J/A+A/665/A54ivo://CDS.VizieR/J/A+A/665/A54doi:10.26093/cds/vizier.36650054CDSMercier W.Epinat B.Contini T.Abril-Melgarejo V.Boogaard L.,Brinchmann J.Finley H.Krajnovic D.Michel-Dansac L.Ventou E.,Bouche N.Dumoulin J.Pineda J.C.B.2026-01-20T12:11:31Z2022-09-09T09:18:07ZCDS support team

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

cds-question@unistra.frgalaxiescatalogsgalaxy-rotationastronomical-modelsgalaxy-classification-systemsgalaxy-kinematicsThe evolution of galaxies is influenced by many physical processes, which may vary depending on their environment. We combine Hubble Space Telescope (HST) and Multi-Unit Spectroscopic Explorer (MUSE) data of galaxies at 0.25<~z<~1.5 to probe the impact of environment on the size-mass relation, the main sequence (MS) relation, and the Tully-Fisher relation (TFR). We perform a morpho-kinematics modelling of 593 [OII] emitters in various environments in the COSMOS area from the MUSE-gAlaxy Groups In Cosmos survey. The HST F814W images are modelled with a bulge-disk decomposition to estimate their bulge-disk ratio, effective radius, and disk inclination. We use the [OII]{lambda}{lambda}3727,3729 doublet to extract the galaxies' ionised gas kinematics maps from the MUSE cubes, and we model those maps for a sample of 146 [OII] emitters, including bulge and disk components constrained from morphology and a dark matter halo. We find an offset of 0.03dex (1{sigma} significant) on the size-mass relation zero point between the field and the large structure sub-samples, with a richness threshold of N=10 to separate between small and large structures, and of 0.06dex (2{sigma}) with N=20. Similarly, we find a 0.1dex (2{sigma}) difference on the MS relation with N=10 and 0.15dex (3{sigma}) with N=20. These results suggest that galaxies in massive structures are smaller by 14% and have star formation rates reduced by a factor of 1.3-1.5 with respect to field galaxies at z=~0.7. Finally, we do not find any impact of the environment on the TFR, except when using N=20 with an offset of 0.04dex (1{sigma}). We discard the effect of quenching for the largest structures, which would lead to an offset in the opposite direction. We find that, at z=~0.7, if quenching impacts the mass budget of galaxies in structures, these galaxies would have been affected quite recently and for roughly 0.7-1.5Gyr. This result holds when including the gas mass but vanishes once we include the asymmetric drift correction.2022A&A...665A..54Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/665/A54CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/665/A54https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/665/A54http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/665/A54https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/665/A54https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/665/A54http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/665/A54GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/665/A54/tablef1 (Morpho-kinematics params for MS galaxies in MAGIC)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/665/A54/tablef1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/665/A54/tablef1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/665/A54/tablef1?GETtext/xml+votable180.050000true149.71806591000691.92161091288780.0055555555555555566/27256 27258https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/665/A54?format=asciiOpticaldefaultJ/A+A/665/A54/tablef1Morpho-kinematics params for MS galaxies in MAGICrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDMUSE galaxy ID (1)meta.id;meta.maincharzSpectroscopic systemic redshift derived from kinematics modellingsrc.redshiftdoubleRAJ2000Right Ascension (J2000) of morphological centredegpos.eq.ra;meta.mainDEJ2000Declination (J2000) of morphological centredegpos.eq.dec;meta.mainN? Number of galaxies in structures with more than three membersmeta.numberintnullableReffdDisk effective radiuskpcphys.size.radiusdoubleReffbBulge effective radiuskpcphys.size.radiusdoubleSimbadSimbad column added by the CDSmeta.ref.urlcharReffGlobal effective radiuskpcphys.size.radiusdoublelogBDLogarithm of the bulge-to-disk ratio at Reffphys.luminosity;arith.ratiodoubleqAxis ratio of the diskphys.size.axisRatiofloatPAmMorphological position angle of the major axisdegpos.posAngfloatFWHMMedian PSF FWHM, corresponding to narrow band OII MUSE observations in arcsecondarcsecphys.angSizedoubleOIIflux(R22)OII flux derived from MUSE flux maps at R22 (2)1e-24W.m**-2phot.fluxdoubleOIIfluxOII] flux derived from MUSE flux maps at 3"1e-24W.m**-2phot.fluxdoubleSNRTotal OII signal-to-noise ratiostat.snrdoubleiDisk inclination corrected for thicknessdegsrc.orbital.inclinationdoublePAkKinematic position angle of the major axisdegpos.posAngdoublersNFW halo scale radiuskpcphys.size.radius;instr.scaledoubleVhmaxMaximum rotation velocity of the NFW rotation curvekm/sphys.veloc.rotat;stat.maxdoubleVr22Rotation velocity at R22km/sphys.veloc.rotatdoublesigmaMedian velocity dispersionkm/sphys.veloc.dispersion;stat.mediandoubleVc22Corrected rotation velocity at R22km/sphys.veloc.rotatdoublelogM*Logarithm of the stellar mass within an aperture of 3"solMassphys.massfloatlogM*(R22)Logarithm of the corrected stellar mass inside R22solMassphys.massdoublelogSFRLogarithm of the SFR at 3" using Gilbank et al. (2010MNRAS.405.2594G, 2011AJ....141...94G or 2011MNRAS.414..304G) prescriptionsolMass/yrphys.SFRdoublelogMgLogarithm of the gas mass computed from the Schmidt-Kennicutt law and OII flux measured at R22solMassphys.massdoublelogMdynLogarithm of the dynamical mass computed at R22 from the mass modelsolMassphys.massdouble