J/MNRAS/441/203ivo://CDS.VizieR/J/MNRAS/441/203doi:10.26093/cds/vizier.74410203CDSDelaye L.Huertas-Company M.Mei S.Lidman C.Licitra R.Newman A.,Raichoor A.Shankar F.Barrientos F.Bernardi M.Cerulo P.Couch W.,Demarco R.Munoz R.Sanchez-Janssen R.Tanaka M.2024-08-09T20:14:58Z2015-05-04T11:07:48ZCDS support team

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

cds-question@unistra.frgalaxy-clustersgalaxiesvisible-astronomygalaxy-classification-systemsWe analyse the mass-size relation of ~400 quiescent massive ETGs (M*/M_{sun}_>3x10^10^) hosted by massive clusters (M200~2-7x10^14^M_{sun}_) at 0.8<z<1.5, compared to those found in the field at the same epoch. Size is parametrized using the mass-normalized B-band rest-frame size, {gamma}=R_e_/M_11_^0.57^. We find that the {gamma} distributions in both environments peak at the same position, but the distributions in clusters are more skewed towards larger sizes. This tail induces average sizes ~ 30-40 percent larger for cluster galaxies than for field galaxies of similar stellar mass, while the median sizes are statistically the same with a difference of ~10+/-10%. Since this size difference is not observed in the local Universe, the evolution of average galaxy size at fixed stellar mass from z~1.5 for cluster galaxies is less steep at more than 3{sigma}({prop.to}(1+z)-0.53+/-0.04) than the evolution of field galaxies ({prop.to}(1+z)-0.92+/-0.04). The difference in evolution is not measured when the median values of {gamma} are considered: {prop.to}(1+z)-0.84+/-0.04 in the field versus {prop.to}(1+z)-0.71+/-0.05 in clusters. In our sample, the tail of large galaxies is dominated by galaxies with 3x10^10^<M*/M_{sun}_<10^11^. At this low-mass end, the difference in the average size is better explained by the accretion of new galaxies that are quenched more efficiently in clusters and/or by different morphological mixing in the cluster and field environments. If part of the size evolution would be due to mergers, the difference that we see between cluster and field galaxies could be caused by higher merger rates in clusters at higher redshift, when galaxy velocities are lower.2014MNRAS.441..203Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/441/203CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AJ/125/1817 : SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)J/MNRAS/422/494 : Optically selected ETGs X-ray properties (Danielson+, 2012)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/441/203https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/441/203http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/441/203https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/441/203https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/441/203http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/441/203GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/441/203/tableb1 (Catalogue of red sequence early-type galaxies)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/441/203/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/441/203/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/441/203/tableb1?GETtext/xml+votable180.050000true28.1795-14.00010.0055555555555555566/16418 16424 17472 17689 17694 18795 26292 43945 43947 47053 48478-48479https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/441/203?format=asciiOpticaldefaultJ/MNRAS/441/203/tableb1Catalogue of red sequence early-type galaxiesID[157/4319] Galaxy Sequential numbermeta.recordintprimaryRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainClusterCluster short designation (1)meta.id.parentcharlogM[10.5/11.59] Mass of galaxylog(solMass)phys.massfloate_logMrms uncertainty on Masslog(solMass)stat.errorfloatRe[0.8/13] Effective radius of galaxykpcphys.size.radiusfloate_Rerms uncertainty on Rekpcstat.errorfloatn[0.7/8] Sersic indexstat.fit.paramfloate_n? rms uncertainty on nstat.errorfloatnullableb/a[0/1] Axis ratiophys.angSize;arith.ratiofloate_b/a? rms uncertainty on b/astat.errorfloatnullablep(ETG)[0.5/1] Probability of early-type galaxystat.fit.goodnessfloat