J/AJ/132/1275ivo://CDS.VizieR/J/AJ/132/1275doi:10.26093/cds/vizier.51321275CDSRines K.Diaferio A.2017-06-19T07:57:02Z2008-07-09T21:26:32ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxy-clustersgalaxy-classification-systemsredshiftedgalaxy-kinematicsWe use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.2006AJ....132.1275Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/132/1275CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/301/881 : The ROSAT brightest cluster sample - I. (Ebeling+, 1998)J/A+A/425/367 : REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)J/MNRAS/318/333 : Extended ROSAT Bright Cluster Sample (Ebeling+ 2000)J/ApJS/129/435 : NORAS galaxy cluster survey. I. (Bohringer+, 2000)http://www.sdss.org : SDSS Home Pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/132/1275https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/132/1275http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/132/1275https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/132/1275https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/132/1275http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/132/1275GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/132/1275/table1 (CIRS Basic Properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/132/1275/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/132/1275/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/132/1275/table1?GETtext/xml+votable180.050000true10.4588-9.30190.005555555555555556Cone search capability for table J/AJ/132/1275/table3 (CIRS Hierarchical Centers and Offsets)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/132/1275/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/132/1275/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/132/1275/table3?GETtext/xml+votable180.050000true10.42629-9.42550.0055555555555555566/4990 5030 5370 5373 5438 5524 5618 5715 5982 5996 6002 6039 6223 7187 8196 9047 9072 9354 9366 9443 9468 9471 9504 9506 9508 9776 9943 9983 10154 10182 10679 10691 11182 11287 11591 11809 17237 17300 17513 17515 17810 18009 18016 18019 18411 18585 18607 19432 19993 21977 25852 25981 26042 26185 26188 26197 26208 26209 26302 26313 26432 26525 26563 26568 27079 27081 27224 27225 27420 27486 27652 27676 27685 27760 27765 27767 31406https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/132/1275?format=asciiOpticaldefaultJ/AJ/132/1275/table1CIRS Basic PropertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameCluster namemeta.id;meta.maincharRAJ2000Right Ascension in decimal degrees (J2000)degpos.eq.ra;meta.mainDEJ2000Declination in decimal degrees (J2000)degpos.eq.dec;meta.mainzHeliocentric redshiftsrc.redshiftfloatLXX-ray luminosity in units of 10^43^erg/s (1)1e+36Wphys.luminosity;em.X-raycharCatX-ray cluster catalog (2)meta.notecharTXX-ray temperaturekeVphys.temperaturefloatsigProjected velocity dispersionkm/sphys.veloc.dispersionintE_sigUpper limit uncertainty in sigkm/sstat.error;stat.maxinte_sigLower limit uncertainty in sigkm/sstat.errorintCl[0/2] Contrast of caustics (3)src.classintRcProjected radius of nearest edge of SDSS DR4 spectra (4)phys.angSize;srcfloatSimbadNameSimbad column added by the CDSmeta.idcharNEDSimbad column added by the CDScharJ/AJ/132/1275/table3CIRS Hierarchical Centers and OffsetsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameCluster namemeta.id;meta.maincharRAJ2000Hierarchical center Right Ascension in decimal degrees (J2000)degpos.eq.ra;meta.mainDEJ2000Hierarchical center Declination in decimal degrees (J2000)degpos.eq.dec;meta.mainDelczHierarchial and X-ray redshift center differencekm/sphys.veloc;arith.diffintDelRHierarchial and X-ray position difference, in h^-1^kpc unitskpcpos.distanceintJ/AJ/132/1275/table46CIRS Characteristic Radii and Masses, Virial and Projected MassesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameCluster namemeta.id;meta.maincharr500Radius at 500 times critical density, in h^-1^Mpc unitsMpcphys.size.radiusfloatr200Radius at 200 times critical density, in h^-1^Mpc unitsMpcphys.size.radiusfloatrtTurnaround radius, in h^-1^Mpc unitsMpcmeta.unit;phys.size.radiusfloatrmaxMaximum caustic extent, in h^-1^Mpc unitsMpcmeta.unit;phys.angSize;stat.maxfloatM200Mass within the r200 radius1e+14solMassphys.massfloate_M200Uncertainty in M2001e+14solMassstat.errorfloatMtMass within the rt radius1e+14solMassphys.massfloate_MtUncertainty in Mt1e+14solMassstat.errorfloatRatioRatio of the mass within rmax and r200phys.mass;arith.ratiofloatMProjProjected mass1e+14solMassphys.massfloate_MProjUncertainty in MProj1e+14solMassstat.errorfloatMVirVirial mass1e+14solMassphys.massfloate_MVirUncertainty in MVir1e+14solMassstat.errorfloatJ/AJ/132/1275/table5CIRS Mass Profile Fit ParametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameCluster namemeta.id;meta.maincharaNFWThe NFW scale radius, in h^-1^Mpc unitsMpcmeta.unitfloatr200Radius at 200 times critical density, in h^-1^Mpc unitsphys.size.radiusfloatcNFWThe NFW concentration; r200/aNFWmeta.notefloatM200Mass within the r200 radius1e+14solMassphys.massfloatPro[HNS] Best-fit profile (1)stat.fit.paramcharc101Concentration, r101/aNFWmeta.notefloat