J/A+A/570/A69ivo://CDS.VizieR/J/A+A/570/A69doi:10.26093/cds/vizier.35700069CDSBoselli A.Voyer E.Boissier S.Cucciati O.Consolandi G.Cortese L.,Fumagalli M.Gavazzi G.Heines S.Roehlly Y.Toloba E.2017-12-15T10:55:09Z2014-10-20T08:54:43ZCDS support team

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

cds-question@unistra.frgalaxy-clustersultraviolet-astronomyWe study the role of the environment on galaxy evolution using a sample of 868 galaxies in the Virgo cluster and in its surrounding regions that are selected from the GALEX Ultraviolet Virgo Cluster Survey (GUViCS) with the purpose of understanding the origin of the red sequence in dense environments. The sample spans a wide range in morphological types (from dwarf ellipticals to Im and BCD) and stellar masses (10^7^<=M_star_<=10^11.5^M_{sun}_). We collected multifrequency data covering the whole electromagnetic spectrum for most of the galaxies, including UV, optical, mid- and far-infrared imaging data, as well as optical and HI spectroscopic data. We first identify the different dynamical substructures that compose the Virgo cluster, and we calculate the local density of galaxies using different methods. We then study the distribution of galaxies belonging to the red sequence, the green valley, and the blue cloud within the different cluster substructures or as a function of galaxy density. Our analysis indicates that all the most massive galaxies M_star_>=10^11^M_{sun}_) are slow rotators and are the dominant galaxies of the different cluster substructures, which are generally associated with a diffuse X-ray emission. They are probably the result of major merging events that occurred at early epochs, as also indicated by their very old stellar populations. Slow rotators of lower stellar mass (10^8.5^<=M_star_<=10^11^M_{sun}_) are also preferentially located within the different high-density substructures of the cluster. Their position in the velocity space indicates that they are virialised within the cluster; thus, they are Virgo members since its formation. They have been shaped by gravitational perturbations occurring within the infalling groups that later form the cluster (pre-processing). On the contrary, low-mass star-forming systems are extremely rare in the inner regions of the Virgo cluster A, where the density of the intergalactic medium is at its maximum. Our ram pressure stripping models consistently indicate that these star-forming systems can be rapidly deprived of their interstellar medium during their interaction with the intergalactic medium. The lack of gas quenches their star-formation activity transforming them into quiescent dwarf ellipticals. This mild transformation does not perturb the kinematic properties of these galaxies, which still have rotation curves typical of star-forming systems.2014A&A...570A..69Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/570/A69CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/528/A107 : GALEX Ultraviolet Virgo Cluster Survey (Boselli+, 2011)J/A+A/569/A124 : GUViCS. Ultraviolet Source Catalogs (Voyer+, 2014)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/570/A69https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/570/A69http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/570/A69https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/570/A69https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/570/A69http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/570/A69GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/570/A69/tablea1 (The WISE 22 micron data)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/570/A69/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/570/A69/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/570/A69/tablea1?GETtext/xml+votable180.050000true179.605420.706880.0055555555555555564/1732-1733 1735 1741 1744 1746 1752 5/6567 6571-6573 6575-6576 6580 6582 6584 6586-6587 6589-6591 6635 6917 6937-6939 6973 6980 7016 7018 6/26175 26217 26220 26222-26223 26232 26234 26261 26263 26265-26267 26277 26279 26281-26282 26297-26299 26308-26309 26311-26314 26316 26318-26319 26324 26326 26332-26333 26335 26340 26342-26343 26354-26355 26528-26529 26537-26539 26554-26555 27648-27649 27652-27654 27661 27663-27664 27672 27674 27677 27679 27711 27745 27747 27841 27843 27845-27847 27853 27855 27889-27891 27900-27901 27903 27926 27928-27929 27931-27932 27934 27954-27956 27958-27960 27962-27963 27967 28002-28003 28008-28010 28048-28050 28054 28056-28058 28068-28070 280768.157980699529898e-21 9.827027931427413e-21https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/570/A69?format=asciiUVdefaultJ/A+A/570/A69/tablea1The WISE 22 micron dataSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGalaxy namemeta.id;meta.maincharRAJ2000Right Ascension (J2000.0)degpos.eq.ra;meta.mainDEJ2000Declination (J2000.0)degpos.eq.dec;meta.mainaAperture major axis radiusarcsecphys.angSizefloatbAperture minor axis radiusarcsecphys.angSize;srcfloatPA[0/360] Position angle measured from north clockwisedegpos.posAngintf_S22um[0/1] Flag indicating galaxy detected (1) or undetected (0, S22um is an upper limit)meta.codeintS22umFlux density (or upper limit if no error) at 22ummJyphot.flux.density;em.IR.15-30umfloate_S22um? Uncertainty on the flux densitymJystat.errorfloatnullableGUViCSDisplay the Voyer et al. 2014 (J/A+A/569/A124) datameta.ref.urlchar