J/A+A/533/A142ivo://CDS.VizieR/J/A+A/533/A142doi:10.26093/cds/vizier.35330142CDSBitsakis T.Charmandaris V.da Cunha E.Diaz-Santos T.le Floc'h E.,Magdis G.2017-06-26T11:50:04Z2011-09-16T09:44:23ZCDS support team

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

cds-question@unistra.frgalaxiesinfrared-sourcesinfrared-photometryvisible-astronomysloan-photometryultraviolet-astronomybroad-band-photometryWe present a comprehensive study on the impact of the environment of compact galaxy groups on the evolution of their members using a multi-wavelength analysis, from the UV to the infrared, for a sample of 32 Hickson compact groups (HCGs) containing 135 galaxies. Fitting the SEDs of all galaxies with the state-of-the-art model of da Cunha (2008MNRAS.388.1595D) we can accurately calculate their mass, SFR, and extinction, as well as estimate their infrared luminosity and dust content. We compare our findings with samples of field galaxies, early-stage interacting pairs, and cluster galaxies with similar data. We find that classifying the groups as dynamically "old" or "young", depending on whether or not at least one quarter of their members are early-type systems, is physical and consistent with past classifications of HCGs based on their atomic gas content. Dynamically "old" groups are more compact and display higher velocity dispersions than "young" groups. Late-type galaxies in dynamically "young" groups have specific star formation rates (sSFRs), NUV-r, and mid-infrared colors which are similar to those of field and early stage interacting pair spirals. Late-type galaxies in dynamically "old" groups have redder NUV-r colors, as they have likely experienced several tidal encounters in the past building up their stellar mass, and display lower sSFRs. We identify several late-type galaxies which have sSFRs and colors similar to those of elliptical galaxies, since they lost part of their gas due to numerous interactions with other group members. Also, 25% of the elliptical galaxies in these groups have bluer UV/optical colors than normal ellipticals in the field, probably due to star formation as they accreted gas from other galaxies of the group, or via merging of dwarf companions. Finally, our SED modeling suggests that in 13 groups, 10 of which are dynamically "old", there is diffuse cold dust in the intragroup medium. All this evidence point to an evolutionary scenario in which the effects of the group environment and the properties of the galaxy members are not instantaneous. Early on, the influence of close companions to group galaxies is similar to the one of galaxy pairs in the field. However, as the time progresses, the effects of tidal torques and minor merging, shape the morphology and star formation history of the group galaxies, leading to an increase of the fraction of early-type members and a rapid built up of the stellar mass in the remaining late-type galaxies.2011A&A...533A.142Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/533/A142CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toVII/213 : Hickson's Compact groups of Galaxies (Hickson+ 1982-1994)VII/248 : Quasars and Active Galactic Nuclei (12th Ed.) (Veron+ 2006)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/533/A142https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/533/A142http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/533/A142https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/533/A142https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/533/A142http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/533/A142GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/533/A142/catalog (HCG galaxies studied; fluxes, morphology, derived physical parameters and nearest neighbor parameters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/533/A142/catalog?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/533/A142/catalog?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/533/A142/catalog?GETtext/xml+votable180.050000true7.84933338.46703330.0055555555555555566/4215 4447 4469 4966 5970 7547 8557 8627 8935 9417 10637 13511 16784 17245 17492 17866 18071 18757 19538 19626 19661 23182 25721 25769 27174 27620 27872 28269 28278 28515 36621 40294 470271.086335461506279e-21 1.4134638842407062e-18https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/533/A142?format=asciiUVOpticalInfrareddefaultJ/A+A/533/A142/catalogHCG galaxies studied; fluxes, morphology, derived physical parameters and nearest neighbor parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHCGHCG galaxy namemeta.id;meta.maincharn_HCG[*+- ] Note on galaxy (1)meta.notecharMTypeMorphological typesrc.morph.typecharSEDSED plot of this galaxymeta.ref.urlcharchi2chi^2^ valuestat.fit.chi2floattauObsObserved optical depthphys.absorption.opticalDepthfloattauISMDiffuse ISM optical depth V,ISMphys.absorption.opticalDepthfloattauTotal optical depth (tauBC+tauISM) (2)phys.absorption.opticalDepthfloatMstarStellar Mass1e+09solMassphys.massfloatSFRStar formation ratesolMass/yrphys.SFRfloatsSFRSpecific star formation rate1e-11yr**-1phys.SFRfloatLIRInfrared luminosity1e+09solLumphys.luminosity;em.IRfloatNucNuclear classification (2)meta.code.classcharDistGalaxy distanceMpcpos.distancefloatFFUVGALEX FUV fluxmJyphot.flux.density;em.UVfloate_FFUVGALEX FUV flux errormJystat.errorfloatFNUVGALEX NUV fluxmJyphot.flux.density;em.UVfloate_FNUVGALEX NUV flux errormJystat.errorfloatFBB fluxmJyphot.flux.density;em.opt.Bfloate_FBB flux errormJystat.errorfloatFRR fluxmJyphot.flux.density;em.opt.Rfloate_FRR flux errormJystat.errorfloatFuSDSS u fluxmJyphot.flux.density;em.opt.Ufloate_FuSDSS u flux errormJystat.errorfloatFgSDSS g fluxmJyphot.flux.densityfloate_FgSDSS g flux errormJystat.errorfloatFrSDSS r fluxmJyphot.flux.density;em.opt.Rfloate_FrSDSS r flux errormJystat.errorfloatFiSDSS i fluxmJyphot.flux.density;em.opt.Ifloate_FiSDSS i flux errormJystat.errorfloatFzSDSS z fluxmJyphot.flux.densityfloate_FzSDSS z flux errormJystat.errorfloatFJJ fluxmJyphot.flux.density;em.IR.Jfloate_FJJ flux errormJystat.errorfloatFHH fluxmJyphot.flux.density;em.IR.Hfloate_FHH flux errormJystat.errorfloatFKsKs fluxmJyphot.flux.density;em.IR.Kfloate_FKsKs flux errormJystat.errorfloatF3.6Spitzer/IRAC 3.6um fluxmJyphot.flux.density;em.IR.3-4umfloate_F3.6Spitzer/IRAC 3.6um flux errormJystat.errorfloatF4.5Spitzer/IRAC 4.5um fluxmJyphot.flux.density;em.IR.4-8umfloate_F4.5Spitzer/IRAC 4.5um flux errormJystat.errorfloatF5.7Spitzer/IRAC 5.7um fluxmJyphot.flux.density;em.IR.4-8umfloate_F5.7Spitzer/IRAC 5.7um flux errormJystat.errorfloatF8.0Spitzer/IRAC 8.0um fluxmJyphot.flux.density;em.IR.8-15umfloate_F8.0Spitzer/IRAC 8.0um flux errormJystat.errorfloatF24Spitzer/MIPS 24um fluxmJyphot.flux.density;em.IR.15-30umfloate_F24Spitzer/MIPS 24um flux errormJystat.errorfloatF60IRAS 60um fluxmJyphot.flux.density;em.IR.30-60uminte_F60IRAS 60um flux errormJystat.errorintF100IRAS 100um fluxmJyphot.flux.density;em.IR.60-100uminte_F100IRAS 100um flux errormJystat.errorintF65AKARI/N60 65um fluxmJyphot.flux.density;em.IR.30-60uminte_F65AKARI/N60 65um flux errormJystat.errorintF90AKARI/WIDE-S 90um fluxmJyphot.flux.density;em.IR.60-100uminte_F90AKARI/WIDE-S 90um flux errormJystat.errorintF140AKARI/WIDE-L 140um fluxmJyphot.flux.density;em.mm.1500-3000GHzinte_F140AKARI/WIDE-L 140um flux errormJystat.errorintF160AKARI/N160 160um fluxmJyphot.flux.density;em.mm.1500-3000GHzinte_F160AKARI/N160 160um flux errormJystat.errorintRefReferences (1)meta.refcharSimbadSimbad column added by the CDSmeta.refcharNEDSimbad column added by the CDSmeta.refcharR? Projected distance to the nearest neighborkpcpos.distanceintnullablervir? Virial radiuskpcphys.size.radiusintnullableStr? "Strength" of interaction as described in Sect. 4.6., <R/r_vir,nei_>/n (1)pos.distance;arith.ratiofloatnullableNType? Morphological type of the nearest neighbor (early or late)src.morph.typechar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.main