J/A+A/647/A152ivo://CDS.VizieR/J/A+A/647/A152doi:10.26093/cds/vizier.36470152CDSAbril-Melgarejo V.Epinat B.Mercier W.Contini T.Boogaard L.A.,Brinchmann J.Finley H.Michel-Dansac L.Ventou E.Amram P.,Krajnovic D.Mahler G.Pineda J.C.B.Richard J.2025-08-21T20:00:50Z2021-03-26T12:07:59ZCDS support team

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

cds-question@unistra.frgalaxy-clustersgalaxiescatalogsgalaxy-rotationredshiftedgalaxy-kinematicsGalaxies in dense environments are subject to interactions and mechanisms that directly affect their evolution by lowering their gas fractions and consequently reducing their star-forming capacity earlier than their isolated counterparts. The aim of our project is to get new insights into the role of environment in the stellar and baryonic content of galaxies using a kinematic approach, through the study of the Tully-Fisher relation (TFR). We study a sample of galaxies in eight groups, over-dense by a factor larger than 25 with respect to the average projected density, spanning a redshift range of 0.5<z<0.8 and located in ten pointings of the MAGIC MUSE Guaranteed Time Observations program. We perform a morpho-kinematics analysis of this sample and set up a selection based on galaxy size, [OII]{lambda}{lambda}3727,3729 emission line doublet signal-to-noise ratio, bulge-to-disk ratio, and nuclear activity to construct a robust kinematic sample of 67 star-forming galaxies. We show that this selection considerably reduces the number of outliers in the TFR, which are predominantly dispersion-dominated galaxies. Similar to other studies, we find that including the velocity dispersion in the velocity budget mainly affects galaxies with low rotation velocities, reduces the scatter in the relation, increases its slope, and decreases its zero-point. Including gas masses is more significant for low-mass galaxies due to a larger gas fraction, and thus decreases the slope and increases the zero-point of the relation. Our results suggest a significant offset of the TFR zero-point between galaxies in low- and high-density environments, regardless of the kinematics estimator used. This can be interpreted as a decrease in either stellar mass by ~0.05-0.3dex or an increase in rotation velocity by ~0.02-0.06dex for galaxies in groups, depending on the samples used for comparison. We also studied the stellar and baryon mass fractions within stellar disks and found they both increase with stellar mass, the trend being more pronounced for the stellar component alone. These fractions do not exceed 50%. We show that this evolution of the TFR is consistent either with a decrease in star formation or with a contraction of the mass distribution due to the environment. These two effects probably act together, with their relative contribution depending on the mass regime.2021A&A...647A.152Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/647/A152CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/647/A152https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/647/A152http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/647/A152https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/647/A152https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/647/A152http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/647/A152GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/647/A152/tableb1 (Kinematic and morphological parameters (corrected version on 09-May-2023))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/647/A152/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/647/A152/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/647/A152/tableb1?GETtext/xml+votable180.050000true150.23019441.80538890.0055555555555555566/27256 27258https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/647/A152?format=asciidefaultJ/A+A/647/A152/tableb1Kinematic and morphological parameters (corrected version on 09-May-2023)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGrIDCOSMOS group IDmeta.id;pos.lgcharIDGalaxy ID (G1)meta.id;meta.mainintzSpectroscopic redshiftsrc.redshiftdoubleRAJ2000Right Ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainSimbadNameSimbad column added by the CDSmeta.idcharnullableFWHMMedian PSF FWHM, corresponding to narrow band [OII] MUSE observationsarcsecphys.angSizefloatF[OII]Flux from [OII] derived from MUSE flux maps (in 10^-21^erg/s/cm^2^)1e-24W.m**-2phot.fluxinte_F[OII]rms uncertainty on F[OII]1e-24W.m**-2stat.errorintqAxis ratiophys.size.axisRatiofloate_qrms uncertainty on axis ratiostat.errorfloatPAmMorphological position angle of the major axisdegpos.posAnginte_PAmrms uncertainty on PAmdegstat.errorintRdDisk scale lengthkpcphys.angSize;srcfloate_Rdrms uncertainty on Rdkpcstat.errorfloatPAkKinematic position angle of the major axisdegpos.posAnginte_PAkrms uncertainty on PAkdegstat.errorintrtRadius at which the plateau velocity iskpcphys.size.radiusfloate_rtrms uncertainty on rt (2)kpcstat.errordoubleVtVelocity of the plateaukm/sspect.dopplerVelocinte_Vtrms uncertainty on Vt (2)km/sstat.errordoubleJ/A+A/647/A152/tableb2Physical propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGrIDCOSMOS group IDmeta.id;pos.lgcharIDGalaxy ID (G1)meta.id;meta.mainintReffGlobal effective radiuskpcphys.size.radiusfloatlogBDlogarithm of the bulge-to-disk ratio at R22phys.luminosity;arith.ratiofloatiDisk inclinationdegsrc.orbital.inclinationinte_irms uncertainty on idegstat.errorintVr22Rotation velocity at R22 (2)km/sphys.veloc.rotatinte_Vr22rms uncertainty on Vr22km/sstat.errorintsigmaMedian velocity dispersionkm/sphys.veloc.dispersion;stat.medianinte_sigmarms uncertainty on sigmakm/sstat.errorintVc22Corrected rotation velocity at R22 (2)km/sphys.veloc.rotatinte_Vc22rms uncertainty on e_sigmakm/sstat.errorintlogM*logarithm of the stellar mass within an aperture of 3"log(solMass)phys.massfloatE_logM*Error on logM* (upper value)log(solMass)stat.error;stat.maxfloate_logM*Error on logM* (lower value)log(solMass)stat.errorfloatlogM*R22logarithm of the corrected stellar mass inside R22 (2)log(solMass)phys.massfloate_logM*R22rms uncertainty on logM*R22log(solMass)stat.errorfloatlogSFRlogarithm of the SFR from the SED fittinglog(solMass.yr**-1)phys.SFRfloatE_logSFRError on logSFR (upper value)log(solMass.yr**-1)stat.error;stat.maxfloate_logSFRError on logSFR (lower value)log(solMass.yr**-1)stat.error;phys.SFRfloatlogMglogarithm of the gas mass computed from the Kennicutt-Schmidt law and from SED SFRslog(solMass)phys.massfloate_logMgrms uncertainty on logMglog(solMass)stat.errorfloatlogMdynVr22logarithm of the dynamical mass computed from Vr22log(solMass)phys.massfloate_logMdynVr22rms uncertainty on logMdynVr22log(solMass)stat.errorfloatlogMdynVc22logarithm of the dynamical mass computed from Vc22log(solMass)phys.massfloate_logMdynVc22rms uncertainty on logMdynVc22log(solMass)stat.errorfloat