-publications/pub/147337
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Publication
# Design and Assembly of SPT-3G Cold Readout Hardware
### Authors
Avva, J.; Ade, P.; Ahmed, Z. ; Anderson, A. J.; Austermann, J.; Basu Thakur, R.; Barron, D.; Bender, A.; Benson, B.; Carlstrom, J.; Carter, F.; Cecil, T.; Chang, C.; Ding, J.; Gannon, R.; Harke-Hosemann, A.; Khaire, T.; Kuhlmann, S.; Novosad, V.; Pearson, J.; Posada, C.; Saunders, L.; Wang, G.; Yefremenko, V.
### Abstract
The third- generation upgrade to the receiver on the South Pole Telescope, SPT- 3G, was installed at the South Pole during the 2016- 2017 austral summer to measure the polarization of the cosmic microwave background. Increasing the number of detectors by a factor of 10 to 16, 000 required the multiplexing factor to increase to 68 and the bandwidth of the frequency- division readout electronics to span 1.6- 5.2 MHz. This increase necessitates low- thermal conductance, low- inductance cryogenic wiring. Our cold readout system consists of planar thin- film aluminum inductive- capacitive resonators, wired in series with the detectors, summed together, and connected to 4K SQUIDs by 10- mu m- thick niobium- titanium ( NbTi) broadsidecoupled striplines. Here, we present an overview of the cold readout electronics for SPT- 3G, including assembly details and characterization of electrical and thermal properties of the system. We report, for the NbTi striplines, values of R = 10 L = 21 +/- 1 nH, and C = 1.47 +/-. 02 nF. Additionally, the striplines’ thermal conductivity is described by kA = 6.0 +/- 0.3 T 0.92 +/- 0.04 mu W mm K - 1. Finally, we provide projections for cross talk induced by parasitic impedances from the stripline and find that the median value of percentage cross talk from leakage current is 0.22 and 0.09% from wiring impedance.
HEP
2018
Article
| 2019-09-22T22:19:13 |
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https://pos.sissa.it/390/396/
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Volume 390 - 40th International Conference on High Energy physics (ICHEP2020) - Parallel: Quark and Lepton Flavour Physics
Time-integrated measurements of the CKM angle gamma
S.S. Malde* on behalf of the LHCb collaboration
*corresponding author
Full text: pdf
Pre-published on: February 09, 2021
Published on:
Abstract
A goal of the LHCb experiment is to measure the CKM angle with a precision of 1$^\circ$. At this precision it is hoped that hints or indeed an observation of physics beyond the standard model could arise. In order to reach this precision it will be necessary to target a number of decays modes. Results from two analyses are presented here which make use of the entire Run1 and Run2 dataset collected at the LHCb experiment. One of them leads to a measurement of $\gamma=(68.7^{+5.2}_{-5.2})^\circ$, which is the most precise result from a single measurement.
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| 2021-02-26T18:30:26 |
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https://www.zbmath.org/authors/?q=mumford.david-b
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## Mumford, David Bryant
Compute Distance To:
Author ID: mumford.david-b Published as: Mumford, David; Mumford, D.; Mumford, David B. more...less Homepage: http://www.dam.brown.edu/people/mumford/ External Links: MacTutor · MGP · Wikidata · Math-Net.Ru · GND · IdRef · theses.fr Awards: Fields Medal (1974) · Shaw Prize (2006) · Wolf Prize (2008)
Documents Indexed: 142 Publications since 1961, including 42 Books 5 Contributions as Editor · 5 Further Contributions Biographic References: 7 Publications Co-Authors: 112 Co-Authors with 72 Joint Publications 2,565 Co-Co-Authors
all top 5
### Co-Authors
69 single-authored 9 Michor, Peter Wolfram 6 Nori, Madhav V. 4 Artin, Michael 4 Gleason, Andrew Mattei 4 Hughes-Hallett, Deborah 4 McCallum, William G. 4 Musili, C. 4 Osgood, Brad G. 4 Previato, Emma 4 Quinney, Douglas 4 Ramanujam, Chidambaram Padmanabhan 4 Stillman, Michael Eugene 4 Tecosky-Feldman, Jeff 4 Tucker, Thomas W. 3 Deligne, Pierre René 3 Flath, Daniel Evans 3 Gordon, Sheldon P. 3 Shiota, Takahiro 3 Tate, John Torrence jun. 3 Thrash, Joe B. 3 Zariski, Oscar 2 Ash, Avner 2 Barnsley, Michael Fielding 2 Bombieri, Enrico 2 Chai, Chingli 2 Chung, Fan 2 Falconer, Kenneth J. 2 Fogarty, John C. 2 Frame, Michael Lee 2 Jackson, Allyn 2 Kempf, George R. 2 Knudsen, Finn Faye 2 Lee, Ann B. 2 Lock, Patti Frazer 2 Manin, Yuri Ivanovich 2 Micheli, Mario 2 Neeman, Amnon 2 Nguyen Minh Chuong 2 Norman, Peter 2 Rapoport, Michael 2 Raskind, Wayne 2 Scott, Dana Stewart 2 Series, Caroline 2 Shah, Jayant 2 Stewart, Ian Nicholas 2 Tai, Yungsheng 2 Umemura, Hiroshi 2 Wright, David James 1 Abhyankar, Shreeram Shankar 1 Abhyankar, Yvonne 1 Arbarello, Enrico 1 Atiyah, Michael Francis 1 Bajai, Chanderjit 1 Balaji, Vikraman 1 Barrallo, Javier 1 Bass, Hyman 1 Bayer, David Allen 1 Bergman, George M. 1 Brothers, Harlan J. 1 Bruveris, Martins 1 Carrell, James B. 1 Cartier, Pierre 1 Chiossi, Simon G. 1 Ciarlet, Philippe Gaston 1 Cohen, Nathan 1 Coppens, Marc-Olivier 1 Cutkosky, Steven Dale 1 Davis, Philip J. 1 Demazure, Michel 1 Desolneux, Agnès 1 Dieudonné, Jean Alexandre 1 Eglash, Ron 1 Egorov, Yuriĭ Vladimirovich 1 Furstenberg, Hillel 1 Giblin, Peter J. 1 Gidas, Basilis 1 Gieseker, David 1 Gordon, Gaile G. 1 Greenberg, Marvin Jay 1 Gurdian, Rodolfo 1 Haboush, William J. 1 Hallinan, Peter W. 1 Harbater, Dale 1 Harris, Joseph Daniel 1 Hartshorne, Robin 1 Heinzer, William J. 1 Helgason, Sigurdur 1 Hironaka, Heisuke 1 Horrocks, Geoffrey 1 Howe, Roger Evans 1 Huang, Jinggang 1 Illusie, Luc 1 Jaffard, Stéphane 1 Jaffe, Arthur Michael 1 Kalayciôglu, Selin 1 Katz, Nicholas Michael 1 Khrennikov, Andreĭ Yur’evich 1 Kirwan, Frances Clare 1 Kleiman, Steven Lawrence 1 Kunz, Ernst ...and 51 more Co-Authors
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### Serials
13 Notices of the American Mathematical Society 9 American Journal of Mathematics 5 Inventiones Mathematicae 4 Ergebnisse der Mathematik und ihrer Grenzgebiete 4 Modern Birkhäuser Classics 3 International Journal of Computer Vision 3 Lecture Notes in Mathematics 3 Progress in Mathematics 2 Compositio Mathematica 2 Publications Mathématiques 2 Quarterly of Applied Mathematics 2 Atti della Accademia Nazionale dei Lincei. Classe di Scienze Fisiche, Matematiche e Naturali. Serie IX. Rendiconti Lincei. Matematica e Applicazioni 2 Grundlehren der Mathematischen Wissenschaften 2 Mathematicians of Our Time 2 Tata Institute of Fundamental Research. Studies in Mathematics 2 Texts and Readings in Mathematics 1 Communications on Pure and Applied Mathematics 1 Journal d’Analyse Mathématique 1 Mathematical Proceedings of the Cambridge Philosophical Society 1 Mitteilungen der Deutschen Mathematiker-Vereinigung (DMV) 1 Uspekhi Matematicheskikh Nauk [N. S.] 1 Acta Mathematica 1 Annales Scientifiques de l’École Normale Supérieure. Quatrième Série 1 Journal of Combinatorial Theory. Series B 1 Journal of Mathematics of Kyoto University 1 Mathematische Annalen 1 Mathematica Scandinavica 1 Proceedings of the American Mathematical Society 1 Proceedings of the London Mathematical Society. Third Series 1 Topology 1 Annals of Global Analysis and Geometry 1 Sūgaku 1 L’Enseignement Mathématique. 2e Série 1 Nova Acta Leopoldina. Neue Folge 1 Applied and Computational Harmonic Analysis 1 Izvestiya: Mathematics 1 Documenta Mathematica 1 European Mathematical Society Newsletter 1 Journal of the European Mathematical Society (JEMS) 1 Bulletin of the American Mathematical Society 1 Rendiconti del Seminario Matematico. Universitá e Politecnico di Torino 1 Annals of Mathematics Studies 1 Lecture Notes in Computer Science 1 Monographies de l’Enseignement Mathématique 1 Science 1 SIAM Journal on Imaging Sciences 1 Foundations and Trends in Computer Graphics and Vision 1 Journal of Geometric Mechanics 1 Forum of Mathematics, Sigma 1 Classics in Mathematics 1 Springer Collected Works in Mathematics 1 Cambridge Mathematical Library
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### Fields
76 Algebraic geometry (14-XX) 23 History and biography (01-XX) 18 General and overarching topics; collections (00-XX) 17 Computer science (68-XX) 11 Global analysis, analysis on manifolds (58-XX) 8 Partial differential equations (35-XX) 8 Statistics (62-XX) 7 Group theory and generalizations (20-XX) 7 Several complex variables and analytic spaces (32-XX) 6 Number theory (11-XX) 6 Differential geometry (53-XX) 6 Probability theory and stochastic processes (60-XX) 5 Commutative algebra (13-XX) 5 Dynamical systems and ergodic theory (37-XX) 4 Real functions (26-XX) 4 Functions of a complex variable (30-XX) 3 Topological groups, Lie groups (22-XX) 3 Information and communication theory, circuits (94-XX) 2 Combinatorics (05-XX) 2 Measure and integration (28-XX) 2 Special functions (33-XX) 2 Harmonic analysis on Euclidean spaces (42-XX) 2 Operator theory (47-XX) 2 Convex and discrete geometry (52-XX) 2 Manifolds and cell complexes (57-XX) 2 Game theory, economics, finance, and other social and behavioral sciences (91-XX) 2 Biology and other natural sciences (92-XX) 2 Mathematics education (97-XX) 1 Field theory and polynomials (12-XX) 1 Associative rings and algebras (16-XX) 1 Category theory; homological algebra (18-XX) 1 Difference and functional equations (39-XX) 1 Abstract harmonic analysis (43-XX) 1 Calculus of variations and optimal control; optimization (49-XX) 1 Geometry (51-XX) 1 General topology (54-XX) 1 Relativity and gravitational theory (83-XX) 1 Astronomy and astrophysics (85-XX)
### Citations contained in zbMATH Open
122 Publications have been cited 9,319 times in 7,434 Documents Cited by Year
Geometric invariant theory. 3rd enl. ed. Zbl 0797.14004
Mumford, D.; Fogarty, J.; Kirwan, F.
1994
Optimal approximations by piecewise smooth functions and associated variational problems. Zbl 0691.49036
Mumford, David; Shah, Jayant
1989
The irreducibility of the space of curves of a given genus. Zbl 0181.48803
Deligne, Pierre; Mumford, D.
1969
Abelian varieties. Zbl 0223.14022
Mumford, David
1970
Toroidal embeddings. I. Zbl 0271.14017
Kempf, G.; Knudsen, F.; Mumford, D.; Saint-Donat, Bernard
1973
Lectures on curves on an algebraic surface. Zbl 0187.42701
Mumford, D.
1966
Geometric invariant theory. Zbl 0147.39304
Mumford, D.
1965
The topology of normal singularities of an algebraic surface and a criterion for simplicity. Zbl 0108.16801
Mumford, D.
1961
Tata lectures on theta. I: Introduction and motivation: Theta functions in one variable. Basic results on theta functions in several variables. With the assistance of C. Musili, M. Nori, E. Previato, and M. Stillman. Zbl 0509.14049
Mumford, David
1983
Geometric invariant theory. 2nd enlarged ed. Zbl 0504.14008
Mumford, D.; Fogarty, J.
1982
Tata lectures on theta. II: Jacobian theta functions and differential equations. With the collaboration of C. Musili, M. Nori, E. Previato, M. Stillman, and H. Umemura. Zbl 0549.14014
Mumford, David
1984
The projectivity of the moduli space of stable curves. I: Preliminaries on ”det” and ”Div”. Zbl 0343.14008
Knudsen, Finn; Mumford, David
1976
Algebraic geometry. I: Complex projective varieties. Zbl 0356.14002
Mumford, David
1976
On the Kodaira dimension of the moduli space of curves. Zbl 0506.14016
Harris, Joe; Mumford, David
1982
Smooth compactification of locally symmetric varieties. Zbl 0334.14007
Ash, A.; Mumford, D.; Rapoport, M.; Tai, Y.
1975
On the equations defining Abelian varieties. I-III. Zbl 0219.14024
Mumford, D.
1966
Varieties defined by quadratic equations. Zbl 0198.25801
Mumford, David
1970
Stability of projective varieties. Zbl 0363.14003
Mumford, David
1977
Towards an enumerative geometry of the moduli space of curves. Zbl 0554.14008
Mumford, David
1983
Abelian varieties. With appendices by C. P. Ramanujam and Yuri Manin. 2nd ed. Zbl 0326.14012
Mumford, David
1974
Some elementary examples of unirational varieties which are not rational. Zbl 0244.14017
Artin, M.; Mumford, D.
1972
What can be computed in algebraic geometry? Zbl 0846.13017
Bayer, Dave; Mumford, David
1993
Theta characteristics of an algebraic curve. Zbl 0216.05904
Mumford, David
1971
Rational equivalence of O-cycles on surfaces. Zbl 0184.46603
Mumford, D.
1969
Hirzebruch’s proportionality theorem in the non-compact case. Zbl 0365.14012
Mumford, D.
1977
Riemannian geometries on spaces of plane curves. Zbl 1101.58005
Michor, Peter W.; Mumford, David
2006
Tata lectures on theta. III. Zbl 0744.14033
Mumford, David; Nori, Madhav; Norman, Peter
1991
The red book of varieties and schemes. Zbl 0658.14001
Mumford, David
1988
Curves and their Jacobians. Zbl 0316.14010
Mumford, David
1975
Further pathologies in algebraic geometry. Zbl 0114.13106
Mumford, D.
1962
The spectrum of difference operators and algebraic curves. Zbl 0502.58032
van Moerbeke, Pierre; Mumford, David
1979
The red book of varieties and schemes. Includes the Michigan lectures (1974) on “Curves and their Jacobians”. 2nd, expanded ed. with contributions by Enrico Arbarello. Zbl 0945.14001
Mumford, David
1999
An analytic construction of degenerating curves over complete local rings. Zbl 0228.14011
Mumford, David
1972
Families of abelian varieties. Zbl 0199.24601
Mumford, D.
1966
An overview of the Riemannian metrics on spaces of curves using the Hamiltonian approach. Zbl 1116.58007
Michor, Peter W.; Mumford, David
2007
Elastica and computer vision. Zbl 0798.53003
Mumford, David
1994
Prym varieties. I. Zbl 0299.14018
Mumford, David
1974
Algebraic surfaces. With appendices by S.S. Abhyankar, J. Lipman, and D. Mumford. 2nd suplemented ed. Zbl 0219.14020
Zariski, O.
1971
Enriques’ classification of surfaces in char p. III. Zbl 0336.14010
Bombieri, E.; Mumford, D.
1976
A stratification of the null cone via the moment map. (With an appendix by David Mumford). Zbl 0604.14006
Ness, Linda
1984
An analytic construction of degenerating Abelian varieties over complete rings. Zbl 0241.14020
Mumford, David
1972
A rank 2 vector bundle on P$$^4$$ with 15,000 symmetries. Zbl 0255.14017
Horrocks, G.; Mumford, D.
1973
A metric on shape space with explicit geodesics. Zbl 1142.58013
Younes, Laurent; Michor, Peter W.; Shah, Jayant; Mumford, David
2008
A remark on Mahler’s compactness theorem. Zbl 0215.23202
Mumford, D.
1971
Vanishing geodesic distance on spaces of submanifolds and diffeomorphisms. Zbl 1083.58010
Michor, Peter W.; Mumford, David
2005
A note of Shimura’s paper: Discontinuous groups and Abelian varieties. Zbl 0169.23301
Mumford, D.
1969
Algebraic Geometry. I: Complex projective varieties. Reprint of the corr. 2nd print. 1976. Zbl 0821.14001
Mumford, David
1995
Abelian varieties. With appendices by C. P. Ramanujam and Yuri Manin. Corrected reprint of the 2nd ed. 1974. Zbl 1177.14001
Mumford, David
2008
Two fundamental theorems on deformations of polarized varieties. Zbl 0128.15505
Matsusaka, T.; Mumford, D.
1964
An algebraic surface with K ample, $$(K^ 2)=9$$, $$p_ g=q=O$$. Zbl 0433.14021
Mumford, D.
1979
Indra’s pearls. The vision of Felix Klein. With cartoons by Larry Gonick. Zbl 1141.00002
Mumford, David; Series, Caroline; Wright, David
2002
Enriques’ classification of surfaces in char. $$p$$. II. Zbl 0348.14021
Bombieri, E.; Mumford, D.
1977
Pathologies. III. Zbl 0146.42403
Mumford, D.
1967
An algebro-geometric construction of commuting operators and of solutions to the Toda lattice equation, Korteweg de Vries equation and related non- linear equations. Zbl 0423.14007
Mumford, D.
1977
Filtering, segmentation and depth. Zbl 0801.68171
Nitzberg, Mark; Mumford, David; Shiota, Takahiro
1993
Periods of a moduli space of bundles on curves. Zbl 0174.52902
1968
Abelian quotients of the Teichmüller modular group. Zbl 0173.22903
Mumford, D.
1967
Smooth compactifications of locally symmetric varieties. With the collaboration of Peter Scholze. 2nd ed. Zbl 1209.14001
Ash, Avner; Mumford, David; Rapoport, Michael; Tai, Yung-Sheng
2010
The nonlinear statistics of high-contrast patches in natural images. Zbl 1070.68661
Lee, Ann B.; Pedersen, Kim S.; Mumford, David
2003
Geodesic completeness for Sobolev metrics on the space of immersed plane curves. Zbl 1315.58009
Bruveris, Martins; Michor, Peter W.; Mumford, David
2014
Stochastic models for generic images. Zbl 1159.68598
Mumford, David; Gidas, Basilis
2001
A remark on Mordell’s conjecture. Zbl 0151.27301
Mumford, D.
1965
On Euler’s equation and ‘EPDiff’. Zbl 1274.35277
Mumford, David; Michor, Peter W.
2013
A zoo of diffeomorphism groups on $$\mathbb R^n$$. Zbl 1364.22009
Michor, Peter W.; Mumford, David
2013
Picard groups of moduli problems. Zbl 0187.42801
Mumford, D.
1965
On the Kodaira dimension of the Siegel modular variety. Zbl 0527.14036
Mumford, David
1983
Deformations and liftings of finite, commutative group schemes. Zbl 0179.49901
Oort, F.; Mumford, D.
1968
Introduction to the theory of moduli. Zbl 0242.14004
Mumford, David; Suominen, Kalevi
1972
A stochastic grammar of images. Zbl 1198.68160
Zhu, Song-Chun; Mumford, David
2006
Indra’s pearls. The vision of Felix Klein. With cartoons by Larry Gonick. Reprint of the 2002 hardback edition. Zbl 1314.00007
Mumford, David; Series, Caroline; Wright, David
2015
Pattern theory. The stochastic analysis of real-world signals. Zbl 1210.94002
Mumford, David; Desolneux, Agnès
2010
Tata lectures on theta. II: Jacobian theta functions and differential equations. With the collaboration of C. Musili, M. Nori, E. Previato, M. Stillman, and H. Umemura. Reprint of the 1984 edition. Zbl 1112.14003
Mumford, David
2007
Pattern theory: The mathematics of perception. Zbl 1057.91072
Mumford, David
2002
Tata lectures on theta. I. With the collaboration of C. Musili, M. Nori, E. Previato, and M. Stillman. Reprint of the 1983 edition. Zbl 1112.14002
Mumford, David
2007
Stability of projective varieties. Zbl 0497.14004
Mumford, David
1977
Sobolev metrics on diffeomorphism groups and the derived geometry of spaces of submanifolds. Zbl 1280.58005
Micheli, M.; Michor, P. W.; Mumford, D.
2013
Harmonic, wavelet and $$p$$-adic analysis. Based on the summer school, Quy Nhon, Vietnam, June 10–15, 2005. Zbl 1117.42001
2007
Pathologies of modular algebraic surfaces. Zbl 0138.42002
Mumford, D.
1961
Bi-extensions of formal groups. Zbl 0216.33101
Mumford, D.
1969
Lectures on curves on an algebraic surface. With a section by G. M. Bergman. Zbl 1079.14002
Mumford, David
2005
Two- and three-dimensional patterns of the face. Zbl 0930.68140
Hallinan, Peter W.; Gordon, Gaile G.; Yuille, A. L.; Giblin, Peter; Mumford, David
1999
Enriques’ classification of surfaces in char p. I. Zbl 0188.53201
Mumford, D.
1969
Projective invariants of projective structures and applications. Zbl 0154.20702
Mumford, D.
1963
The dawning of the age of stochasticity. Zbl 0962.60003
Mumford, David
2000
Some footnotes to the work of C. P. Ramanujam. Zbl 0444.14002
Mumford, D.
1978
Sectional curvature in terms of the cometric, with applications to the Riemannian manifolds of landmarks. Zbl 1276.37047
Micheli, Mario; Michor, Peter W.; Mumford, David
2012
Chordal completions of planar graphs. Zbl 0809.05038
Chung, F. R. K.; Mumford, David
1994
Abelian varieties. With appendices by C. P. Ramanujam and Yuri Manin. 2nd ed. Reprint. Zbl 0583.14015
Mumford, David
1985
2D-shape analysis using conformal mapping. Zbl 1477.68492
Sharon, E.; Mumford, D.
2006
The structure of the moduli spaces of curves and abelian varieties. Zbl 0222.14023
Mumford, David
1971
Tata lectures on theta III. In collaboration with Madhav Nori and Peter Norman. Reprint of the 1991 edition. Zbl 1124.14043
Mumford, David
2007
The self-intersection formula and the ’formule-clef’. Zbl 0341.14002
Lascu, A. T.; Mumford, D.; Scott, D. B.
1975
Occlusion models for natural images: A statistical study of a scale-invariant dead leaves model. Zbl 1012.68715
Lee, Ann B.; Mumford, David; Huang, Jinggang
2001
Pathologies. IV. Zbl 0315.14012
Mumford, David
1975
Lectures on curves on a algebraic surface. Zbl 0187.42702
Mumford, D.
1968
Pattern theory: A unifying perspective. Zbl 0939.68820
Mumford, David
1994
Algebraic geometry II. Zbl 1325.14001
2015
Advances in deterministic and stochastic analysis. Proceedings of the 2nd international conference on abstract and applied analysis, Quy Nhon, Vietnam, June 4–9. 2005. Zbl 1115.35008
2007
A remark on the paper of M. Schlessinger. Zbl 0279.32007
Mumford, David
1973
Matsusaka’s big theorem. Zbl 0321.14004
Liebermann, D.; Mumford, D.
1975
Alexandre Grothendieck 1928–2014. I. Zbl 1338.01022
Atiyah, Michael; Bass, Hyman; Cartier, Pierre; Deligne, Pierre; Demazure, Michel; Greenberg, Marvin Jay; Hartshorne, Robin; Illusie, Luc; Katz, Nicholas; Kleiman, Steven L.
2016
Alexandre Grothendieck 1928–2014, part 2. Zbl 1338.01023
Ladegaillerie, Yves; Lichtenbaum, Stephen; Lochak, Pierre; Mazur, Barry; Messing, William; Murre, Jacob; Schneps, Leila
2016
Indra’s pearls. The vision of Felix Klein. With cartoons by Larry Gonick. Reprint of the 2002 hardback edition. Zbl 1314.00007
Mumford, David; Series, Caroline; Wright, David
2015
Algebraic geometry II. Zbl 1325.14001
2015
Geodesic completeness for Sobolev metrics on the space of immersed plane curves. Zbl 1315.58009
Bruveris, Martins; Michor, Peter W.; Mumford, David
2014
Shreeram Abhyankar (July 22, 1930 – November 2, 2012). Zbl 1338.13001
Abhyankar, Yvonne; Bajai, Chanderjit; Cutkosky, Steven Dale; Harbater, Dale; Heinzer, William; Shannon, David; Mulay, Shashikant; Mumford, David; Thakur, Dinesh
2014
On Euler’s equation and ‘EPDiff’. Zbl 1274.35277
Mumford, David; Michor, Peter W.
2013
A zoo of diffeomorphism groups on $$\mathbb R^n$$. Zbl 1364.22009
Michor, Peter W.; Mumford, David
2013
Sobolev metrics on diffeomorphism groups and the derived geometry of spaces of submanifolds. Zbl 1280.58005
Micheli, M.; Michor, P. W.; Mumford, D.
2013
Introduction to commutative algebra and algebraic geometry. Transl. from the German by Michael Ackerman. With a preface by David Mumford. Reprint of the 1985 edition. Zbl 1263.13001
Kunz, Ernst
2013
Sectional curvature in terms of the cometric, with applications to the Riemannian manifolds of landmarks. Zbl 1276.37047
Micheli, Mario; Michor, Peter W.; Mumford, David
2012
Glimpses of Benoît B. Mandelbrot (1924–2010). Zbl 1284.01047
Stewart, Ian; Mumford, David; Falconer, Kenneth; Eglash, Ron; Brothers, Harlan; Lesmoir-Gordon, Nigel; Barrallo, Javier; Berry, Michael; Frame, Michael
2012
The influence of Benoît B. Mandelbrot on mathematics. Zbl 1284.01048
Stewart, Ian; Mumford, David; Howe, Roger; Furstenberg, Hillel; Falconer, Kenneth; West, Bruce J.; Coppens, Marc-Olivier; Cohen, Nathan; Jaffard, Stéphane; Berry, Michael; Frame, Michael
2012
Intuition and rigor and Enriques’s quest. Zbl 1268.14003
Mumford, David
2011
Smooth compactifications of locally symmetric varieties. With the collaboration of Peter Scholze. 2nd ed. Zbl 1209.14001
Ash, Avner; Mumford, David; Rapoport, Michael; Tai, Yung-Sheng
2010
Pattern theory. The stochastic analysis of real-world signals. Zbl 1210.94002
Mumford, David; Desolneux, Agnès
2010
A metric on shape space with explicit geodesics. Zbl 1142.58013
Younes, Laurent; Michor, Peter W.; Shah, Jayant; Mumford, David
2008
Abelian varieties. With appendices by C. P. Ramanujam and Yuri Manin. Corrected reprint of the 2nd ed. 1974. Zbl 1177.14001
Mumford, David
2008
An overview of the Riemannian metrics on spaces of curves using the Hamiltonian approach. Zbl 1116.58007
Michor, Peter W.; Mumford, David
2007
Tata lectures on theta. II: Jacobian theta functions and differential equations. With the collaboration of C. Musili, M. Nori, E. Previato, M. Stillman, and H. Umemura. Reprint of the 1984 edition. Zbl 1112.14003
Mumford, David
2007
Tata lectures on theta. I. With the collaboration of C. Musili, M. Nori, E. Previato, and M. Stillman. Reprint of the 1983 edition. Zbl 1112.14002
Mumford, David
2007
Harmonic, wavelet and $$p$$-adic analysis. Based on the summer school, Quy Nhon, Vietnam, June 10–15, 2005. Zbl 1117.42001
2007
Tata lectures on theta III. In collaboration with Madhav Nori and Peter Norman. Reprint of the 1991 edition. Zbl 1124.14043
Mumford, David
2007
Advances in deterministic and stochastic analysis. Proceedings of the 2nd international conference on abstract and applied analysis, Quy Nhon, Vietnam, June 4–9. 2005. Zbl 1115.35008
2007
Riemannian geometries on spaces of plane curves. Zbl 1101.58005
Michor, Peter W.; Mumford, David
2006
A stochastic grammar of images. Zbl 1198.68160
Zhu, Song-Chun; Mumford, David
2006
2D-shape analysis using conformal mapping. Zbl 1477.68492
Sharon, E.; Mumford, D.
2006
Vanishing geodesic distance on spaces of submanifolds and diffeomorphisms. Zbl 1083.58010
Michor, Peter W.; Mumford, David
2005
Lectures on curves on an algebraic surface. With a section by G. M. Bergman. Zbl 1079.14002
Mumford, David
2005
The nonlinear statistics of high-contrast patches in natural images. Zbl 1070.68661
Lee, Ann B.; Pedersen, Kim S.; Mumford, David
2003
Indra’s pearls. The vision of Felix Klein. With cartoons by Larry Gonick. Zbl 1141.00002
Mumford, David; Series, Caroline; Wright, David
2002
Pattern theory: The mathematics of perception. Zbl 1057.91072
Mumford, David
2002
Stochastic models for generic images. Zbl 1159.68598
Mumford, David; Gidas, Basilis
2001
Occlusion models for natural images: A statistical study of a scale-invariant dead leaves model. Zbl 1012.68715
Lee, Ann B.; Mumford, David; Huang, Jinggang
2001
The dawning of the age of stochasticity. Zbl 0962.60003
Mumford, David
2000
The dawning of the age of stochasticity. Zbl 1149.00309
Mumford, David
2000
The red book of varieties and schemes. Includes the Michigan lectures (1974) on “Curves and their Jacobians”. 2nd, expanded ed. with contributions by Enrico Arbarello. Zbl 0945.14001
Mumford, David
1999
Two- and three-dimensional patterns of the face. Zbl 0930.68140
Hallinan, Peter W.; Gordon, Gaile G.; Yuille, A. L.; Giblin, Peter; Mumford, David
1999
Calculus. Single and multivariable. 2nd ed. Zbl 0913.26003
Hughes-Hallett, Deborah; Gleason, Andrew M.; McCallum, William G.; Flath, Daniel E.; Lock, Patti Frazer; Gordon, Sheldon P.; Lomen, David O.; Lovelock, David; Mumford, David; Osgood, Brad G.; Pasquale, Andrew; Quinney, Douglas; Tecosky-Feldman, Jeff; Thrash, Joe B.; Thrash, Karen R.; Tucker, Thomas W.
1998
Trends in the profession of mathematics. Zbl 1288.00054
Mumford, David
1998
Multivariable calculus. Zbl 0892.26002
McCallum, William G.; Hughes-Hallett, Deborah; Gleason, Andrew M.; Flath, Daniel; Gordon, Sheldon P.; Mumford, David; Osgood, Brad G.; Quinney, Douglas; Raskind, Wayne; Tecosky-Feldman, Jeff; Thrash, Joe B.; Tucker, Thomas W.
1997
Algebraic Geometry. I: Complex projective varieties. Reprint of the corr. 2nd print. 1976. Zbl 0821.14001
Mumford, David
1995
Geometric invariant theory. 3rd enl. ed. Zbl 0797.14004
Mumford, D.; Fogarty, J.; Kirwan, F.
1994
Elastica and computer vision. Zbl 0798.53003
Mumford, David
1994
Chordal completions of planar graphs. Zbl 0809.05038
Chung, F. R. K.; Mumford, David
1994
Pattern theory: A unifying perspective. Zbl 0939.68820
Mumford, David
1994
What can be computed in algebraic geometry? Zbl 0846.13017
Bayer, Dave; Mumford, David
1993
Filtering, segmentation and depth. Zbl 0801.68171
Nitzberg, Mark; Mumford, David; Shiota, Takahiro
1993
Tata lectures on theta. III. Zbl 0744.14033
Mumford, David; Nori, Madhav; Norman, Peter
1991
Optimal approximations by piecewise smooth functions and associated variational problems. Zbl 0691.49036
Mumford, David; Shah, Jayant
1989
The red book of varieties and schemes. Zbl 0658.14001
Mumford, David
1988
Abelian varieties. With appendices by C. P. Ramanujam and Yuri Manin. 2nd ed. Reprint. Zbl 0583.14015
Mumford, David
1985
Tata lectures on theta. II: Jacobian theta functions and differential equations. With the collaboration of C. Musili, M. Nori, E. Previato, M. Stillman, and H. Umemura. Zbl 0549.14014
Mumford, David
1984
A stratification of the null cone via the moment map. (With an appendix by David Mumford). Zbl 0604.14006
Ness, Linda
1984
Tata lectures on theta. I: Introduction and motivation: Theta functions in one variable. Basic results on theta functions in several variables. With the assistance of C. Musili, M. Nori, E. Previato, and M. Stillman. Zbl 0509.14049
Mumford, David
1983
Towards an enumerative geometry of the moduli space of curves. Zbl 0554.14008
Mumford, David
1983
On the Kodaira dimension of the Siegel modular variety. Zbl 0527.14036
Mumford, David
1983
Geometric invariant theory. 2nd enlarged ed. Zbl 0504.14008
Mumford, D.; Fogarty, J.
1982
On the Kodaira dimension of the moduli space of curves. Zbl 0506.14016
Harris, Joe; Mumford, David
1982
Algebraic geometry. I: Complex projective varieties. Corr. 2nd printing. Zbl 0456.14001
Mumford, David
1980
The spectrum of difference operators and algebraic curves. Zbl 0502.58032
van Moerbeke, Pierre; Mumford, David
1979
An algebraic surface with K ample, $$(K^ 2)=9$$, $$p_ g=q=O$$. Zbl 0433.14021
Mumford, D.
1979
Some footnotes to the work of C. P. Ramanujam. Zbl 0444.14002
Mumford, D.
1978
Fields Medals. IV: An instinct for the key idea. Zbl 1225.01080
Mumford, David; Tate, John
1978
Stability of projective varieties. Zbl 0363.14003
Mumford, David
1977
Hirzebruch’s proportionality theorem in the non-compact case. Zbl 0365.14012
Mumford, D.
1977
Enriques’ classification of surfaces in char. $$p$$. II. Zbl 0348.14021
Bombieri, E.; Mumford, D.
1977
An algebro-geometric construction of commuting operators and of solutions to the Toda lattice equation, Korteweg de Vries equation and related non- linear equations. Zbl 0423.14007
Mumford, D.
1977
Stability of projective varieties. Zbl 0497.14004
Mumford, David
1977
Stability of projective varieties. Zbl 0376.14007
Mumford, David
1977
The projectivity of the moduli space of stable curves. I: Preliminaries on ”det” and ”Div”. Zbl 0343.14008
Knudsen, Finn; Mumford, David
1976
Algebraic geometry. I: Complex projective varieties. Zbl 0356.14002
Mumford, David
1976
Enriques’ classification of surfaces in char p. III. Zbl 0336.14010
Bombieri, E.; Mumford, D.
1976
Hilbert’s fourteenth problem - the finite generation of subrings such as rings of invariants. Zbl 0341.14019
Mumford, David
1976
Smooth compactification of locally symmetric varieties. Zbl 0334.14007
Ash, A.; Mumford, D.; Rapoport, M.; Tai, Y.
1975
Curves and their Jacobians. Zbl 0316.14010
Mumford, David
1975
The self-intersection formula and the ’formule-clef’. Zbl 0341.14002
Lascu, A. T.; Mumford, D.; Scott, D. B.
1975
Pathologies. IV. Zbl 0315.14012
Mumford, David
1975
Matsusaka’s big theorem. Zbl 0321.14004
Liebermann, D.; Mumford, D.
1975
A new approach to compactifying locally symmetric varieties. Zbl 0322.32016
Mumford, David
1975
Abelian varieties. With appendices by C. P. Ramanujam and Yuri Manin. 2nd ed. Zbl 0326.14012
Mumford, David
1974
Prym varieties. I. Zbl 0299.14018
Mumford, David
1974
Toroidal embeddings. I. Zbl 0271.14017
Kempf, G.; Knudsen, F.; Mumford, D.; Saint-Donat, Bernard
1973
A rank 2 vector bundle on P$$^4$$ with 15,000 symmetries. Zbl 0255.14017
Horrocks, G.; Mumford, D.
1973
A remark on the paper of M. Schlessinger. Zbl 0279.32007
Mumford, David
1973
Collected papers. Volume II: Holomorphic functions and linear systems. Ed. by M. Artin and D. Mumford. Zbl 0564.14001
Zariski, Oscar
1973
Some elementary examples of unirational varieties which are not rational. Zbl 0244.14017
Artin, M.; Mumford, D.
1972
An analytic construction of degenerating curves over complete local rings. Zbl 0228.14011
Mumford, David
1972
An analytic construction of degenerating Abelian varieties over complete rings. Zbl 0241.14020
Mumford, David
1972
Introduction to the theory of moduli. Zbl 0242.14004
Mumford, David; Suominen, Kalevi
1972
The irreducibility of the space of curves of a given genus. Zbl 0233.14008
Deligne, Pierre; Mumford, D.
1972
Rational equivalence of 0-cycles on surfaces. Zbl 0228.14005
Mumford, D.
1972
Collected papers. Vol. I: Foundations of algebraic geometry and resolution of singularities. Edited by H. Hironaka and D. Mumford. Zbl 0234.14001
Zariski, Oscar
1972
An analytic construction of degenerating curves over complete local rings. Zbl 0243.14010
Mumford, David
1972
Theta characteristics of an algebraic curve. Zbl 0216.05904
Mumford, David
1971
Algebraic surfaces. With appendices by S.S. Abhyankar, J. Lipman, and D. Mumford. 2nd suplemented ed. Zbl 0219.14020
Zariski, O.
1971
A remark on Mahler’s compactness theorem. Zbl 0215.23202
Mumford, D.
1971
The structure of the moduli spaces of curves and abelian varieties. Zbl 0222.14023
Mumford, David
1971
Abelian varieties. Zbl 0223.14022
Mumford, David
1970
Varieties defined by quadratic equations. Zbl 0198.25801
Mumford, David
1970
...and 22 more Documents
all top 5
### Cited by 6,675 Authors
55 Ballico, Edoardo 42 Biswas, Indranil 36 Zarkhin, Yuriĭ Gennad’evich 27 Bauer, Martin 23 Brion, Michel 22 Geng, Xianguo 21 Michor, Peter Wolfram 20 Harris, Joseph Daniel 19 Abramovich, Dan 19 Bruveris, Martins 19 Oort, Frans 19 Pirola, Gian Pietro 19 Tai, Xuecheng 18 Hulek, Klaus 18 Lange, Herbert 17 Eisenbud, David 17 Reichstein, Zinovy B. 17 Srivastava, Anuj 17 Voisin, Claire 16 Katsura, Toshiyuki 16 Kollár, János 16 Mumford, David Bryant 15 Beauville, Arnaud 15 Catanese, Fabrizio M. E. 15 Farkas, Gavril 14 Chen, Ke 14 Debarre, Olivier 14 Ichikawa, Takashi 13 Kannan, Subramaniam Senthamarai 13 Kleiman, Steven Lawrence 13 Previato, Emma 13 Zuo, Kang 12 Cremers, Daniel 12 Gurjar, Rajendra Vasant 12 Kumar, Shrawan 12 Renner, Lex E. 12 Salvati Manni, Riccardo 12 Schröer, Stefan 12 Van der Geer, Gerard 12 Viehweg, Eckart 11 Alper, Jarod 11 Brodmann, Markus P. 11 Caporaso, Lucia 11 Chen, Dawei 11 Dolgachev, Igor’ Vladimirovich 11 Duits, Remco 11 Edidin, Dan 11 Harris, Michael Howard 11 Lesfari, Ahmed 11 Nguyen Minh Chuong 11 Nicaise, Johannes 11 Pandharipande, Rahul 11 Silverman, Joseph Hillel 11 Sturmfels, Bernd 11 van Moerbeke, Pierre 11 Weinmann, Andreas 10 Adler, Mark 10 Arapura, Donu 10 Bismut, Jean-Michel 10 Braides, Andrea 10 Chambolle, Antonin 10 Chardin, Marc 10 Ciliberto, Ciro 10 Ellia, Philippe 10 Ford, Timothy J. 10 Grushevsky, Samuel 10 Harms, Philipp 10 Hassett, Brendan 10 Hausen, Jürgen 10 Kani, Ernst J. 10 Kato, Fumiharu 10 Katzarkov, Ludmil 10 Kirwan, Frances Clare 10 Leaci, Antonio 10 Sankaran, Gregory Kumar 10 Sommese, Andrew John 10 Soulé, Christophe 10 Srinivas, Vasudevan 10 Van den Bergh, Michel 10 Viviani, Filippo 10 Xu, Chenyang 10 Zhu, Wei 9 Alexeev, Valery A. 9 Bastianelli, Francesco 9 Bost, Jean-Benoît 9 Carriero, Michele 9 Chan, Tony Fan-Cheong 9 Donagi, Ron Y. 9 Esnault, Hélène 9 Focardi, Matteo 9 Gross, Mark 9 Korotkin, Dmitrii A. 9 Lan, Kai-Wen 9 Lee, Yongnam 9 Lieblich, Max David 9 Liedtke, Christian 9 Mabuchi, Toshiki 9 Manin, Yuri Ivanovich 9 Mazur, Barry 9 Mehta, Vikram Bhagvandas ...and 6,575 more Authors
all top 5
### Cited in 548 Serials
356 Mathematische Annalen 344 Inventiones Mathematicae 270 Journal of Algebra 257 Transactions of the American Mathematical Society 239 Compositio Mathematica 222 Duke Mathematical Journal 199 Advances in Mathematics 158 Mathematische Zeitschrift 150 Annales de l’Institut Fourier 149 Journal of Pure and Applied Algebra 134 Manuscripta Mathematica 133 Proceedings of the American Mathematical Society 115 Communications in Mathematical Physics 99 Journal of Algebraic Geometry 88 Annales Scientifiques de l’École Normale Supérieure. Quatrième Série 82 Communications in Algebra 82 Journal of Mathematical Imaging and Vision 81 Tohoku Mathematical Journal. Second Series 74 Journal of Number Theory 72 Journal of the American Mathematical Society 70 Journal für die Reine und Angewandte Mathematik 69 International Journal of Mathematics 65 Geometriae Dedicata 59 Journal of Geometry and Physics 55 International Journal of Computer Vision 52 Israel Journal of Mathematics 48 Michigan Mathematical Journal 47 Nagoya Mathematical Journal 47 Transformation Groups 46 SIAM Journal on Imaging Sciences 45 Bulletin of the American Mathematical Society. New Series 44 Selecta Mathematica. New Series 43 Archiv der Mathematik 43 Proceedings of the Japan Academy. Series A 43 Publications of the Research Institute for Mathematical Sciences, Kyoto University 43 Journal of Symbolic Computation 42 Journal of High Energy Physics 40 Annali di Matematica Pura ed Applicata. Serie Quarta 38 Publications Mathématiques 38 Geometry & Topology 37 Journal of the European Mathematical Society (JEMS) 36 Journal of Mathematical Physics 36 Letters in Mathematical Physics 36 Annals of Mathematics. Second Series 35 Mathematics of Computation 35 Bulletin de la Société Mathématique de France 35 European Journal of Mathematics 33 Annali della Scuola Normale Superiore di Pisa. Classe di Scienze. Serie IV 32 Computer Methods in Applied Mechanics and Engineering 31 Mathematische Nachrichten 30 Nuclear Physics. B 29 Abhandlungen aus dem Mathematischen Seminar der Universität Hamburg 29 Journal of Scientific Computing 29 Calculus of Variations and Partial Differential Equations 29 Comptes Rendus. Mathématique. Académie des Sciences, Paris 28 Functional Analysis and its Applications 28 Proceedings of the Indian Academy of Sciences. Mathematical Sciences 28 Annales de la Faculté des Sciences de Toulouse. Mathématiques. Série VI 28 Journal de Théorie des Nombres de Bordeaux 28 Journal of Mathematical Sciences (New York) 26 Pattern Recognition 25 Rendiconti del Seminario Matematico della Università di Padova 25 Linear Algebra and its Applications 24 Annals of Global Analysis and Geometry 24 The Journal of Geometric Analysis 24 Journal de Mathématiques Pures et Appliquées. Neuvième Série 23 Acta Mathematica 22 Indagationes Mathematicae. New Series 22 Documenta Mathematica 21 Archive for Rational Mechanics and Analysis 21 Mathematical Notes 21 Mathematical Proceedings of the Cambridge Philosophical Society 21 Theoretical and Mathematical Physics 21 Osaka Journal of Mathematics 21 Bulletin of the American Mathematical Society 20 Bulletin des Sciences Mathématiques 20 Communications in Contemporary Mathematics 20 Inverse Problems and Imaging 20 Algebra & Number Theory 20 Kyoto Journal of Mathematics 19 Proceedings of the Steklov Institute of Mathematics 18 Applied Mathematics and Computation 18 Advances in Geometry 18 Journal of the Institute of Mathematics of Jussieu 18 Annali della Scuola Normale Superiore di Pisa. Classe di Scienze. Serie V 18 SIGMA. Symmetry, Integrability and Geometry: Methods and Applications 18 Forum of Mathematics, Sigma 18 Journal de l’École Polytechnique – Mathématiques 17 Journal of Soviet Mathematics 17 Applied and Computational Harmonic Analysis 16 Journal of the Mathematical Society of Japan 16 Geometric and Functional Analysis. GAFA 16 Central European Journal of Mathematics 15 Journal of Functional Analysis 15 Topology and its Applications 15 Acta Applicandae Mathematicae 15 Differential Geometry and its Applications 15 European Series in Applied and Industrial Mathematics (ESAIM): Control, Optimization and Calculus of Variations 15 Foundations of Computational Mathematics 14 Journal of Computational Physics ...and 448 more Serials
all top 5
### Cited in 62 Fields
4,732 Algebraic geometry (14-XX) 1,005 Number theory (11-XX) 853 Several complex variables and analytic spaces (32-XX) 523 Differential geometry (53-XX) 496 Commutative algebra (13-XX) 433 Computer science (68-XX) 382 Group theory and generalizations (20-XX) 356 Dynamical systems and ergodic theory (37-XX) 348 Information and communication theory, circuits (94-XX) 328 Numerical analysis (65-XX) 326 Partial differential equations (35-XX) 310 Global analysis, analysis on manifolds (58-XX) 281 Manifolds and cell complexes (57-XX) 276 Quantum theory (81-XX) 267 Calculus of variations and optimal control; optimization (49-XX) 242 Functions of a complex variable (30-XX) 200 Associative rings and algebras (16-XX) 193 Topological groups, Lie groups (22-XX) 162 Nonassociative rings and algebras (17-XX) 126 Category theory; homological algebra (18-XX) 126 Mechanics of deformable solids (74-XX) 117 Algebraic topology (55-XX) 111 Field theory and polynomials (12-XX) 104 Statistics (62-XX) 103 Biology and other natural sciences (92-XX) 94 Combinatorics (05-XX) 87 Convex and discrete geometry (52-XX) 86 Linear and multilinear algebra; matrix theory (15-XX) 76 $$K$$-theory (19-XX) 69 Mechanics of particles and systems (70-XX) 66 Operations research, mathematical programming (90-XX) 64 Special functions (33-XX) 63 Operator theory (47-XX) 58 Ordinary differential equations (34-XX) 57 Probability theory and stochastic processes (60-XX) 54 Functional analysis (46-XX) 52 Relativity and gravitational theory (83-XX) 49 Harmonic analysis on Euclidean spaces (42-XX) 46 Geometry (51-XX) 32 Fluid mechanics (76-XX) 32 Statistical mechanics, structure of matter (82-XX) 32 Systems theory; control (93-XX) 29 Difference and functional equations (39-XX) 28 History and biography (01-XX) 27 Measure and integration (28-XX) 26 Real functions (26-XX) 24 Mathematical logic and foundations (03-XX) 19 General and overarching topics; collections (00-XX) 19 Abstract harmonic analysis (43-XX) 17 Game theory, economics, finance, and other social and behavioral sciences (91-XX) 16 Approximations and expansions (41-XX) 12 Potential theory (31-XX) 9 General topology (54-XX) 7 Geophysics (86-XX) 6 Order, lattices, ordered algebraic structures (06-XX) 6 Integral transforms, operational calculus (44-XX) 5 Mathematics education (97-XX) 4 General algebraic systems (08-XX) 4 Optics, electromagnetic theory (78-XX) 3 Integral equations (45-XX) 3 Classical thermodynamics, heat transfer (80-XX) 1 Astronomy and astrophysics (85-XX)
### Wikidata Timeline
The data are displayed as stored in Wikidata under a Creative Commons CC0 License. Updates and corrections should be made in Wikidata.
| 2022-07-01T04:27:06 |
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|
https://par.nsf.gov/biblio/10203525
|
The FHD/εppsilon Epoch of Reionisation power spectrum pipeline
Abstract Epoch of Reionisation (EoR) data analysis requires unprecedented levels of accuracy in radio interferometer pipelines. We have developed an imaging power spectrum analysis to meet these requirements and generate robust 21 cm EoR measurements. In this work, we build a signal path framework to mathematically describe each step in the analysis, from data reduction in the Fast Holographic Deconvolution (FHD) package to power spectrum generation in the ε ppsilon package. In particular, we focus on the distinguishing characteristics of FHD/ ε ppsilon: highly accurate spectral calibration, extensive data verification products, and end-to-end error propagation. We present our key data analysis products in detail to facilitate understanding of the prominent systematics in image-based power spectrum analyses. As a verification to our analysis, we also highlight a full-pipeline analysis simulation to demonstrate signal preservation and lack of signal loss. This careful treatment ensures that the FHD/ ε ppsilon power spectrum pipeline can reduce radio interferometric data to produce credible 21 cm EoR measurements.
Authors:
; ; ; ; ; ;
Award ID(s):
Publication Date:
NSF-PAR ID:
10203525
Journal Name:
Publications of the Astronomical Society of Australia
Volume:
36
ISSN:
1323-3580
2. ABSTRACT We quantify the effect of radio frequency interference (RFI) on measurements of the 21-cm power spectrum during the Epoch of Reionization (EoR). Specifically, we investigate how the frequency structure of RFI source emission generates contamination in higher order wave modes, which is much more problematic than smooth-spectrum foreground sources. Using a relatively optimistic EoR model, we find that even a single relatively dim RFI source can overwhelm the EoR power spectrum signal of $\sim 10\, {\rm mK}^2$ for modes $0.1 \ \lt k \lt 2 \, h\, {\rm Mpc}^{-1}$. If the total apparent RFI flux density in the final power spectrum integration is kept below 1 mJy, an EoR signal resembling this optimistic model should be detectable for modes $k \lt 0.9\, h\, {\rm Mpc}^{-1}$, given no other systematic contaminants and an error tolerance as high as 10 per cent. More pessimistic models will be more restrictive. These results emphasize the need for highly effective RFI mitigation strategies for telescopes used to search for the EoR.
| 2023-01-31T12:51:25 |
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|
https://aperta.ulakbim.gov.tr/record/10371/export/xd
|
Dergi makalesi Açık Erişim
The Effects of COVID-19 Measures on Air Pollutant Concentrations at Urban and Traffic Sites in Istanbul
Sahin, Ulku Alver
Dublin Core
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<dc:creator>Sahin, Ulku Alver</dc:creator>
<dc:date>2020-01-01</dc:date>
<dc:description>Since December 2019, most countries have been working to stop the spread of SARS-CoV-2, the virus responsible for COVID-19. These measures, which include restricting movement, have environmental consequences. This study assessed the impact of COVID-19 measures on air pollutant concentrations measured in urban areas and traffic stations on both the European and Asian sides of Istanbul during March 2020. Significant reductions in pollutants: 32-43% (PM10), 19-47% (PM2.5), 29-44% (NO2), 40-58% (CO) and 34-69% (SO2) were calculated. The clearest reductions at the traffic stations were in NO2 which originates primarily from vehicle exhaust. The reduction of NO2 at the traffic station on the European side was found higher comparing the Asian side. The average concentrations of NO2, PM2.5, PM10 and CO during peak traffic hours were significantly (p < 0.01) decreased under COVID-19 measures. The results indicate that due to the measures taken in Istanbul and across Turkey and to control the spread of the virus, anthropogenic activities such as industry, vehicle traffic and sea transport have decreased, and consequently, air pollution has been significantly reduced. These pollutant levels demonstrate the anthropogenic contribution to air pollution and can inform clean air actions in Istanbul and in others cities throughout the world.</dc:description>
<dc:identifier>https://aperta.ulakbim.gov.tr/record/10371</dc:identifier>
<dc:identifier>oai:zenodo.org:10371</dc:identifier>
<dc:rights>info:eu-repo/semantics/openAccess</dc:rights>
<dc:source>AEROSOL AND AIR QUALITY RESEARCH 20(9) 1874-1885</dc:source>
<dc:title>The Effects of COVID-19 Measures on Air Pollutant Concentrations at Urban and Traffic Sites in Istanbul</dc:title>
<dc:type>info:eu-repo/semantics/article</dc:type>
<dc:type>publication-article</dc:type>
</oai_dc:dc>
3
1
görüntülenme
indirilme
Görüntülenme 3 İndirme 1 Veri hacmi 174 Bytes Tekil görüntülenme 3 Tekil indirme 1
| 2022-08-11T17:02:37 |
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https://alldimensions.fandom.com/wiki/Ghuipsuperverse
|
## FANDOM
2,847 Pages
Ghuipsuperverse (GHUSUV) is The Near Everything but from the super reality, it owns $\frac{1}{\sqrt{\eth}}$ of the super-everything.
Community content is available under CC-BY-SA unless otherwise noted.
| 2019-11-23T02:54:24 |
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http://webarchive.nationalarchives.gov.uk/20110809091832/http:/www.teachingandlearningresources.org.uk/node/24968
|
This snapshot, taken on
10/08/2011
, shows web content acquired for preservation by The National Archives. External links, forms and search may not work in archived websites and contact details are likely to be out of date.
The UK Government Web Archive does not use cookies but some may be left in your browser from archived websites.
# Step 8
Know and use the formulae for the area and circumference of a circle
## Probing questions
• What is the minimum information you need to be able to find the circumference and area of a circle?
• Give pupils some work that includes mistakes.
• Ask them to identify and correct the mistakes.
• How would you go about finding the area of a circle if you knew the circumference?
## What if pupils find this a barrier?
Ensure that pupils understand that $\mathrm{\Pi }$ is the ratio of the length of the circumference of a circle to its diameter.
Demonstrate an approximation to the area by cutting a circle into 16 sectors and forming an approximation to a rectangle to establish a visual approximation to $\pi {r}^{2}$.
Ensure that $\pi {r}^{2}$ is seen as $\pi ×r×r$.
Give pupils some work that includes mistakes and ask them to correct them. Be specific about common mistakes.
| 2015-07-02T04:01:16 |
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http://tex.wikidot.com/snippets:footnotes
|
Footnotes in TeX
rating: +1
« All Snippets
The format for footnotes is simple:
````Here is the sentence you are writing.\footnote{And here is your footnote.}`
```
To make it easier to read, I like to put the footnote on a separate line:
``````Here is the sentence you are writing.%
\footnote{And here is your footnote.}```
```
The percent % ensures that there is not an extra space between the end of the sentence and the footnote number.
# Details
````\footnote[number]{text}`
```
The \footnote command places the text at the bottom of the page where it is inserted and places an autonumbered number in superscript before the text of the footnote. The optional argument, number, is used to change the default footnote number. Remember that the footnotes are automatically numbered and so the numbers don't need to be changed.
````\footnotemark`
```
The \footnotemark command puts the footnote number in the text. This command can be used in inner paragraph mode. The text of the footnote is supplied by the \footnotetext command.
This command can be used to produce several consecutive footnote markers referring to the same footnote by using
\footnotemark[\value{footnote}] after the first \footnote command.
````\footnotetext[number]{text}`
```
The \footnotetext command produces the text to be placed at the bottom of the page. This command can come anywhere after the \footnotemark command. The \footnotetext command must appear in outer paragraph mode.
The optional argument, number, is used to change the default footnote number.
# References
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| 2018-12-18T23:07:09 |
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|
https://par.nsf.gov/biblio/10374946-massive-dusty-hi-absorptionselected-galaxy-identified-co-emission-survey
|
A Massive, Dusty, Hi Absorption–Selected Galaxy at z ≈ 2.46 Identified in a CO Emission Survey
Abstract
We report a NOrthern Extended Millimeter Array (NOEMA) and Atacama Large Millimeter/submillimeter Array search for redshifted CO emission from the galaxies associated with seven high-metallicity ([M/H] ≥ −1.03) damped Lyαabsorbers (DLAs) atz≈ 1.64–2.51. Our observations yielded one new detection of CO(3–2) emission from a galaxy atz= 2.4604 using NOEMA, associated with thez= 2.4628 DLA toward QSO B0201+365. Including previous searches, our search results in detection rates of CO emission of$≈56−24+38$% and$≈11−9+26$%, respectively, in the fields of DLAs with [M/H] > −0.3 and [M/H] < −0.3. Further, the Hi–selected galaxies associated with five DLAs with [M/H] > −0.3 all have high molecular gas masses, ≳5 × 1010M. This indicates that the highest-metallicity DLAs atz≈ 2 are associated with the most massive galaxies. The newly identifiedz≈ 2.4604 Hi–selected galaxy, DLA0201+365g, has an impact parameter of ≈7 kpc to the QSO sightline, and an implied molecular gas mass of (5.04 ± 0.78) × 1010× (αCO/4.36) × (r31/0.55)M. Archival Hubble Space Telescope Wide Field and Planetary Camera 2 imaging covering the rest-frame near-ultraviolet (NUV) and far-ultraviolet (FUV) emission from this galaxy yield nondetections of rest-frame NUV and FUV emission, and a 5σupper limit of 2.3Myr−1on the unobscured more »
Authors:
; ; ; ; ; ;
Award ID(s):
Publication Date:
NSF-PAR ID:
10374946
Journal Name:
The Astrophysical Journal
Volume:
934
Issue:
1
Page Range or eLocation-ID:
Article No. 87
ISSN:
0004-637X
Publisher:
DOI PREFIX: 10.3847
National Science Foundation
##### More Like this
1. Abstract
The bimodal absorption system imaging campaign (BASIC) aims to characterize the galaxy environments of a sample of 36 Hi-selected partial Lyman limit systems (pLLSs) and Lyman limit systems (LLSs) in 23 QSO fields atz≲ 1. These pLLSs/LLSs provide a unique sample of absorbers with unbiased and well-constrained metallicities, allowing us to explore the origins of metal-rich and low-metallicity circumgalactic medium (CGM) atz< 1. Here we present Keck/KCWI and Very Large Telescope/MUSE observations of 11 of these QSO fields (19 pLLSs) that we combine with Hubble Space Telescope/Advanced Camera for Surveys imaging to identify and characterize the absorber-associated galaxies at 0.16 ≲z≲ 0.84. We find 23 unique absorber-associated galaxies, with an average of one associated galaxy per absorber. For seven absorbers, all with <10% solar metallicities, we find no associated galaxies with$logM⋆≳9.0$withinρ/Rvirand ∣Δv∣/vesc≤ 1.5 with respect to the absorber. We do not find any strong correlations between the metallicities or Hicolumn densities of the gas and most of the galaxy properties, except for the stellar mass of the galaxies: the low-metallicity ([X/H] ≤ −1.4) systems have a probability of$0.39−0.15+0.16$for having a host galaxy with$logM⋆≥9.0$withinρ/Rvir≤ 1.5, while the higher metallicity absorbers havemore »
2. Abstract
We report CO(5 → 4) and CO(6 → 5) line observations in the dusty starbursting galaxy CRLE (z= 5.667) and the main-sequence (MS) galaxy HZ10 (z= 5.654) with the Northern Extended Millimeter Array. CRLE is the most luminousz> 5 starburst in the COSMOS field and HZ10 is the most gas-rich “normal” galaxy currently known atz> 5. We find line luminosities for CO(5 → 4) and CO(6 → 5) of (4.9 ± 0.5) and (3.8 ± 0.4) × 1010K km s−1pc2for CRLE and upper limits of < 0.76 and < 0.60 × 1010K km s−1pc2for HZ10, respectively. The CO excitation of CRLE appears comparable to otherz> 5 dusty star-forming galaxies. For HZ10, these line luminosity limits provide the first significant constraints of this kind for an MS galaxy atz> 5. We find the upper limit of$L5→4′/L2→1′$in HZ10 could be similar to the average value for MS galaxies aroundz≈ 1.5, suggesting that MS galaxies with comparable gas excitation may already have existed one billion years after the Big Bang. For CRLE we determine the most likely values for the H2density, kinetic temperature, and dust temperature based on excitation modeling of the CO line ladder. Wemore »
3. Abstract
We present spatially resolved morphological properties of [CII] 158μm, [OIII] 88μm, dust, and rest-frame ultraviolet (UV) continuum emission for A1689-zD1, a strongly lensed, sub-L* galaxy atz= 7.13, by utilizing deep Atacama Large Millimeter/submillimeter Array (ALMA) and Hubble Space Telescope (HST) observations. While the [OIII] line and UV continuum are compact, the [CII] line is extended up to a radius ofr∼ 12 kpc. Using multi-band rest-frame far-infrared continuum data ranging from 52 to 400μm, we find an average dust temperature and emissivity index of$Tdust=41−14+17$K and$β=1.7−0.7+1.1$, respectively, across the galaxy. We find slight differences in the dust continuum profiles at different wavelengths, which may indicate that the dust temperature decreases with distance. We map the star formation rate (SFR) via IR and UV luminosities and determine a total SFR of 37 ± 1Myr−1with an obscured fraction of 87%. While the [OIII] line is a good tracer of the SFR, the [CII] line shows deviation from the localL[CII]-SFR relations in the outskirts of the galaxy. Finally, we observe a clear difference in the line profile between [CII] and [OIII], with significant residuals (∼5σ) in the [OIII] line spectrum after subtracting a single Gaussian model. This suggestsmore »
4. Abstract
We measure the molecular-to-atomic gas ratio,Rmol, and the star formation rate (SFR) per unit molecular gas mass, SFEmol, in 38 nearby galaxies selected from the Virgo Environment Traced in CO (VERTICO) survey. We stack ALMA12CO (J= 2−1) spectra coherently using Hivelocities from the VIVA survey to detect faint CO emission out to galactocentric radiirgal∼ 1.2r25. We determine the scale lengths for the molecular and stellar components, finding a ∼3:5 relation compared to ∼1:1 in field galaxies, indicating that the CO emission is more centrally concentrated than the stars. We computeRmolas a function of different physical quantities. While the spatially resolvedRmolon average decreases with increasing radius, we find that the mean molecular-to-atomic gas ratio within the stellar effective radiusRe,Rmol(r<Re), shows a systematic increase with the level of Hi, truncation and/or asymmetry (HIperturbation). Analysis of the molecular- and the atomic-to-stellar mass ratios withinRe,$R⋆mol(rand$R⋆atom(r, shows that VERTICO galaxies have increasingly lower$R⋆atom(rfor larger levels of HIperturbation (compared to field galaxies matched in stellar mass), but no significant change in$R⋆mol(r. We also measure a clear systematic decrease of the SFEmolwithinRe, SFEmol(r<Re),more »
5. Abstract
We present a multiwavelength analysis of the galaxy cluster SPT-CL J0607-4448 (SPT0607), which is one of the most distant clusters discovered by the South Pole Telescope atz= 1.4010 ± 0.0028. The high-redshift cluster shows clear signs of being relaxed with well-regulated feedback from the active galactic nucleus (AGN) in the brightest cluster galaxy (BCG). Using Chandra X-ray data, we construct thermodynamic profiles and determine the properties of the intracluster medium. The cool-core nature of the cluster is supported by a centrally peaked density profile and low central entropy ($K0=18−9+11$keV cm2), which we estimate assuming an isothermal temperature profile due to the limited spectral information given the distance to the cluster. Using the density profile and gas cooling time inferred from the X-ray data, we find a mass-cooling rate$Ṁcool=100−60+90M⊙$yr−1. From optical spectroscopy and photometry around the [Oii] emission line, we estimate that the BCG star formation rate is$SFR[OII]=1.7−0.6+1.0M⊙$yr−1, roughly two orders of magnitude lower than the predicted mass-cooling rate. In addition, using ATCA radio data at 2.1 GHz, we measure a radio jet power$Pcav=3.2−1.3+2.1×1044$erg s−1, which is consistent withmore »
| 2023-04-01T23:51:19 |
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http://xxx.lanl.gov/abs/astro-ph/0005106
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astro-ph
(what is this?)
# Title: The Intergalactic Medium
Abstract: About half a million years after the Big Bang, the ever-fading cosmic blackbody radiation cooled below 3000 K and shifted first into the infrared and then into the radio, and the smooth baryonic plasma that filled the Universe became neutral. The Universe then entered a dark age'' which persisted until the first cosmic structures collapsed into gravitationally-bound systems, and evolved into stars, galaxies, and black holes that lit up the Universe again. Some time between redshift of 7 and 15, stars within protogalaxies created the first heavy elements; these systems, together perhaps with an early population of quasars, generated the ultraviolet radiation that reheated and reionized the cosmos. The history of the Universe during and soon after these crucial formative stages is recorded in the all-pervading intergalactic medium (IGM), which is believed to contain most of the ordinary baryonic material left over from the Big Bang. Throughout the epoch of structure formation, the IGM becomes clumpy and acquires peculiar motions under the influence of gravity, and acts as a source for the gas that gets accreted, cools, and forms stars within galaxies, and as a sink for the metal enriched material, energy, and radiation which they eject. Observations of absorption lines in quasar spectra at redshifts up to 5 provide invaluable insight into the chemical composition of the IGM and primordial density fluctuation spectrum of some of the earliest formed cosmological structures, as well as of the ultraviolet background radiation that ionizes them.
| 2014-04-24T00:24:43 |
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http://pdglive.lbl.gov/DataBlock.action;jsessionid=ADA5FA63EE416D93B4E8F7D8A01FBA34?node=Q009TP5&init=0
|
# ${{\mathit t}^{\,'}}$(5/3)-quark/hadron mass limits in ${{\mathit p}}{{\overline{\mathit p}}}$ and ${{\mathit p}}{{\mathit p}}$ collisions INSPIRE search
VALUE (GeV) CL% DOCUMENT ID TECN COMMENT
$\bf{> 800}$ 95 1
2014 T
CMS ${{\mathit t}^{\,'}{(5/3)}}$ $\rightarrow$ ${{\mathit t}}{{\mathit W}^{+}}$
$> 750$ 95 2
2015 BY
ATLS ${{\mathit t}^{\,'}{(5/3)}}$ $\rightarrow$ ${{\mathit t}}{{\mathit W}^{+}}$
$> 840$ 95 3
2015 Z
ATLS ${{\mathit t}^{\,'}{(5/3)}}$ $\rightarrow$ ${{\mathit t}}{{\mathit W}^{+}}$
1 Based on 19.5 fb${}^{-1}$ of ${{\mathit p}}{{\mathit p}}$ data at $\sqrt {s }$ = 8 TeV. Non-observation of anomaly in ${{\mathit H}_{{T}}}$ distribution in the same sign dilepton events leads to the limit when pair produced ${{\mathit t}^{\,'}{(5/3)}}$ quark decays exclusively into ${{\mathit t}}$ and ${{\mathit W}^{+}}$, resulting in the final state with ${{\mathit b}}{{\overline{\mathit b}}}{{\mathit W}^{+}}{{\mathit W}^{-}}{{\mathit W}^{+}}{{\mathit W}^{-}}$ .
2 AAD 2015BY based on 20.3 fb${}^{-1}$ of ${{\mathit p}}{{\mathit p}}$ data at $\sqrt {s }$ = 8 TeV. Limit on ${{\mathit t}^{\,'}{(5/3)}}$ in pair and single production assuming its coupling to ${{\mathit W}}{{\mathit t}}$ is equal to one. Used events containing ${}\geq{}2{{\mathit \ell}}$ + $\not E_T$ + ${}\geq{}$2j (${}\geq{}$1 ${{\mathit b}}$) and including a same-sign lepton pair.
3 AAD 2015Z based on 20.3 fb${}^{-1}$ of ${{\mathit p}}{{\mathit p}}$ data at $\sqrt {s }$ = 8 TeV. Used events with ${{\mathit \ell}}$ + $\not E_T$ + ${}\geq{}$6j (${}\geq{}$1 ${{\mathit b}}$) and at least one pair of jets from weak boson decay, sensitive to the final state ${{\mathit b}}{{\overline{\mathit b}}}{{\mathit W}^{+}}{{\mathit W}^{-}}{{\mathit W}^{+}}{{\mathit W}^{-}}$ .
References:
JHEP 1510 150 Analysis of Events with ${\mathit {\mathit b}}$-Jets and a Pair of Leptons of the Same Charge in ${{\mathit p}}{{\mathit p}}$ Collisions at $\sqrt {s }$ = 8 TeV with the ATLAS Detector
PR D91 112011 Search for Vector-Like Quarks in Events with One Isolated Lepton, Missing Transverse Momentum and Jets at $\sqrt {s }$ = 8 TeV with the ATLAS Detector
| 2017-12-16T10:47:50 |
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https://www.zbmath.org/authors/?q=ai%3Adubickas.arturas
|
# zbMATH — the first resource for mathematics
## Dubickas, Artūras
Compute Distance To:
Author ID: dubickas.arturas Published as: Dubickas, Artūras; Dubickas, A.; Dubickas, Arturas; Dubickas, Artũras External Links: Wikidata
Documents Indexed: 229 Publications since 1986 3 Contributions as Editor Reviewing Activity: 253 Reviews
all top 5
#### Co-Authors
157 single-authored 11 Jankauskas, Jonas 10 Drungilas, Paulius 10 Smyth, Christopher J. 8 Sha, Min 5 Laurinčikas, Antanas 5 Novikas, Aivaras 4 Šarka, Paulius 2 Bugeaud, Yann 2 Garunkštis, Ramūnas 2 Macaitienė, Renata 2 Manstavičius, Eugenijus 2 Mossinghoff, Michael J. 2 Pritsker, Igor E. 2 Shparlinski, Igor E. 2 Šiurys, Jonas 2 Stepanauskas, Gediminas 2 Steuding, Jörn 1 Alkauskas, Giedrius 1 Balčiūnas, Aidas 1 Bang, Sejeong 1 Bentkus, Vidmants-Kastytis 1 Berend, Daniel 1 Berry, Neil 1 Dixon, John D. 1 Elkies, Noam David 1 Hare, Kevin G. 1 Konyagin, Sergeĭ Vladimirovich 1 Koolen, Jack H. 1 Kreso, Dijana 1 Luca, Florian 1 Moulton, Vincent L. 1 Plankis, Tomas 1 Poonen, Bjorn 1 Puriuškis, Gintaras 1 Schoen, Tomasz 1 Šemetulskis, Gražvydas 1 Stankevičius, Andrius 1 Steuding, Rasa 1 Xu, Zhiqiang
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#### Serials
21 Lithuanian Mathematical Journal 13 Acta Arithmetica 9 Journal of Number Theory 5 Archiv der Mathematik 4 Bulletin of the Australian Mathematical Society 4 Mathematical Notes 4 International Journal of Number Theory 3 Moscow University Mathematics Bulletin 3 Periodica Mathematica Hungarica 3 Mathematics of Computation 3 Canadian Mathematical Bulletin 3 Colloquium Mathematicum 3 Glasgow Mathematical Journal 3 Monatshefte für Mathematik 3 Publicationes Mathematicae 3 Acta Mathematica Hungarica 3 Proceedings of the Indian Academy of Sciences. Mathematical Sciences 3 Journal de Théorie des Nombres de Bordeaux 3 Fizikos ir Matematikos Fakulteto Mokslinio Seminaro Darbai 2 Analysis Mathematica 2 Discrete Mathematics 2 Bulletin of the London Mathematical Society 2 Czechoslovak Mathematical Journal 2 Manuscripta Mathematica 2 Mathematische Nachrichten 2 Proceedings of the American Mathematical Society 2 Proceedings of the Edinburgh Mathematical Society. Series II 2 Quaestiones Mathematicae 2 Results in Mathematics 2 Glasnik Matematički. Serija III 2 Litovskiĭ Matematicheskiĭ Sbornik 2 Vestnik Moskovskogo Universiteta. Seriya I. Matematika, Mekhanika 2 Expositiones Mathematicae 2 Indagationes Mathematicae. New Series 2 Applicable Algebra in Engineering, Communication and Computing 2 Bulletin Mathématique de la Société des Sciences Mathématiques de Roumanie. Nouvelle Série 2 St. Petersburg Mathematical Journal 2 Mathematical Communications 2 Mathematical Inequalities & Applications 2 Nonlinear Analysis. Modelling and Control 2 Journal of the Australian Mathematical Society 2 Mediterranean Journal of Mathematics 2 Chebyshevskiĭ Sbornik 2 Moscow Journal of Combinatorics and Number Theory 1 Indian Journal of Pure & Applied Mathematics 1 Israel Journal of Mathematics 1 Mathematical Proceedings of the Cambridge Philosophical Society 1 Rocky Mountain Journal of Mathematics 1 Russian Mathematical Surveys 1 Ukraïns’kyĭ Matematychnyĭ Zhurnal 1 Abhandlungen aus dem Mathematischen Seminar der Universität Hamburg 1 Acta Scientiarum Mathematicarum 1 Advances in Mathematics 1 Annali di Matematica Pura ed Applicata. Serie Quarta 1 Annales Polonici Mathematici 1 Archivum Mathematicum 1 Canadian Journal of Mathematics 1 Commentationes Mathematicae Universitatis Carolinae 1 Functiones et Approximatio. Commentarii Mathematici 1 Illinois Journal of Mathematics 1 Journal of Approximation Theory 1 Journal of the Korean Mathematical Society 1 Kodai Mathematical Journal 1 Mathematica Scandinavica 1 Mathematica Slovaca 1 Mathematische Zeitschrift 1 Mathematika 1 Michigan Mathematical Journal 1 Proceedings of the Japan Academy. Series A 1 Publications de l’Institut Mathématique. Nouvelle Série 1 Rendiconti del Seminario Matematico della Università di Padova 1 Siberian Mathematical Journal 1 Sibirskiĭ Matematicheskiĭ Zhurnal 1 Studia Scientiarum Mathematicarum Hungarica 1 Theoretical Computer Science 1 European Journal of Combinatorics 1 Bulletin of the Korean Mathematical Society 1 Statistics & Probability Letters 1 Acta Applicandae Mathematicae 1 Graphs and Combinatorics 1 Revista Matemática Iberoamericana 1 Publicacions Matemàtiques 1 Journal of the Ramanujan Mathematical Society 1 Acta Mathematica Universitatis Comenianae. New Series 1 Aequationes Mathematicae 1 Elemente der Mathematik 1 Experimental Mathematics 1 Combinatorics, Probability and Computing 1 Journal of Mathematical Sciences (New York) 1 Turkish Journal of Mathematics 1 The Electronic Journal of Combinatorics 1 The New York Journal of Mathematics 1 Mathematical Research Letters 1 Advances in Computational Mathematics 1 Integral Transforms and Special Functions 1 Annales Academiae Scientiarum Fennicae. Mathematica 1 The Ramanujan Journal 1 Electronic Journal of Qualitative Theory of Differential Equations 1 Journal of Integer Sequences 1 Analysis (München) ...and 18 more Serials
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#### Fields
214 Number theory (11-XX) 50 Field theory and polynomials (12-XX) 16 Functions of a complex variable (30-XX) 7 Combinatorics (05-XX) 7 Computer science (68-XX) 5 Real functions (26-XX) 3 General and overarching topics; collections (00-XX) 3 History and biography (01-XX) 3 Approximations and expansions (41-XX) 3 Convex and discrete geometry (52-XX) 2 Commutative algebra (13-XX) 2 Linear and multilinear algebra; matrix theory (15-XX) 2 Potential theory (31-XX) 2 Difference and functional equations (39-XX) 2 Differential geometry (53-XX) 1 Algebraic geometry (14-XX) 1 Group theory and generalizations (20-XX) 1 Special functions (33-XX) 1 Partial differential equations (35-XX) 1 Dynamical systems and ergodic theory (37-XX) 1 Sequences, series, summability (40-XX) 1 Calculus of variations and optimal control; optimization (49-XX) 1 Geometry (51-XX) 1 Probability theory and stochastic processes (60-XX) 1 Information and communication theory, circuits (94-XX)
#### Citations contained in zbMATH Open
142 Publications have been cited 537 times in 324 Documents Cited by Year
Arithmetical properties of powers of algebraic numbers. Zbl 1164.11025
Dubickas, Artūras
2006
On the distance from a rational power to the nearest integer. Zbl 1097.11035
Dubickas, Artūras
2006
On the metric Mahler measure. Zbl 1030.11056
Dubickas, A.; Smyth, C. J.
2001
There are only finitely many distance-regular graphs of fixed valency greater than two. Zbl 1303.05044
Bang, S.; Dubickas, A.; Koolen, J. H.; Moulton, V.
2015
Distribution modulo 1 and the discrete universality of the Riemann zeta-function. Zbl 1409.11061
Dubickas, Artūras; Laurinčikas, Antanas
2016
On the number of reducible polynomials of bounded naive height. Zbl 1305.11089
Dubickas, Artūras
2014
Integer parts of powers of rational numbers. Zbl 1084.11009
Dubickas, Artūras; Novikas, Aivaras
2005
Integer parts of powers of Pisot and Salem numbers. Zbl 1004.11059
Dubickas, Artūras
2002
On metric heights. Zbl 1050.11089
Dubickas, A.; Smyth, C. J.
2003
On multiplicative functions which are additive on sums of primes. Zbl 1344.11005
Dubickas, Artūras; Šarka, Paulius
2013
Prime and composite numbers as integer parts of powers. Zbl 1102.11004
Alkauskas, G.; Dubickas, A.
2004
On the maximal product of distances between points on a sphere. Zbl 0890.11023
Dubickas, A.
1996
Fractional parts of powers and Sturmian words. Zbl 1140.11318
Bugeaud, Yann; Dubickas, Artūras
2005
Auxiliary polynomials for some problems regarding Mahler’s measure. Zbl 1074.11018
Dubickas, Artūras; Mossinghoff, Michael J.
2005
Polynomials irreducible by Eisenstein’s criterion. Zbl 1045.11019
Dubickas, Artūras
2003
On the degree of a linear form in conjugates of an algebraic number. Zbl 1028.11066
Dubickas, Arturas
2002
The polynomial Pell equation. Zbl 1077.11020
Dubickas, Artūras; Steuding, Jörn
2004
On the Remak height, the Mahler measure and conjugate sets of algebraic numbers lying on two circles. Zbl 0997.11087
Dubickas, A.; Smyth, C. J.
2001
Three problems for polynomials of small measure. Zbl 0972.11102
Dubickas, Artūras
2001
Variations on the theme of Hilbert’s theorem 90. Zbl 1112.11308
Dubickas, A.; Smyth, C. J.
2002
Counting and testing dominant polynomials. Zbl 1409.11021
Dubickas, Artūras; Sha, Min
2015
On the limit points of the fractional parts of powers of Pisot numbers. Zbl 1164.11026
Dubickas, Artūras
2006
On a conjecture of A. Schinzel and H. Zassenhaus. Zbl 0777.11039
Dubickas, Artūras
1993
On algebraic numbers of small measure. Zbl 0860.11063
Dubickas, A.
1995
Mahler measures close to an integer. Zbl 1086.11049
Dubickas, Artūras
2002
On the order of vanishing at 1 of a polynomial. Zbl 0963.12001
Dubickas, A.
1999
Refinement equations and spline functions. Zbl 1187.41005
Dubickas, Artūras; Xu, Zhiqiang
2010
Nonreciprocal units in a number field with an application to Oeljeklaus-Toma manifolds. Zbl 1290.11148
Dubickas, Artūras
2014
The lonely runner problem for many runners. Zbl 1253.11073
Dubickas, Artūras
2011
On Newman polynomials which divide no Littlewood polynomial. Zbl 1208.11123
Dubickas, Arturas; Jankauskas, Jonas
2009
On the fractional parts of lacunary sequences. Zbl 1140.11038
Dubickas, Artũras
2006
On the lines passing through two conjugates of a Salem number. Zbl 1166.11031
Dubickas, Artūras; Smyth, Chris
2008
On the powers of 3/2 and other rational numbers. Zbl 1144.11053
Dubickas, Artūras
2008
On roots of polynomials with positive coefficients. Zbl 1172.11036
Dubickas, Artūras
2007
On numbers which are Mahler measures. Zbl 1065.11084
Dubickas, Artūras
2004
Counting degenerate polynomials of fixed degree and bounded height. Zbl 1347.11026
Dubickas, Artūras; Sha, Min
2015
Joint discrete universality of Dirichlet $$L$$-functions. Zbl 1316.11077
Dubickas, Artūras; Laurinčikas, Antanas
2015
No two non-real conjugates of a Pisot number have the same imaginary part. Zbl 1361.11062
Dubickas, Artūras; Hare, Kevin G.; Jankauskas, Jonas
2017
Powers of a rational number modulo 1 cannot lie in a small interval. Zbl 1245.11082
Dubickas, Artūras
2009
On a sequence related to that of Thue-Morse and its applications. Zbl 1113.11008
Dubickas, Artūras
2007
On the discriminant of the power of an algebraic number. Zbl 1127.11069
Dubickas, Arturas
2007
A binary linear recurrence sequence of composite numbers. Zbl 1197.11019
Dubickas, Artūras; Novikas, Aivaras; Šiurys, Jonas
2010
The conjugate dimension of algebraic numbers. Zbl 1062.11064
Berry, Neil; Dubickas, Artūras; Elkies, Noam D.; Poonen, Bjorn; Smyth, Chris
2004
On the powers of some transcendental numbers. Zbl 1146.11039
Dubickas, Artūras
2007
On numbers which are differences of two conjugates of an algebraic integer. Zbl 1028.11065
Dubickas, Artūras
2002
The values of Mahler measures. Zbl 1107.11044
Dixon, John D.; Dubickas, Artūras
2004
A lower bound for the quantity $$\| (3/2)^ k\|$$. Zbl 0712.11037
Dubickas, Artūras
1990
Diophantine equations with truncated binomial polynomials. Zbl 1339.11044
Dubickas, Artūras; Kreso, Dijana
2016
Roots of unity as quotients of two roots of a polynomial. Zbl 1321.11110
Dubickas, Artūras
2012
Two exercises concerning the degree of the product of algebraic numbers. Zbl 1220.11131
Dubickas, Artūras
2005
On the limit points of $$(a_n\xi )_{n=1}^\infty$$ mod 1 for slowly increasing integer sequences $$(a_n)_{n=1}^\infty$$. Zbl 1221.11161
Dubickas, Arturas
2009
Positive density of integer polynomials with some prescribed properties. Zbl 1352.11031
Dubickas, Artūras; Sha, Min
2016
A degree problem for two algebraic numbers and their sum. Zbl 1297.11133
Drungilas, Paulius; Dubickas, Artūras; Smyth, Chris
2012
An estimation of the difference between two zeros of a polynomial. Zbl 0770.12003
Dubickas, Artūras
1992
Mahler measures generate the largest possible groups. Zbl 1093.11064
Dubickas, Artūras
2004
On subfields of a field generated by two conjugate algebraic numbers. Zbl 1154.11337
Drungilas, Paulius; Dubickas, Artūras
2004
Additive relations with conjugate algebraic numbers. Zbl 1158.11341
Dubickas, Artūras
2003
Multiplicative dependence of shifted algebraic numbers. Zbl 1041.11067
Drungilas, Paulius; Dubickas, Artūras
2003
The divisors of Newman polynomials. Zbl 1132.11311
Dubickas, Artūras
2003
Additive Hilbert’s theorem 90 in the ring of algebraic integers. Zbl 1112.11050
Dubickas, Artūras
2006
Nonreciprocal algebraic numbers of small measure. Zbl 1127.11070
Dubickas, Artūras
2004
Even and odd integral parts of powers of a real number. Zbl 1138.11026
Dubickas, Arturas
2006
Arithmetical properties of linear recurrent sequences. Zbl 1111.11044
Dubickas, Artūras
2007
There are infinitely many limit points of the fractional parts of powers. Zbl 1092.11041
Dubickas, Artūras
2005
Conjugate algebraic numbers close to a symmetric set. Zbl 1092.11040
Dubickas, A.
2005
On intervals containing full sets of conjugates of algebraic integers. Zbl 0935.11037
Dubickas, Artūras
1999
Polynomials with multiple roots at 1. Zbl 1307.11033
Dubickas, Artūras
2014
On the number of polynomials of bounded measure. Zbl 0926.11080
Dubickas, A.; Konyagin, S. V.
1998
An approximation by lacunary sequence of vectors. Zbl 1221.11164
Dubickas, Artūras
2008
Salem numbers as Mahler measures of nonreciprocal units. Zbl 1356.11075
Dubickas, Artūras
2016
On the degree of compositum of two number fields. Zbl 1277.11097
Drungilas, Paulius; Dubickas, Artūras; Luca, Florian
2013
On the Hurwitz zeta functions with algebraic irrational parameter. Zbl 1428.11153
Balčiūnas, Aidas; Dubickas, Arturas; Laurinčikas, Antanas
2019
Counting integer reducible polynomials with bounded measure. Zbl 1456.11205
Dubickas, Artūras
2016
Length of the sum and product of algebraic numbers. Zbl 1085.11051
Dubickas, A.; Smyth, C. J.
2005
Explicit form of Cassels’ $$p$$-adic embedding theorem for number fields. Zbl 1326.11062
Dubickas, Arturas; Sha, Min; Shparlinski, Igor
2015
The Lehmer constants of an annulus. Zbl 1030.11057
Dubickas, Artūras; Smyth, Chris J.
2001
Distribution of some quadratic linear recurrence sequences modulo 1. Zbl 1324.11048
Dubickas, Arturas
2014
Multiplicative dependence of the translations of algebraic numbers. Zbl 1423.11166
Dubickas, Artūras; Sha, Min
2018
Simple linear relations between conjugate algebraic numbers of low degree. Zbl 1425.11169
Dubickas, Arturas; Jankauskas, Jonas
2015
Zeros of the Estermann zeta function. Zbl 1291.11122
Dubickas, A.; Garunkštis, R.; Steuding, J.; Steuding, R.
2013
Roots of polynomials of bounded height. Zbl 1186.12001
Drungilas, Paulius; Dubickas, Artūras
2009
On the average difference between two conjugates of an algebraic number. Zbl 0862.11058
Dubickas, Artūras
1995
Good points for Diophantine approximation. Zbl 1234.11095
Berend, Daniel; Dubickas, Artūras
2009
Sumsets of Pisot and Salem numbers. Zbl 1204.11167
Dubickas, Artūras
2008
A note on powers of Pisot numbers. Zbl 0999.11035
Dubickas, A.
2000
On the measure of a nonreciprocal algebraic number. Zbl 0962.11033
Dubickas, Artūras
2000
Multiplicative dependence of quadratic polynomials. Zbl 0938.11013
Dubickas, A.
1998
Heights of powers of Newman and Littlewood polynomials. Zbl 1172.11007
Dubickas, Artūras
2007
On a certain geometric mean of the values of a polynomial. Zbl 0990.11062
Dubickas, A.
2000
On the fractional parts of rational powers. Zbl 1228.11104
Dubickas, Artūras
2009
On the supremum of the representation function of a sumset. Zbl 1357.11014
Dubickas, Artūras
2014
A basis of finite and infinite sets with small representation function. Zbl 1288.11012
Dubickas, Artūras
2012
On the location of roots of non-reciprocal integer polynomials. Zbl 1258.11051
Dubickas, Artūras
2011
On the approximation of the Thue-Morse generating sequence. Zbl 1389.11104
Dubickas, Artūras
2014
On the approximation of $$\pi/\sqrt{3}$$ by rational fractions. Zbl 0635.10026
Dubickas, Artūras
1987
On the distribution of roots of polynomials in sectors. I. Zbl 0920.12001
Dubickas, A.
1998
On algebraic numbers close to 1. Zbl 0927.11050
Dubickas, Artūras
1998
An estimate for a linear form in algebraic numbers. Zbl 0786.11038
Dubickas, Artūras
1991
Polynomial root separation in terms of the Remak height. Zbl 1275.11053
Dubickas, Artūras
2013
Sums of primes and quadratic linear recurrence sequences. Zbl 1288.11095
Dubickas, Artūras
2013
On the distance between two algebraic numbers. Zbl 1470.11045
Dubickas, Artūras
2020
Reducibility of polynomials after a polynomial substitution. Zbl 1449.12001
Drungilas, Paulius; Dubickas, Arturas
2020
Extremal problems for polynomials with real roots. Zbl 1431.12001
Dubickas, Artūras; Pritsker, Igor
2020
On the Hurwitz zeta functions with algebraic irrational parameter. Zbl 1428.11153
Balčiūnas, Aidas; Dubickas, Arturas; Laurinčikas, Antanas
2019
Multiplicative dependence of the translations of algebraic numbers. Zbl 1423.11166
Dubickas, Artūras; Sha, Min
2018
The distance to square-free polynomials. Zbl 1441.11053
Dubickas, Artūras; Sha, Min
2018
No two non-real conjugates of a Pisot number have the same imaginary part. Zbl 1361.11062
Dubickas, Artūras; Hare, Kevin G.; Jankauskas, Jonas
2017
On distances in lattices from algebraic number fields. Zbl 1433.11083
Dubickas, Artūras; Sha, Min; Shparlinski, Igor E.
2017
On rational approximations to two irrational numbers. Zbl 1428.11129
Dubickas, Artūras
2017
Roots of unity as quotients of two conjugate algebraic numbers. Zbl 1432.11154
Dubickas, Artūras
2017
Distribution modulo 1 and the discrete universality of the Riemann zeta-function. Zbl 1409.11061
Dubickas, Artūras; Laurinčikas, Antanas
2016
Diophantine equations with truncated binomial polynomials. Zbl 1339.11044
Dubickas, Artūras; Kreso, Dijana
2016
Positive density of integer polynomials with some prescribed properties. Zbl 1352.11031
Dubickas, Artūras; Sha, Min
2016
Salem numbers as Mahler measures of nonreciprocal units. Zbl 1356.11075
Dubickas, Artūras
2016
Counting integer reducible polynomials with bounded measure. Zbl 1456.11205
Dubickas, Artūras
2016
On degrees of three algebraic numbers with zero sum or unit product. Zbl 1409.11084
Drungilas, Paulius; Dubickas, Artūras
2016
There are only finitely many distance-regular graphs of fixed valency greater than two. Zbl 1303.05044
Bang, S.; Dubickas, A.; Koolen, J. H.; Moulton, V.
2015
Counting and testing dominant polynomials. Zbl 1409.11021
Dubickas, Artūras; Sha, Min
2015
Counting degenerate polynomials of fixed degree and bounded height. Zbl 1347.11026
Dubickas, Artūras; Sha, Min
2015
Joint discrete universality of Dirichlet $$L$$-functions. Zbl 1316.11077
Dubickas, Artūras; Laurinčikas, Antanas
2015
Explicit form of Cassels’ $$p$$-adic embedding theorem for number fields. Zbl 1326.11062
Dubickas, Arturas; Sha, Min; Shparlinski, Igor
2015
Simple linear relations between conjugate algebraic numbers of low degree. Zbl 1425.11169
Dubickas, Arturas; Jankauskas, Jonas
2015
On the number of reducible polynomials of bounded naive height. Zbl 1305.11089
Dubickas, Artūras
2014
Nonreciprocal units in a number field with an application to Oeljeklaus-Toma manifolds. Zbl 1290.11148
Dubickas, Artūras
2014
Polynomials with multiple roots at 1. Zbl 1307.11033
Dubickas, Artūras
2014
Distribution of some quadratic linear recurrence sequences modulo 1. Zbl 1324.11048
Dubickas, Arturas
2014
On the supremum of the representation function of a sumset. Zbl 1357.11014
Dubickas, Artūras
2014
On the approximation of the Thue-Morse generating sequence. Zbl 1389.11104
Dubickas, Artūras
2014
Linear recurrence sequences without zeros. Zbl 1349.11017
Dubickas, Artūras; Novikas, Aivaras
2014
On the fractional parts of powers of Pisot numbers of length at most 4. Zbl 1385.11064
Dubickas, Artūras; Jankauskas, Jonas
2014
On multiplicative functions which are additive on sums of primes. Zbl 1344.11005
Dubickas, Artūras; Šarka, Paulius
2013
On the degree of compositum of two number fields. Zbl 1277.11097
Drungilas, Paulius; Dubickas, Artūras; Luca, Florian
2013
Zeros of the Estermann zeta function. Zbl 1291.11122
Dubickas, A.; Garunkštis, R.; Steuding, J.; Steuding, R.
2013
Polynomial root separation in terms of the Remak height. Zbl 1275.11053
Dubickas, Artūras
2013
Sums of primes and quadratic linear recurrence sequences. Zbl 1288.11095
Dubickas, Artūras
2013
Nonreciprocal algebraic numbers of small Mahler’s measure. Zbl 1284.11137
Dubickas, Artūras; Jankauskas, Jonas
2013
Roots of unity as quotients of two roots of a polynomial. Zbl 1321.11110
Dubickas, Artūras
2012
A degree problem for two algebraic numbers and their sum. Zbl 1297.11133
Drungilas, Paulius; Dubickas, Artūras; Smyth, Chris
2012
A basis of finite and infinite sets with small representation function. Zbl 1288.11012
Dubickas, Artūras
2012
On the linear independence of the set of Dirichlet exponents. Zbl 1282.11112
Dubickas, Artūras
2012
The lonely runner problem for many runners. Zbl 1253.11073
Dubickas, Artūras
2011
On the location of roots of non-reciprocal integer polynomials. Zbl 1258.11051
Dubickas, Artūras
2011
Polynomials expressible by sums of monic integer irreducible polynomials. Zbl 1224.11045
Dubickas, Arturas
2011
Roots of polynomials with dominant term. Zbl 1225.11132
Dubickas, Artūras
2011
On $$\beta$$-expansions of unity for rational and transcendental numbers $$\beta$$. Zbl 1274.11023
Dubickas, Artūras
2011
Refinement equations and spline functions. Zbl 1187.41005
Dubickas, Artūras; Xu, Zhiqiang
2010
A binary linear recurrence sequence of composite numbers. Zbl 1197.11019
Dubickas, Artūras; Novikas, Aivaras; Šiurys, Jonas
2010
On the distribution of powers of a complex number. Zbl 1227.11083
Dubickas, Artūras
2010
On the intersection of infinite geometric and arithmetic progressions. Zbl 1257.11011
Dubickas, Artūras; Jankauskas, Jonas
2010
Powers of rational numbers modulo 1 lying in short intervals. Zbl 1205.11085
Dubickas, Artūras
2010
Rational difference equations with positive equilibrium point. Zbl 1193.39003
Dubickas, Artūras
2010
On Newman polynomials which divide no Littlewood polynomial. Zbl 1208.11123
Dubickas, Arturas; Jankauskas, Jonas
2009
Powers of a rational number modulo 1 cannot lie in a small interval. Zbl 1245.11082
Dubickas, Artūras
2009
On the limit points of $$(a_n\xi )_{n=1}^\infty$$ mod 1 for slowly increasing integer sequences $$(a_n)_{n=1}^\infty$$. Zbl 1221.11161
Dubickas, Arturas
2009
Roots of polynomials of bounded height. Zbl 1186.12001
Drungilas, Paulius; Dubickas, Artūras
2009
Good points for Diophantine approximation. Zbl 1234.11095
Berend, Daniel; Dubickas, Artūras
2009
On the fractional parts of rational powers. Zbl 1228.11104
Dubickas, Artūras
2009
The maximal value of polynomials with restricted coefficients. Zbl 1172.30002
Dubickas, Artūras; Jankauskas, Jonas
2009
On integer sequences generated by linear maps. Zbl 1196.11034
Dubickas, Artūras
2009
Squares and cubes in Sturmian sequences. Zbl 1176.68150
Dubickas, Artūras
2009
Prime and composite integers close to powers of a number. Zbl 1210.11080
Dubickas, Artūras
2009
On the lines passing through two conjugates of a Salem number. Zbl 1166.11031
Dubickas, Artūras; Smyth, Chris
2008
On the powers of 3/2 and other rational numbers. Zbl 1144.11053
Dubickas, Artūras
2008
An approximation by lacunary sequence of vectors. Zbl 1221.11164
Dubickas, Artūras
2008
Sumsets of Pisot and Salem numbers. Zbl 1204.11167
Dubickas, Artūras
2008
An inequality for the multiplicity of the roots of a polynomial. Zbl 1266.11054
Dubickas, Artūras
2008
Partitions of positive integers into sets without infinite progressions. Zbl 1140.05008
Dubickas, Artūras
2008
An estimate for the probability of dependent events. Zbl 1153.60004
Dubickas, Artūras
2008
On a problem of Mahler and Szekeres on approximation by roots of integers. Zbl 1172.11023
Bugeaud, Yann; Dubickas, Artūras
2008
On roots of polynomials with positive coefficients. Zbl 1172.11036
Dubickas, Artūras
2007
On a sequence related to that of Thue-Morse and its applications. Zbl 1113.11008
Dubickas, Artūras
2007
On the discriminant of the power of an algebraic number. Zbl 1127.11069
Dubickas, Arturas
2007
On the powers of some transcendental numbers. Zbl 1146.11039
Dubickas, Artūras
2007
Arithmetical properties of linear recurrent sequences. Zbl 1111.11044
Dubickas, Artūras
2007
Heights of powers of Newman and Littlewood polynomials. Zbl 1172.11007
Dubickas, Artūras
2007
On the reduced height of a polynomial. Zbl 1135.12300
Dubickas, Arturas; Jankauskas, Jonas
2007
Arithmetical properties of powers of algebraic numbers. Zbl 1164.11025
Dubickas, Artūras
2006
On the distance from a rational power to the nearest integer. Zbl 1097.11035
Dubickas, Artūras
2006
On the limit points of the fractional parts of powers of Pisot numbers. Zbl 1164.11026
Dubickas, Artūras
2006
On the fractional parts of lacunary sequences. Zbl 1140.11038
Dubickas, Artũras
2006
Additive Hilbert’s theorem 90 in the ring of algebraic integers. Zbl 1112.11050
Dubickas, Artūras
2006
Even and odd integral parts of powers of a real number. Zbl 1138.11026
Dubickas, Arturas
2006
On the fractional parts of the natural powers of a fixed number. Zbl 1150.11025
Dubickas, Arturas
2006
Mahler measures in a cubic field. Zbl 1164.11068
Dubickas, Artūras
2006
Integer parts of powers of rational numbers. Zbl 1084.11009
Dubickas, Artūras; Novikas, Aivaras
2005
Fractional parts of powers and Sturmian words. Zbl 1140.11318
Bugeaud, Yann; Dubickas, Artūras
2005
Auxiliary polynomials for some problems regarding Mahler’s measure. Zbl 1074.11018
Dubickas, Artūras; Mossinghoff, Michael J.
2005
Two exercises concerning the degree of the product of algebraic numbers. Zbl 1220.11131
Dubickas, Artūras
2005
There are infinitely many limit points of the fractional parts of powers. Zbl 1092.11041
Dubickas, Artūras
2005
Conjugate algebraic numbers close to a symmetric set. Zbl 1092.11040
Dubickas, A.
2005
Length of the sum and product of algebraic numbers. Zbl 1085.11051
Dubickas, A.; Smyth, C. J.
2005
Prime and composite numbers as integer parts of powers. Zbl 1102.11004
Alkauskas, G.; Dubickas, A.
2004
The polynomial Pell equation. Zbl 1077.11020
Dubickas, Artūras; Steuding, Jörn
2004
On numbers which are Mahler measures. Zbl 1065.11084
Dubickas, Artūras
2004
The conjugate dimension of algebraic numbers. Zbl 1062.11064
Berry, Neil; Dubickas, Artūras; Elkies, Noam D.; Poonen, Bjorn; Smyth, Chris
2004
The values of Mahler measures. Zbl 1107.11044
Dixon, John D.; Dubickas, Artūras
2004
Mahler measures generate the largest possible groups. Zbl 1093.11064
Dubickas, Artūras
2004
On subfields of a field generated by two conjugate algebraic numbers. Zbl 1154.11337
Drungilas, Paulius; Dubickas, Artūras
2004
Nonreciprocal algebraic numbers of small measure. Zbl 1127.11070
Dubickas, Artūras
2004
Large integer polynomials in several variables. Zbl 1167.11303
Dubickas, A.
2004
...and 42 more Documents
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#### Cited by 271 Authors
87 Dubickas, Artūras 16 Laurinčikas, Antanas 11 Jankauskas, Jonas 11 Samuels, Charles L. 10 Zaïmi, Toufik Mostepha 8 Drungilas, Paulius 8 Koolen, Jack H. 8 Macaitienė, Renata 8 Sha, Min 7 Bugeaud, Yann 6 Park, Poo-Sung 6 Šiaučiūnas, Darius 5 Beltrán, Carlos 5 Fili, Paul A. 5 Luca, Florian 5 Mossinghoff, Michael J. 5 Shparlinski, Igor E. 5 Šiurys, Jonas 4 Hare, Kevin G. 4 Kaliada, Dzianis 4 Kapica, Rafał 4 Morawiec, Janusz 4 Novikas, Aivaras 4 Smyth, Christopher J. 4 Zhuravleva, Victoria V. 3 Akiyama, Shigeki 3 Bang, Sejeong 3 Bonciocat, Nicolae Ciprian 3 Brunotte, Horst 3 Cox, Ben Lewis 3 Erdélyi, Tamás 3 Etayo, Ujué 3 Pottmeyer, Lukas 3 Pritsker, Igor E. 3 Zaharescu, Alexandru 2 Aistleitner, Christoph 2 Bonciocat, Anca Iuliana 2 Chen, Yonggao 2 Chow, Sam 2 Garunkštis, Ramūnas 2 Hajdu, Lajos 2 Hata, Masayoshi 2 Heyman, Randell 2 Ishak, M. I. M. 2 Kaneko, Hajime 2 Kim, Byungchan 2 Kim, Ji Young 2 Kopra, Johan 2 Kreso, Dijana 2 Lee, Chong Gyu 2 Liao, Lingmin 2 Louboutin, Stéphane R. 2 McGown, Kevin J. 2 Micheli, Giacomo 2 Mignotte, Maurice 2 Miner, Zachary 2 Mišík, Ladislav jun. 2 Moshchevitin, Nikolay G. 2 Ostafe, Alina 2 Otiman, Alexandra 2 Park, Jongyook 2 Pethő, Attila 2 Pinner, Christopher G. 2 Qiao, Zhi 2 Rhin, Georges 2 Saff, Edward Barry 2 Schinzel, Andrzej 2 Strauch, Oto 2 Van Dam, Edwin Robert 2 Wiles, Benjamin 2 Wu, Qiang 2 Zannier, Umberto M. 2 Zhao, Kaiming 1 Adam, Marcin 1 Allouche, Jean-Paul Simon 1 Amoroso, Francesco Antonio 1 Andrada, Adrián 1 Angella, Daniele 1 Bašić, Bojan 1 Bazsó, András 1 Beck, Matthias 1 Bennett, Michael A. 1 Bérczes, Attila 1 Berenhaut, Kenneth S. 1 Bertók, Csanád 1 Bi, Ning 1 Blau, Harvey I. 1 Bräunling, Oliver 1 Browkin, Jerzy 1 Cafure, Antonio 1 Cámara, Marc 1 Cao, Mengyue 1 Carpenter, Ryan 1 Cesaratto, Eda 1 Chand, Arya Kumar Bedabrata 1 Chang, Sungkon 1 Chew, Jackel Vui Ling 1 Choi, Jongwoo 1 Choi, Kwok-Kwong Stephen 1 Coons, Michael ...and 171 more Authors
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#### Cited in 127 Serials
23 Journal of Number Theory 17 Lithuanian Mathematical Journal 13 International Journal of Number Theory 11 Journal de Théorie des Nombres de Bordeaux 9 Mathematics of Computation 8 Monatshefte für Mathematik 7 Bulletin of the Australian Mathematical Society 6 Mathematical Notes 6 Periodica Mathematica Hungarica 5 Acta Arithmetica 5 Acta Mathematica Hungarica 5 Indagationes Mathematicae. New Series 4 Israel Journal of Mathematics 4 Archiv der Mathematik 4 Functiones et Approximatio. Commentarii Mathematici 4 Mathematische Zeitschrift 4 Proceedings of the American Mathematical Society 4 Applicable Algebra in Engineering, Communication and Computing 4 St. Petersburg Mathematical Journal 4 The Ramanujan Journal 4 Integers 4 Chebyshevskiĭ Sbornik 3 Discrete Mathematics 3 Journal of Mathematical Analysis and Applications 3 Rocky Mountain Journal of Mathematics 3 Advances in Mathematics 3 Illinois Journal of Mathematics 3 Journal of Combinatorial Theory. Series B 3 Mathematika 3 Results in Mathematics 3 Transactions of the American Mathematical Society 3 European Journal of Combinatorics 3 Graphs and Combinatorics 3 Aequationes Mathematicae 3 Linear Algebra and its Applications 3 Acta Mathematica Sinica. English Series 3 Proceedings of the Steklov Institute of Mathematics 2 American Mathematical Monthly 2 Communications in Algebra 2 Annales de l’Institut Fourier 2 Annali di Matematica Pura ed Applicata. Serie Quarta 2 Applied Mathematics and Computation 2 Czechoslovak Mathematical Journal 2 Glasgow Mathematical Journal 2 Manuscripta Mathematica 2 Proceedings of the Edinburgh Mathematical Society. Series II 2 Proceedings of the Japan Academy. Series A 2 Siberian Mathematical Journal 2 Theoretical Computer Science 2 Ergodic Theory and Dynamical Systems 2 Bulletin of the Korean Mathematical Society 2 Revista Matemática Iberoamericana 2 Journal of the Ramanujan Mathematical Society 2 Proceedings of the Indian Academy of Sciences. Mathematical Sciences 2 Tatra Mountains Mathematical Publications 2 Journal of Mathematical Sciences (New York) 2 The Electronic Journal of Combinatorics 2 Journal of Integer Sequences 2 LMS Journal of Computation and Mathematics 2 RAIRO. Theoretical Informatics and Applications 2 Journal of the Australian Mathematical Society 2 Comptes Rendus. Mathématique. Académie des Sciences, Paris 2 Acta Mathematica Universitatis Ostraviensis 2 Ars Mathematica Contemporanea 2 Research in Number Theory 2 Journal of Applied Mathematics and Computational Mechanics 1 Archive for Rational Mechanics and Analysis 1 Journal d’Analyse Mathématique 1 Journal of Mathematical Physics 1 Mathematical Methods in the Applied Sciences 1 Mathematical Proceedings of the Cambridge Philosophical Society 1 Russian Mathematical Surveys 1 Zeitschrift für Angewandte Mathematik und Mechanik (ZAMM) 1 Chaos, Solitons and Fractals 1 Bulletin of the London Mathematical Society 1 Bulletin de la Société Mathématique de France 1 Canadian Mathematical Bulletin 1 Colloquium Mathematicum 1 Integral Equations and Operator Theory 1 Journal of Computational and Applied Mathematics 1 Journal of Functional Analysis 1 Mathematische Nachrichten 1 Michigan Mathematical Journal 1 Quaestiones Mathematicae 1 Rendiconti del Seminario Matematico della Università di Padova 1 Advances in Applied Mathematics 1 Statistics & Probability Letters 1 Journal of Complexity 1 Constructive Approximation 1 Journal of the American Mathematical Society 1 Publicacions Matemàtiques 1 Atti della Accademia Nazionale dei Lincei. Classe di Scienze Fisiche, Matematiche e Naturali. Serie IX. Rendiconti Lincei. Matematica e Applicazioni 1 Glasnik Matematički. Serija III 1 Expositiones Mathematicae 1 Potential Analysis 1 Combinatorics, Probability and Computing 1 The New York Journal of Mathematics 1 Advances in Computational Mathematics 1 Integral Transforms and Special Functions 1 Journal of Difference Equations and Applications ...and 27 more Serials
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#### Cited in 42 Fields
269 Number theory (11-XX) 37 Field theory and polynomials (12-XX) 24 Combinatorics (05-XX) 23 Functions of a complex variable (30-XX) 16 Computer science (68-XX) 12 Dynamical systems and ergodic theory (37-XX) 12 Harmonic analysis on Euclidean spaces (42-XX) 8 Group theory and generalizations (20-XX) 8 Real functions (26-XX) 8 Probability theory and stochastic processes (60-XX) 7 Difference and functional equations (39-XX) 7 Approximations and expansions (41-XX) 6 Potential theory (31-XX) 6 Numerical analysis (65-XX) 5 Algebraic geometry (14-XX) 4 Measure and integration (28-XX) 4 Differential geometry (53-XX) 3 Linear and multilinear algebra; matrix theory (15-XX) 3 Nonassociative rings and algebras (17-XX) 3 Convex and discrete geometry (52-XX) 2 Several complex variables and analytic spaces (32-XX) 2 Special functions (33-XX) 2 General topology (54-XX) 2 Global analysis, analysis on manifolds (58-XX) 2 Statistical mechanics, structure of matter (82-XX) 1 History and biography (01-XX) 1 Mathematical logic and foundations (03-XX) 1 Commutative algebra (13-XX) 1 Associative rings and algebras (16-XX) 1 Topological groups, Lie groups (22-XX) 1 Ordinary differential equations (34-XX) 1 Partial differential equations (35-XX) 1 Functional analysis (46-XX) 1 Operator theory (47-XX) 1 Calculus of variations and optimal control; optimization (49-XX) 1 Algebraic topology (55-XX) 1 Manifolds and cell complexes (57-XX) 1 Statistics (62-XX) 1 Mechanics of deformable solids (74-XX) 1 Optics, electromagnetic theory (78-XX) 1 Operations research, mathematical programming (90-XX) 1 Information and communication theory, circuits (94-XX)
#### Wikidata Timeline
The data are displayed as stored in Wikidata under a Creative Commons CC0 License. Updates and corrections should be made in Wikidata.
| 2021-12-08T21:30:09 |
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https://par.nsf.gov/biblio/10304429-erratum-azimuthal-anisotropy-ks0-production-midrapidity-from-au+au-collisions-snn-phys-rev-lett
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This content will become publicly available on August 1, 2022
Erratum: Azimuthal Anisotropy of $KS0$ and $Λ+Λ¯$ Production at Midrapidity from $Au+Au$ Collisions at $sNN=130 GeV$ [Phys. Rev. Lett. 89 , 132301 (2002)]
Authors:
; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; more »
Award ID(s):
Publication Date:
NSF-PAR ID:
10304429
Journal Name:
Physical Review Letters
Volume:
127
Issue:
8
ISSN:
0031-9007
| 2022-06-26T20:17:35 |
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https://www.federalreserve.gov/econres/notes/feds-notes/implementing-monetary-policy-in-an-ample-reserves-regime-maintaining-an-ample-quantity-of-reserves-note-2-of-3-20200828.htm
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August 28, 2020
### Implementing Monetary Policy in an “Ample-Reserves” Regime: Maintaining an Ample Quantity of Reserves (Note 2 of 3)
Note 1 in this three-part series described how the Federal Reserve (or Fed) implements monetary policy with an ample quantity of reserves in the banking system. There we discussed how the Fed primarily relies on two key administered interest rates to keep the federal funds rate in the FOMC's target range, and why this approach is both appropriate and effective. In this second note, we describe some important influences on the supply of and demand for reserves and how the Fed will need to account for these influences in maintaining an ample quantity of reserves over the long run. These considerations are most relevant in normal times, not in periods in which there are severe strains in financial markets or weakness in economic activity that necessitate aggressive policy actions by the Fed that substantially increase reserves. Note 3 in the series describes how the Fed operates in an ample-reserves regime in such stressed periods, such as the COVID-19 pandemic.
#### Reserve supply considerations
As illustrated in figure 1, to stay in an ample-reserves regime over time, the Fed needs to maintain a quantity of reserves that is at least as large as the (stylized) quantity "A." But where in the gray shaded region does the Fed seek to maintain reserve supply? The answer is, it depends. Sometimes the Fed temporarily supplies a substantial quantity of reserves—when the Fed judges that it needs to alleviate severe strains in financial markets or stimulate an excessively weak economy, or both—resulting in the supply curve temporarily being positioned very far to the right of "A." This situation happened, for example, as a result of the Fed's actions in response to the Global Financial Crisis of 2007-09 and the COVID-19 shock. But eventually the Fed's unusual policy actions unwind and the level of reserves declines. As reserves decline, the Fed needs to monitor reserve conditions carefully and assess whether it needs to take actions to keep the level of reserves in the gray shaded region. Monitoring is important because factors outside of the Fed's control—referred to as "autonomous factors"—routinely affect the level of reserves over time.
##### Figure 1. The Fed's Ample-Reserves Regime
Autonomous factors are liability items on the Fed's balance sheet other than reserves; we will also refer to them as "non-reserve liabilities." Because the activities that result in changes in each of the Fed's non-reserve liabilities clear through reserve accounts at the Fed, the level of reserves in the banking system is directly affected by movements in the autonomous factors. In general, reserves decline dollar-for-dollar with increases in the Fed's non-reserve liabilities, and vice versa. To keep reserve supply amply over time, the Fed must take account of movements in its non-reserve liabilities, both their long-run trend growth and their short-run fluctuations.
Two key autonomous factors are currency in circulation and the Treasury's cash account, or General Account, at the Fed (the TGA). As shown in figure 2, each of these non-reserve liabilities has grown over time. Such growth causes reserves to decline, all else equal. For example, currency in circulation (the purple broken line) has grown on average about 6 percent a year. When a bank requests currency for its customers, an armored truck comes to a regional Federal Reserve Bank, picks up the cash that was ordered, and delivers it to the ordering bank. The Fed decreases the ordering bank's reserve account to take payment for the cash.
##### Figure 2. Selected Fed Non-Reserve Liabilities
When currency or another non-reserve liability grows, the Fed has to decide if it needs to offset the corresponding decline in reserves. The Fed controls the aggregate quantity of reserves in the banking system through open market operations, or OMOs. When the Fed purchases (sells) some U.S government securities in the open market it increases (decreases) the amount of reserves in the banking system.1 To offset a decline in reserves resulting from growth in its non-reserve liabilities, the Fed would purchase securities in the open market to increase reserve supply. The Fed would conduct a permanent operation (buy securities and hold them to maturity) if it thought a drain in reserves was permanent; it would conduct a temporary OMO (a repurchase agreement or repo) if it thought a drain was temporary.2 Either of these actions would immediately expand the supply of reserves in the banking system, shifting the supply curve in figure 1 rightward within the gray region. Whether the Fed judges it needs to undertake one of these actions or not depends on the original location of the supply curve and the size of the decline in reserves relative to the quantity associated with the vertical line "A." For example, if the supply curve were sufficiently far to the right of "A" when the decline in reserves occurred, an immediate response from the Fed would not be necessary.3
To stay in an ample-reserves regime over the long run, the Fed will eventually need to offset trend growth in the autonomous factors. As noted above, currency has expanded an average of about 6 percent per year, and with more than $1.5 trillion of currency in circulation, such growth amounts to a large dollar increase each year. The TGA (the red solid line in figure 2) has also grown over the past decade, and the size of this account could continue to expand as the nominal value of payment flows managed by the Treasury increases over time. Overall, the long-term growth of these autonomous factors will slowly, and permanently, drain reserves, as illustrated in figure 3 with the leftward shift in the supply curve, from S0 to S1. At some point, when the FOMC judges that it does not want the supply curve to decline further relative to "A," the Fed will need to offset declines in reserves by conducting permanent OMOs, termed "reserve management purchases." For example, when that time has come and if the Fed estimates that its non-reserve liabilities will grow by$10 billion a month, it could purchase $10 billion of Treasury securities each month to inject reserves back into the banking system to keep the quantity of reserves ample. ##### Figure 3. Reserve Supply is Drained by an Expansion of Autonomous Factors In addition to their trend growth, non-reserve liabilities also exhibit variability in the short-run. For example, the TGA (red solid line in figure 2) exhibits some substantial fluctuations, typically around tax payment dates for businesses and households. Increases and decreases in the TGA cause reserves in the banking system to fluctuate in the opposite direction—down and up, respectively. Moreover, the degree of variation in the autonomous factors can change over time. In particular, the TGA exhibits much more variability now than prior to the Global Financial Crisis of 2007-09. Taken together, the size of the weekly swings in the autonomous factors over the past few years suggests that, at the extreme, they can cause the quantity of reserves in the banking system to move by about$200 billion from one week to the next.
Over the long run, the Fed needs to consider these short-run movements in the autonomous factors to ensure its supply of reserves remains ample. In particular, the variability of the autonomous factors influences the Fed's judgment about the practical location of the vertical line "A." This is the case because the Fed aims to keep reserve supply large enough to stay consistently in an ample reserves-regime, even when autonomous factors may temporarily cause very large drains in reserves. In addition, given that the behavior of the autonomous factors could evolve over time, the Fed's view of the location of "A" could change going forward.
#### Reserve demand considerations
The Fed's judgment about the location of "A" could also change for reasons associated with banks' demand for reserves. For example, suppose banks' preference for holding reserves increased, such as due to heightened perceptions of liquidity risk. Figure 4 illustrates this case, showing a rightward shift in banks' demand curve, from D0 to D1. In this scenario, the vertical line "A" would move to the right along with the outward shift of the demand curve. Would the Fed need to adjust its reserve supply curve in this case? Again, the answer is that it depends. If supply was sufficiently to the right of "A" when the demand shift occurred, the Fed's current quantity of reserves would still be ample and its implementation regime would still work fine. If instead reserve supply was very close to "A" when the demand shift occurred, the Fed would need to add some reserves to the banking system, by conducting OMOs in the form of permanent purchases of securities, to remain in an ample-reserves regime relative to the new position of "A."
##### Figure 4. Increase in Demand for Reserves in an Ample-Reserves Regime
Conversely, a development that significantly reduced banks' demand for reserves could arise going forward. For example, a technological change could enable banks to speed the processing of payments and economize on holding cash for operational purposes, or the Fed could introduce a change to its existing policies or tools that leads banks to have a greater preference for investing in non-reserve liquid assets. In such cases, banks' demand for reserves could materially decline, and if so, the demand curve would shift to the left (or inward). Contrary to the case of a rightward shift explained above, in this case the Fed's existing supply of reserves would remain ample.
#### Final thoughts
To keep operating in an ample-reserves regime over the long run, the Fed will, at some point, likely need to add reserves to the banking system to accommodate ongoing trend growth in its non-reserve liabilities. These open market operations, ceteris paribus, will permanently expand the size of the Fed's balance sheet. The Fed will also need to monitor developments that could necessitate a shift in its assessment of the minimal quantity of reserves needed to stay in an ample-reserves regime. In particular, the Fed will need to watch the behavior of the autonomous factors that affect reserve supply, banks' reserve demand, and other dynamics that might influence the Fed's maintenance of an ample reserve supply as the economy and financial markets continue to evolve. More information about the Fed's ample-reserves implementation regime may be found in Ihrig, Senyuz, and Weinbach (2020), the paper on which Note 1 and Note 2 in this series are based. In Note 3 (forthcoming) in this series, we describe how the Fed operates in an ample-reserves regime when responding to a crisis, such as the COVID-19 pandemic.
#### References
Ihrig, Jane, Zeynep Senyuz, and Gretchen C. Weinbach (2020). "The Fed's "Ample-Reserves" Approach to Implementing Monetary Policy," Finance and Economics Discussion Series 2020-022. Washington: Board of Governors of the Federal Reserve System, https://doi.org/10.17016/FEDS.2020.022.
Ihrig, Jane E., Lawrence Mize, Gretchen C. Weinbach (2017). "How does the Fed adjust its Securities Holdings and Who is Affected?," Finance and Economics Discussion Series 2017-099. Washington: Board of Governors of the Federal Reserve System, https://doi.org/10.17016/FEDS.2017.099.
| 2022-08-20T00:46:50 |
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|
https://pdglive.lbl.gov/Particle.action?init=0&node=S060&home=BXXX045
|
BOTTOM BARYONS($\mathit B$ = $-1$) ${{\mathit \Lambda}_{{b}}^{0}}$ = ${{\mathit u}}{{\mathit d}}{{\mathit b}}$ , ${{\mathit \Xi}_{{b}}^{0}}$ = ${{\mathit u}}{{\mathit s}}{{\mathit b}}$ , ${{\mathit \Xi}_{{b}}^{-}}$ = ${{\mathit d}}{{\mathit s}}{{\mathit b}}$ , ${{\mathit \Omega}_{{b}}^{-}}$ = ${{\mathit s}}{{\mathit s}}{{\mathit b}}$
#### ${{\mathit \Xi}_{{b}}^{0}}$ , ${{\mathit \Xi}_{{b}}^{-}}$
$I(J^P)$ = $1/2(1/2^{+})$ I, J, P need confirmation.
In the quark model, ${{\mathit \Xi}_{{b}}^{0}}$ and ${{\mathit \Xi}_{{b}}^{-}}$ are an isodoublet ($\mathit usb$, $\mathit dsb$) state; the lowest ${{\mathit \Xi}_{{b}}^{0}}$ and ${{\mathit \Xi}_{{b}}^{-}}$ ought to have $\mathit J{}^{P} = 1/2{}^{+}$. None of $\mathit I$, $\mathit J$, or ${}^{P}$ have actually been measured.
FOOTNOTES
| 2023-03-22T00:56:50 |
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https://indico.fnal.gov/event/44492/contributions/214269/
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The Indico system will be unavailable due to system upgrades on August 30th from 6 - 9PM CST. Please email Indico support with any questions or concerns.
# The 28th International Workshop on Weak Interactions and Neutrinos (WIN2021)
Jun 7 – 12, 2021
US/Central timezone
## The Singly-Charged Scalar Singlet as the Origin of Neutrino Masses
Not scheduled
20m
Asynchronous Talk Neutrino Physics
### Speaker
Tobias Felkl (University of New South Wales)
### Description
We consider the generation of neutrino masses via a singly-charged scalar singlet. Under general assumptions we identify two distinct structures for the neutrino mass matrix. This yields a constraint for the antisymmetric Yukawa coupling of the singly-charged scalar singlet to two left-handed lepton doublets, irrespective of how the breaking of lepton-number conservation is achieved. The constraint disfavours large hierarchies among the Yukawa couplings. We study the implications for the phenomenology of lepton-flavour universality, measurements of the $W$-boson mass, flavour violation in the charged-lepton sector and decays of the singly-charged scalar singlet. We also discuss the parameter space that can address the Cabibbo Angle Anomaly.
### Primary authors
Tobias Felkl (University of New South Wales) Michael Schmidt (UNSW Sydney) Juan Herrero Garcia
### Presentation materials
poster-win2021-felkl.pdf talk-win2021-felkl.pdf The Singly-Charged Scalar Singlet as the Origin of Neutrino Masses | Tobias Felkl | WIN 2021
| 2022-08-13T21:11:11 |
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https://zims-en.kiwix.campusafrica.gos.orange.com/wikipedia_en_all_nopic/A/Hall_algebra
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Hall algebra
In mathematics, the Hall algebra is an associative algebra with a basis corresponding to isomorphism classes of finite abelian p-groups. It was first discussed by Steinitz (1901) but forgotten until it was rediscovered by Philip Hall (1959), both of whom published no more than brief summaries of their work. The Hall polynomials are the structure constants of the Hall algebra. The Hall algebra plays an important role in the theory of Masaki Kashiwara and George Lusztig regarding canonical bases in quantum groups. Ringel (1990) generalized Hall algebras to more general categories, such as the category of representations of a quiver.
Construction
A finite abelian p-group M is a direct sum of cyclic p-power components ${\displaystyle C_{p^{\lambda _{i}}},}$ where ${\displaystyle \lambda =(\lambda _{1},\lambda _{2},\ldots )}$ is a partition of ${\displaystyle n}$ called the type of M. Let ${\displaystyle g_{\mu ,\nu }^{\lambda }(p)}$ be the number of subgroups N of M such that N has type ${\displaystyle \nu }$ and the quotient M/N has type ${\displaystyle \mu }$. Hall proved that the functions g are polynomial functions of p with integer coefficients. Thus we may replace p with an indeterminate q, which results in the Hall polynomials
${\displaystyle g_{\mu ,\nu }^{\lambda }(q)\in \mathbb {Z} [q].\,}$
Hall next constructs an associative ring ${\displaystyle H}$ over ${\displaystyle \mathbb {Z} [q]}$, now called the Hall algebra. This ring has a basis consisting of the symbols ${\displaystyle u_{\lambda }}$ and the structure constants of the multiplication in this basis are given by the Hall polynomials:
${\displaystyle u_{\mu }u_{\nu }=\sum _{\lambda }g_{\mu ,\nu }^{\lambda }(q)u_{\lambda }.\,}$
It turns out that H is a commutative ring, freely generated by the elements ${\displaystyle u_{\mathbf {1} ^{n}}}$ corresponding to the elementary p-groups. The linear map from H to the algebra of symmetric functions defined on the generators by the formula
${\displaystyle u_{\mathbf {1} ^{n}}\mapsto q^{-n(n-1)/2}e_{n}\,}$
(where en is the nth elementary symmetric function) uniquely extends to a ring homomorphism and the images of the basis elements ${\displaystyle u_{\lambda }}$ may be interpreted via the Hall–Littlewood symmetric functions. Specializing q to 0, these symmetric functions become Schur functions, which are thus closely connected with the theory of Hall polynomials.
References
• Hall, Philip (1959), "The algebra of partitions", Proceedings of the 4th Canadian mathematical congress, Banff, pp. 147–159
• George Lusztig, Quivers, perverse sheaves, and quantized enveloping algebras, Journal of the American Mathematical Society 4 (1991), no. 2, 365421.
• Macdonald, Ian G. (1995), Symmetric functions and Hall polynomials, Oxford Mathematical Monographs (2nd ed.), The Clarendon Press Oxford University Press, ISBN 978-0-19-853489-1, MR 1354144
• Ringel, Claus Michael (1990), "Hall algebras and quantum groups", Inventiones Mathematicae, 101 (3): 583–591, Bibcode:1990InMat.101..583R, doi:10.1007/BF01231516, MR 1062796
• Schiffmann, Olivier (2012), "Lectures on Hall algebras", Geometric methods in representation theory. II, Sémin. Congr., 24-II, Paris: Soc. Math. France, pp. 1–141, arXiv:math/0611617, Bibcode:2006math.....11617S, MR 3202707
• Steinitz, Ernst (1901), "Zur Theorie der Abel'schen Gruppen", Jahresbericht der Deutschen Mathematiker-Vereinigung, 9: 80–85
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.
| 2021-05-16T16:14:48 |
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https://dlmf.nist.gov/35.2
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# §35.2 Laplace Transform
## Definition
For any complex symmetric matrix $\mathbf{Z}$,
35.2.1 $g(\mathbf{Z})=\int_{\boldsymbol{\Omega}}\mathrm{etr}\left(-\mathbf{Z}\mathbf{X% }\right)f(\mathbf{X})\mathrm{d}\mathbf{X},$
where the integration variable $\mathbf{X}$ ranges over the space ${\boldsymbol{\Omega}}$.
Suppose there exists a constant $\mathbf{X}_{0}\in{\boldsymbol{\Omega}}$ such that $|f(\mathbf{X})|<\mathrm{etr}\left(-\mathbf{X}_{0}\mathbf{X}\right)$ for all $\mathbf{X}\in{\boldsymbol{\Omega}}$. Then (35.2.1) converges absolutely on the region $\Re(\mathbf{Z})>\mathbf{X}_{0}$, and $g(\mathbf{Z})$ is a complex analytic function of all elements $z_{j,k}$ of $\mathbf{Z}$.
## Inversion Formula
Assume that $\int_{\boldsymbol{\mathcal{S}}}\left|g(\mathbf{Z})\right|\mathrm{d}\mathbf{V}$ converges, and also that $\lim_{\mathbf{U}\to\infty}\int_{\boldsymbol{\mathcal{S}}}\left|g(\mathbf{Z})% \right|\mathrm{d}\mathbf{V}=0$. Then
35.2.2 $f(\mathbf{X})=\dfrac{1}{(2\pi\mathrm{i})^{m(m+1)/2}}\int\mathrm{etr}\left(% \mathbf{Z}\mathbf{X}\right)g(\mathbf{Z})\mathrm{d}\mathbf{Z},$
where the integral is taken over all $\mathbf{Z}=\mathbf{U}+\mathrm{i}\mathbf{V}$ such that $\mathbf{U}>\mathbf{X}_{0}$ and $\mathbf{V}$ ranges over $\boldsymbol{\mathcal{S}}$.
## Convolution Theorem
If $g_{j}$ is the Laplace transform of $f_{j}$, $j=1,2$, then $g_{1}g_{2}$ is the Laplace transform of the convolution $f_{1}*f_{2}$, where
35.2.3 $f_{1}*f_{2}(\mathbf{T})=\int\limits_{\boldsymbol{{0}}<\mathbf{X}<\mathbf{T}}f_% {1}(\mathbf{T}-\mathbf{X})f_{2}(\mathbf{X})\mathrm{d}\mathbf{X}.$
| 2019-02-18T09:12:40 |
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|
https://pos.sissa.it/414/1130/
|
Volume 414 - 41st International Conference on High Energy physics (ICHEP2022) - Poster Session
Magnetic field simulations and measurements on mini-ICAL
H. Khindr
Full text: pdf
Pre-published on: December 29, 2022
Published on:
Abstract
The proposed ICAL detector is designed to detect muons generated from interaction of $\nu_{\mu}$ and anti-$\nu_{\mu}$ with Iron. It is designed with a maximum magnetic field of about 1.5 Tesla (with 90$\%$ of its volume having > 1 Tesla magnetic field). The magnetic field is intended for charge identification and momentum reconstruction of the muons. The mini-ICAL is a fully functional 85-ton prototype detector. One of the main challenges of the mini-ICAL detector is to produce the required B-field and to measure it as accurately as possible to study muons. For the purpose of measuring the B-field in the detector, Hall sensor PCBs are used. Hall sensors provide real time measurement of B-field. Calibration and systematic study of characteristics of the Hall sensors which are used for the measurement are carried out. Out of 11 layers of iron, 3 layers (1, 6 and 11) have provision for measurement of B-field using Hall sensor. In the mentioned layers, the gap between the adjacent plates is kept 3-4 mm for the purpose of inserting of the Hall sensor PCBs. In the rest of the layers, the gap between the plates is kept 2 mm. Measurements of magnetic field in the air gap between the plates and measurement of fringe field is done with a precision of 3$\%$ for the top layer. This will help in completing the study on the final magnetic field configuration of ICAL.
DOI: https://doi.org/10.22323/1.414.1130
How to cite
Metadata are provided both in "article" format (very similar to INSPIRE) as this helps creating very compact bibliographies which can be beneficial to authors and readers, and in "proceeding" format which is more detailed and complete.
Open Access
Copyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.
| 2023-02-04T00:22:54 |
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|
http://www.legisquebec.gouv.qc.ca/en/version/cs/C-38?code=se:123_130&historique=20210921
|
### C-38 - Companies Act
123.130. Subsidiaries all of whose shares are held by the same legal person may, if the shares issued by the subsidiary whose shares are not cancelled are without par value, amalgamate without conforming to Division II if their board of directors adopts a resolution providing that
(1) the shares of the subsidiaries, except those of one of them, will be cancelled, without reimbursement of the capital represented by these shares;
(2) the articles of amalgamation will be identical to the constituting act of the subsidiary whose shares are not cancelled, taking account, however, of this Part and the regulations of the Government;
(3) the issued and paid-up share capital account of the amalgamated subsidiaries will be added, to the extent that the subsidiaries determine, to the account of the subsidiary whose shares are not cancelled.
1980, c. 28, s. 14; 1987, c. 5, s. 10; 1999, c. 40, s. 70.
123.130. Subsidiaries all of whose shares are held by the same corporation may, if the shares issued by the subsidiary whose shares are not cancelled are without par value, amalgamate without conforming to Division II if their board of directors adopts a resolution providing that
(1) the shares of the subsidiaries, except those of one of them, will be cancelled, without reimbursement of the capital represented by these shares;
(2) the articles of amalgamation will be identical to the deed of incorporation of the subsidiary whose shares are not cancelled, taking account, however, of this Part and the regulations of the Government;
(3) the issued and paid-up share capital account of the amalgamated subsidiaries will be added, to the extent that the subsidiaries determine, to the account of the subsidiary whose shares are not cancelled.
1980, c. 28, s. 14; 1987, c. 5, s. 10.
123.130. Subsidiaries all of whose shares are held by the same corporation may, if their shares are without par value, amalgamate without conforming to Division II if their board of directors adopts a resolution providing that
(1) the shares of the subsidiaries, except those of one of them, will be cancelled, without reimbursement of the capital represented by these shares;
(2) the articles of amalgamation will be identical to the deed of incorporation of the subsidiary whose shares are not cancelled, taking account, however, of this Part and the regulations of the Government;
(3) the issued and paid-up share capital account of the amalgamated subsidiaries will be added, to the extent that the subsidiaries determine, to the account of the subsidiary whose shares are not cancelled.
1980, c. 28, s. 14.
| 2022-01-25T18:11:46 |
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|
http://www.gfdl.noaa.gov/blog/isaac-held/page/2/
|
# Isaac Held's Blog
## 34. Summer temperature trends over Asia
Anomalies in near surface air temperature over land (1979-2008) averaged over Asia and the months of June-July-August from CRUTEM4 (green) — and as simulated by atmosphere/land models in which oceanic boundary conditions are prescribed to follow observations (gray shading). See text and Post #32 for details.
This is a follow up to Post #32 on Northern Hemisphere land temperatures as simulated in models in which sea surface temperatures (SSTs) and sea ice extent are prescribed to follow observations. I am interested in whether we can use simulations of this “AMIP” type to learn something about how well a climate model is handling the response of land temperatures to different forcing agents such as aerosols and well-mixed greenhouse gases. If a model forced with prescribed SST/ice boundary conditions and prescribed variations in the forcing agents does a reasonably good job of simulating observations, we can then ask how much of this response is due to the SST variations and how much is due to the forcing agents (assuming linearity). If the response to SST variations is robust enough, we have a chance to subtract it off and see if different assumptions about aerosol forcing, in particular, improve or degrade the fit to observations.
## 33. Can we trust simulations of TC statistics in global models?
Globally integrated, annual mean tropical cyclone (TC) and hurricane frequency simulated in the global model described in Post #2, as a function of a parameter in the model’s sub-grid moist convection closure scheme, from Zhao etal 2012.
It is difficult to convey to non-specialists the degree to which climate models are based on firm physical theory on the one hand, or tuned (I actually prefer optimized) to fit observations on the other. Rather than try to provide a general overview, it is easier to provide examples. Here is one related to post #2 in which I described the simulation of hurricanes in an atmospheric model.
## 32. Modeling land warming given oceanic warming
Anomalies in annual mean near surface air temperature over land (1979-2008), averaged over the Northern Hemisphere, from CRUTEM4 (green) and as simulated by an ensemble of atmosphere/land models in which oceanic boundary conditions are prescribed to follow observations.
As discussed in previous posts, it is interesting to take the atmosphere and land surface components of a climate model and run it over sea surface temperatures (SSTs) and sea ice extents that, in turn, are prescribed to evolve according to observations. In Post #2 I discussed simulations of trend and variability in hurricane frequency in such a model, and Post #21 focused on the vertical structure of temperature trends in the tropical troposphere. A basic feature worth looking at in this kind of model is simply the land temperature – or, more precisely, the near-surface air temperature over land. How well do models simulate temperature variations and trends over land when SSTs and ice are specified? These simulations are referred to as AMIP simulations, and there are quite a few of these in the CMIP5 archive, covering the period 1979-2008.
## 31. Relative humidity in GCMs
Relative humidity evolution over one year in a 50km resolution atmospheric model
in the upper (250hPa) and lower (850hPa) troposphere.
In their 1-D radiative-convective paper of 1967, Manabe and Wetherald examined the consequences for climate sensitivity of the assumption that the tropospheric relative humidity (RH) remains fixed as the climate is warmed by increasing CO2. In the first (albeit rather idealized) GCM simulation of the response of climate to an increase in CO2, the same authors found, in 1975, that water vapor did increase throughout the model troposphere at roughly the rate needed to maintain fixed RH. The robustness of this result in the world’s climate models in the intervening decades has been impressive to those of us working with these models, given the differences in model resolution and the underlying algorithms, a robustness in sharp contrast to the diversity of cloud feedbacks in these same models.
## 30. Extremes
Percentage change in the precipitation falling on days within which the daily precipitation is above the pth percentile (p is horizontal axis) as a function of latitude and averaged over longtitude, over the 21st century in a GCM projection for a business-as-usual scenario, from Pall et al 2007.
(I have added a paragraph under element (1) below in response to some off-line comments — Aug 15)
When I think about global warming enhancing “extremes”, I tend to distinguish in my own mind between different aspects of the problem as follows (there is nothing new here, but these distinctions are not always made very explicit):
1) increases in the frequency of extreme high temperatures that result from an increase in the mean of the temperature distribution without change in the shape of the distribution or in temporal correlations
The assumption that the distribution about the mean and correlations in time do not change certainly seems like an appropriately conservative starting point. But if you look far out on the distribution, the effects on the frequency of occurrence of days above a fixed high temperature, or of consecutive occurrences of very hot days (heat waves), can be surprisingly large. Just assuming a normal distribution, or playing with the shape of the tails of the distribution, and asking simple questions of this sort can be illuminating. I’m often struck by the statement that “we don’t care about the mean; we care about extremes” when these two things are so closely related (in the case of temperature). Uncertainty in the temperature response translates directly into uncertainty in changes in extreme temperatures in this fixed distribution limit. It would be nice if, in model projections, it was more commonplace to divide up the responses in extreme temperatures into a part due just to the increase in mean and a part due to everything else. It would make it easier to see if there was much that was robust across models in the “everything else” part. And it also emphasizes the importance of comparing the shape of the tails of the distributions in models and observations. Of course from this fixed-distribution perspective every statement about the increase in hot extremes is balanced by one about decreases in cold extremes.
## 29. Eddy resolving ocean models
Animation of the sea surface temperature in a coupled climate model under development at GFDL,
the ocean component having an average resolution of roughly 0.1 degree latitude and longitude.
(Visualization created by Remik Ziemlinski; model developed by T. Delworth, A. Rosati, K. Dixon, W. Anderson using MOM4 as the oceanic code base.)
As models gradually move to finer spatial resolution we naturally expect to gradually improve our simulations of atmospheric and oceanic flows. But things get especially interesting when one passes thresholds at which new phenomena are simulated that were not present in anything like a realistic form at lower resolution. The animation illustrates what happens after one passes through an important oceanic threshold, allowing mesoscale eddies to form, filling the oceanic interior with what we refer to as geostrophic turbulence. At resolutions too coarse to simulate the formation of these eddies, flows in ocean models tend to be quite laminar except for some relatively large scale instabilities of intense currents of the kind seen in the snapshot north of the equator in the Eastern Pacific. (For a transition comparably fundamental in atmospheric models, one has to turn to the point at which global models begin to resolve the deep convective elements in the tropical atmosphere — see for example Post #19).
## 28. The “fruit fly” of climate models
Animations of the near surface temperature (top) and upper tropospheric zonal winds (bottom) in an idealized dry atmospheric model. The first 500 days of spinup from a state of rest are shown at one frame per day for the entire globe.
As a change of pace from discussions of climate sensitivity, I’ll describe an idealized atmospheric model that I think of as an important element in a model hierarchy essential to our thinking about atmospheric circulation and climate.
## 27. Estimating TCR from recent warming
GISTEMP annual mean surface temperatures (degrees C)
for the Northern and Southern Hemispheres.
Here’s an argument that suggests to me that the transient climate response (TCR) is unlikely to be larger than about 1.8C. This is roughly the median of the TCR’s from the CMIP3 model archive, implying that this ensemble of models is, on average, overestimating TCR
## 26. Relative humidity in “cloud resolving” models
Time and spatially averaged relative humidity profiles from radiative-convective equilibrium simulations with cloud-resolving models. The figure on the left is from Held et al, 1993 and shows results from two simulations differing by 5C in the prescribed surface temperature. That on the right is from Romps 2011 and shows the result of changing the CO2 and adjusting surface temperatures to keep the net flux at the top of the atmosphere unchanged. (Also shown on the right is the observed profile at a tropical western Pacific ARM site.)
Regarding water vapor or, equivalently, relative humidity feedback, we can think of theory/modeling as providing a “prior” which is then modified by observations (trends, interannual variability, Pinatubo response). My personal “prior” is that relative humidity feedback is weak. or, conversely, that the strength of water vapor feedback in our global models is about right.
In justifying this prior, I like to start with the rather trivial argument, already mentioned in the last post, that the amount of water vapor in the atmosphere cannot possibly stay unchanged as the climate cools since many regions will become supersaturated, including the upper tropical troposphere where most of the water vapor feedback is generated.. So to expect specific humidity to remain unchanged as the climate warms requires the present climate to be close to a distinguished point as a function of temperature – the point at which water vapor stops increasing as temperatures increase. Its not impossible that we do reside at such a point, but you’re going to have work pretty hard to convince me of that — it doesn’t strike me as a plausible starting point.
Of course, there is also the community’s collective experience with global atmospheric models over the past several decades. Less familiarly, there is experience more recently with the kind of “cloud-resolving” models (CRMs) discussed in Posts #19-20. I am going to focus on the latter here. This will have the advantage of introducing what I consider to be the physical mechanism that could most plausibly alter the strength of water vapor feedback.
## 25. Relative humidity feedback
Some feedbacks in AR4 models, from Held and Shell 2012. The three red columns on the right provide the traditional perspective: the “Planck feedback”– the response to uniform warming of surface and troposphere with fixed specific humidity ($\lambda_T$), the lapse rate feedback at fixed specific humidity ($\lambda_L$), and the water vapor feedback ($\lambda_Q$). The three blue columns on the left provide an alternative perspective — with the fixed relative humidity uniform warming feedback ($\tilde{\lambda}_T$), the fixed relative humidity lapse rate feedback, ($\tilde{\lambda}_L$), and the relative humidity feedback ($\tilde{\lambda}_H$). The sum of the three terms, shown in the middle black column, is the same from either perspective. Surface albedo and cloud feedbacks are omitted. Each model is a dot.
This is the continuation of the previous post, describing how we can try to simplify the analysis of climate feedbacks by taking advantage of the arbitrariness in the definition of our reference point, or equivalently, in the choice of variables that we use to describe the climate response. There is nothing fundamentally new here — it is just making explicit the way that many people in the field actually think, myself included. And if you don’t like this reformulation, that’s fine — it’s just an alternative language that you’re free to adopt or reject.
| 2014-03-09T20:28:47 |
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|
https://www.federalreserve.gov/econres/notes/feds-notes/gender-diversity-on-bank-board-of-directors-and-performance-20190212.htm
|
February 12, 2019
### Gender Diversity on Bank Board of Directors and Performance1
Ann L. Owen and Judit Temesvary
1. Introduction
Women are underrepresented in leadership positions in financial services, where they generally remain in lower-paying first or mid-level positions. While women made up 54.3 percent of the workforce at S&P 500 finance companies in 2014, only 18.7 percent of S&P 500 finance company boards and only 2.1 percent of CEOs were women (Catalyst, 2015). Many papers have studied the effects of boards' gender composition on firm performance and a few have studied it in the banking industry specifically (Adams and Mehran, 2012; Garcia-Meca et al, 2015; Berger et al, 2014; Pathan and Faff, 2013), showing mixed results. We study this issue using a newly compiled annual dataset on bank boards and financial performance, and we propose the resolution to these conflicting findings is that the impact of greater gender diversity depends on bank and board traits. Specifically, we find significant non-linearities in the relationship between bank performance and board gender diversity, suggesting that the impact of increasing gender diversity depends on its existing level. We also find that the effects of gender diversity depend on bank managerial quality. These results suggest that banks' continued voluntary expansion of board gender diversity is likely to bring performance benefits, provided that the banks are well-managed or capitalized.
Overall, we find that banks with more gender diversity on their board perform better once the composition of these boards reaches a critical level of gender diversity, corresponding to a board female share of around 13-17 percent. Given the size and composition of most boards, this result essentially means that adding more women to the board improves overall performance if there is already at least one woman on the board; adding the first woman to the board does not have this positive effect. This implies that currently about half of the banks in our sample enjoy the performance-enhancing effects of board gender diversity. This non-linear relationship between gender diversity and bank performance continues to hold, even after we account for banks' risk. Specifically, while greater gender diversity corresponds to lower risk-adjusted returns when female participation on bank boards is low, this relationship turns positive once the female share of board reaches around 20 percent. Higher risk-adjusted returns and bank performance in general may in part be due to better monitoring by the board. Consistently, we find some evidence suggesting that increasing gender diversity beyond a threshold is associated with fewer regulatory enforcement actions.
2. Empirical analysis
We compile a new dataset on nearly 90 U.S. bank holding companies' (from here on, banks) boards' gender composition, and these banks' financial performance and balance sheet characteristics from 1999 to 2015.2
Our main measure of gender diversity on boards is the Blau Index (Blau, 1977; Bear et al, 2010):
$$B = \Bigg[ 1-\sum_{g=1}^G P_g^2 \Bigg] \times 100$$
In this expression, P is the fraction of women and men on bank boards, and g indexes gender. By construction, this measure has a maximum value of 50 if both men and women have 50 percent shares. Lower values of the Blau Index indicate greater gender inequality. The average and median female share of board in our sample is around 12.5 percent, corresponding to one out of eight board members being female. The median size of a board is 13 members, meaning that the typical bank board has one or two women on it. However, the distribution has a long right tail: while the maximum female share is high at 42.8 percent, three-quarters of the boards in our sample have less than 16.8 percent female share. That said, gender diversity has risen over time, with the median Blau Index across all banks in a given year increasing from 16 to over 30, translating into an uptick in the median board female share from 9 to 20 percent (Figure 1).
#### Figure 1: Average and Median Female Share and Blau Index of Board, over time 1999-2015
We run first-differenced Instrumental Variables regressions to address the endogeneity of gender diversity that may arise if shocks to performance affect board composition (Fich, 2005; Mateos de Cabo et al, 2012):
$(1) \ \ \ Y_t^b = \alpha_0 + \alpha_1 X_{t-1}^b + \alpha_2 (X_{t-1}^b)^2 + C_{t-1}^b \times[\alpha_3 X_{t-1}^b + \alpha_4 (X_{t-1}^b)^2] + \alpha_5 S_{t-1}^b + \alpha_6 T_t + \alpha_7 B_b + \varepsilon_t^b$
In Equation 1, $Y_t^b$ denotes one of four measures of bank performance: three are based on banks' financial statements and the fourth is a market-based measure. Revenue to Expense Ratio is the ratio of banks' operating revenue to operating expenses and is our measure of the efficiency of a banks' operations.3 Return on Assets is net income divided by total assets and is included to measure banks' profitability. We also account for the implications that risk-taking behavior may have for bank performance by using the Sharpe Ratio on a bank's books as an indicator of risk. Stock Price Growth, which is a market-based measure of bank performance, is the annual growth rate of the bank's stock price. In addition, $X_{t-1}^b$ is the (one-year) lagged value of the Blau Index, which is our main gender diversity measure. We also add the square of this measure $(X_{t-1}^b)^2$, to capture non-linearities in the relationship between bank performance and gender diversity. We interact both the Blau Index and its square with the Risk-weighted Capital Ratio $C_{t-1}^b$, which we use to proxy a bank's quality of management (Mehran and Thakor, 2011). The banks in our sample are well-capitalized, with mean and median capital ratios between 13 and 14 percent. However, we see a substantial variation in capitalization across banks, which helps our identification.
The vector $S_{t-1}^b$ contains (lagged) bank balance sheet characteristics to control for non-board related developments that may affect performance. These are: the Loan to Deposit Ratio (to measure bank liquidity conditions); an Acquisition dummy (to capture the performance impact of bank M&A activity); Board Size (a control for the scale of the board, ranging from 6 to 32 members, with a mean of 13). The sets $B_b$ and $T_t$ are bank and year fixed effects (Adams and Ferreira, 2009; Adams and Mehran, 2012).4
We use two different types of instruments for the Blau Index $X_t^b$ in Equation 2: $I_t^b$ is the Share of Independent Directors as described in Boardex, bank and year fixed effects and the initial Blau Index (measured in 1999) times year fixed effects (Ahern and Dittmar, 2012). We also add bank traits $S_{t-1}^b$:
$(2) \ \ \ X_t^b = \beta_0 + \beta_1 I_t^b + \beta_2 (X_{1999}^b \times T_t) + \beta_3 Z_{t-1}^b + \beta_4 S_{t-1}^b + \beta_5 T_t + \beta_6 B_b + \upsilon_t^b$
We examine two hypotheses about the ways in which the impact of gender diversity is context-dependent. First, we test the hypothesis that the impact of increasing gender diversity depends on its existing level (Karpowitz and Mendelberg, 2014; Gneezy et al, 2003). Second, we examine if the impact of diversity is conditional on the quality of bank management, which we proxy with banks' capital ratios.
3. Estimation Results: Bank Performance and Board Gender Diversity
Table 1 summarizes our findings on the relationship between bank performance and the gender diversity of its board. Each column presents the results of the second stage of an IV estimation. The p-values for Sargan tests, reported at the bottom of Table 1, show that we cannot reject the validity of the instruments in any of our specifications. All regressions include the Blau Index for gender diversity and three interaction terms that allow for the impact of gender diversity to vary with bank traits: the Blau Index times the Risk-weighted Capital Ratio, the Blau Index squared, and the Blau Index squared times the Risk-weighted Capital Ratio. We also add balance sheet traits and bank and year fixed effects throughout.
#### Table 1: The Role of Gender Diversity in Determining US Banks' Performance 1999 - 2015
Model [1] [2] [3] [4]
Measure of Bank Performance Revenue to Expense Ratio Return on Assets Sharpe Ratio Annual Stock Price Growth
Gender Diversity
Blau Index {t-1} 3.790*
[2.101]
0.289**
[0.132]
0.779**
[0.378]
3.753*
[2.165]
Blau Index {t-1} * Risk-Weighted Capital Ratio {t-1} -0.327**
[0.145]
-0.0215**
[0.009]
-0.0710***
[0.0264]
-0.266*
[0.162]
Blau Index {t-1} * Blau Index {t-1} -0.0752*
[0.0450]
-0.00619*
[0.003]
-0.0142*
[0.00741]
-0.0836*
[0.0443]
Blau Index {t-1} * Blau Index {t-1} * Risk-Weighted Capital Ratio {t-1} 0.00639**
[0.00312]
0.000467**
[0.0002]
0.00124**
[0.000500]
0.00614*
[0.00333]
Bank Characteristics
Acquisition Dummy {t-1} -3.034**
[1.515]
-0.149*
[0.0850]
0.052
[0.278]
0.606
[1.776]
Loan to Deposit Ratio {t-1} -19.27**
[7.532]
-0.814*
[0.429]
-0.261
[1.930]
24.31*
[14.69]
Board Size {t-1} -0.205
[0.279]
0.0047
[0.0171]
0.0731
[0.0766]
-0.281
[0.387]
Risk-Weighted Capital Ratio {t-1} 3.109**
[1.498]
0.183**
[0.0910]
0.680**
[0.329]
3.316*
[1.749]
Constant -0.408
[0.523]
-0.0879**
[0.0389]
0.393***
[0.121]
-0.739
[1.035]
Bank Fixed Effects Yes Yes Yes Yes
Year Fixed Effects Yes Yes Yes Yes
Observations 730 632 328 687
P-Value of Sargan Test Statistic 0.26 0.82 0.71 0.84
R-squared 0.24 0.11 0.01 0.46
Marginal effect of a one standard deviation increase in the Blau index, for well-capitalized banks (at the 90th percentile) with low Blau index (at the 10th percentile):
-21.15 -0.90 -5.08 -9.210
Marginal effect of a one standard deviation increase in the Blau index, for well-capitalized banks (at the 90th percentile) with high Blau index (at the 90th percentile):
7.41 0.59 0.86 8.721
Note: This table shows the results of Instrumental Variables regressions. The dependent variable is various measures of bank performance, as indicated at the top of each column. The explanatory variables are as described in the text. The coefficients show the impact of a one-unit increase in the explanatory variable on percentage points changes in banks' performance measure. All regressions contain bank and year fixed effects. The instrumented variable is the Blau Index measure of gender diversity. The set of instuments consists of: the share of independent directors, bank and year fixed effects, and the 1999 (beginning of sample) value of the Blau Index interacted with the year dummies. Robust standard errors in square brackets. *** p<0.01, ** p<0.05, * p<0.1
We first show results for a broad measure of bank performance, the Revenue to Expense Ratio (Column 1). The Blau Index enters significantly and positively, but it does so in a non-linear way. Importantly, we find that the impact of board gender diversity on bank performance is more complicated than a simple "level" effect suggests. The marginal effect of additional gender diversity depends on its existing level and on the bank's capitalization, as can be seen from the squared Blau Index and the interactions with the Risk-weighted Capital Ratio. At the bottom of Table 1, we take all these effects into account and calculate the marginal effects of a one standard deviation increase in the Blau Index for well-capitalized banks with low and high existing gender diversity (at the 10th and 90th percentile of the Blau Index distribution, respectively). For well-capitalized banks with a very low level of board gender diversity, a small increase in gender diversity has a negative effect on performance. However, as board gender diversity increases, the evidence of a negative effect disappears. Bank efficiency (as measured by the Revenue to Expense Ratio) no longer decreases with gender diversity once the share of women on the board reaches around 17 percent at well-capitalized banks (paralleling a Blau Index of around 27). This represents around the top 25 percent of our sample banks. There is a significant relationship between the Revenue to Expense Ratio and board gender diversity only in well-capitalized banks, consistent with our hypothesis that better management can lower the costs of potential conflict and reap the benefits of different perspectives in the boardroom.
We examine another broad measure of bank performance, Return on Assets (Column 2). In line with the Column 1 results, the Blau Index enters positively, and the interactions of the Blau Index are also all statistically significant. This time, however, when we calculate the marginal effect of an increase in the gender diversity of the board for well-capitalized banks, the effects are statistically significant for banks with both low and high existing board gender diversity (the effects for the worst-capitalized banks are insignificant.) When a well-capitalized bank has low board gender diversity, a one standard deviation rise in the Blau Index reduces Return on Assets by about one percentage point. However, when a well-capitalized bank has higher existing gender diversity on its board, a comparable rise in gender diversity raises its Return on Assets by around 0.6 percentage points. This result is consistent with the idea that board room dynamics are influenced by the number of women in the room. When there is a threshold share of women on the board and the bank is well-managed (as proxied for by the Risk-weighted Capital Ratio), more board gender diversity makes a positive contribution to bank performance. The impact of increased diversity is significant and positive on Return on Assets at well-capitalized banks once the female share of the board reaches around 13 percent (a Blau Index of around 22). This implies that around 50 percent of well-capitalized banks in our sample enjoy the performance-enhancing effects of gender diversity.
Although some risks that banks take will pay off in the form of higher income, higher returns at the cost of excessive risk-taking will hinder bank performance in the longer term. Therefore, in Column 3 we examine the relationship between gender diversity on banks' boards and risk-adjusted returns on bank assets, as captured by the Sharpe Ratio on a bank's overall portfolio. Previous studies provide mixed predictions for what this relationship looks like.6 We confirm that our earlier non-linearity results hold even after we control for risk-taking: the link between risk-adjusted returns (the Sharpe Ratio) and gender diversity is similar to those we documented in Columns 1 and 2. The Blau Index enters positively and significantly, and the interaction terms are also significant. At low levels of board gender diversity an increase in diversity is significantly and negatively associated with the overall Sharpe Ratio on a bank's books (bottom of Table 1). However, this negative relationship disappears at higher levels of gender diversity, once well-capitalized banks reach a Blau Index of around 30, corresponding to 15-20 percent of banks in our sample.
In addition to measures of performance that are derived from bank financial statements, we also study if market-based measures of performance improve when gender diversity increases. To this end, we use a fourth measure, Growth of Stock Prices (Column 4). These findings are consistent with those presented earlier, with the coefficients on the Blau Index, its square and interactions with the capital ratio entering with the predicted statistically significant signs. While estimates for well-capitalized banks (90th percentile) are not significant, we find significant and positive marginal effects of board gender diversity at the extremes (at the sample maximum capital ratio). Given the complex nature of the interactions, it makes sense that the market perception of performance is not precisely the same as in our earlier estimations.
We further explore the hypothesis that board gender diversity may exert its influence on bank performance through its effect on monitoring. In Table 2, we do so by examining how higher board gender diversity is related to regulatory enforcement actions against banks. Using the number of enforcement actions by the Federal Reserve as the dependent variable (Column 1), we find that higher gender diversity is in fact negatively related to the number of regulatory enforcement actions in the non-linear way that we find earlier. A one standard deviation increase in gender diversity at well-capitalized banks corresponds to a reduction in enforcement actions of 0.47 per year, and this effect is smaller at poorly capitalized banks at 0.27 percent per year. Diamond and Rajan (2001) argue that higher bank capital interferes with market discipline and adversely affects the board's incentive to monitor – and therefore impedes performance. Based on this interpretation, this larger gender diversity impact at well-capitalized banks suggests that higher gender diversity may impact bank performance by counteracting the monitoring-reducing impact of better capitalization.
#### Table 2: The Role of Gender Diversity in Determining Enforcement Actions against US Banks 1999 - 2015
Model [1] [2] [3] [4]
Measure of Bank Performance Number of Fed Enforcement Actions Probability of Fed Enforcement Actions Probability of "Financial Health" Enforcement Actions Probability of "Misconduct" Enforcement Actions
Gender Diversity
Blau Index {t-1} 0.126*
[0.0661]
0.240*
[0.129]
-0.35
[0.243]
0.00115
[0.0812]
Blau Index {t-1} * Risk-Weighted Capital Ratio {t-1} -0.00867*
[0.00487]
-0.0145
[0.00938]
0.0336*
[0.0192]
-0.000441
[0.00584]
Blau Index {t-1} * Blau Index {t-1} -0.00287**
[0.00140]
-0.00732**
[0.00323]
0.00485
[0.00568]
0.000227
[0.00200]
Blau Index {t-1} * Blau Index {t-1} * Risk-Weighted Capital Ratio {t-1} 0.000155
[0.000106]
0.000407*
[0.000242]
-0.000572
[0.000451]
-0.00000179
[0.000139]
Bank Characteristics
Acquisition Dummy {t-1} 0.0706
[0.0496]
-0.0645
[0.243]
0.366
[0.306]
0.0539
[0.178]
Loan to Deposit Ratio {t-1} 0.0571
[0.212]
-0.427
[1.136]
-4.803***
[1.789]
0.0665
[0.682]
Board Size {t-1} 0.00578
[0.0115]
-0.151***
[0.0471]
-0.0841
[0.0883]
-0.0386
[0.0318]
Risk-Weighted Capital Ratio {t-1} 0.100*
[0.0538]
-0.0289
[0.0714]
-0.418**
[0.200]
-0.0142
[0.0543]
Constant 0.0252
[0.0457]
1.581
[1.773]
14.28***
[3.689]
0.21
[1.520]
Bank Fixed Effects Yes Yes Yes Yes
Year Fixed Effects Yes Yes Yes Yes
Observations 737 339 263 586
P-Value of Sargan Test Statistic -- -- -- --
R-squared 0.02 0.33 0.44 0.23
Marginal effect of a one standard deviation increase in the Blau index, for well-capitalized banks (at the 90th percentile) with low Blau index (at the 10th percentile):
-0.270 0.010 0.360 -0.020
Marginal effect of a one standard deviation increase in the Blau index, for well-capitalized banks (at the 90th percentile) with high Blau index (at the 90th percentile):
-0.470 -0.100 -0.220 0.020
Note: This table shows the results of Instrumental Variables regressions. The dependent variable is various measures of enforcement actions against banks, as indicated at the top of each column. The explanatory variables are as described in the text. The coefficients show the impact of a one-unit increase in the explanatory variable on percentage points changes in banks' performance measure. All regressions contain bank and year fixed effects. The instrumented variable is the Blau Index measure of gender diversity. The set of instuments consists of: the share of independent directors, bank and year fixed effects, and the 1999 (beginning of sample) value of the Blau Index interacted with the year dummies. Robust standard errors in square brackets. *** p<0.01, ** p<0.05, * p<0.1
Of course, in our sample we have several banks that have no enforcement actions over the entire time period. To separate out the effect of gender diversity on the occurrence of an enforcement action vs. the number of enforcement actions, we fit a (discrete) probit model to the probability of any enforcement action against a bank.7 We find statistically significant evidence that gender diversity reduces the occurrence of any regulatory enforcement action (Column 2). There is a 10 percent reduction in the probability of having any enforcement action for well-capitalized banks when gender diversity rises by one standard deviation.
If we compile data from several bank regulators (Federal Reserve, FDIC, and OCC) we have a sufficient number of regulatory enforcement actions in our sample to be able to take a more nuanced look at the ways in which gender diversity may increase regulatory compliance. We categorize the enforcement actions into two broad groups: those related to misconduct by the bank or affiliated parties (Column 3) and those related to financial health (Column 4). Using probit models, we find that increased gender diversity is associated with significantly lower probabilities of financial health enforcement actions, once a threshold level of board gender diversity is achieved – consistent with our earlier findings on improved bank performance. We find no evidence that higher gender diversity would reduce enforcement actions related to misconduct by the bank or affiliated parties.
Throughout, we interpret our results based on the hypothesis that the main benefit of diversity is that it provides multiple perspectives that improve decision-making. Consistent with this hypothesis, when we re-estimate our models interacting each independent variable with a financial crisis period indicator, we find that the effects of gender diversity at well-capitalized banks are much larger during the crisis period.
4. Conclusion
Using a sample of large U.S. banks over the 1999-2015 period, we study the relationship between various measures of bank performance and gender diversity on bank boards. We find that the impact of board gender diversity on bank performance is highly non-linear. We identify "threshold" results, which indicate that the relationship between bank performance and board gender diversity changes directions once banks increase gender diversity on their boards from low to higher levels. Our non-linearity results help shed light on the very wide-ranging findings of previous papers on the role of board gender diversity in bank (and in general, firm) performance. Our findings suggest that banks' continued voluntary expansion of board gender diversity is likely to bring overall performance benefits for well-capitalized (well-managed) banks.
References
Adams, Renee B. and Daniel Ferreira (2009). "Women in the boardroom and their impact on governance and performance," Journal of Financial Economics 94, 291-309.
Adams, Renee B. and Hamid Mehran (2012). "Bank board structure and performance: Evidence for large bank holding companies," Journal of Financial Intermediation 21, 243-267.
Ahern, Kenneth and Amy K. Dittmar (2012). "The changing of the boards: The impact on firm valuation of mandated female board representation," The Quarterly Journal of Economics 127(1), 137-197.
Bear, Stephen, Noushi Rahman and Corrine Post (2010). "The impact of board diversity and gender composition on corporate social responsibility and firm reputation," Journal of Business Ethics 97, 207-21.
Berger, Allen N., Thomas Kick and Klaus Schaeck (2014). "Executive board composition and bank risk taking," Journal of Corporate Finance 28, 48-65.
Blau, Peter M. (1977). Inequality and heterogeneity. New York, NY: Free Press.
Catalyst (2015). Pyramid: Women in S&P 500 finance. New York: January 13.
Croson, Rachel and Uri Gneezy (2009). "Gender differences in preferences," Journal of Economic Literature 47(2), 448-74.
Diamond, Douglas and Raghuram Rajan (2000). "A theory of bank capital," The Journal of Finance 55(6), 2431-65.
Fich, Elizier M. (2005). "Are some outside directors better than others? Evidence from director appointments by Fortune 1000 firms," The Journal of Business 78(5), 1943-1972.
Garcia-Meca, Emma, Isabel-Maria Garcia-Sanchez and Jennifer Martinez-Ferrero (2015). "Board diversity and its effects on bank performance: An international analysis," Journal of Banking & Finance 53, 202-14.
Gneezy, Uri, Muriel Niederle and Aldo Rustichini (2003). "Performance in competitive environments: Gender differences," Quarterly Journal of Economics 118(3), 1049-74.
Karpowitz, C., & Mendelberg, T. (2014). The Silent Sex: Gender, Deliberation, and Institutions. Princeton University Press.
Mehran, Hamid and Anjan Thakor (2011). "Bank capital and value in the cross-section," Review of Financial Studies 24(4), 1019-1067.
Mateos de Cabo, Ruth, Ricardo Gimeno and Maria J. Nieto (2012). "Gender diversity on European banks' boards of directors," Journal of Business Ethics 109(2), 145-162.
Pathan, Shams (2009). "Strong boards, CEO power and bank risk-taking," Journal of Banking & Finance 33, 1340-1350.
Pathan, Shams and Robert Faff (2013). "Does board structure in banks really affect their performance?" Journal of Banking & Finance 37(5), 1573-89.
Wang, Taiwei and Carol Hsu (2013). "Board composition and operational risk events at financial institutions," Journal of Banking & Finance (37), 2042-2051.
1. Temesvary: Division of Monetary Affairs, Federal Reserve Board. Owen: Department of Economics Hamilton College. This note is based on Owen, Ann and Judit Temesvary (2018). "The Performance Effects of Gender Diversity on Bank Boards," Journal of Banking & Finance 90, 50-63. Return to text
2. Data sources: BoardEx; S&P Global Market Intelligence: Compustat; Center for Research in Security Prices, CRSP 1925 US Stock Database, Wharton Research Data Services; Bureau van Dijk: Orbis Bank Focus. Our sample covers 40 percent of U.S. bank assets. Return to text
3. This measure is therefore the inverse of the "efficiency ratio" – a common proxy of performance in banking. Return to text
4. In auxiliary regressions, we use the Female Share of Board as our dependent variable and the Share of Board Members with Post-BA Education to measure managerial quality, and reach similar conclusions. In more complete specifications (shown in the paper), we also control for board demographic traits and experience. Return to text
5. The Share of Independent Directors is an appropriate instrument because it may be associated with more women on the board if it signals banks' boards being selected from a larger pool of qualified professionals rather than a smaller, internally-generated pool. On average, three-quarters of bank boards are made up of independent directors. Return to text
6. Croson and Gneezy (2009) conclude that experimental evidence suggests that women are more risk-averse than men, although gender differences in preference for financial risk are smaller among managers than in the general population. In the context of banks, Berger et al (2014) and Wang and Hsu (2013) find a positive tie between risk-taking and gender diversity – perhaps suggesting that gender-diverse boards are stronger, and take more risks (Pathan, 2009). Return to text
7. We aggregate enforcement actions on individual commercial banks up to the level of the holding company. The sample is smaller since for banks that had no enforcement the bank fixed effect perfectly predicts no occurrence. Enforcement actions related to misconduct by the bank or affiliated parties could result from an employee that has committed an offense. Actions related to financial health may result from a bank failing to implement a plan to address safety concerns. Return to text
| 2019-05-25T19:18:30 |
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