J/MNRAS/496/3841ivo://CDS.VizieR/J/MNRAS/496/3841doi:10.26093/cds/vizier.74963841CDSVaughan S.P.Tiley A.L.Davies R.L.Prichard L.J.Croom S.M.,Bureau M.Stott J.P.Bunker A.Cappellari M.Ansarinejad B.,Jarvis M.J.2025-05-22T20:16:05Z2023-10-12T15:34:38ZCDS support team

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

cds-question@unistra.frgalaxy-clustersinfrared-astronomyGalaxy clusters have long been theorized to quench the star formation of their members. This study uses integral-field unit observations from the K-band MultiObject Spectrograph (KMOS) - Cluster Lensing And Supernova survey with Hubble (CLASH) survey (K-CLASH) to search for evidence of quenching in massive galaxy clusters at redshifts 0.3<z<0.6. We first construct mass-matched samples of exclusively star-forming cluster and field galaxies, then investigate the spatial extent of their H{alpha} emission and study their interstellar medium conditions using emission line ratios. The average ratio of H{alpha} half-light radius to optical half-light radius (r_e,H{alpha}_/r_e,Rc_) for all galaxies is 1.14+/-0.06, showing that star formation is taking place throughout stellar discs at these redshifts. However, on average, cluster galaxies have a smaller r_e,H{alpha}_/r_e,Rc_ ratio than field galaxies: <r_e,H{alpha}_/r_e,Rc_> =0.96+/-0.09 compared to 1.22+/-0.08 (smaller at a 98 per cent credibility level). These values are uncorrected for the wavelength difference between H{alpha} emission and R_c_-band stellar light but implementing such a correction only reinforces our results. We also show that whilst the cluster and field samples follow indistinguishable mass-metallicity (MZ) relations, the residuals around the MZ relation of cluster members correlate with cluster-centric distance; galaxies residing closer to the cluster centre tend to have enhanced metallicities (significant at the 2.6{sigma} level). Finally, in contrast to previous studies, we find no significant differences in electron number density between the cluster and field galaxies. We use simple chemical evolution models to conclude that the effects of disc strangulation and ram-pressure stripping can quantitatively explain our observations.2020MNRAS.496.3841Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/496/3841CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/496/3841https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/496/3841http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/496/3841https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/496/3841https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/496/3841http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/496/3841GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/496/3841/tablec1 (Table of Measurements)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/496/3841/tablec1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/496/3841/tablec1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/496/3841/tablec1?GETtext/xml+votable180.050000true197.8145972-3.26119830.0055555555555555566/26177 26180 48076 48423 49012https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/496/3841?format=asciiInfrareddefaultJ/MNRAS/496/3841/tablec1Table of MeasurementsIDGalaxy IDmeta.idintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainzSpectroscopic redshift from the H{alpha} linesrc.redshiftfloatHalpha[0/1] Indicates if we detect H{alpha} in either the 0.6", 1.2" or 2.4" aperture at a S/N ratio greater than 5meta.codeintCsample[0/1] Indicates if the galaxy is a member of the cluster samplemeta.codeintFsample[0/1] Indicates if the galaxy is a member of the mass-matched field samplemeta.codeintAGN[0/1] Indicates if the galaxy contains an AGNmeta.codeintIHa? Integrated H{alpha} flux in a 0.6" diameter aperture1e-07W.arcsec**-1phot.fluxdoublenullablee_IHa? Error on IHa1e-07W.arcsec**-1stat.errordoublenullablelogMassLogarithm of the stellar mass derived from the SED fittinglog(solMass)phys.massdoublevdiffVelocity difference to cluster redshiftkm/sphys.veloc;arith.diffdoubleRp? Projected radius from cluster centrearcsecphys.size.radiusdoublenullableRp/R200? Projected radius scaled to the cluster R_200_ valuephys.size;arith.ratiofloatnullablereHa? Half light radius from the H{alpha} image (1)arcsecphys.angSize;srcdoublenullablereRc? Half light radius from the R_c_ band image (2)arcsecphys.angSize;srcdoublenullablereHa/reRc? Ratio of effective radii r_e,H{alpha}_/r_e,Rc_phys.size;arith.ratiodoublenullableqsize[0/1] Indicates if the size measurement is reliable (3)meta.codeintchi2Ha? Reduced chi-squared from the H{alpha} image fittingstat.fit.chi2doublenullablechi2RcReduced chi-squared from the R_c_ band image fittingstat.fit.chi2doubleS/Nimg? Average S/N from within r_e_ in the H{alpha} imagestat.snrdoublenullablen? Best-fitting Sersic index uncertaintystat.fit.paramdoublenullablee_n? Error on nstat.errordoublenullableS/NHa? S/N of the H{alpha} line in a spectrum integrated in a 2.4" diameter aperturestat.snrdoublenullableFHa? H{alpha} flux measured by ppxf from a 2.4" diameter aperture1e-07W.arcsec**-1phot.flux;em.line.Halphadoublenullablee_FHa? Error on FHa1e-07W.arcsec**-1stat.errordoublenullableFNII? Flux in the [NII] line measured by ppxf from a 2.4" diameter aperture1e-07W.arcsec**-1phot.fluxdoublenullablee_FNII? Error on FNII1e-07W.arcsec**-1stat.errordoublenullableSIIratio? Ratio of the [SII] linesspect.line.intensity;arith.ratiodoublenullablee_SIIratio? Error on SIIratiostat.errordoublenullableFSII? Total [SII] flux measured by ppxf from a 2.4" diameter aperture1e-07W.arcsec**-1phot.fluxdoublenullablee_FSII? Error on FSII1e-07W.arcsec**-1stat.errordoublenullablechi2? Reduced chi-squared from the ppxf fitstat.fit.chi2doublenullablevdisp? Velocity dispersion from the ppxf fitkm/sphys.veloc.dispersiondoublenullable12+log(O/H)? Gas-phase metallicity measured in a 2.4" diameter aperture using the [NII]/H{alpha} ratiophys.abunddoublenullablee_12+log(O/H)? Error on 12+log(O/H)stat.errordoublenullableNameGalaxy name (Cluster+ID)meta.id;meta.maincharClusterObservation field the galaxy is located in (MACS1311, MACS1931, MACS2129 or MS2137)meta.id.parentchar