J/A+A/677/A143ivo://CDS.VizieR/J/A+A/677/A143doi:10.26093/cds/vizier.36770143CDSMercier W.Epinat B.Contini T.Krajnovic D.Ciesla L.Lemaux B.C.,Abril-Melgarejo V.Boogaard L.Pelliccia D.2024-11-06T20:05:47Z2023-09-18T07:41:05ZCDS support team

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

cds-question@unistra.frgalaxiescatalogsgalaxy-rotationastronomical-modelsgalaxy-kinematicssurveysvisible-astronomyAt intermediate redshift, galaxy groups/clusters are thought to impact galaxy properties such as their angular momentum. We investigate whether the environment has an impact on the galaxies' stellar angular momentum and identify underlying driving physical mechanisms. We derive robust estimates of the stellar angular momentum using Hubble Space Telescope (HST) images combined with spatially resolved ionised gas kinematics from the Multi-Unit Spectroscopic Explorer (MUSE) for a sample of ~200 galaxies in groups and in the field at z~0.7 drawn from the MAGIC survey. Using various environmental tracers, we study the position of the galaxies in the the angular momentum-stellar mass (Fall) relation as a function of environment. We measure a 0.12dex (2{sigma} significant) depletion of stellar angular momentum for low-mass galaxies (M*<10^10^M_{sun}_) located in groups with respect to the field. Massive galaxies located in dense environments have less angular momentum than expected from the low-mass Fall relation but, without a comparable field sample, we cannot infer whether this effect is mass- or environmentally-driven. Furthermore, these massive galaxies are found in the central parts of the structures and have low systemic velocities. The observed depletion of angular momentum at low stellar mass does not appear linked with the strength of the over-density around the galaxies but it is strongly correlated with (i) the systemic velocity of the galaxies normalised by the dispersion of their host group and (ii) their ionised gas velocity dispersion. Galaxies in groups appear depleted in angular momentum, especially at low stellar mass. Our results suggest that this depletion might be induced by physical mechanisms that scale with the systemic velocity of the galaxies (e.g. stripping or merging) and that such mechanism might be responsible for enhancing the velocity dispersion of the gas as galaxies lose angular momentum.2023A&A...677A.143Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A143CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/665/A54 : MAGIC morpho-kinematics MS catalogue (Mercier+, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/677/A143https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/677/A143http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/677/A143https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/677/A143https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/677/A143http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/677/A143GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/677/A143/tablee1 (Parameters for the kinematics sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/677/A143/tablee1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/677/A143/tablee1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/677/A143/tablee1?GETtext/xml+votable180.050000true149.71806315775711.9216141620910.0055555555555555566/27256 27258https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/677/A143?format=asciiOpticaldefaultJ/A+A/677/A143/tablee1Parameters for the kinematics samplerecnoRecord 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 kinematicssrc.redshiftdoubleRAJ2000Right Ascension of morphological centre (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of morphological centre (J2000)degpos.eq.dec;meta.mainN? Richness (i.e. number of galaxies) in the structure the galaxy belongs tosrc.class.richnessintnullableR/R200? Ratio of the projected distance of a galaxy to its host group's centre with its host group's radius. Field galaxies have a value of -99pos.distance;arith.ratiodoublenullabledV/sigma? Ratio of the systemic velocity of the galaxy along the line-of-sight with its host group's velocity dispersion. Field galaxies have a value of -99phys.velocdoublenullableEta? Environmental tracer combining R/R200 and dV/sigmastat.fit.paramdoublenullablelogOverDensLog10 of the over-density around galaxies as measured by the VMC techniquephys.density;arith.ratiodoublelogjHSTMMLog10 of the specific stellar angular momentum derived from HST images and a mass model rotation curvelog(kpc.km.s**-1)phys.angMomentumdoublelogjHSTflatLog10 of the specific stellar angular momentum derived from HST images and a flat model rotation curvelog(kpc.km.s**-1)phys.angMomentumdoublelogjexpMMLog10 of the specific stellar angular momentum derived from an exponential mass distribution and a mass model rotation curvelog(kpc.km.s**-1)phys.angMomentumdoublelogjexpflatLog10 of the specific stellar angular momentum derived from an exponential mass distribution and a flat model rotation curvelog(kpc.km.s**-1)phys.angMomentumdoubleGasDispAverage ionised gas dispersion with LSF and beam-smearing corrections appliedkm/sarith.factor;instr.dispersion;stat.meandoublelogM*Stellar mass within R22=2.2*Rd, with Rd the stellar disk scale lengthlog(solMass)phys.massdouble