J/A+A/564/A85ivo://CDS.VizieR/J/A+A/564/A85doi:10.26093/cds/vizier.35640085CDSMuriel H.Coenda V.2014-08-05T19:57:38Z2014-07-23T12:52:45ZCDS support team

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

cds-question@unistra.frgalaxy-clustersx-ray-sourcesredshiftedgalaxy-kinematicsWe explore the properties of galaxies on the outskirts of clusters and their dependence on recent dynamical history in order to understand the real impact that the cluster core has on the evolution of galaxies. We analyse the properties of more than 1000 galaxies brighter than M_r_^0.1^=-19.6 on the outskirts of 90 clusters (1<r/r_vir_<2) in the redshift range 0.05<z<0.10. Using the line of sight velocity of galaxies relative to the cluster's mean, we selected low and high velocity subsamples. Theoretical predictions indicate that a significant fraction of the first subsample should be backsplash galaxies, that is, objects that have already orbited near the cluster centre. A significant proportion of the sample of high relative velocity (HV) galaxies seems to be composed of infalling objects. Our results suggest that, at fixed stellar mass, late-type galaxies in the low-velocity (LV) sample are systematically older, redder, and have formed fewer stars during the last 3Gyrs than galaxies in the HV sample. This result is consistent with models that assume that the central regions of clusters are effective in quenching the star formation by means of processes such as ram pressure stripping or strangulation. At fixed stellar mass, LV galaxies show some evidence of having higher surface brightness and smaller size than HV galaxies. These results are consistent with the scenario where galaxies that have orbited the central regions of clusters are more likely to suffer tidal effects, producing loss of mass as well as a re-distribution of matter towards more compact configurations. Finally, we found a higher fraction of ET galaxies in the LV sample, supporting the idea that the central region of clusters of galaxies may contribute to the transformation of morphological types towards earlier types.2014A&A...564A..85Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/564/A85CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJS/129/435 : NORAS galaxy cluster survey. I. (Bohringer+, 2000)J/A+A/504/347 : Galaxy properties in clusters (Coenda+, 2009)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/A+A/564/A85https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/564/A85http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/564/A85https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/564/A85https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/564/A85http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/564/A85GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/564/A85/table1 (The C-B00-I cluster sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/564/A85/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/564/A85/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/564/A85/table1?GETtext/xml+votable180.050000true111.46166741.3813060.0055555555555555566/4394 4665 5030 5161 5227 5250 5327 5438 5524 5536 5585 5715 6247 6494 6603 6655 6740 7536 8258 8608 8788 8823 8832 8866 8919 8970 9047 9168 9354 9366 9478 9508 10271 10312 10318 10594 10679 10691 10717 11195 11287 11443 22007 26048 27676 27736 27765 28005 28265 28430 28453 28477 28534 32445 32683https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/564/A85?format=asciiX-rayOpticaldefaultJ/A+A/564/A85/table1The C-B00-I cluster samplez[0.04/0.18] Redshiftsrc.redshiftfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainsigmaVelocity dispersionkm/sphys.veloc.dispersionfloatMvirVirial mass (in M_{sun}_/h, Ho=70km/s/Mpc)solMassphys.massdoubleRvirVirial radius (in Mpc/h)Mpcphys.size.radiusfloatR200Radius at the mean density of 200 times the mean density of the universe (in Mpc/h)Mpcphys.size.radiusfloatB00Display the NORAS data (Bohringer et al. 2000 Cat. J/ApJS/129/435)meta.ref.urlchar