J/A+A/607/A81ivo://CDS.VizieR/J/A+A/607/A81doi:10.26093/cds/vizier.36070081CDSBiviano A.Moretti A.Paccagnella A.Poggianti B.M.Bettoni D.,Gullieuszik M.Vulcani B.Fasano G.D'Onofrio M.Fritz J.Cava A.2018-01-11T11:19:47Z2018-01-11T12:18:07ZCDS support team

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

cds-question@unistra.frgalaxy-clustersgalaxy-kinematicsgalaxy-classification-systemsThe relation between a cosmological halo concentration and its mass (cMr) is a powerful tool to constrain cosmological models of halo formation and evolution. On the scale of galaxy clusters the cMr has so far been determined mostly with X-ray and gravitational lensing data. The use of independent techniques is helpful in assessing possible systematics. Here we provide one of the few determinations of the cMr by the dynamical analysis of the projected-phase-space distribution of cluster members. Based on the WINGS and OmegaWINGS data sets, we used the Jeans analysis with the MAMPOSSt technique to determine masses and concentrations for 49 nearby clusters, each of which has >~60 spectroscopic members within the virial region, after removal of substructures. Our cMr is in statistical agreement with theoretical predictions based on {LAMBDA}CDM cosmological simulations. Our cMr is different from most previous observational determinations because of its flatter slope and lower normalization. It is however in agreement with two recent cMr obtained using the lensing technique on the CLASH and LoCuSS cluster data sets. The dynamical study of the projected-phase-space of cluster members is an independent and valid technique to determine the cMr of galaxy clusters. Our cMr shows no tension with theoretical predictions from {LAMBDA}CDM cosmological simulations for low-redshift, massive galaxy clusters. In the future we will extend our analysis to galaxy systems of lower mass and at higher redshifts.2017A&A...607A..81Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/607/A81CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/581/A41 : OmegaWINGS BV photometry of galaxy clusters (Gullieuszik+ 2015)J/A+A/599/A81 : OmegaWINGS local clusters of galaxies redshifts (Moretti+ 2017)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/607/A81https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/607/A81http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/607/A81https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/607/A81https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/607/A81http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/607/A81GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/607/A81/table1 (Properties of 49 clusters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/607/A81/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/607/A81/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/607/A81/table1?GETtext/xml+votable180.050000true10.3613-9.3030.0055555555555555566/1006 5030 5305 8268 8442 8648 8788 9776 10312 15085 16410 16434 16492 16767 17237 18009 18016 18324 18411 18607 18622 18939 19130 19204 19993 20021 20083 20483 24943 25042 26734 26770 27224 33235 33628 33649 34805 39077 40809 43830 43835 43838 43939 43948 45981 45984 46652 46911 48594https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/607/A81?format=asciiOpticaldefaultJ/A+A/607/A81/table1Properties of 49 clustersSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClusterCluster namemeta.id;meta.maincharRAJ2000Right-ascension of the BCG (adopted as cluster center) (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of the BCG (J2000)degpos.eq.dec;meta.mainNzNumber of galaxies with measured redshift in the cluster fieldmeta.numberintNmNumber of cluster members before removal of galaxies in subclustersmeta.numberintNmnsFinal number of cluster members after removal of galaxies in subclustersmeta.numberintNdynNumber of cluster members effectively used in the dynamical analysis, i.e. those located between 0.05 Mpc and r200meta.numberintRmaxLargest distance from the BCG among cluster members outside substructuresMpcpos.distancefloatzcMean cluster redshiftsrc.redshiftdoublesigmalosCluster velocity dispersionkm/sphys.veloc.dispersioninte_sigmalosLower 1 sigma error on sigmaloskm/sstat.errorintE_sigmalosUpper 1 sigma error on sigmaloskm/sstat.error;stat.maxintnRmodModel, pNFW or King, which provides the best fit to the cluster galaxy number density profilestat.param;meta.modelledcharrgBest-fit value of the scale radius of the cluster galaxy number density profileMpcphys.size.radiusfloate_rgLower 1 sigma error on rgMpcstat.errorfloatE_rgUpper 1 sigma error on rgMpcstat.error;stat.maxfloatMrmodModel, Burkert, Hernquist, or NFW, which provides the best fit to the cluster mass profilemeta.id;stat.fitcharr200Best-fit value of the virial radiusMpcphys.size.radius;meta.modelledfloate_r200Lower 1 sigma error on r200Mpcstat.errorfloatE_r200Upper 1 sigma error on r200Mpcstat.error;stat.maxfloatrm2Best-fit value of the mass profile scale radiusMpcphys.size.radiusfloate_rm2Lower 1 sigma error on rm2Mpcstat.errorfloatE_rm2Upper 1 sigma error on rm2Mpcstat.error;stat.maxfloat