J/ApJ/750/93ivo://CDS.VizieR/J/ApJ/750/93doi:10.26093/cds/vizier.17500093CDSPapovich C.Bassett R.Lotz J.M.van der Wel A.Tran K.-V.,Finkelstein S.L.Bell E.F.Conselice C.J.Dekel A.Dunlop J.S.Guo Y.,Faber S.M.Farrah D.Ferguson H.C.Finkelstein K.D.Haussler B.,Kocevski D.D.Koekemoer A.M.Koo D.C.McGrath E.J.McLure R.J.,McIntosh D.H.Momcheva I.Newman J.A.Rudnick G.Weiner B.,Willmer C.N.A.Wuyts S.2017-09-29T09:02:29Z2014-01-20T14:20:35ZCDS support team

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

cds-question@unistra.frgalaxy-clustersinfrared-photometrygalaxiesinfrared-sourcesredshiftedWe discuss the structural and morphological properties of galaxies in a z=1.62 proto-cluster using near-IR imaging data from Hubble Space Telescope Wide Field Camera 3 data of the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). The cluster galaxies exhibit a clear color-morphology relation: galaxies with colors of quiescent stellar populations generally have morphologies consistent with spheroids, and galaxies with colors consistent with ongoing star formation have disk-like and irregular morphologies. The size distribution of the quiescent cluster galaxies shows a deficit of compact (<~1kpc), massive galaxies compared to CANDELS field galaxies at z=1.6. As a result, the cluster quiescent galaxies have larger average effective sizes compared to field galaxies at fixed mass at greater than 90% significance. Combined with data from the literature, the size evolution of quiescent cluster galaxies is relatively slow from z=~1.6 to the present, growing as (1+z)^-0.6+/-0.1^. If this result is generalizable, then it implies that physical processes associated with the denser cluster region seem to have caused accelerated size growth in quiescent galaxies prior to z=1.6 and slower subsequent growth at z<1.6 compared to galaxies in the lower density field. The quiescent cluster galaxies at z=1.6 have higher ellipticities compared to lower redshift samples at fixed mass, and their surface-brightness profiles suggest that they contain extended stellar disks. We argue that the cluster galaxies require dissipationless (i.e., gas-poor or "dry") mergers to reorganize the disk material and to match the relations for ellipticity, stellar mass, size, and color of early-type galaxies in z<1 clusters.2012ApJ...750...93Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/750/93CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toB/hst : HST Archived Exposures Catalog (STScI, 2007)II/319 : UKIDSS-DR9 LAS, GCS and DXS Surveys (Lawrence+ 2012)J/ApJS/206/10 : CANDELS multiwavelength catalog (Galametz+, 2013)J/MNRAS/427/1666 : Massive galaxies in CANDELS-UDS field (Bruce+, 2012)J/ApJS/203/24 : Structural parameters of CANDELS galaxies (van der Wel+, 2012)J/ApJ/742/111 : Extreme emission-line galaxies in CANDELS (van der Wel+, 2011)J/ApJS/176/1 : Subaru/XMM-Newton deep survey (SXDS). II. (Furusawa+, 2008)http://candels.ucolick.org/data_access/UDS.html : CANDELS UDS Data Releasehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/750/93https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/750/93http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/750/93https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/750/93https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/750/93http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/750/93GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/750/93/table1 (Properties of z=1.6 galaxy samples in the UDS CANDELS field)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/750/93/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/750/93/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/750/93/table1?GETtext/xml+votable180.050000true34.58987-5.174870.0055555555555555566/17679 176901.4096873584774176e-19 1.7721910056019106e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/750/93?format=asciiOpticalInfrareddefaultJ/ApJ/750/93/table1Properties of z=1.6 galaxy samples in the UDS CANDELS fieldrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[28489/45319] Object identification number <[PBL2012] NNNNN> in Simbadmeta.id;meta.mainintRAJ2000[34.2/34.6] Right Ascension (J2000)degpos.eq.ra;meta.mainDEJ2000[-5.3/-5.1] Declination (J2000)degpos.eq.dec;meta.mainzph[1.4/1.9] Photometric redshiftsrc.redshiftfloatPz[0/1] Integrated photometric redshift probability distribution function (1)stat.fit.goodnessfloatz-J[0.4/2.4] (Suprime z-UKIDSS J) color indexmagphot.color;em.IR;em.IRfloatJ-3.6[-0.7/3.2]? (UKIDSS J-Spitzer/IRAC 3.6um) color indexmagphot.color;em.IR;em.IRfloatnullableJmag[20.6/35.4] HST/WFC3 F125W band magnitude measured from GALFITmagphot.mag;em.IR.JfloatReff[0/41] Circularized effective radiuskpcphys.size.radiusfloate_Reff[0.1/33] Uncertainty in Reffkpcstat.errorfloatn[0/20] Sersic indexstat.fit.paramfloate_n[0.1/9] Uncertainty in nstat.errorfloatEll[0/0.83] Ellipticity (Ell=1-b/a)src.ellipticityfloatlogM*[8.2/11.5]? Log of stellar masslog(solMass)phys.massfloatnullableE_logM*[0.03/0.7]? Uncertainty in logM*log(solMass)stat.error;stat.maxfloatnullablee_logM*[0.03/0.8]? Uncertainty in logM*log(solMass)stat.errorfloatnullablel_logPhiLimit flag on logPhimeta.code.errorcharlogPhi[-1/3.5]? Log star formation rate (2)log(solMass.yr**-1)meta.idfloatnullableRproj[0.04/11.3] Projected distance (3)Mpcpos.distancefloatCCatCross-match with CANDELS catalogs (Cats J/ApJS/206/10, J/ApJS/203/24) within 0.5"meta.ref.urlintnullableSimbadSimbad column added by the CDSmeta.ref.urlchar