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Finally. analysing cillerent subsamples of host clusters we found that. the more massive is the host cluster the ereater is the effect on the group velocity dispersion. which is also consistent with the previous mocel. | Finally, analysing different subsamples of host clusters we found that, the more massive is the host cluster the greater is the effect on the group velocity dispersion, which is also consistent with the previous model. |
Using the final version of the 20 redshift survey. we repeated the velocity dispersion. analysis performed to the VLS groups. | Using the final version of the 2dF redshift survey, we repeated the velocity dispersion analysis performed to the VLS groups. |
In this case we take a subsample of VLS groups. which reproduces the velocity dispersion distribution of groups identified in the 2d0EXGIUS. | In this case we take a subsample of VLS groups, which reproduces the velocity dispersion distribution of groups identified in the 2dFGRS. |
The trend we find for the observational data is in excellent agreement with the result we obtain for the simulation subsample. | The trend we find for the observational data is in excellent agreement with the result we obtain for the simulation subsample. |
Moreover. 2dE groups velocity dispersion show a dependence on the host masses very similar to that found in the simulation. | Moreover, 2dF groups velocity dispersion show a dependence on the host masses very similar to that found in the simulation. |
Phe good agreement between the results coming from the numerical simulation and the observational data sugeests that no astrophysical mechanisms. other than the eravitational forces. are needed in order to explain. the dynamical properties of groups of galaxies. | The good agreement between the results coming from the numerical simulation and the observational data suggests that no astrophysical mechanisms, other than the gravitational forces, are needed in order to explain the dynamical properties of groups of galaxies. |
We thank the referee for useful suggestions that improved he original version of the paper. | We thank the referee for useful suggestions that improved the original version of the paper. |
“Phe simulations in this uper were carried out bv the Virgo Supercomputing Consortium using computers based at Computing Centre of he Max-Planck Society in Garching and at the Ecinbureh Parallel Computing Contre. | The simulations in this paper were carried out by the Virgo Supercomputing Consortium using computers based at Computing Centre of the Max-Planck Society in Garching and at the Edinburgh Parallel Computing Centre. |
The data are publicly available ab www.mpa-egarchineg.mpe.de/NumCos. | The data are publicly available at www.mpa-garching.mpg.de/NumCos. |
We thank to Peder vorbere and Shaun Cole for kindly providing the software describing the masks of the 2dkFGRS and to the 2dEGIUS σαι for having made available the final. version of the catalogue. | We thank to Peder Norberg and Shaun Cole for kindly providing the software describing the masks of the 2dFGRS and to the 2dFGRS Team for having made available the final version of the catalogue. |
This work has been partially supported. by Agencia Nacional cde Promociónn Científica v Téccenica. Secretariaa de Ciencia v Téccnica. (οςνι the Agencia Cordoba Ciencia and Fundaciónn Antorchas. Argentina. | This work has been partially supported by Agencia Nacional de Promociónn fica y Téccnica, a de Ciencia y Téccnica (SeCyT), the Agencia Córrdoba Ciencia and Fundaciónn Antorchas, Argentina. |
of the total mass budget in the two-dimensional simulations and is very insensitive to the details of the AGN feedback. | of the total mass budget in the two-dimensional simulations and is very insensitive to the details of the AGN feedback. |
This is in good agreement with the one-dimensional simulations at low mechanical efficiencies. | This is in good agreement with the one-dimensional simulations at low mechanical efficiencies. |
However, at high feedback efficiencies, the one-dimensional simulations drive significant quantities of gas out of the galaxy, leading to low star formation rates and low final gas content. | However, at high feedback efficiencies, the one-dimensional simulations drive significant quantities of gas out of the galaxy, leading to low star formation rates and low final gas content. |
In this respect the one-dimensional and two-dimensional simulations disagree. | In this respect the one-dimensional and two-dimensional simulations disagree. |
However, this is to be expected since assuming spherical symmetry gives the most favorable situation for turning a central energy source into a global outflow. | However, this is to be expected since assuming spherical symmetry gives the most favorable situation for turning a central energy source into a global outflow. |
In two dimensions, energy can escape via low-density channels and fail to participate in driving an outflow. | In two dimensions, energy can escape via low-density channels and fail to participate in driving an outflow. |
Figure 10. shows the mean mechanical energy input versus the mean efficiency for one-dimensional and two-dimensional A models. | Figure \ref{fig:efb-vs-eff} shows the mean mechanical energy input versus the mean efficiency for one-dimensional and two-dimensional A models. |
For two-dimensional A models, the energy input is nearly constant—the SMBH accretion self-regulates to provide energy at this rate. | For two-dimensional A models, the energy input is nearly constant—the SMBH accretion self-regulates to provide energy at this rate. |
The one-dimensional A models have lower energy input rates. | The one-dimensional A models have lower energy input rates. |
That is, two-dimensional models require more energy to reach equilibrium between inflow (due to cooling) and outflow (due to mechanical feedback). | That is, two-dimensional models require more energy to reach equilibrium between inflow (due to cooling) and outflow (due to mechanical feedback). |
We have performed two-dimensional simulations of the entire cosmic history (12 Gyr) of an isolated L. elliptical galaxy. | We have performed two-dimensional simulations of the entire cosmic history (12 Gyr) of an isolated $L_*$ elliptical galaxy. |
Planetary nebulae and red giant winds produced by evolving low-mass stars serve as the source of gas in the galaxy. | Planetary nebulae and red giant winds produced by evolving low-mass stars serve as the source of gas in the galaxy. |
This gas finally ends up either in the central BH, in long-lived low-mass stars (formed in the simulation), in the ISM within the galaxy (at the end of the or outside the galaxy as part of the intergalactic simulation),medium. | This gas finally ends up either in the central BH, in long-lived low-mass stars (formed in the simulation), in the ISM within the galaxy (at the end of the simulation), or outside the galaxy as part of the intergalactic medium. |
As gas finds its way to one of those four final states, it can engage in star formation, mass/energy injection into the ISM via Type Ia or Type | As gas finds its way to one of those four final states, it can engage in star formation, mass/energy injection into the ISM via Type Ia or Type |
63 and 71 and the secondary mass between 0.124.AM. and 0.133AL... | $^\circ$ and $^\circ$ and the secondary mass between $0.124\ M_\odot$ and $0.133\ M_\odot$. |
For à sdD mass of 0.5Δι we obtain an inclination ranging from 65 to τοῦ. and. a secondary mass between 0.143AZ. and 0.149AL.. | For a sdB mass of $0.5\ M_\odot$, we obtain an inclination ranging from $^\circ$ to $^\circ$ , and a secondary mass between $0.143\ M_\odot$ and $0.149\ M_\odot$. |
Again. using the mass function and assuming a mass of 0.5AL. for the hot subdwarl GALEN | 3844. the ΠΠ secondary mass is 0.27Al. that corresponds to a spectral tvpe of ALL (Ixirkpatrick&AleCarthy1L994). | Again, using the mass function and assuming a mass of $0.5\ M_\odot$ for the hot subdwarf GALEX $+$ 3844, the minimum secondary mass is $0.27\ M_\odot$ that corresponds to a spectral type of M4 \citep{kir1994}. |
. Assuming an absolute J magnitude of 5.6 for the hot subcwarl a MA spectral tvpe star with AZ,=8.6 would also be outshone by the hot subdwart. | Assuming an absolute $J$ magnitude of 5.6 for the hot subdwarf, a M4 spectral type star with $M_J = 8.6$ would also be outshone by the hot subdwarf. |
Llowever. the NSVS time series do not show variations down to a limit of Am=0.009. | However, the NSVS time series do not show variations down to a limit of $\Delta m = 0.009$. |
Hlumination of a 0.3AL. star. which is the suggested. mass at a high. inclination. would. cause a variation of Amoo~θε magnitudes. | Illumination of a $0.3\ M_\odot$ star, which is the suggested mass at a high inclination, would cause a variation of $\Delta m \sim 0.4$ magnitudes. |
Lower inclinations would require larger companions causing even larger variations that are incompatible with the observations. | Lower inclinations would require larger companions causing even larger variations that are incompatible with the observations. |
The lack of variability suggests. that. the companion is most likely a white dwarf. (κοςMaxted.Morales-Itueda.&Alarsh2004) | The lack of variability suggests that the companion is most likely a white dwarf \citep[see][]{max2004}. |
We show that GALEN | 4727 and GALEN 2349] 3844 are hot. hyvdrogen-rich subdwarfs in close binaries. | We show that GALEX $+$ 4727 and GALEX $+$ 3844 are hot hydrogen-rich subdwarfs in close binaries. |
Jed on a analysis of periodic light. variations in GALEN 1 ME4727 we infer that its companion is a low-mass star (A~0.13 AL.) | Based on a preliminary analysis of periodic light variations in GALEX $+$ 4727 we infer that its companion is a low-mass star $M\sim0.13\,M_\odot$ ). |
The secondary star in GALEN J2349| 3844. is probably a white dwarf with 0.3M... | The secondary star in GALEX $+$ 3844 is probably a white dwarf with $M\ga 0.3\, M_\odot$. |
Phe two new svstenis are post-CI5 systems with a hot subedwarf. primary. | The two new systems are post-CE systems with a hot subdwarf primary. |
Their orbital periods locate them close to. the peak of the period. distribution for such systems (seeHeber.2009). | Their orbital periods locate them close to the peak of the period distribution for such systems \citep[see][]{heb2009}. |
. AC future study of GALEN J032114727. will involve phase-resolved high signal-to-noise ratio spectroscopic and photometric observations aimed at resolving the nature of the companion. | A future study of GALEX $+$ 4727 will involve phase-resolved high signal-to-noise ratio spectroscopic and photometric observations aimed at resolving the nature of the companion. |
Searches for close binaries in the πα) population have a relatively high vieldl (6054.κουMaxtedetal. 2001).. and. therefore. we expect that many new systems remain to be discovered in our CALEN€SC catalogue of EB stars. | Searches for close binaries in the sdB population have a relatively high yield \citep[69\%, see][]{max2001}, and, therefore, we expect that many new systems remain to be discovered in our GALEX/GSC catalogue of EHB stars. |
S.V. and ur are by GA AV erant. numbers LAA300030908 ane LX:NOMini30901. respectively. ancl by CoA CRE erant der P20!ContreVOGT. | S.V. and A.K. are supported by GA AV grant numbers IAA300030908 and IAA301630901, respectively, and by GA ČRR grant number P209/10/0967. |
Ak. also acknowledges support from the for "Theoretical Astrophysics (LCOGOLL). | A.K. also acknowledges support from the Centre for Theoretical Astrophysics (LC06014). |
Some of the cata presented. in this paper were obtained from the Multimission Archive at the Space ‘Telescope Science Institute (ALAS). | Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). |
οσοι is operated by the Association of Universities Esearch in Astrononiv. Ine.. under NASA contract NAS5-26555. | STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. |
tor‘he Support for NLASTfor non-LIST datais provided by NASA Ollice of Space Science via erant NNXO9:APOSG and by other grants and contracts. | Support for MASTfor non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. |
he fugers-of-god. coutamination and completeness in filament samples fouud iu the mock M,<—20.5 galaxy distribution are ~26 aud ~SL per cout. respectively. | the fingers-of-god, contamination and completeness in filament samples found in the mock $M_r<-20.5$ galaxy distribution are $\sim 26$ and $\sim 81$ per cent, respectively. |
Galaxy clusters are muportaut for defining large-scale filaments aud should uot be removed before runniug he filament finder. | Galaxy clusters are important for defining large-scale filaments and should not be removed before running the filament finder. |
In redshift space aud on smoothing scales above ~10Ape. collapsing fingers-of-eo. o their mcan position produces mock filament samples comparable to those in real space. | In redshift space and on smoothing scales above $\sim 10$, collapsing fingers-of-god to their mean position produces mock filament samples comparable to those in real space. |
Tn this paper. we presented two volumce-lTHuüite subsauples from the northern portion of the SDSS spectroscopic survey (using the NYU-VACGC catalogue) and computed their filament distributions on 10 ux 15 ssinoothing scales. | In this paper, we presented two volume-limited subsamples from the northern portion of the SDSS spectroscopic survey (using the NYU-VAGC catalogue) and computed their filament distributions on $10$ and $15$ smoothing scales. |
These distributions were then directly compared to those found iu a series of recdshift-space mock galaxy catalogues generated from a cosimologica siauulatiou using the concordance cosnologv. | These distributions were then directly compared to those found in a series of redshift-space mock galaxy catalogues generated from a cosmological simulation using the concordance cosmology. |
The fluneut leneth distributions found iu/ SDSS data are very simular to those found iu mock catalogues ai are consistent with being drawn from an underline exponential distribution. | The filament length distributions found in SDSS data are very similar to those found in mock catalogues and are consistent with being drawn from an underlying exponential distribution. |
The width distributions of filament elements are also very simular between the SDSS data aud mock catalogues. suggesting that real filameuts are consistent with those in a ACDM universe having σε=O85. Q4=0,71. O,,=0.29. and =0.69. | The width distributions of filament elements are also very similar between the SDSS data and mock catalogues, suggesting that real filaments are consistent with those in a $\Lambda$ CDM universe having $\sigma_8=0.85$, $\Omega_\Lambda=0.71$, $\Omega_m=0.29$, and $h=0.69$. |
Tests on a range of cosimological simulations are needed before this can be turned iuto a cosmological constraiut. | Tests on a range of cosmological simulations are needed before this can be turned into a cosmological constraint. |
We also generated filament distributions at six redshifts in the output of a ACDM cosmological N-body simulation. from +=3 to ;=0. | We also generated filament distributions at six redshifts in the output of a $\Lambda$ CDM cosmological N-body simulation, from $z=3$ to $z=0$. |
The oricutation of the flament network is stable out to :=3 ou comoving smoothing scales at least as lavee as 15Mpe. | The orientation of the filament network is stable out to $z=3$ on comoving smoothing scales at least as large as $15$. |
. Most of the filaments detected on 15 scales at 2=0 can be detected at 2=3. | Most of the filaments detected on $15$ scales at $z=0$ can be detected at $z=3$. |
Iu addition. on a eiven comoving snoothing scale. filament width distributions shift to sinaller widths as the filameuts continue to collapse. | In addition, on a given comoving smoothing scale, filament width distributions shift to smaller widths as the filaments continue to collapse. |
Narrower filaments will collapse iore rapidly. so this also leads to a broadening of the width distributions. | Narrower filaments will collapse more rapidly, so this also leads to a broadening of the width distributions. |
We lave demoustrated that our filament finder is able to locate and follow real structures. perhaps most strikinely in L1. in which we showed that niu of the same structures could be seen iu a cosmological simulation at both τν=3 and :=0. | We have demonstrated that our filament finder is able to locate and follow real structures, perhaps most strikingly in \ref{subsec:FilEvolve}, , in which we showed that many of the same structures could be seen in a cosmological simulation at both $z=3$ and $z=0$. |
There is some subjective freedom in deciding what constitutes the eud ofa fibbunent. as no single physical threshold stands out as a cliscrinunator. | There is some subjective freedom in deciding what constitutes the end of a filament, as no single physical threshold stands out as a discriminator. |
Nevertheless. we demonstrated in 3.2 that the total length of the cosmic network is mseusitive to the choice of C above a certain scale-dependent threshold (ouce double cleteetions are removed). | Nevertheless, we demonstrated in \ref{subsubsec:Ct} that the total length of the cosmic network is insensitive to the choice of $C$ above a certain scale-dependent threshold (once double detections are removed). |
The iininuin value of C needed to probe the eutire fikuneut network may be telling us about theintrinsic clunpiuess of filamentary structure. aud may therefore be able to distinguish models of wari and cold dark matter. | The minimum value of $C$ needed to probe the entire filament network may be telling us about the clumpiness of filamentary structure, and may therefore be able to distinguish models of warm and cold dark matter. |
Iu this paper. we fully developed the SUALAFF algovitlin aud applied it to the low-redshitt galaxy distribution. but there is much that can still be learned οι its application to redshift surveys. | In this paper, we fully developed the SHMAFF algorithm and applied it to the low-redshift galaxy distribution, but there is much that can still be learned from its application to redshift surveys. |
The filament evolution seen in cosmological simulations (see L1)) can be tested in the DEEP? galaxy survey (7). at.—~1. and the results of this comparison have already Όσσα presented iu ο, | The filament evolution seen in cosmological simulations (see \ref{subsec:FilEvolve}) ) can be tested in the DEEP2 galaxy survey \citep{DEEP2} at $z \sim 1$, and the results of this comparison have already been presented in \citet{EnaFil}. |
On 25 aand /—10/5 sscales. they confirma a shift iu the filament width distribution to smaller widths from 2~0.8 to z0.1. as well as a broadening of the flament width distribution. | On $l=5$ and $l=10$ scales, they confirm a shift in the filament width distribution to smaller widths from $z \sim 0.8$ to $z \sim 0.1$ , as well as a broadening of the filament width distribution. |
A possible extension of this work is a careful test of the ACDAL cosinological model. including precision constraints ou cosmological parameters. such as es. aud tests for primordial non-Gaussianity usine the leusth distribution of filuueutarv structures. | A possible extension of this work is a careful test of the $\Lambda CDM$ cosmological model, including precision constraints on cosmological parameters, such as $\sigma_8$, and tests for primordial non-Gaussianity using the length distribution of filamentary structures. |
Iu addition. it would be useful to elaborate on the relationship of laree-scale filaments to salaxw clusters and to explore the properties of ealaxies in fBlaunents relative to the general ealaxv population. | In addition, it would be useful to elaborate on the relationship of large-scale filaments to galaxy clusters and to explore the properties of galaxies in filaments relative to the general galaxy population. |
Finally. it would boe interesting to conduct a careful search for walls in SDSS. | Finally, it would be interesting to conduct a careful search for walls in SDSS. |
Paper 1 hinted at their preseuce in the data. but they were only present at low contrast and the A-space distributions were nof optimal for ideutifviug individual walllike structures. | Paper $1$ hinted at their presence in the data, but they were only present at low contrast and the $\lambda$ -space distributions were not optimal for identifying individual wall-like structures. |
Funding for the SDSS aud SDSS-II has been provided bv the Alfred P. Sloan Foundation. the Participatiug Tustitutions. the National Science Foundation. the U.S. Department of Enerev. the National Acronautics aud Space Acuninistration. the Japanese \loubukagalasho. the Max Planck Society. and the IHigher. Education Funding Council for Enelaud. | 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:/Awww.scdss.ore/ The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. | The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. |
The Participating Tustitutious are the American Mauseuia of Natural Historv. Astrophysical Institute Potsdam. University of Basel. University of Cambridge. Case Western. Reserve University. Uuiversity of Chicago. Drexel Universitv. Fermilab. the Institute for Advauced Study. the Japan Participation Group. Jolus Hopkins University. the Joint Institute for Nuclear Astrophysics. the Ἱνανα Tustitute for Particle Astrophysics and Cosimnologv. the Iworean Scicutist Group. the Chinese Academy of Scicuces (LAMOST). Los Alamos National Laboratory. the AMas-Plauck-Institute for Astronomi (MIPTA). the Mas-Planck-Institute for Astroplivsics (AIPA). New Moxico. State University. Olio StateUniversity. University of Pittsburgh. University of Portsmouth. Princeton UWuiversity. theUuited States Naval Observatory. and the University of Washineton. | 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 StateUniversity, University of Pittsburgh, University of Portsmouth, Princeton University, theUnited States Naval Observatory, and the University of Washington. |
After all these considerations. the cooling rate due to IC scattering for electrons of energy E’ can be obtained by integrating in the photon energy [n and in energy of the scattered photon E%ο) where F(qy= 2q Ing + (1 4 2g = gi with I;24£7phΕ/Γ} and Proton interactions with the photon background can be an important cooling process. with à rate appoximated às Here. ειUrnh=150 MeV and we use the expressions" forc the cross section: c7,UD and the inelasticityῃD ΚονUD givenos in"un2. | After all these considerations, the cooling rate due to IC scattering for electrons of energy $E'$ can be obtained by integrating in the photon energy $E'_{\rm ph}$ and in energy of the scattered photon $E'_\gamma$: where F(q)= 2q q + (1 + 2q) (1 - q)+ - with $\Gamma'_{\rm e}=4 E'_{\rm ph}E'/(m_e^2c^4)$ and Proton interactions with the photon background can be an important cooling process, with a rate appoximated as Here, $\epsilon_{\rm th}^{(\pi)}=150$ MeV and we use the expressions for the cross section $\sigma_{p\gamma}^{(\pi)}$ and the inelasticity $K_{p\gamma}^{(\pi)}$ given in. |
. The energy distribution for each particle population is obtained as a solution to the following 1-D stationary transport equation22): This equation includes the effects of convection. with a speed ον-ο. and particle cooling with an energy loss b(E'.z)=dE'/dt. | The energy distribution for each particle population is obtained as a solution to the following $1$ -D stationary transport equation: + This equation includes the effects of convection with a speed $v_{\rm b}\sim c$, and particle cooling with an energy loss $b(E',z)=dE'/dt$. |
Particle decay with a timescale T4CE') ts also considered in the cases of secondary pions and muons,??). | Particle decay with a timescale $T_{\rm d}(E')$ is also considered in the cases of secondary pions and muons. |
The source term is given by a function Q'CE'.z). which in the case of primary particles is given by Eq. (6)). | The source term is given by a function $Q'(E',z)$ , which in the case of primary particles is given by Eq. \ref{Qep}) ), |
while for secondaries 1t 15 obtained using theparent particle distribution (N'(E'.z)) along with the secondary particle production rates (see Section ??)). | while for secondaries it is obtained using theparent particle distribution $N'(E',z)$ ) along with the secondary particle production rates (see Section \ref{subsubsec:pimu_prod}) ). |
We can solve the transport equation using the method of characteristics. 1.e.. writingwhere the first two terms allow us to find a characteristic curve MCz(£,.) for each pair (£’.2) of interest. | We can solve the transport equation using the method of characteristics, i.e., writingwhere the first two terms allow us to find a characteristic curve $z_c(E_c)$ for each pair $(E',z)$ of interest. |
Equating the second and third members it follows that As high energy protons interact with background matter and radiation. they produce pions. | Equating the second and third members it follows that As high energy protons interact with background matter and radiation, they produce pions. |
The pion injection dueto pp interactionsin thejet frame is calculated as where is the distribution of pions produced per pp collision. with v2 ELE. B,α+ 0.25. a!=3.67+0.83L 0.075L?. r'22.6/ Va’. and «e=0.98/Va"22). | The pion injection dueto $pp$ interactionsin thejet frame is calculated as where is the distribution of pions produced per $pp$ collision, with $x=
E'_\pi/E'$ , $ B_\pi=a'+ 0.25$ , $a'= 3.67+ 0.83 L+ 0.075 L^2$ , $r'=
2.6/\sqrt{a'}$ , and $\alpha= 0.98/\sqrt{a'}$. |
of these studies are biased toward the highly excited gas that does not necessarily trace the entire molecular gas reservoir seen in20). | of these studies are biased toward the highly excited gas that does not necessarily trace the entire molecular gas reservoir seen in. |
.. To overcome the limitations of previous studies. we have initiated a systematic study of the cconteut of ligh-: quasars aud other galaxy populations with the Expanded Very Large Array (EVLA: Perley et citevearperll)) aud the min Robert BByrd Green Bank Telescope (GBT). | To overcome the limitations of previous studies, we have initiated a systematic study of the content of $z$ quasars and other galaxy populations with the Expanded Very Large Array (EVLA; Perley et \\citeyear{per11}) ) and the m Robert Byrd Green Bank Telescope (GBT). |
Iu. this Letter. we report the detection of eenission toward five stronely leused 22 quasars. sie the EVLA aud the GBT. | In this Letter, we report the detection of emission toward five strongly lensed $z$$>$ 2 quasars, using the EVLA and the GBT. |
We use a coucordauce. flat ACDM cosmology throughout. with J7y=71 tb. 4,2027. and 420.73 (Spergel citevearspet3.. 20073). | We use a concordance, flat $\Lambda$ CDM cosmology throughout, with $H_0$ $^{-1}$, $\Omega_{\rm M}$ =0.27, and $\Omega_{\Lambda}$ =0.73 (Spergel \\citeyear{spe03}, \citeyear{spe07}) ). |
We observed the (eur=115.2712 GGIIz) emission line toward IRASFFIO0211]1721 (1—2.280). the Cloverleaf (1—2.5585). JJO911|0551 :—2.196). and 00751|2716 (223.200). using the EVLA. | We observed the $\nu_{\rm rest} = 115.2712$ GHz) emission line toward F10214+4724 $z$ =2.286), the Cloverleaf $z$ =2.558), J0911+0551 $z$ =2.796), and 0751+2716 $z$ =3.200), using the EVLA. |
At these redshifts. all lues are shüfted to the Na baud. cci: see Table 1 for vedshifted line frequeucies). | At these redshifts, all lines are shifted to the Ka band cm; see Table \ref{t1} for redshifted line frequencies). |
Observations were carried out wader good weather conditions iu six D array tracks between 2009 October 26 aud December 09. anc ou 2010 July 17 aud 18. | Observations were carried out under good weather conditions in six D array tracks between 2009 October 26 and December 09, and on 2010 July 17 and 18. |
This resulted in 5.0. 1.0. 12.0. aud L.Ohbr (2.1. 0.6. 5.1. and 0.6hhir) total (o11-501rcc) observing time for FF1021111721. the Cloverleaf. RXJJO91110551. and 0075112716. respectively. | This resulted in 5.0, 1.0, 12.0, and hr (2.1, 0.6, 5.1, and hr) total (on-source) observing time for F10214+4724, the Cloverleaf, J0911+0551, and 0751+2716, respectively. |
For IRASFEF10211]1721. and JJOO01110551. an additional 0.9 aud 2.3hhr on source were spent on separate continuun settings. | For F10214+4724 and J0911+0551, an additional 0.9 and hr on source were spent on separate continuum settings. |
The nearby quasars JOOSS|1725. 31115|1320. J0909|0121. and JO?Ls|2400 were observed every 3.5 to Taundautes for poiuting. secondary amplitude aud phase calibration. | The nearby quasars J0958+4725, J1415+1320, J0909+0121, and J0748+2400 were observed every 3.5 to minutes for pointing, secondary amplitude and phase calibration. |
For primary flux calibration. the standard calibrators 3C286 aud 3CLLIT were observed. leading to a calibration that is accurate within —10'4.. | For primary flux calibration, the standard calibrators 3C286 and 3C147 were observed, leading to a calibration that is accurate within $\sim$. |
Observatious for the Cloverleaf aud 00751|2716 were carried out with the WIDAR correlator. using two intermediate frequencies (Fs) of MMIIZz. (dual polarization) each at 2MMIIz resolution. | Observations for the Cloverleaf and 0751+2716 were carried out with the WIDAR correlator, using two intermediate frequencies (IFs) of MHz (dual polarization) each at MHz resolution. |
For the Cloverleaf. the two IEs were overlapped by two cliauncls. centered on the CO line. vielding MMIIz contiguous bandwidth. | For the Cloverleaf, the two IFs were overlapped by two channels, centered on the CO line, yielding MHz contiguous bandwidth. |
For 00751]2716. one IF was ceutered ou the CO line. aud the secoud IF was centered ou the contimmu at CCIz. | For 0751+2716, one IF was centered on the CO line, and the second IF was centered on the continuum at GHz. |
Observations for IRASFEF102111|ΙΤ. and. JJOOLL|O551 (Gvehich. have narrow CO lines) were carried out with the previous ecucration correlator. with two MMIIz (dual polarization) IEs at MAMI2 resolution. | Observations for F10214+4724 and J0911+0551 (which have narrow CO lines) were carried out with the previous generation correlator, with two MHz (dual polarization) IFs at MHz resolution. |
For IRASFFLO201)1721. both TFs were centered on the CO line. vielding MMITZ contiguous bandwidth. | For F10214+4724, both IFs were centered on the CO line, yielding MHz contiguous bandwidth. |
For JJO9LL|0551. one IE was ceutered on the CO line. aud the second DIF was centered on the contimmum at GGIIz. | For J0911+0551, one IF was centered on the CO line, and the second IF was centered on the continuum at GHz. |
For these two sources. one third of the on-source time was spent to observe a second frequency sctting with two AIANTz contimmuu IEs offset by E150 MMIIz from the CO lines. vielding more scusitive constraints on the continu CLUISSIOL. | For these two sources, one third of the on-source time was spent to observe a second frequency setting with two MHz continuum IFs offset by $\pm$ MHz from the CO lines, yielding more sensitive constraints on the continuum emission. |
For data reduction and analysis. the AIPS package was used. | For data reduction and analysis, the AIPS package was used. |
All data were mapped using "natural weiehtine. | All data were mapped using `natural' weighting. |
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