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One of the most spectacular predictions of theories with low-scale quantum gravity is the possibility of microscopic black hole (BH) production in proton-proton collisions at the high energies offered by the Large Hadron Collider (LHC) [CIT]. Such models are motivated mainly by the puzzling large difference between the electroweak scale (${\sim}0.1$) and the Planck scale ($\Mpl\sim10^{16}$), known as the hierarchy problem. In this analysis, we focus on black hole production in a model with $n$ large, flat, extra spatial dimensions (ADD model) [CIT]. In this and in other models, the fundamental scale of new physics in $n$ extra dimensions is given in terms of a multidimensional Planck scale ${M_D}$, such that $M_D^{n+2} \propto M_\mathrm{Pl}^{2} R^{-n}$, where $R$ is the size of extra dimensions. Some of the conclusions also apply to black holes in the Randall--Sundrum model [CIT], with a single warped extra dimension. | 931 | 1202.6396 | 9,290,866 | 2,012 | 2 | 28 | false | true | 2 | UNITS, UNITS |
Much below the Planck energy scale, gravity can be considered as a classical theory, and the laws of physics can be described to a good approximation by an effective action and continuum fields. As the energies however approach the Planck scale, the quantum nature of space-time becomes apparent, and the simple prescription, dictating that physics can be described by the sum of the Einstein-Hilbert and the Standard Model (SM) action ceases to be valid. In the framework of NonCommutative Spectral Geometry (NCSG) [CIT], gravity and the SM fields were put together into matter and geometry on a noncommutative space made from the product of a four-dimensional standard commutative manifold by a noncommutative internal space. | 727 | 1203.2161 | 9,316,470 | 2,012 | 3 | 9 | true | true | 2 | UNITS, UNITS |
Instead we will focus in this review on the effective field theory approach. Since all relevant physics is well below the Planck scale, all arguments of the Kerr/CFT correspondence can be formulated using semi-classical gravity. We will limit our arguments to the action FORMULA where the dimension-dependent Lagrangian piece $L^d$ is given by FORMULA where $C_{IJK} = C_{(IJK)}$. The action is possibly supplemented with highly suppressed higher-derivative corrections. This theory allows to discuss in detail the embedding REF) does not contain charged scalars, non-abelian gauge fields nor fermions. | 602 | 1203.3561 | 9,331,933 | 2,012 | 3 | 15 | false | true | 1 | UNITS |
Over the last decade there has been a strong effort [CIT] aimed at seeking experimental evidence of Planck-scale ($M_p \sim 10^{19} GeV$) effects which could be motivated from the study of the quantum-gravity problem. One of the most studied opportunities concerns the possibility that the speed of massless particles (photons) might have a Planck-scale-induced dependence on wavelength/momentum, as suggested by several preliminary studies in some of the alternative directions of research on quantum gravity (see, *e.g.*, Refs. [CIT]). This is of particular interest in the context of observations of gamma-ray-bursts where some of the possible scenarios for the form of this momentum (and Planck-scale) dependence could have observably-large manifestations [CIT]. | 766 | 1203.4677 | 9,344,036 | 2,012 | 3 | 21 | false | true | 3 | UNITS, UNITS, UNITS |
The author acknowledges support by the LEXI program of the state of Hamburg, Germany. --- The H.E.S.S. Collaboration acknowledges support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S., as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and in Namibia in the construction and operation of the equipment. --- This research has made use of NASA's Astrophysics Data System. | 1,005 | 1203.5956 | 9,360,873 | 2,012 | 3 | 27 | true | false | 1 | MPS |
We now analyse how a coupled quintessence-dark matter system affects the dynamics of the Universe [CIT]. Possible Planck suppressed couplings between dark energy and dark matter are allowed in our set-up if dark matter is constituted by bulk KK modes or moduli fields. | 268 | 1203.6655 | 9,369,681 | 2,012 | 3 | 29 | true | true | 1 | UNITS |
The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. | 928 | 1204.3896 | 9,415,283 | 2,012 | 4 | 17 | true | false | 2 | MPS, MPS |
We also compare our measurements with the Planck Early Release Compact Source Catalog (ERCSC) of the Planck Collaboration [CIT]. The catalogue contains flux densities derived from several method. To be consistent with this work, we use the measurements determined from aperture photometry. Cross-matching the two catalogues, we find 155 galaxies in common at 350 $\mu$m and 76 galaxies in common at 550 $\mu$m. The Planck FWHM are $4.23'$ at 350 $\mu$m and $4.47'$ at 550 $\mu$m. The photometry on the Planck compact sources was carried out using the FWHM of the band as the radius of the aperture. After visually inspecting each HRS galaxy with a corresponding Planck source, we excluded 11 sources because the Planck measurements may have potentially included other bright sources that lie within 5of the galaxies. | 816 | 1204.4726 | 9,426,312 | 2,012 | 4 | 20 | true | false | 6 | MISSION, MISSION, MISSION, MISSION, MISSION, MISSION |
The effective potential for the Kähler moduli is given by FORMULA where $\chi (M)$ is Euler number of the manifold given by $\chi (M) = 2 (h^{1,1} - h^{2,1})$, which can be negative. Since we assume these complex moduli were already frozen at high scale, we consider $\hat{\xi}$ as just a parameter here though $\hat{\xi}$ has the dilaton dependence. It is worth noting that the ${\cal V}$ is a dimensionless volume measured in the $\alpha'$ unit. If we recover the dimensionality of the volume by redefining ${\cal V} = \mathrm{vol}/ \alpha'^3$, we see immediately that the $\hat{\xi}$ parameter is suppressed by $\alpha'^3$ relative to $\mathrm{vol}$, so it may be treated as an $\alpha'$ correction. Note also that the Planck scale is related to string length by $M_P^2 = {4\pi {\cal V} / (g_s^2 (2\pi)^2 \alpha')}$ where we consider ${\cal V}$ as given after moduli stabilization so that $M_P$ is the constant. If we fix $\alpha'$ as motivated by the string theory setups, the Planck scale is defined differently depending on the ${\cal V}$; that is, it depends on the vacuum expectation values of the moduli fields. However, since our focus is the cosmological constant observed in Planck unit, we shall consider the dimensionless ratio $V/M_P^4$, in which the Planck scale dependence is cancelled out. | 1,307 | 1204.5177 | 9,430,779 | 2,012 | 4 | 23 | true | true | 4 | UNITS, UNITS, UNITS, UNITS |
In Section 4 we showed results calculated using the SPT 150 GHz bandpass filter. Since the CIB intensity and clustered power amplitude are falling off very steeply with decreasing frequency in the mm-bands [e.g. [CIT] /etal:1998; [CIT] :2011], the contribution to the power spectrum from clustered CIB sources is $\sim$ 20 per cent lower in the ACT 148 GHz channel [CIT]. This means that the tSZ$\times$CIB power in the ACT 148 GHz $\times$ SPIRE cross-spectra will be around 10 per cent larger relative to the CIB$\times$CIB contribution compared to in SPT 150 GHz $\times$ SPIRE. The SPT 95 GHz channel is also potentially well-suited to constraining the tSZ$\times$CIB signal; the ratio of the tSZ$\times$CIB to the CIB power in SPT 95 GHz $\times$ SPIRE spectra will be some five times larger than for SPT 150 GHz $\times$ SPIRE, based on the frequency scaling of the tSZ and clustered CIB ([CIT] /etal:2012 2012; R12). Cross-correlations of mm and sub-mm Planck High- and Low-Frequency Instrument channels (e.g., 70$\times$ 857 GHz, 100$\times$ 857 GHz) may also be of use for constraining the tSZ$\times$CIB power for $\ell\lesssim2500$. Which channels give the best constraints in practice will also depend on the amount of noise in the maps and the size of the Poisson CIB power. | 1,287 | 1204.5927 | 9,438,975 | 2,012 | 4 | 26 | true | false | 1 | MISSION |
An essential digression is in order at this point. In Planck units $M$ has dimensions of length. For that matter, so does $\omega$ in (26). Consequently, $\omega$ in (26) does not coincide with $\omega$ in (24) since - as (21) explicitly shows - the latter has dimensions of mass. In spite of that, the $\omega$ which appears in (26) unduly multiplies the expression $M - \frac{\omega}{2}$ in the final result for the emission probability $\Gamma \sim e^{-8\pi \omega(M - \frac{\omega}{2})}$ and in all associated expressions which appear in [CIT] resulting in length-dimensionality of order two in the exponent. Taken at "face value\" such a result is incorrect as it identically contradicts the fact that the exponent which it features must have dimensions of action. A careful consideration of the mass dimensionality in the derivation cited in [CIT] reveals, indeed, that the $\omega$ which multiplies $M - \frac{\omega}{2}$ in that exponent is of mass-dimensionality of order one and coincides, for that matter, with the $\omega$ in (24) whereas the $\omega$ which appears in $M - \frac{\omega}{2}$ and in (26) is of length dimensionality of order one. In order to bring my result into line with that in [CIT] I shall, in what follows, adhere to the stated convention which the authors of [CIT] have made. | 1,310 | 1204.6501 | 9,444,988 | 2,012 | 4 | 29 | false | true | 1 | UNITS |
Since in (REF) SM particles are minimally coupled to gravity, this implies that, as in GR, interactions between SM particles and gravitons are expected to be Planck scale suppressed. Therefore one expects that Lorentz symmetry breaking loop corrections to SM propagators are Planck scale suppressed and Lorentz symmetry is safe. | 328 | 1205.1722 | 9,467,160 | 2,012 | 5 | 8 | false | true | 2 | UNITS, UNITS |
Inflation has emerged as the leading paradigm for early universe and structure formation [CIT] which is strongly supported by cosmological observations [CIT]. The simplest models of inflation predict almost scale invariant, almost Gaussian and almost adiabatic perturbations on the CMB. In this work we would like to examine the effects of a time-dependent Newton constant in inflationary predictions. We present the formalism for curvature perturbations in inflationary models with a time-dependent $G$. As a particular example, we consider the toy model in which the reduced Planck mass $\Omega \equiv 1/8\pi G$ undergoes a sharp change from $\Omega= \Omega_-$ to $\Omega= \Omega_+$ in which both $\Omega_\pm$ are constant. We put this change in $\Omega$ at an early stage of inflation so the effects of change in Planck mass is within the CMB observational window. As a result one expects to find local features to be imprinted on curvature perturbations from this sudden change in Planck mass. Indeed there has been a lot of interest in the literature to consider the effects of local features in inflation. These features may originate from a sudden change in slow-roll conditions, sudden change in the inflaton mass, particle creation during inflation, field annihilations during inflation, change in sound speed of perturbations or change in fluids equation of state [CIT]. The observational motivations behind these models are to address the glitches in curvature power spectrum on scales associated with $\ell \sim 20-40$. | 1,531 | 1206.0903 | 9,540,212 | 2,012 | 6 | 5 | true | true | 3 | UNITS, UNITS, UNITS |
In the large $N$ limit of the $\beta$-ensemble, we send $g\to0$ so that the fixed product $gN$ obeys the relation (REF), and the large $N$ topological expansion is an expansion at small $g$. There are two possibilities to define this expansion, considering either $\beta$ or $\hbar$ fixed. Due to the scale invariance mentioned above, it seems more natural in the context of AGT to fix $\beta$ so that $\hbar=O(g)$. However, it reveals more convenient here to keep the two variables ($g,\hbar$) independent and take the double expansion of the $\beta$-ensemble quantities. In this paper, we should focus on the zeroth order in $g$, but all orders in $\hbar$, which we refer as the "planar limit". This limit is equivalent to the Nekrasov-Shatashvili limit [CIT] where one of the deformation parameters is set to zero, while the second one is identified with the Planck constant $2\hbar$. The remaining $\hbar$ expansion of planar quantities is interpreted as a WKB expansion. The planar limit also coincides with the semi-classical limit of Liouville theory in which $c\to\infty$. | 1,080 | 1206.1696 | 9,550,020 | 2,012 | 6 | 8 | false | true | 1 | CONSTANT |
As the current experimental constraints on our scenario are still relatively weak, we forecast the sensitivity of the Planck satellite to the effect of these particles on the CMB. We find that Planck is highly sensitive to the effects of such particles. If the value of $N_{\rm{eff}}$ derived from Planck agrees with that of standard cosmology with three neutrinos, we showed in the upper panel of figure REF that it will rule out (for example) the existence of a light Majorana fermion with a mass of less than 7.4 MeV which couples to the neutrinos. The lower panel of figure REF indicates that it will be difficult to distinguish between our scenario and the standard case of dark radiation (in which $N_{\rm{eff}}$ is the same at BBN and photon decoupling) at much more than $1\sigma$ when only data from astrophysical measurements of $^4\rm{He}$ and Planck is considered. On the other hand, considering only particles in thermal equilibrium with neutrinos, we demonstrated in the lower panel of figure REF that as well as providing significantly improved constraints on $m_{\chi}$, in some regions of parameter space, Planck is even able to discriminate between a real scalar and a complex scalar or Majorana fermion. | 1,222 | 1207.0497 | 9,619,046 | 2,012 | 7 | 2 | true | true | 5 | MISSION, MISSION, MISSION, MISSION, MISSION |
In the larger Planck community, I found support and enjoyed working with people from IASF-Bologna, like Fabrizio Villa, Luca Terenzi, Francesco Cuttaia, Gianluca Morgante, Enrico Franceschi; from Trieste, like Andrea Zacchei, Samuele Galeotta, Marco Frailis, Anna Gregorio; from UCSB, Peter Meinhold and Rodrigo Leonardi; from ESA Luis Mendes; from IFP, Ocleto D'Arcangelo, from Alcatel, Cristian Franceschet, Paola Battaglia, Roberto Silvestri, Paolo Leutenegger, Maurizio Miccolis and Flavio Ferrari; from UBC Andrew Walker. | 526 | 1208.1950 | 9,715,605 | 2,012 | 8 | 9 | true | false | 1 | MISSION |
The possibility of the spontaneous violation of Lorentz and CPT symmetries in the framework of the string theory was proposed in [CIT]. Thus, the Standard Model was extended and the Lorentz invariance violation (LIV) can be described by the effective field theory [CIT]. From experiment, bounds on LIV coefficients within the effective field theory were obtained [CIT]. Different models of LIV in the photon sector [CIT] and fermion sector [CIT] were investigated (there are many other publications). At present energies stringy effects are suppressed by the Planck scale $M_P=1.22\times 10^{19}$ GeV and there are not signs yet of LIV in experiments. It should be mentioned that any LIV models modify dispersion relations. It was mentioned in [CIT] that quantum gravity corrections can lead to deformed dispersion relation: FORMULA where the speed of light in vacuum $c=1$, $p_0$ is an energy and $\textbf{p}$ is a momentum of a particle and $L$ can be considered as "minimal length\" which is of the order of the Plank length $L_P=M_P^{-1}$. The subluminal propagation of particles corresponds to $L>0$ at $\alpha=1$. The last term in Eq.(1) violates the Lorentz invariance. The modified dispersion relation (1) with the parameter $\alpha=1$ was introduced in the framework of space-time foam Liouville-string models [CIT]. The wave equation for spinless particles with the dispersion equation (1) for $\alpha=1$ was considered in [CIT]. From the analysis of the Crab Nebula synchrotron radiation some constrains on the parameters $L$ and $\alpha$ were made [CIT]. In this paper, I postulate the modified Dirac equation for particles with spin-1/2 leading to the deformed dispersion relation (1) with $\alpha=2$. This modified Dirac equation can be considered within effective field theory with LIV in flat space-time. | 1,820 | 1210.0509 | 9,807,955 | 2,012 | 9 | 17 | false | true | 1 | UNITS |
We have studied the domain wall formation as a result of spontaneous breaking of a discrete symmetry called D parity in generic left right symmetric models. Since stable domain walls are in conflict with cosmology, we consider the effects of Planck scale suppressed operators in destabilizing them. We consider the evolution and decay of domain walls in two different epochs: radiation dominated as well as matter dominated. We find that in minimal versions of these models, the successful removal of domain walls put such constraints on the D-parity breaking scale $M_R$, which are not possible to realize in any physical theory, for example $M_R > M_{Planck}$. We also study gauge coupling unification in minimal versions of these models and find that with the minimal field content $M_R$ has to be as high as $10^9-10^{11} \; \text{GeV}$ (far beyond the reach of present experiments) for successful gauge coupling unification to be achieved. | 944 | 1209.4252 | 9,813,097 | 2,012 | 9 | 19 | false | true | 2 | UNITS, UNITS |
The notion of *discrete* space-time is usually associated with the assumption that all physical length-scales are bound from below by a presumed minimal length ('Planck limit'). Instead of this, we assert that the assumed discreteness primarily involves a lower limit of the *changes* of length-scales, $\Delta L$, and of time-scales, $\Delta T$, in the course of an interaction; the usual Planck limit is then an implicit corollary. Though this assertion appears to be self-evident, it has not, to the knowledge of the author, been explicitely considered in the literature so far. However, as is shown below, this seemingly minor modification establishes a conceptional shift that turns out to play a key role in order to tackle the well-known UV divergency problem. Hence, the *scale differences* $\Delta L$ and $\Delta T$ must fulfill the conditions FORMULA where $l_{\mathrm{Pl}}$ denotes the Planck length. The latter is related to the gravitational constant $G$ by FORMULA The factor $\eta$ serves as a structure parameter which allows one to account for the possibility that the effective minimal length scale may be a multiple (e.g. $\eta = \sqrt{8\pi}$) of the Planck length. | 1,184 | 1209.5386 | 9,822,332 | 2,012 | 9 | 22 | true | false | 4 | UNITS, UNITS, UNITS, UNITS |
The Planck Early Cold Cores Catalog (ECC) provides an unbiased list of Galactic cold clumps, which form an ideal sample for studying the early phases of star formation (\cite[Planck Collabrators et al. 2011]{Planck_etal11}). To study their properties, we have carried out a molecular line ($^{12}$CO/$^{13}$CO/C$^{18}$O) survey towards 674 Planck cold clumps in the ECC with the PMO 13.7 m telescope. | 400 | 1210.3766 | 9,876,879 | 2,012 | 10 | 14 | true | false | 3 | MISSION, MISSION, MISSION |
With the next generation of large-volume proton-decay searches and neutrino experiments currently in the R&D phase (in particular, LBNE [CIT], LENA [CIT] and Hyper-K [CIT]) there are good prospects to push the current lower bounds on the proton lifetime to the unprecedented level of $10^{35}$ years. On the theory side, the new information may be, at least in principle, used for further testing of the grand unification paradigm; however, this would require a very good grip on the proton lifetime predictions supplied by specific GUTs. Unfortunately, the quality of the existing estimates is rather limited even in very simple scenarios, see FIGURE REF, and it is namely due to the low accuracy of the leading-order methods used in most of the relevant calculations. On the other hand, consistent next-to-leading-order (NLO) proton lifetime estimates are parametrically more difficult: First, at the NLO level, the GUT scale $M_{G}$ must be determined at two-loops; this, however, requires a detailed understanding of the one-loop theory spectrum. Second, the flavour structure of the relevant baryon-number-violating (BNV) currents must be constrained by the existing data to a maximum attainable degree. Third, one has to account for several classes of almost irreducible uncertainties related to the Planck-scale physics (such as, e.g., gravity smearing of the gauge unification pattern [CIT]) which are often comparable to the NLO effects. | 1,446 | 1210.3789 | 9,877,585 | 2,012 | 10 | 14 | false | true | 1 | UNITS |
Recent observations of the cosmic microwave background anisotropy show a very good agreement of the observational data with the predictions of conventional, single-field slow-roll models of inflation, that is, adiabatic Gaussian random primordial fluctuations with an almost scale-invariant spectrum [CIT]. Nevertheless, possible non-Gaussianities from inflation has been a focus of much attention in recent years, mainly driven by recent advances in cosmological observations. In particular, the PLANCK satellite [CIT] is expected to bring us preciser data and it is hoped that a small but finite primordial non-Gaussianity may actually be detected. | 650 | 1210.6525 | 9,907,960 | 2,012 | 10 | 24 | true | true | 1 | MISSION |
The local metric for each throat far from the tip can be written as a warped product with the generic form: FORMULA where $\mu,\nu=0,1,2,3$ run through the $4$-dimensional metric. The radial coordinate $r$ reaches a minimum value of $r_{\text{min}}$ at the tip of the throat, and the local string scale at the tip of the $i$-th throat is given by FORMULA where $h_i$ is the maximum warping factor of the $i$-th throat ($h_i=1$ corresponds to no warping), and $M_s= \ell_s^{-1}$ is the 10-dimensional string mass scale which is usually taken to be smaller than the reduced Planck mass $M_{\rm PL}= \ell_{\rm PL}^{-1}=2.4\times 10^{18}$ GeV. | 639 | 1211.0250 | 9,932,723 | 2,012 | 11 | 1 | true | true | 1 | UNITS |
Inflation generates perturbations $\delta\phi$ which are frozen on superhorizon wavelengths with an amplitude $\delta\phi \simeq \frac{H}{2 \pi}$. Coarse-graining of the subhorizon fluctuations leads to a diffusion source term $f(x,t)$ for the long wavelengths modes [CIT] such that FORMULA where $z = a H |x_1 - x_2|$. The coarse-graining of short wavelength modes results in a Langevin equation for the field [CIT] FORMULA where the second derivative terms have, as usual, been ignored. The probability distribution function for the field, $P_\phi$, satisfying Eq. REF is given by a Fokker-Planck equation which provides the diffusion equation that describes the brownian motion of the field | 693 | 1211.1347 | 9,946,911 | 2,012 | 11 | 6 | false | true | 1 | FOKKER |
The typical decay length of the staus is large compared to their traveling range in the detector material. Hence, staus always decay at rest, i.e., we know the center-of-mass frame. Accordingly, if the mass of the stau is known, the LSP mass can be determined from the recoil energy of the $\tau$ produced in the 2-body decay, $E_\tau$, FORMULA As pointed out in [CIT], we can probe the hypothesis of a gravitino LSP by computing the Planck mass from (REF) once $m_{\widetilde\tau_1}$, $m_{\text{LSP}}$ and lifetime $\tau_{\widetilde\tau_1}=\Gamma_{\widetilde\tau_1}^{-1}$ are known. An agreement with the Planck mass measured in macroscopic experiments would provide a strong evidence for supergravity and the existence of the gravitino. Since the gravitino mass is directly related to the scale of spontaneous SUSY breaking, FORMULA these measurements would provide us with insights in the SUSY breaking sector that are otherwise beyond the reach of any experiment in the near future. For the axino LSP case, from (REF) we may be able to estimate the Peccei-Quinn scale and confront it with limits from astrophysical axion studies and axion searches in the laboratory. | 1,170 | 1211.2195 | 9,956,847 | 2,012 | 11 | 9 | false | true | 2 | UNITS, UNITS |
H.Z. would like to thank for financial support the Göran Gustafsson Foundation, and for the hospitality the KTH Royal Institute of Technology, where part of this work was performed. This work was supported by the Swedish Research Council (Vetenskapsrådet), contract no. 621-2011-3985 (T.O.), the Max Planck Society through the Strategic Innovation Fund in the project MANITOP (H.Z.), and the Göran Gustafsson Foundation (S.Z.). | 427 | 1211.3153 | 9,967,773 | 2,012 | 11 | 13 | false | true | 1 | MPS |
Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. | 382 | 1211.3418 | 9,971,069 | 2,012 | 11 | 14 | true | false | 1 | MPS |
The overlap between the Planck and the SLUGS samples is poor (only 5 galaxies are in common) mainly because of the low-$z$ cut adopted by Dunne et al. (2000). The luminosity function derived by the latter authors is shown by the blue squares in Fig.,REF. It agrees with the Planck measurements for $L_{353\rm GHz},\lower 2truept\hbox{${> \atop\hbox{\raise 4truept\hbox{$\sim$}}}$},10^{23},$W/Hz but lies significantly below them at fainter luminosities. A likely explanation of the difference is the bias against cold dusty galaxies implicit in the SLUGS sample. In fact, the selection at 60,$\mu$m combined with the imposed minimum redshift tends to favor galaxies with relatively bright infrared luminosities which usually have warmer SEDs (e.g. Smith et al. 2011). This bias has been demonstrated by Vlahakis et al. (2005) and, more recently, by Planck Collaboration XVI (2011) who have performed a detailed analysis of the SED properties of a sample of low-redshift galaxies extracted from the ERCSC. We confirm those results by comparing the sub-mm/far-infrared colours of the SLUGS sample with those of the Planck sources used to derive the luminosity function at 850,$\mu$m. The results are shown in Fig.,REF together with the track of a grey-body with dust emissivity index $\beta=1.3$ and temperatures ranging from 20 to 50,K (in steps of 5,K). The SLUGS sample has higher dust temperatures than the 850$,\mu$m Planck-selected sample, and the difference is more pronounced for galaxies with lower 850,$\mu$m luminosities (yellow dots). | 1,544 | 1211.3832 | 9,975,506 | 2,012 | 11 | 16 | true | false | 5 | MISSION, MISSION, MISSION, MISSION, MISSION |
We report multiple epoch VLA/JVLA observations of 89 northern hemisphere sources, most with 37,GHz flux density $>$,1,Jy, observed at 4.8, 8.5, 33.5, and 43.3,GHz. The high frequency selection leads to a predominantly flat spectrum sample, with 85,% of our sources being in the Planck Early Release Compact Source Catalog (ERCSC). These observations allow us to: 1) validate Planck's 30 and 44,GHz flux density scale, 2) extend the radio SEDs of Planck sources to lower frequencies allowing for the full 5-857GHz regime to be studied, and 3) characterize the variability of these sources. At 30,GHz and 44,GHz, the JVLA and Planck flux densities agree to within $\sim$,3%. On timescales of less than two months the median variability of our sources is 2%. On timescales of about a year the median variability increases to 14%. Using the WMAP 7-year data, the 30,GHz median variability on a 1-6 years timescale is 16%. | 917 | 1211.3931 | 9,976,303 | 2,012 | 11 | 16 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
Recently, a number of new galaxy clusters have been detected by the ESA-Planck satellite, the South Pole Telescope and the Atacama Cosmology Telescope using the Sunyaev-Zeldovich effect. Several of the newly detected clusters are massive, merging systems with disturbed morphology in the X-ray surface brightness. Diffuse radio sources in clusters, called giant radio halos and relics, are direct probes of cosmic rays and magnetic fields in the intra-cluster medium. These radio sources are found to occur mainly in massive merging clusters. Thus, the new SZ-discovered clusters are good candidates to search for new radio halos and relics. We have initiated radio observations of the clusters detected by Planck with the Giant Metrewave Radio Telescope. These observations have already led to the detection of a radio halo in PLCKG171.9-40.7, the first giant halo discovered in one of the new Planck clusters. | 911 | 1211.4485 | 9,979,167 | 2,012 | 11 | 19 | true | false | 3 | MISSION, MISSION, MISSION |
On the other hand, the ICP pressure $p\approx n k_B T/\mu$ (with the mean molecular weight $\mu\approx 0.60$) may be also derived from combining the density $n$ and temperature $T$ provided by X-ray observations of the thermal bremsstrahlung radiation emitted by the plasma. The overall trend emerging from the Planck data is toward a *deficit* in the SZ relative to the X-ray pressure, see Ade et al. (2012). In detail, to fit the SZ data these authors based on empirical formulae suggested by numerical simulations (see Nagai et al. 2007) and by X-ray analyses (see Arnaud et al. 2010). These formulae provide a 'universal' pressure profile for the whole cluster population, or a specific version for unrelaxed clusters. However, when applied to fit the precise Planck SZ data these formulae perform inadequately, as discussed by Ade et al. (2012); specifically, the first version turns out to overshoot the data in the core, and both to appreciably undershoot them in the outskirts, well beyond the quoted uncertainties. Aimed modifications of the parameter values in the fitting formulae, that include suppression of unphysical central divergencies, can improve the SZ fits at the cost of inconsistencies with the X-ray pressure. As discussed by the above authors, this is also the case with multiparametric fitting formulae of the type proposed by Vikhlinin et al. (2006) for the X-ray observables. | 1,403 | 1212.3082 | 10,047,098 | 2,012 | 12 | 13 | true | false | 2 | MISSION, MISSION |
For Coma a decay scale is not needed, and a nearly uniform $\delta p/p$ applies to a good approximation. Thus the net outcome is to *lower* the normalization applying to the thermal pressure at the virial radius, to read $p_R\propto (1+\delta p/p)^{-1}$. Resolving the tension between the SZ vs. the X-ray data requires $\delta p/p\approx 15\%$ (up to $20\%$ for *XMM-Newton*, which may however include a $5\%$ bias due to clumpiness, see above). The outcome is illustrated in Fig. 2 by the solid line; we remark that while the SZ profile from the SM has not been derived from a formal fit, yet it turns out to represent well the Planck data over their whole radial range. In particular, the *thermal* pressure derived with the SM is now lower by $\approx 15\%$, as in fact sensed by the SZ effect. | 798 | 1212.3082 | 10,047,110 | 2,012 | 12 | 13 | true | false | 1 | MISSION |
1. Gamma ray spectroscopy with High Purity Germanium spectrometers in four underground laboratories: at the Max-Planck-Institut für Kernphysik (MPIK) in Germany, HADES (IRMM) in Belgium, the Baksan Neutrino Observatory (BNO INR RAS) in Russia and at LNGS in Italy. The ultimate detection limit for the best spectrometers in deep underground laboratories lies around 10 $\upmu$Bq/kg for $^{226}$Raand $^{228}$Th [CIT]. | 417 | 1212.4067 | 10,056,205 | 2,012 | 12 | 17 | false | true | 1 | MPS |
To illustrate the technique, we studied models with fermionic $b$ quark partners, i.e. colored fermions with electric charge $-1/3$ with sizable coupling to the $b$ quark. In our example, we considered the case of $b$ quark partners with mass at or below the TeV scale. The possibility of such is motivated by extensions to the SM that solve the Planck-weak hierarchy problem, since they contain top partners and, thus by $SU(2)_L$ symmetry, bottom partners. In the same model, it is also possible to have a WIMP DM. The $b$ quark partners, as the typical states of the new physics sector, are charged under this stabilization symmetry and will then decay into a bottom quark, plus DM. Furthermore, thanks to their color gauge interactions, the $b$ quark partners have a large production cross-section at hadronic colliders. Therefore the study of $b$ quark partners is very well-suited to illustrate our technique. | 915 | 1212.5230 | 10,072,093 | 2,012 | 12 | 20 | false | true | 1 | UNITS |
The Fokker-Planck equation can also be written as FORMULA where FORMULA Here $S$ can be interpreted as a probability current. We will discuss the one variable Fokker-Planck equation with time-independent drift and diffusion coefficients given by FORMULA | 254 | 1212.5535 | 10,074,935 | 2,012 | 12 | 21 | false | true | 2 | FOKKER, FOKKER |
We study the role of the Gauss-Bonnet corrections and two loop higher genus contribution to the gravity action on the Kaluza-Klien modes and their interactions for different bulk fields which enable one to study various phenomenological implications of string loop corrected Gauss-Bonnet modified warped geometry model in one canvas. We have explicitly derived a phenomenological bound on the Gauss-Bonnet parameter so that the required Planck to TeV scale hierarchy can be achieved through the warp factor in the light of recently discovered Higgs like boson at 125 GeV. Moreover due to the presence of small perturbative Gauss-Bonnet as well as string loop corrections we have shown that the warping solution can be obtained for both de-Sitter and anti-de-Sitter bulk which is quite distinct from Randall-Sundrum scenario. Finally we have evaluated various interactions among these bulk fields and determined the coupling parameters and the Kaluza- Klien mode masses which is crucial to understand the phenomenology of a string two loop corrected Einstein-Gauss-Bonnet warp geometry. | 1,085 | 1301.0918 | 10,095,309 | 2,013 | 1 | 5 | false | true | 1 | UNITS |
In the following results, we use a realistic point source mask constructed from the Planck Early Release Compact Source Catalog [CIT]. More precisely, we considered the compact sources from the 100, 143 and 217 GHz channels and masked disks with radius equal to three times the values of the beam of the corresponding channel. We therefore use a point sources mask which is composed of holes of various sizes, about 30, 21 and 15 arcmin. Some of the holes overlap, resulting in an enlarged distribution of holes sizes (Fig. REF). We anticipate on the following section, and we will only include in this mask the point sources which are outside a realistic Galactic mask which masks about 20% of the sky. | 703 | 1301.4145 | 10,126,192 | 2,013 | 1 | 17 | true | false | 1 | MISSION |
Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. | 382 | 1301.5484 | 10,138,550 | 2,013 | 1 | 23 | true | false | 1 | MPS |
The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington. | 545 | 1301.5870 | 10,142,691 | 2,013 | 1 | 24 | true | false | 2 | MPS, MPS |
On the way of understanding the early universe cosmology, the inflationary mechanism has been proven to be quite fascinating as it successfully addresses several outstanding issues of the standard big bang scenario, e.g. the horizon problem, the flatness problem and the monopole problem. Initially, the idea of inflation was introduced to explain the homogeneous and isotropic nature of the universe at large scale structure [CIT], however its best advantage is being utilized in studying the inhomogeneities and anisotropies of the universe, which is a consequence of the vacuum fluctuations of the inflaton (as well as the metric fluctuations). In this regard, the idea of inflation also provides a way to understand the physics which could be responsible for generating the correct amount of primordial density perturbations initiating the structure formation of the universe and the cosmic microwave background (CMB) anisotropies. The simplest (single-field) inflationary process can be understood via a (single) scalar field slowly rolling towards its in a nearly flat potential. The vacuum fluctuations of the inflaton result in an almost scale invariant spectrum with a small tilt reflecting unique predictions via the CMB radiation. Although the single-field inflationary models fit well with the current observation constraints [CIT], the present observational data is not sufficient to discriminate among the various models. In this regard, the detection of non-Gaussianity can be a crucial data to distinguish the various models in the ongoing/future experiments such as PLANCK [CIT]. | 1,596 | 1301.6076 | 10,144,930 | 2,013 | 1 | 25 | true | true | 1 | MISSION |
As this discrete symmetry is meant to constrain Planck suppressed as well as renormalizable couplings, it must be anomaly-free and gauged.[^9] The discrete symmetry could be an ordinary symmetry or an R-symmetry. In the case of a discrete R-symmetry the superspace coordinate obtains a non-trivial phase $\eta_{\theta}$ under the discrete transformation, implying that gauginos are rotated by $\eta_{\theta}$ as well whereas the superpotential must pick up a phase $\eta_W= \eta_{\theta}^2$. In Appendix REF we show that the anomaly cancellation conditions for the discrete symmetry together with the requirement that the operators in (REF) are forbidden requires a discrete R-symmetry. Focusing on the case with $E,\bar{E}$ leptons and the regular embedding, we further argue that the smallest order choice for a discrete symmetry group forbidding all problematic operators while allowing for a semirealistic flavor Higgs potential is a $\mathbb{Z}_{11}$ discrete R-symmetry, where we assume that the flavor Higgs sector is completely vector-like. | 1,048 | 1302.0004 | 10,160,287 | 2,013 | 1 | 31 | false | true | 1 | UNITS |
The potential energy for the large field models is given by FORMULA where $M$ is a constant of mass dimension (in Planck unit) and $p$ is a positive number. In order to be definite, we assume that this potential is correct not only for large $\phi$ responsible for inflation but also for small $\phi$ relevant for oscillating period and reheating. For this potential, the field value at which inflation terminates is given by FORMULA the solution of ${\epsilon_1}(\phi_\mathrm{end}) = 1$ where FORMULA The slow-roll evolution of $\phi$ during inflation is given by integrating Eq. (REF). In Planck units, one gets FORMULA where, as before $\Delta N=N-N_\mathrm{end}$, is the number of e-fold measured from the end of inflation. After inflation, $\phi$ oscillates around the minimum such that the natural equation of state parameter is given by $w_\mathrm{reh}=(p-2)/(p+2)$ [CIT]. | 879 | 1302.6013 | 10,214,479 | 2,013 | 2 | 25 | true | true | 2 | UNITS, UNITS |
In previous literature thermal statistical fluctuations have been considered in a variety of contexts: The earliest hint that these could be relevant for CMB was perhaps provided by Peebles [CIT], and further developed in [CIT] (see also [CIT]). Since then thermal fluctuations have found applications in several models: string cosmology [CIT], inflation inflation (in particular warm inflation [CIT] - for reviews see e.g. [CIT] - but see also [CIT]), bouncing cosmologies [CIT] Milne/holographic universe [CIT]. In the present paper we first generalize the calculation of the curvature perturbations to the case when the thermal matter could have an arbitrary equation of state [^3], in the process clarifying several conceptual issues related to gauge choices, and transfer of perturbations from sub- to super-Hubble phase. These generalizations can be particularly important and interesting for early universe cosmology where stringy thermodynamics [CIT] and/or phase transitions may be relevant, neither of which is described by a constant equation of state parameter which is what previous studies have been mostly confined to. Next, we provide general formulas to compute not only the scalar power spectrum, but also the spectrum of gravity waves and higher point correlation functions. These results when applied to phase transitions in cyclic inflationary models turn out to produce interesting signatures for Planck, and will be discussed in [CIT]. | 1,458 | 1302.6463 | 10,219,748 | 2,013 | 2 | 26 | true | true | 1 | MISSION |
Our results illustrate the extra constraining power of anisotropic clustering measurements with respect to that of angle-averaged quantities. The large volume and high number density of the CMASS DR9 sample make it possible to explore these measurements with a sufficiently high signal-to-noise ratio to derive meaningful cosmological constraints. By probing larger volumes, the galaxy samples from subsequent SDSS data releases will provide more accurate anisotropic clustering measurements. The availability of these new samples will be accompanied by the release of the CMB measurements from the Planck satellite. The combination of these datasets will undoubtedly push the achievable precision on our cosmological constraints to a new level, allowing us to put the $\Lambda$CDM paradigm under even stricter scrutiny. | 820 | 1303.4396 | 10,273,374 | 2,013 | 3 | 18 | true | false | 1 | MISSION |
considering the case $\Lambda$CDM+$m_\nu$+$N_{\text{eff}}+\Omega_{\rm k}$. Since current data do not support departures from the flat $\Lambda$CDM model either through $\Omega_{\rm k} \neq 0$ or $w \neq -1$, we introduce these parameters separately. From the combination of Planck and Euclid-Cl datasets we obtain, for the curvature parameter, the following constraint: $-0.0024<\Omega_{\rm k}<0.0024$ ($95 \%$CL). As CMB power spectrum suffer from a well known " geometrical degeneracy"[e.g. [CIT]], Euclid-CL data considerably improves the error on $\Omega_{\rm k}$ breaking such degeneracy thanks to the tight constraint on $\Omega_{\rm m}$ (given by the growth information encoded in the dataset). The spatial curvature mainly affects the expansion rate via the Friedmann equation, as well as the total neutrino mass and number of effective species do. As it can be seen in Fig. REF (b), this results in a correlation with both $\sum m_\nu$ and $N_{\text{eff}}$ of the order of $\sim0.5$ and $\sim0.6$, respectively. Despite these quite large degeneracies with $\Omega_{\rm k}$, the small error associated to the curvature parameter leads to a slight relaxation of the constraints on neutrino properties: the upper limit for neutrino mass degrades by $\sim 10\%$, passing from $0.040, \text{eV}$ to $0.046, \text{eV}$ ($95 \%$CL), while the $2\sigma$ error on $N_{\text{eff}}$ shift from $0.14$ to $0.17$, a $20\%$ degradation. | 1,431 | 1303.4550 | 10,274,992 | 2,013 | 3 | 19 | true | false | 1 | MISSION |
It is important to note that applying the consistency relation to modified boundary conditions requires not only that $\zeta_{{\bf k}_3}$ freezes out before $\zeta_{{\bf k}_{1,2}}$ do, it is also necessary that it freezes out before these boundary conditions for $\zeta_{{\bf k}_{1,2}}$ are defined. This means that FORMULA This is a factor $M/H$ stronger than the usual condition $k_3 \ll k_{1,2}$, and was also noted for the resonance model in [CIT]. If this more restrictive condition is not obeyed, the boundary term will not be included in the spatial rescaling due to $\zeta_{{\bf k}_3}$ and hence will not be included in the estimation of the bispectrum. The fact that Planck is sensitive to momentum scales over a wider range than its predecessor $(l \sim 2500)$ is essential in testing this very squeezed limit relation. | 829 | 1303.4973 | 10,280,242 | 2,013 | 3 | 20 | true | true | 1 | MISSION |
We develop an integral form for the bispectrum in general single-field inflation whose domain of validity includes models of inflation where the background evolution is not constrained to be slowly varying everywhere. Our integral form preserves the squeezed-limit consistency relation, allows for fast evaluation of the bispectrum for all triangle configurations expediting the efficient comparison of slow-roll violating models with data, and provides complete and compact slow-roll expressions correct to first order in slow-roll parameters. Motivated by the recent Planck results, we consider as an example a sharp step in the warped-brane tension of DBI inflation and provide analytic solutions for the peak of the resulting bispectrum. For the step in the warp that reproduces the oscillations in the power spectrum favored by the Planck data, the corresponding equilateral bispectrum is both extremely large and highly scale dependent. The bispectrum serves as a means of distinguishing such a model from alternative scenarios that generate otherwise indistinguishable power spectra, such as a step in the potential in canonical single-field inflation. | 1,159 | 1303.7004 | 10,299,175 | 2,013 | 3 | 27 | true | false | 2 | MISSION, MISSION |
The nominal value of the best fit quadrupole measured by Planck is $[2 (2 + 1)/2\pi]C_2= 299.495 \times 10^{-12}$ [CIT]. Therefore the recent observational results can be used to constrain the parameters of the non-comoving dark energy--dark matter model. | 255 | 1304.0757 | 10,313,305 | 2,013 | 4 | 2 | true | true | 1 | MISSION |
Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org. The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The participating institutions are the American Museum of Natural History, the Astrophysical Institute Potsdam, the University of Basel, the University of Cambridge, Case Western Reserve University, the University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max Planck Institute for Astronomy (MPIA), the Max Planck Institute for Astrophysics (MPA), NewMexico State University,Ohio State University, the University of Pittsburgh, the University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. | 1,340 | 1304.3537 | 10,338,361 | 2,013 | 4 | 12 | true | false | 3 | MPS, MPS, MPS |
When dark energy equation of state is assumed to be a linear function in the cosmic scale factor $a(t)$, the dark energy constraints depend on the base parameters used, the highly correlated $\{w_0,w_a\}$, or the much less correlated $\{w_0,w_{0.5}\}$. The constraints on $\{w_0,w_a\}$ are consistent with a cosmological constant and a flat universe for both Planck+lensing+WP and WMAP9 priors, while that on $\{w_0,w_{0.5}\}$ are marginally inconsistent with a cosmological constant in a flat universe (see Fig.REF and Fig.REF) for Planck+lensing+WP priors, similar to our findings in the $X(z)$ case. | 602 | 1304.4514 | 10,347,592 | 2,013 | 4 | 16 | true | true | 2 | MISSION, MISSION |
In this paper, we ask how the Gaussianity of the CMB can be used to place constraints on hidden sector fields. We consider a hidden sector field $\Sigma$ that is coupled to a shift-symmetric inflaton $\Phi$ via irrelevant operators suppressed by a high scale $\Lambda$. We construct a general effective field theory (EFT) involving these fields, FORMULA The leading mixing respecting the shift symmetry is the dimension-five operator FORMULA Such a coupling to the inflaton kinetic term arises rather naturally in ultraviolet (UV) completions of inflation [CIT]. If $\Sigma$ is light enough[^3] to be quantum-mechanically active during inflation ($m < \frac{3}{2} H$), self-interactions in the $\Sigma$ sector can be imprinted as non-Gaussianities in the visible curvature perturbations, through the mixing (REF). In fact, the theory has two distinct sources of non-Gaussianity: self-interactions in the hidden sector, (REF), and nonlinear couplings between the two sectors, (REF). As a result, the phenomenology of the model is rather rich, with all three bispectrum shapes probed by Planck realized in different regions of the parameter space. We will use the Planck bounds on non-Gaussianity to put a lower bound on the scale $\Lambda$ in (REF), FORMULA where the precise numerical coefficient on the r.h.s. depends on the couplings of the hidden sector. A detection of primordial tensors would show that $H \gtrsim 10^{-5} M_{\rm pl}$, so that $\Lambda$ can exceed the Planck scale. In this case, the limits on the bispectrum [CIT] constrain the ultraviolet completion of gravity. | 1,584 | 1304.5226 | 10,354,084 | 2,013 | 4 | 18 | true | true | 3 | MISSION, MISSION, UNITS |
The Planck collaboration has already presented results in [CIT] on $N_{\rm eff}$ and $A_{\rm L}$ separately. Here we extend this analysis by varying $N_{\rm eff}$ and $A_{\rm L}$ simultaneously, i.e. taking into account the possible correlations between these two parameters as in [CIT], and by properly comparing the results with the previous ACT and SPT measurements in the $N_{\rm eff}$-$A_{\rm L}$ plane. | 408 | 1304.6217 | 10,363,164 | 2,013 | 4 | 23 | true | true | 1 | MISSION |
For future surveys, the cosmological parameter space will have to be enlarged beyond what was considered here. In the case of DES, for example, predictions for dynamical dark energy models are needed. Increasing the sample space will further increase the associated computational costs. On the positive side, results from surveys such as Planck help to narrow down the parameter ranges substantially, which in turn will help to reduce the number of models we have to investigate. Multi-level sampling schemes can be devised to deal with these situations, one of our directions for future work. | 593 | 1304.7849 | 10,380,010 | 2,013 | 4 | 30 | true | false | 1 | MISSION |
We have run simulations with initial values of $\gamma$ varying from $1 \lesssim \gamma \lesssim 10$, consistent with the Planck 2013 constraint $\gamma \lesssim 14$ at $95\%$ confidence [CIT]. In all simulations, we see significant effects due to parametric resonance by approximately $t \sim 100,m^{-1}$. We can identify parametric resonance by the exponential amplification of particular modes of the matter field $\chi$, which result in an exponential increase in the variance of the matter field over time. We can see this schematically by noting the inflaton is a coherently oscillating field $\phi = \Phi(t)$; the mode equations for the matter field, FORMULA are then damped harmonic oscillators with a time-dependent mass. In the case of a sinusoidally varying $\Phi$, we can reduce Eq. REF(#chimode){reference-type="eqref" reference="chimode"}, after ignoring the expansion of the universe, to the Mathieu equation and predict the spectrum of amplifications. If we allow $\Phi$ to be a sawtooth function whose amplitude decreases and whose period increases, the consequences for preheating are unclear. On one hand, we expect that the time-varying period of oscillation should do harm to the period of parametric resonance. Some modes will experience small amplifications during each oscillation, but there is no assurance that any particular mode is amplified repeatedly. | 1,381 | 1305.0561 | 10,388,080 | 2,013 | 5 | 2 | true | true | 1 | MISSION |
SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. | 962 | 1305.2923 | 10,411,838 | 2,013 | 5 | 13 | true | false | 2 | MPS, MPS |
center $\sigma(p)$ Planck Planck + $\gamma \gamma$ (known $\sigma_z, b_z$) Planck + $\gamma \gamma$ ("free" $\sigma_z, b_z$) ------------------------------ --------- -------------------------------------------------- --------------------------------------------------- $\omega_b$ 0.00013 0.000097 0.0012 $\omega_c$ 0.0011 0.00044 0.0011 $\Omega_\Lambda$ 0.18 0.018 0.13 $n_s$ 0.0033 0.0023 0.0031 $\sigma_8$ 0.20 0.019 0.15 $w_0$ 1.5 0.29 0.85 $w_a$ 3.7 0.82 1.6 FOM$=1/\sqrt{{\rm Det Cov}}$ 0.47 29 1.7 | 504 | 1306.0534 | 10,461,684 | 2,013 | 6 | 3 | true | false | 3 | MISSION, MISSION, MISSION |
Following the same steps as in [CIT], the amplitude of local type non-Gaussianity, $f_{NL}$, defined in the squeezed limit, $k_1\ll k_2=k_3$, as FORMULA is obtained to be FORMULA This value of $f_{NL}$ is consistent with the recent Planck constraints on primordial non-Gaussianity [CIT]. | 287 | 1306.2901 | 10,486,592 | 2,013 | 6 | 12 | true | true | 1 | MISSION |
With the discovery of a Higgs-like resonance at 126 GeV, the Standard Model appears to be complete and from a purely phenomenological standpoint no new physics seems to be required up to a very large scale, e.g. up to the Planck scale. While the description of gauge interactions in the Standard Model is quite economical (requiring only 3 parameters), the fact that there are three generations of fermions is not explained in the Standard Model and necessitates the introduction of many additional parameters into the model. Furthermore, these flavor parameters show certain structures that may suggest a deeper explanation: the quark sector exhibits a strongly hierarchical mass spectrum and small mixing angles while the lepton sector is less hierarchical and has larger mixing angles. | 788 | 1306.4356 | 10,503,713 | 2,013 | 6 | 18 | false | true | 1 | UNITS |
Solving the Fokker-Planck equation, Starobinsky and Yokoyama [CIT] showed that the variance of a massless scalar field with a quartic potential $\lambda \Phi^4$ approaches a constant value FORMULA at late times, where $c$ is an ${\cal O}(1)$ numerical factor. Note that the late time behaviour of the variance does not suffer from the logarithmic enhancement. This equilibrium state can be understood as the balance between the potential force (the first term in Eq. (REF)) and the quantum fluctuation (the second term). | 520 | 1306.4461 | 10,505,211 | 2,013 | 6 | 19 | true | true | 1 | FOKKER |
where $\kappa^2=32\pi G=32\pi/M_P^2$, with $M_P$ being the Planck mass and $G$ the Newtonian gravitational constant, $e$ the electric charge of the pions and $\lambda$ a self-interaction constant (already present in the scalar electrodynamics, in the absence of gravitation). $\mathcal{L}_{HO}$ is the Lagrangian of higher derivatives monomials, necessary to compensate higher order infinities induced by the nonrenormalizable gravitational interactions [CIT], $\mathcal{L}_{GF}$ is the gauge fixing plus Faddeev-Popov ghost Lagrangian (for the graviton and the photon) and $\mathcal{L}_{CT}$ is the Lagrangian of counterterms. We work in the context of renormalized perturbation theory, so all coupling constants are the physical ones. | 736 | 1306.4865 | 10,509,265 | 2,013 | 6 | 20 | false | true | 1 | UNITS |
The second term of Eq. REF represents the external constraint on $H_0$. Because the value obtained from HST observations ($H_0^{\rm HST}=73.8 \pm 2.4$) given in [CIT] and the value from Planck ($H_0^{\rm Planck}=67.4 \pm 1.4$) given in [CIT] differ by over $2\sigma$, we write this $H_0$ constraint so as to give equal weight to both measurements:\ | 348 | 1306.5896 | 10,521,772 | 2,013 | 6 | 25 | true | false | 2 | MISSION, MISSION |
The Planck early release data included observations of 0836+710 in 2009 October and 2010 March, both also during the quiescent period. The SED for the source using these data has been included in Planck Collaboration (2011) and Giommi et al. (2012). The frequency range of Planck extends higher than that included in the F-GAMMA program. | 337 | 1307.0529 | 10,538,222 | 2,013 | 7 | 1 | true | false | 3 | MISSION, MISSION, MISSION |
In this work, we adopt the CMB data from the Planck satellite [CIT], as well as the high-$l$ data from the Atacama Cosmology Telescope(ACT) [CIT] and the South Pole Telescope(SPT) [CIT]. For the Planck data, we use the likelihood code provided by the Planck team, which includes the high-multipoles $l>50$ likelihood following the `CamSpec` methodology and the low-multipoles ($2<l< 49$) likelihood based on a Blackwell-Rao estimator applied to Gibbs samples computed by the `Commander` algorithm. For the high-$l$ data, we include the ACT $148\times148$ spectra for $l\geq1000$, and the ACT $148\times218$ and $218\times218$ spectra for $l\geq1500$. For SPT data, we only use the high multipoles with $l>2000$. In our analysis, the WMAP polarization data will be used along with Planck temperature data. | 804 | 1307.4876 | 10,585,750 | 2,013 | 7 | 18 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
We study the 't Hooft's brick wall model for black holes in a holographic context. The brick wall model suggests that without an appropriate near horizon IR cut-off, the free energy of the probe fields show the divergence due to the large degenerate states near the horizons. After studying the universal nature of the divergence in various holographic setting in various dimensions, we interpret the nature of the divergence in a holographic context. The free energy divergence is due to the large degeneracy and continuity of the low energy spectrum in the boundary theory at the deconfinement phase. These divergence and continuity should be removed by finite N effects, which make the spectrum discrete even at the deconfinement phase. On the other hand, in the bulk, these degenerate states are localized near the horizon, and the universal divergence of these degenerate states implies that the naive counting of the degrees of freedom in bulk should be modified once we take into account the non-perturbative quantum gravity effects near the horizon. Depending on the microscopic degrees of freedom, the position, where the effective field theory description to count the states breaks down, has different Planck scale dependence. It also implies the difficulty to have an electron like gauge-singlet elementary field in the boundary theory Lagrangian. These singlet fields are at most composite fields, because they show divergent free energy, suggesting a positive power of N at the deconfinement phase. | 1,512 | 1307.5933 | 10,595,934 | 2,013 | 7 | 23 | false | true | 1 | UNITS |
Based on observations collected at the German-Spanish Astronomical Center, Calar Alto, jointly operated by the Max-Planck-Institut für Astronomie Heidelberg and the Instituto de Astrofı́sica de Andalucı́a (CSIC). We also thank Calar Alto Observatory for allocation of director's discretionary time to this program. | 314 | 1308.0114 | 10,625,551 | 2,013 | 8 | 1 | true | false | 1 | MPS |
In what follows, we will consider extending the "gravitational baryogenesis\" mechanism proposed in Ref. [CIT] to include the generation of a DM asymmetry. In this scenario, dynamical violation of CPT in an expanding universe leads to the generation of asymmetries, in thermal equilibrium, through the coupling [CIT] FORMULA where $M_c$ is the gravity cutoff scale, ${\cal R}$ is the Ricci scalar curvature, and $J_Q^\mu$ is the current associated with a quantum number $Q$. The scale $M_c$ is typically of order the reduced Planck mass $\bar{M}_{\rm Pl}\approx 2.4\times 10^{18}$ GeV, but could be somewhat different. The universality of gravitational interactions suggests that such couplings generally exist. | 711 | 1308.3473 | 10,662,600 | 2,013 | 8 | 15 | true | true | 1 | UNITS |
To provide observed relic density measured by Planck, Higgs-portal couplings $\lambda_{hVV,hSS}$ need to live in the region $0.05<\lambda_{hVV,hSS}<0.35$. If $\lambda_{hSS}=\lambda_{hVV}$, for the case $M_S>M_V$($M_S<M_V$), the region of $M_{V}$ permitted under the XENON100 bound satisfies the unitarity constraint. If $\lambda_{hVV}\neq\lambda_{hVV}$, the suitable value of Higgs-portal couplings is $\lambda_{hVV}(\lambda_{hSS})=0.3(0.1)$ for $M_S>M_V$, which is almost precluded by unitarity constraint. And the suitable values of Higgs-portal couplings $\lambda_{hVV}(\lambda_{hSS})$ is 0.05(0.35) for $M_V>M_S$, which is permitted by unitarity constraint for $M_V>$ 28 GeV, where all our computations are reliable. In addition, we would like to mention that invisible decay width constraint region [CIT] comes from LHC has already been excluded by XENON100, see the right panel of Fig. REF(Fig. REF). With the two component dark matter $S$ and $V$, the fine-tuning problem is relaxed, and the stability of the Higgs potential is improved up to Planck scale in some parameter regions with correct relic density. | 1,116 | 1308.3851 | 10,666,021 | 2,013 | 8 | 18 | false | true | 2 | MISSION, UNITS |
In this paper we place observational constraints on two anisotropic inflation models based on the vector and the two-form fields in the light of the recent Planck data [CIT]. We first derive the anisotropic power spectra of gravitational waves to evaluate the tensor-to-scalar ratio $r$ correctly. Using the observational bounds of $r$ as well as the scalar spectral index $n_s$ constrained by the joint data analysis of Planck and other measurements [CIT], we test for several representative models such as chaotic and natural inflation in the presence of anisotropic corrections to the scalar and tensor power spectra. | 620 | 1308.4488 | 10,673,141 | 2,013 | 8 | 21 | true | true | 2 | MISSION, MISSION |
We will start our discussion with the case where $\Psi_n(C)= C^{n-2}$, dual to pure supergravity model with higher curvature terms, $-{1\over 2} R+{\alpha \over 2} R^2 + \xi_n R^n$. For this case the analysis will be more detailed and specific. This is the supergravity scalar/vector model which is dual to pure super gravitational model with higher curvature terms. The bosonic part of this action is FORMULA It is dual to ${\cal L}^\xi(R)= -{1\over 2} R +{1\over 18 g^2} R^2 + \xi_4 R^{4}$. On the pure gravity side the reason for making a choice of $\xi$ to be equal or greater that $10^{22}$ in Planck units, taken in [CIT], is questionable and requires justification which was not given in [CIT]. At $\xi_4=0$ the potential in this model is given by ${9\over 8} g^2 (1+C^{-1})^2$ where $C=- e^{\sqrt{2/3} {\varphi}}$ and ${\varphi}$ is a canonically normalized scalar, the potential is flat at large ${\varphi}$ and inflation takes place and agrees with the data under condition that $g^2\sim 10 ^{-10}$. When $\xi_4\gtrsim 10^{25}$ it can destroy the flatness of the potential and inflationary cosmology, according to either the simple reasoning given in the Section 2, or using the analysis performed on the scalar side (REF) in [CIT]. A more complete analysis will be given below. | 1,288 | 1309.1085 | 10,710,313 | 2,013 | 9 | 4 | true | true | 1 | UNITS |
In this subsection we adopt another type of potential motivated by axion monodromy, as $V(\varphi)=\sigma\varphi^{\frac{2}{3}}$ [33]. As shown in Ref. [26], a minimally coupled 4-dimensional model with this type of potential lies within the $95\%$ CL of the Planck+WMAP9+BAO data. Although a minimally coupled DGP model with this potential lies in the $95\%$ CL of the WMAP7+BAO+H$_{0}$, it is now well outside the $95\%$ CL of the Planck+WMAP9+BAO data. If we consider a non-minimally coupled scalar field on the DGP brane, we find that the model in some range of $\xi$ is compatible with newly released observational data. The evolution of the tensor to scalar ratio versus the scalar spectral index is shown in the left panel of figure REF. For $N=70$, the non-minimally coupled DGP model with $\xi\geq0.076$, for $N=60$, the model with $\xi\geq0.0768$, for $N=50$, the model with $\xi\geq0.0775$ and for $N=40$, the model with $\xi\geq0.078$ lies inside the $95\%$ CL of the Planck+WMAP9+BAO data. Note that, as $\xi$ increases the non-minimally coupled DGP model with this potential becomes independent of the value of $N$. We have also plotted the evolution of the running of the scalar spectral index versus the scalar spectral index (right panel of figure REF). For this case, the running is negative and in some range of $\xi$ is compatible with recent data. | 1,367 | 1309.1950 | 10,718,659 | 2,013 | 9 | 8 | true | false | 3 | MISSION, MISSION, MISSION |
All over this paper energy, mass and momentum is measured in multiples of the Planck mass, $M_P$, while length and time in multiples of the Planck length, $L_P$. All equations relating unlike quantities are to be supported by corresponding powers of $M_P$ and $L_P$. The entropy is measured in units of the Boltzmann constant, $k_B$. In a $c=1$, $k_B=1$ system one expresses the Planck constant as $\hbar = L_P M_P$ and Newton's gravity constant as $G=L_P / M_P$. | 463 | 1309.4261 | 10,741,727 | 2,013 | 9 | 17 | false | true | 3 | UNITS, UNITS, CONSTANT |
The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Economía y Competitividad, the Conselleria d'Economia Hisenda i Innovació of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, OTKA of Hungary, the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. | 1,756 | 1309.6160 | 10,760,143 | 2,013 | 9 | 24 | true | false | 1 | MPS |
Special attention has to be paid on the validity conditions of approximation assumed tacitly throughout the above discussion. We have taken gravitational field on the equal footing with the matter fields, that is, QFT picture for gravity is taken as a starting point. This means that the graviton field is defined as the difference between the full metric and its Minkowski background value and a field theory on flat Minkowski spacetime is assumed to hold for this graviton field. Such QFT approach to gravity, pioneered by Kraichnan (the only post-doctoral student that Einstein ever had) [CIT] and Gupta [CIT], is reviewed in [CIT]. However, we have used this QFT approach to gravity, suitably modified, only to get the generalization of the Newton potential and then embarked on more traditional geometric approach by substituting this generalized potential into the Schwarzschild-Tangherlini metric. Although quite reasonable in a weak-field limit, it seems completely impossible to justify the use of this substitution up to the Planck scale. Nevertheless, the following rather ingenious, though somewhat heuristic, argument can be envisaged to justify such kind of business. We will assume $n=0$ (that is 3D case) in the following. | 1,238 | 1309.7427 | 10,773,367 | 2,013 | 9 | 28 | false | true | 1 | UNITS |
The framework of a warped extra dimension with the Standard Model (SM) fields propagating in it is a very well-motivated extension of the SM since it can address both the Planck-weak and flavor hierarchy problems of the SM. We consider signals at the 14 and 33 TeV large hadron collider (LHC) resulting from the direct production of the new particles in this framework, i.e.,Kaluza-Klein (KK) excitations of the SM particles. We focus on spin-1 (gauge boson) and spin-2 (graviton) KK particles and their decays to top/bottom quarks (flavor-conserving) and W/Z and Higgs bosons, in particular. We propose two benchmarks for this purpose, with the right-handed (RH) or LH top quark, respectively, being localized very close to the TeV end of the extra dimension. We present some new results at the 14 TeV (with 300 fb$^-1$ and 3000 fb$^-1$) and 33 TeV LHC. We find that the prospects for discovery of these particles are quite promising, especially at the high-luminosity upgrade. | 978 | 1309.7847 | 10,776,436 | 2,013 | 9 | 30 | false | true | 1 | UNITS |
In this paper, we have investigated the constraints to the equation of state of dark matter by using the currently available cosmic observational data sets, which include the CMB of the first 15.5 months from Planck, SNLS3, SDSS BAO and WiggleZ measurements of power spectrum. The previous results were updated. We have found that the latest data provide the constraints $w_{dm}=0.000707_{-0.000747}^{+0.000746}$ at $95\%$ C.L.. This result is compatible with the previous results, but a relative tighter constraint was obtained due to the high quality of the currently available data points. The difference of the minimum $\chi^2$ between the $\Lambda$CDM and $\Lambda$wDM models is $\Delta\chi^2_{min}=0.446$ for one extra model parameter $w_{dm}$. Although the currently available cosmic observations favor the $\Lambda$wDM mildly, no significant deviation from the $\Lambda$CDM model is found in the $1\sigma$ region. | 921 | 1310.1532 | 10,795,873 | 2,013 | 10 | 6 | true | false | 1 | MISSION |
In an attempt to revive the Planck scale suppressed operators, we shall consider them in the context of extradimensional models. One advantage of considering such models is that in the effective 4D theory the suppressing scale is in general less than the Planck scale. This is because the effective 4D scale is defined in terms of the Planck scale as $\Lambda=f_{bulk}M_{Pl}$, where $f_{bulk}$ is a function of fundamental bulk parameters of the theory. A particular realization of the extra-dimensional framework we consider here, is the one proposed by Randall and Sundrum [CIT]. It consists of a single extra-dimension compactified on an $S_1/Z_2$ orbifold. A 3-brane is introduced at each of the orbifold fixed points *i.e.* at $y=0$ and $y=\pi R$. The presence of a large negative bulk energy density attributes a warped geometry to the bulk. Introduction of brane-localized sources results in a vanishing cosmological constant on the branes. Identifying the scale of physics at the $y=0$ brane as the Planck scale, the effective UV scale induced at the brane at $y=\pi R$ is given as $e^{-kR\pi}k$ where $R$ is the radius of compactification and $k$ is the reduced Planck scale. Choosing $kR\sim 11$ we find that Planck scale masses are naturally warped down to the $TeV$ scale on the $y=\pi R$ brane with $\mathcal{O}$(1) choice of model parameters thus providing an elegant solution to the hierarchy problem. The geometry of RS also offers a natural explanation to the observed hierarchical masses of fermions by means of the split fermion approach introduced in [CIT] and applied to the RS framework in [CIT]. | 1,618 | 1310.1948 | 10,800,172 | 2,013 | 10 | 7 | false | true | 6 | UNITS, UNITS, UNITS, UNITS, UNITS, UNITS |
As is seen from Table. REF, **Planck-z03** gives the smallest $\chi^{2}$, while the difference is small. The constraints on $(f,D_{\rm A},H)$ are all consistent with each other, excepting **Planck-cbias**. The bias parameters are in fact more important than the others in order to well fit to the monopole. Comparison between **WMAP5** and **Planck-z03** shows that our constraints are not sensitive to choice of the underlying cosmology for the model power spectrum. We thus conclude that our results are robust against such systematics. | 538 | 1310.2820 | 10,808,966 | 2,013 | 10 | 10 | true | false | 3 | MISSION, MISSION, MISSION |
The CMB shows a lack of correlations on large angular scales. This can be quantified by the $\ensuremath{S_{1/2}}$ statistics proposed by [CIT] -cosmology which is best calculated on the portion of the sky outside the Galaxy. Unlike attempts to infer properties of the the full-sky correlation function, the cut-sky $\ensuremath{S_{1/2}}$ appears remarkably robust and trustworthy. In our analysis we find that the $p$-value for the observed cut-sky $\ensuremath{S_{1/2}}$ in an ensemble of realizations of the best-fitting $\Lambda$CDMmodel never exceeds $0.33$ per cent for any of the analysed combinations of maps and masks, with and without correcting for the Doppler quadrupole. This has remained the case since the *WMAP*three-year data release,[^9] for both the individual ($V$ and $W$) band maps and the synthesized (ILC) map, and for the first Planckdata release for both the *LFI*and *HFI*band maps and all the released synthesized maps (`NILC`, `SMICA`, `SEVEM`), when masked by either the *WMAP*KQ75y9 mask or the less conservative U74 mask (which is very similar to the PlanckU73 mask). The *HFI*$100\;\rmn{GHz}$ map -- the presumably cleanest CMB band of *HFI*-- with the more conservative mask that has been defined by *WMAP*gives a $p$-value of only $0.03$ per cent! As general trends we note that a larger mask tends to produce smaller $p$-values, the Doppler quadrupole correction does not change the results in a significant way, and the Planckdata yield somewhat smaller $p$-values than the *WMAP*data. | 1,522 | 1310.3831 | 10,819,192 | 2,013 | 10 | 14 | true | false | 3 | MISSION, MISSION, MISSION |
The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). | 935 | 1310.4170 | 10,822,584 | 2,013 | 10 | 15 | true | false | 3 | MPS, MPS, MPS |
The main $f_{\mathrm{NL}}^{\mathrm{local}}\;$measurements from the clustering of the BOSS quasar sample are significantly non-zero in contrast to the recent results from Planck [CIT], where they calculate the amplitude of non-Gaussianity to be consistent with the predictions of the standard model ($f_{\mathrm{NL}}^{\mathrm{local}}=2.7\pm5.8$ at $68\%$ CL). However, in [CIT] they found that the low-$l$ spectrum of the Planck data ($l\lesssim30$) deviates from the best-fit $\Lambda$CDM model at the $2.7\sigma$ significance level. This could have essential implications for the parameters estimated by Planck including $f_{\mathrm{NL}}$. In addition to this, in [CIT] they found a significant deviation from Gaussianity in the form of positive kurtosis of the wavelet coefficients, which is in contrast to the measured amount of non-Gaussianity from the CMB angular bispectrum (see Tables 2,3,4 of [CIT]). These findings are more likely to correspond to numerous anomalies (e.g. dipolar power modulation, hemisphere asymmetry, generalised power modulation, phase correlations) observed at the large angular scales of the Planck sky. Most of these features were also detected in the WMAP data, ruling out the possibility that they are systematic artefacts. More tests have been made in [CIT] proving that they are real features of the CMB. The nature of the anomalies is unknown, and the polarization data to be released in 2014 are expected to give the information needed to resolve this issue. | 1,497 | 1310.6716 | 10,849,321 | 2,013 | 10 | 24 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
It is worth to write down the the effective theory on the brane. It is derived by making use of the braneworld holography [CIT]. This method gives FORMULA Here $\Gamma_{\text{CFT}}$ is the effective action for the holographic CFT on the brane, $R(g)$ is the Ricci scalar on the brane, $M_4^2=lM_5^3=M_P^2$ plays the role of Planck mass, with $l$ the the curvature radius of the AdS spacetime, and ${\cal L}_{\text{matter}}$ is the Lagrangian density matter localized on the brane. The parameter $\epsilon$ determines the renormalization scale of CFT, whereas the field $\phi$ corresponds to the zero mode of the bulk complex scalar field $\Phi$ localized on the brane ($\varphi$ could represent squarks or sleptons on the brane carrying baryon/lepton number). Notice that (REF) is written as and Hilbert-Einstein action FORMULA plus scalar field (in the so called Jordan frame). In this respect it is similar to scalar tensor theories. | 935 | 1310.8459 | 10,868,099 | 2,013 | 10 | 31 | true | true | 1 | UNITS |
Almheiri et al. [CIT] argue that two standard assumptions made in discussions of quantum properties of black holes, namely that "i) Hawking radiation is in a pure state, ii) the information carried by the radiation is emitted near the horizon, with low energy effective field theory valid beyond some distance from the horizon," are incompatible with a statement that iii) the infalling observer encounters nothing unusual at the horizon [CIT]. Their proposed "resolution [of the apparent contradiction] is that the infalling observer burns up at the horizon." Specifically, they suggest that "the infalling observer encounters a Planck density of Planck scale radiation and burns up." This phenomenon has been called a "firewall," and firewalls were supposed to be present both in stellar-mass and supermassive black holes. While the presence of a firewall is subject to an ongoing controversy (e.g., [CIT]), the internal contradiction of the set of three assumptions seems to be real and supported by detailed calculations in [CIT] and numerous other papers (e.g., [CIT] and references therein). | 1,097 | 1311.0239 | 10,873,434 | 2,013 | 11 | 1 | false | true | 2 | UNITS, UNITS |
We propose a single field inflationary model by generalizing the inverse power law potential from the intermediate model. We study the implication of our model on the primordial anisotropy of cosmological microwave background radiation. Specifically, we apply the slow-roll approximation to calculate the scalar spectral tilt $n_s$ and the tensor-to-scalar ratio $r$. The results are compared with the recent data measured by the Planck satellite. We found that by choosing proper values for the parameters, our model can well describe the Planck data. | 552 | 1311.0348 | 10,874,657 | 2,013 | 11 | 2 | true | true | 2 | MISSION, MISSION |
In this work, we consider an alternative single field inflationary model, motivated by the intermediate model [CIT] which contains only the inverse power law term: FORMULA with $\beta>0$. A notable feature of intermediate model is that it leads to exact solution to the equation of motion. Like many other models, the inverse power law potential is disfavored by the Planck data, being outside the joint 95% CL contour of $n_s$ and $r$ for any $\beta$. However, as we will show blow, after slightly modifying the original model, we find that the new form of potential, as a generalization of the inverse power law potential, can well describe the Planck $n_s$ and $r$ data. | 673 | 1311.0348 | 10,874,806 | 2,013 | 11 | 2 | true | true | 2 | MISSION, MISSION |
- The first public release of Planck Collaboration temperature data, combined with WMAP-$9$ year polarization information at low $\ell$, and the corresponding likelihood codes [CIT] : `Commander`, that computes the low-$l$ Planck likelihood, `CamSpec`, that computes the Planck likelihood for the multipoles with $50\leq l\leq 2500$, `LowLike`, that computes the likelihoods from the $2\leq l\leq 32$ temperature and polarization data [^4] and `Lensing`, that computes the likelihoods from Planck lensing power spectrum data, for multipoles between 40 and 400 [CIT]. | 566 | 1311.3856 | 10,913,553 | 2,013 | 11 | 15 | true | true | 4 | MISSION, MISSION, MISSION, MISSION |
The planarity of the octopole and alignment of the quadrupole and octopole in the CMB as observed by *WMAP*was first studied by [CIT] -alignment through the maximum angular momentum dispersion. This statistic has subsequently been applied to the Planckdata [CIT]. A more complete picture of CMB alignments is obtained through the use of the multipole vectors [CIT]. Here we study both of these approaches. | 405 | 1311.4562 | 10,920,502 | 2,013 | 11 | 18 | true | false | 1 | MISSION |
We have studied several models and derived their predictions within the slow-roll approximation. Now we present these predictions by visualising them against the latest constraints on inflation models compiled by the Planck collaboration [CIT]. The Planck+WP observational data favours a concave potential for viable canonical inflation models and limits the tensor-to-scalar ratio below $r=0.11$ at 95% confidence. In Figure [REF]{.underline} we can see that for canonical inflation models with the polynomial potential $V\propto \phi^m$, the $m=3,4$ cases are ruled out by the observational requirements, while potentials with $m=2/3$, $1$, $4/3$ and $2$ are within 95% confidence, though at $N_*=50$ the quadratic potential ($m=2$) lies outside the 95% confidence region [CIT]. | 780 | 1311.4664 | 10,921,871 | 2,013 | 11 | 19 | true | false | 2 | MISSION, MISSION |
In this work, we focus on improving in the measurement of $T_{\rm CMB}$ at redshifts $z>0$ from the Planck data using the tSZ effect from galaxy clusters. In Sect. [2] we present the Planck intensity maps and galaxy cluster catalog that were used. Sect. [3] briefly presents the tSZ effect. Then in Sect. [4], we present the stacking method used to extract the tSZ flux in the different Planck frequency channels to constrain $T_{\rm CMB}$. In Sect. [5], we estimate the uncertainty levels on our measurement that are caused, on the one hand, by foreground/background contributions to Planck intensity maps and, on the other hand, by instrumental systematic effects. Next in Sect. [6], we carefully model our measurement to determine $T_{\rm CMB}$ from the tSZ spectral law. In Sect. [7], we present our results and compare them with previous measurements. Finally in Sect. [8], we discuss our results and their cosmological implications. | 938 | 1311.4694 | 10,922,089 | 2,013 | 11 | 19 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
In cosmology, the search for primordial non-Gaussian random fields has attracted great attention because their detection and identification allows for a differentiation between various models of inflation. While e.g. multi-field inflation or self-interactions of the inflaton field generally yield measurable non-Gaussianity (NG), the standard isotropic cosmology with the simple single-field slow-roll inflationary scenario and a Friedmann-Robertson-Walker (FRW) metric predicts a Gaussian distribution of the first density perturbations of the Universe [CIT]. The latest, most precise measurements of parametrized NGs of the local, equilateral and orthogonal type by the Planck team did not reveal significant deviations from Gaussianity [CIT]. A model independent test using the well-established method of surrogates [CIT] applied to the Planck CMB maps revealed, however, NGs or hemispherical asymmetries for higher order statistics [CIT], which can be traced back to harmonic space phase correlations on large spatial scales at low spherical harmonic modes $\ell$ with $\ell < 20$, confirming previous findings in WMAP data [CIT]. Evidence was found that a best-fit Bianchi type $\mathrm{VII_h}$ template (BT) correlates with the large-scale anomalies in the CMB sky [CIT], although the best-fit Bianchi model itself is not compatible with the parameters of the cosmological concordance model (see e.g. [CIT]). Bianchi models provide a generic description of anisotropic homogeneous cosmologies [CIT] that are only asymptotically close to a FRW universe. Applying a BT correction to CMB data yields a sky which is statistically isotropic for at least some subset of statistical measures, e.g. the local power estimates. In [CIT], it was found that the signal stemming from low-$\ell$ phase correlations can also be significantly reduced if the best-fitting BT is subtracted from the Planck maps. These results could hint at the properties of fully compliant cosmological models, especially when the behavior of the data is studied as a function of the correction and on isolated scales. | 2,091 | 1311.5053 | 10,925,751 | 2,013 | 11 | 20 | true | false | 3 | MISSION, MISSION, MISSION |
An alternative way to estimate cluster masses is offered the SZ effect [e.g., [CIT]]. Of the 21 minihalo clusters considered here, 14 are in the all-sky cluster catalog of validated clusters from the first 15.5 months of Planck observations (Planck Collaboration 2013). In Table 5, we report their total masses within $R_{500}$ inferred from the Planck observations. Fig. REF(b) shows the distribution of our sub-sample of minihalo clusters that have Planck data in the $P_{\rm MH,,1.4, GHz}-M_{\rm 500}$ plane. No obvious correlation is visible between the radio luminosity and cluster mass -- in this case we find $r_s \sim 0.3$ and $P_{\rm no, corr} \sim 10\%$ -- in agreement with the lack of a clear correlation with the global temperature in panel (a). We note that this is in contrast with the *giant* radio halos found in cluster mergers, whose radio luminosity correlates with the cluster mass (Cassano et al. 2013 and references therein). Again, we find evidence that minihalos are hosted by massive clusters, as all minihalos are in $M_{\rm 500} \gtrsim 5 \times 10^{14}$ $M_{\odot}$, except for the sligthly less massive system 2A,0335+096 ($M_{\rm 500} = 2\times 10^{14}$ $M_{\odot}$). | 1,198 | 1311.5248 | 10,927,846 | 2,013 | 11 | 20 | true | false | 4 | MISSION, MISSION, MISSION, MISSION |
Photometric redshifts in the Boötes field are based on the multi-wavelength dataset described in Section 4.1.1. Where IRAC data are available, we rely only on the two bluer channels, 3.6 and 4.5$\mu$m, to minimise contamination of the stellar SED by any hot dust component. Based on tests against simulated catalogues and collected archival spectroscopic redshifts in this field (Vaccari et al., in prep), we find an intrinsic scatter $\Delta z/(1+z) = 0.042$ out to $z \sim 4$ in the photometric redshift measure. Comparison of the redshift distribution in the whole NDWFS Boötes field with that along the line of sight of the Planck clump (see Fig. 10) shows a marked spike of objects at a photometric redshift of about 2.3. This peak is also found to be associated with a strong overdensity of objects ($\sim 10\sigma$) at the position of the clump. Our analysis shows no significant overdensity of objects along the clump's line of sight at any other redshift, thus confirming this peak to be the only cluster candidate. The robust mean estimate of the redshift for this peak is $2.27 \pm 0.14$. Monte Carlo simulations, looking for photometric redshift spikes of similar significance to that found for this clump within Planck beams placed at random locations in the Boötes field, show that similar significance redshift spikes are found $\leq$ 1% of the time. This thus represents the chance that the association of this Planck clump with a redshift spike is a false positive. | 1,482 | 1311.5758 | 10,933,561 | 2,013 | 11 | 22 | true | false | 3 | MISSION, MISSION, MISSION |
Fitting the thermal spectrum of an isolated NS with a blackbody model, one can determine the apparent blackbody temperature $T_{\rm BB}$ and the normalization parameter $K_{\rm BB}=R_{\rm BB}^2/d^2$, where $R_{\rm BB}$ is the apparent blackbody radius and $d$ is the distance. However, the actual thermal spectrum can differ significantly from the Planck spectrum, and $T_{\rm BB}$ and $R_{\rm BB}$ can be different from the actual temperature and radius. In particular, if the NS surface is covered by an optically thick hydrogen or helium plasma envelope (atmosphere), the emergent spectrum is harder than the blackbody spectrum with the same effective temperature, $B_{E}(T_{\rm eff})$, because photons with higher energies $E$ are emitted from deeper, hotter layers due to the opacity decrease with increasing $E$ (e.g., the free-free opacity $k_{\rm ff}\propto E^{-3}$ at low magnetic fields) --- see, e.g., [CIT] :96. Therefore, the temperature obtained from a blackbody fit is higher than the effective temperature, $T_{\rm BB} = f T_{\rm eff}$, where $f \approx 1.5$--3, while the blackbody radius is smaller than the true radius because the observed flux does not depend on the model chosen for fitting (e.g., $R_{\rm BB}\sim f^{-2} R$ if the observed energy range includes a substantial fraction of the bolometric flux, $F_{\rm bol}= (R^2/d^2)\sigma_{\rm SB}T_{\rm eff}^4$[^1]. Thus, to measure the NS surface temperature and radius, one should fit the observed spectra with model atmosphere spectra rather than with the blackbody model. | 1,547 | 1311.6037 | 10,936,024 | 2,013 | 11 | 23 | true | false | 1 | LAW |
We would like to thank Drew Keppel, Reinhard Prix, Andrew Lundgren, Ian Harry and Walter Del Pozzo for enlightening discussions; Will Farr for carefully reading an earlier draft of this paper; the LIGO Scientific Collaboration for the generation and storage of the standard Gaussian data set used in this study; and the Albert-Einstein-Institut (Hannover) for the use of the Atlas computing cluster. JV was supported by the research programme of the Foundation for Fundamental Research on Matter (FOM), which is partially supported by the Netherlands Organisation for Scientific Research (NWO); TD acknowledges support from the Max-Planck-Gesellschaft. | 652 | 1311.7174 | 10,947,421 | 2,013 | 11 | 27 | true | false | 1 | MPS |
The main observable related to the primordial perturbations is the power spectrum of the CMB fluctuations. Roughly speaking, the power spectrum is the amplitude of the perturbations squared as a function of their scale. When the almost scale-invariant primordial curvature perturbations re-enter inside the horizon, they begin to evolve. Due to the Einstein equations this is translated into the evolution of the matter-photon plasma perturbations. After recombination, when photons decouple from baryons, baryonic matter fluctuations grow and eventually gravitationally collapse, giving rise to the large-scale structure we observe today. On the other hand, photons mainly cool down due to the expansion of the universe, carrying the profile of their temperature fluctuations at the time of recombination (in reality, their profile also evolves with time due to sources of secondary anisotropies, like the ISW effect discussed later in this section). Their angular power spectrum today, as measured by Planck, is shown in figure REF. | 1,034 | 1312.0126 | 10,953,819 | 2,013 | 11 | 30 | true | false | 1 | MISSION |
Neutrinos could be viable DM candidates since we saw in chapter REF that they interact weakly with the other SM particles. Nevertheless the neutrino relic density is given by \_h\^2 = \_i=e,,, which, using limits on neutrino masses like the ones obtained with the Planck satellite [CIT], exclude neutrinos as the main component of DM. Moreover, since neutrinos are relativistic particles, they only could form HDM which is disfavoured as explained in section [1.3]. Thus no SM particles fit the DM hypothesis. | 509 | 1312.0257 | 10,955,075 | 2,013 | 12 | 1 | false | true | 1 | MISSION |
The previous HS simulations are based on the WMAP seven-year best fit cosmology [CIT] (WMAP7 hereafter, parameters summarised in Eq (REF)). In this work, we need new HS simulations for other background cosmologies to calibrate `MGHalofit`to make it robust for a range of cosmological parameters. We choose to run new HS simulations using `ECOSMOG` for the Planck [CIT] (summarised in Eq (REF)) and WMAP nine-year [CIT] (WMAP9, summarised in Eq (REF)) best fit cosmologies for the calibration because they sizably differ from the WMAP7 cosmology, *e.g.*, $\Omega_{\rm M}^{\rm Planck}$ and $\Omega_{\rm M}^{\rm WMAP9}$ is larger than $\Omega_{\rm M}^{\rm WMAP7}$ by 28% and 7% respectively. We use the previous WMAP7 simulation [CIT] as well for the calibration. FORMULA For each set of parameters, we simulate three $f(R)$ models with $n=1, |f_{R0}|=10^{-4,-5,-6}$ (F4, F5, F6 models hereafter). We simulate the $|f_{R0}|=0$ ($\Lambda$CDM) model as well using the same initial condition to make direct comparison. | 1,012 | 1312.1291 | 10,967,427 | 2,013 | 12 | 4 | true | false | 2 | MISSION, MISSION |
We outline a very simple, closed-form radiative transfer model which incorporates and connects well-understood asymptotic behavior for particles smaller than and larger than the wavelength. The approach is simple enough to provide good physical insight and to include in evolutionary models requiring radiative transfer. The model is easily adapted to arbitrary combinations of particle size, composition, and porosity across the range of plausible protoplanetary nebula and exoplanet cloud particle properties (excepting highly elongated particles), and yields values of Rosseland mean opacity which are in good agreement with more sophisticated but more time consuming Mie or DDA calculations. Planck opacities are even simpler to calculate (they are straight Blackbody-weighted means over wavelength). We illustrate the significant roles of particle growth and porosity in determining opacity. The model is *not* recommended even for Rosseland opacities in cases where ensembles of large, pure metal particles are expected. The method even gives very good approximations to *monochromatic* opacities *unless* the particles are solid and the specific wavelength of interest is comparable to the dominant particle size, where the model is unable to track "resonance\" behavior of the absorption efficiency. Thus for detailed spectral index analysis of mm-cm wavelength protoplanetary nebula emission spectra, in cases where particles in the mm-cm radius range might be solid and contribute significant mass and area, full Mie theory should be used. It appears that canonical mm-wavelength spectral slopes are more plausibly explained by solid, cm-size particles than larger, but more porous, aggregates. | 1,704 | 1312.1798 | 10,973,325 | 2,013 | 12 | 6 | true | false | 1 | OPACITY |
We consider here a sample of galaxy clusters which exhibit RHs and that have also X-ray and SZE information. The cluster data that are used in our analysis are selected from the Planck Collaboration (2011) and from Brunetti et al. (2009). The cluster redshifts and the radio power $P_{1.4}$ are taken from Brunetti et al. (2009) and from Giovannini et al. (2009), the bolometric X-ray luminosity $L_X$ are taken from Reichert et al (2011) while the integrated Compton parameter $Y_{SZ}$ are taken from the Planck Collaboration (2011). We also used information on the cluster velocity dispersion collected from various authors like Wu et al. (2009), Zhang et al. (2011). As for the cluster A781 we used the information given by Cook et al. (2012) and from Geller et al. (2013) Our final cluster sample extends the cluster sample considered by Basu (2012) by including some additional clusters for which the integrated Compton parameter is now available. The final RH cluster sample we use in this work is reported in Tables REF and REF. | 1,035 | 1312.1846 | 10,973,773 | 2,013 | 12 | 6 | true | false | 2 | MISSION, MISSION |
A nice and simple way to generate these one-loop masses is through anomaly like contributions. If the regulated theory has Pauli-Villar fields which interact with the hidden sector, the theory will have one-loop masses generated by the gauge and Yukawa couplings [CIT]. The interactions of the Pauli-Villar fields with the hidden sector may be a natural part of string theory and by merely including this additional interaction at the Planck scale, we obtain one-loop masses. Since we are quite ignorant about what the universe is like at the Planck scale, this is an acceptable assumption. | 590 | 1312.1984 | 10,974,989 | 2,013 | 12 | 6 | false | true | 2 | UNITS, UNITS |
This is closely analogous to what happens in GR. The Einstein-Hilbert action, expanded in powers of the canonically-normalized metric perturbation $g_{\mu\nu} = \eta_{\mu\nu}+\frac{h_{\mu\nu}}{M_{\rm Pl}}$, is schematically of the form FORMULA where we have suppressed indices for simplicity. In other words, the action consists of a kinetic term $h\partial\partial h$, and an infinite number of interaction terms with exactly two derivatives and arbitrary powers of $h/M_{\rm Pl}$. Like the galileon cubic term, the relative coefficients of these terms are not renormalized, thanks to diffeomorphism invariance. The measure of classical non-linearity is FORMULA Quantum effects generate higher-curvature terms, which expanded in $h$ are of the form FORMULA These are suppressed relative to classical operators by powers of the factor FORMULA A point source induces the spherically-symmetric profile $h\sim \frac{r_{\rm Sch}}{r}$, for which FORMULA Therefore, for $r\gg r_{\rm Sch}$ (such as in the solar system), classical non-linearities are unimportant, whereas for $r\ll r_{\rm Sch}$ (such as inside and near the horizon of a black hole) they dominate. Meanwhile, quantum effects are negligible for $r\gg {1\over M_{\rm Pl}}$ but become important near and below the Planck length. The black hole horizon is the analogue of the Vainshtein radius: this is where classical non-linearities are large and produce important effects, while quantum effects are under control. This is illustrated in Fig. REFb). | 1,506 | 1312.2006 | 10,975,174 | 2,013 | 12 | 6 | true | true | 1 | UNITS |
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