J/A+A/708/A290ivo://CDS.VizieR/J/A+A/708/A290CDSGallazzi A.R.Zibetti S.van der Wel A.Nersesian A.Kaushal Y.,Bezanson R.Mattolini D.Bell E.F.Scholz-Diaz L.Leja J.D'Eugenio F.,Wu P.-F.Pacifici C.Maseda M.2026-05-04T07:43:19Z2026-04-14T10:08:34ZCDS support team

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

cds-question@unistra.frgalaxiesspectroscopystellar-ageschemical-abundancescatalogsvisible-astronomyWe analysed a sample of 552 galaxies from the LEGA-C spectroscopic survey (0.6<z<0.77), for which we estimated the stellar population parameters by a Bayesian analysis of the stellar absorption features and photometry. We investigated the effect of the current star formation activity on light-weighted mean stellar ages and metallicities and their median trends with stellar mass or velocity dispersion. The bimodality in the global age-mass relation stems from the different age distributions in the quiescent and star-forming populations. No bimodality is observed in the stellar metallicity-mass relation, although quiescent and star-forming galaxies have different distributions in this parameter space. We identified a high-metallicity sequence populated by quiescent and weakly star-forming galaxies. At masses lower than 10^10.8^M_{sun}_, the median stellar metallicity-mass relation of star-forming galaxies steepens as a consequence of the increasing scatter towards lower stellar metallicities for galaxies with an increasing specific star formation rate at fixed mass. Relying on a consistent analysis of SDSS DR7 spectra and accounting for aperture corrections, we quantified the evolution of the volume-weighted stellar age and stellar metallicity scaling relations between z=0.7 and the present. We found negligible evolution in the stellar metallicity-mass relation of quiescent galaxies and for M*>10^11^M_{sun}_ galaxies in general. Lower-mass star-forming galaxies instead have typically lower metallicities than their local counterparts, indicating significant enrichment since z~0.7 in the low-mass regime. Notably, the median of the stellar ages of the general population and of quiescent galaxies has changed by only 2Gyr between z=0.7 and z=0.1, which is less than expected from cosmic ageing. Some quiescent galaxies must evolve passively to reach the old boundary of the local population. In order to explain the evolution of the median trends, however, both individual evolution through rejuvenation and/or minor merging that affects the outer galaxy regions and population evolution through quenching of massive metal-rich star-forming galaxies are required.2026A&A...708A.290Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/708/A290CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJS/256/44 : LEGA-C DR3 catalog (van der Wel+, 2021)J/A+A/703/A5 : Local galaxies scaling relations (Mattolini+, 2025)J/A+A/708/A289 : LEGA-C stellar population scaling relation. I.https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/708/A290https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/708/A290http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/708/A290https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/708/A290https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/708/A290http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/708/A290GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/708/A290/qpar_m_gMedian trends of light-weighted age and stellar metallicity as a function of stellar mass for quiescent galaxies in the golden sample (Table B1)recnoRecord number assigned by the VizieR team. 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Should Not be used for identification.meta.recordintlogSigmaLogarithm of the central value of 0.1dex-wide bin of stellar velocity dispersionlog(solMass)phys.veloc.dispersionfloatlogAgep50Median of logarithm light-weighted mean age of galaxies in the velocity dispersion binlog(yr)time.age;stat.medianfloatE_logAgep50Upper error on median logarithm light-weighted age of galaxies in the velocity dispersion binlog(yr)stat.error;stat.maxfloate_logAgep50[] Lower error on median logarithm light-weighted age of galaxies in the velocity dispersion binlog(yr)stat.errorfloatlogAgep1616th percentile of logarithm light-weighted age of galaxies in the velocity dispersion binlog(yr)time.agefloatlogAgep8484th percentile of logarithm light-weighted age of galaxies in the velocity dispersion binlog(yr)time.agefloatmedelogAgeMean of 84-16 percentile range of individual logAge PDFs for galaxies in velocity dispersion binlog(yr)time.agefloatlogZp50Median of logarithm light-weighted mean metallicity of galaxies in the velocity dispersion binlog(Sun)phys.abund.ZfloatE_logZp50Upper error on median logarithm light-weighted metallicity of galaxies in the velocity dispersion binlog(Sun)stat.error;stat.maxfloate_logZp50[] Lower error on median logarithm light-weighted metallicity of galaxies in the velocity dispersion binlog(Sun)stat.errorfloatlogZp1616th percentile of logarithm light-weighted metallicity of galaxies in the velocity dispersion binlog(Sun)phys.abund.ZfloatlogZp8484th percentile of logarithm light-weighted metallicity of galaxies in the velocity dispersion binlog(Sun)phys.abund.ZfloatmedelogZMean of 84-16 percentile range of individual logZ PDFs for galaxies in velocity dispersion binlog(Sun)phys.abund.Zfloat