J/A+A/633/A139ivo://CDS.VizieR/J/A+A/633/A139doi:10.26093/cds/vizier.36330139CDSCiocan B.I.Maier C.Ziegler B.L.Verdugo M.2021-09-06T14:53:21Z2020-05-14T08:35:09ZCDS support team

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

cds-question@unistra.frgalaxy-clustersgalaxiescatalogschemical-abundancesAims. Gas-phase metallicities offer insight into the chemical evolution of galaxies as they reflect the recycling of gas through star formation and galactic inflows and outflows. Environmental effects such as star-formation quenching mechanisms play an important role in shaping the evolution of galaxies. Clusters of galaxies at z<0.5 are expected to be the sites where environmental effects can be clearly observed with present-day telescopes. Methods. We explored the Frontier Fields cluster RX J2248-443 at z=0.348 with VIMOS/VLT spectroscopy from CLASH-VLT, which covers a central region corresponding to almost 2 virial radii. The fluxes of [OII]{lambda}3727, H{beta}, [OIII]{lambda}5007, H{alpha} and [NII]{lambda}6584 emission lines were measured allowing the derivation of (O/H) gas metallicities, star formation rates based on extinction-corrected H{alpha} fluxes, and contamination from active galactic nuclei. We compared our sample of cluster galaxies to a population of field galaxies at similar redshifts. Results. We use the location of galaxies in projected phase-space to distinguish between cluster and field galaxies. Both populations follow the star-forming sequence in the diagnostic diagrams, which allow the ionising sources in a galaxy to be disentangled, with only a low number of galaxies classified as Seyfert II. Both field and cluster galaxies follow the "main sequence" of star-forming galaxies, with no substantial difference observed between the two populations. In the mass-metallicity (MZ) plane, both high-mass field and cluster galaxies show comparable (O/H)s to the local SDSS MZ relation, with an offset of low-mass galaxies (log(M/M_{sun}_)<9.2) towards higher metallicities. While both the metallicities of "accreted" (R<R_500_) and "infalling" (R>R_500_) cluster members are comparable at all masses, the cluster galaxies from the "mass complete" bin (which is the intermediate mass bin in this study: 9.2<log(M/M_{sun}_)<10.2), show more enhanced metallicities than their field counterparts by a factor of 0.065 dex with a ~1.8{sigma} significance. The intermediate-mass field galaxies are in accordance with the expected (O/H)s from the fundamental metallicity relation, while the cluster members deviate strongly from the model predictions, namely by a factor of ~0.12dex. The results of this work are in accordance with studies of other clusters at z<0.5 and favour the scenario in which the hot halo gas of low- and intermediate-mass cluster galaxies is removed due to ram pressure stripping, leading to an increase in their gas-phase metallicity.2020A&A...633A.139Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/633/A139CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/633/A139https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/633/A139http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/633/A139https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/633/A139https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/633/A139http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/633/A139GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/633/A139/tablea1Catalogue for the RX J2248 cluster galaxiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalaxyGalaxy identification number (1)meta.id;meta.mainintF(Hbeta)? H{beta} emission line flux1e-20W.m**-2phot.flux;em.line.Hbetafloatnullablee_F(Hbeta)? rms uncertainty on F(Hbeta)1e-20W.m**-2stat.errorfloatnullableF([OIII])? [OIII] emission line flux1e-20W.m**-2phot.flux;em.line.OIII;spect.linefloatnullablee_F([OIII])? rms uncertainty on F([OIII])1e-20W.m**-2stat.errorfloatnullableF(Halpha)? H{alpha} emission line flux1e-20W.m**-2phot.flux;em.line.Halpha;spect.linefloatnullablee_F(Halpha)? rms uncertainty on F(Halpha)1e-20W.m**-2stat.errorfloatnullableF([NII])? [NII] emission line flux1e-20W.m**-2phot.flux;spect.linefloatnullablee_F([NII])? rms uncertainty on F([NII])1e-20W.m**-2stat.errorfloatnullablelogMStellar mass, as computed by LePharelog(solMass)phys.mass;meta.modelledfloatlogsSFR? Specific SFR (2)log(Gyr)phys.SFRfloatnullable12+log(O/H)? 12+log(O/H) abundancephys.abundfloatnullable