J/MNRAS/490/417ivo://CDS.VizieR/J/MNRAS/490/417doi:10.26093/cds/vizier.74900417CDSCarnall A.C.McLure R.J.Dunlop J.S.Cullen F.McLeod D.J.Wild V.,Johnson B.D.Appleby S.Dave R.Amorin R.Bolzonella M.Castellano M.,Cimatti A.Cucciati O.Gargiulo A.Garilli B.Marchi F.Pentericci L.,Pozzetti L.Schreiber C.Talia M.Zamorani G.2024-08-20T20:14:03Z2023-02-17T12:54:51ZCDS support team

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

cds-question@unistra.frgalaxiesredshiftedphotometryspectroscopyultraviolet-astronomyvisible-astronomyinfrared-astronomyWe present a Bayesian full-spectral-fitting analysis of 75 massive (M_*_>10^10.3^M_{sun}_) UVJ-selected galaxies at redshifts of 1.0<z<1.3, combining extremely deep rest-frame ultraviolet spectroscopy from VANDELS with multiwavelength photometry. By the use of a sophisticated physical plus systematic uncertainties model, constructed within the BAGPIPES code, we place strong constraints on the star-formation histories (SFHs) of individual objects. We first constrain the stellar mass versus stellar age relationship, finding a steep trend towards earlier average formation time with increasing stellar mass (downsizing) of 1.48^+0.34^_-0.39_Gyr per decade in mass, although this shows signs of flattening at M_*_>10^11^M_{sun}_. We show that this is consistent with other spectroscopic studies from 0<z<2. This relationship places strong constraints on the AGN-feedback models used in cosmological simulations. We demonstrate that, although the relationships predicted by SIMBA and ILLUSTRISTNG agree well with observations at z=0.1, they are too shallow at z=1, predicting an evolution of =<0.5Gyr per decade in mass. Secondly, we consider the connections between green-valley, post-starburst, and quiescent galaxies, using our inferred SFH shapes and the distributions of galaxy physical properties on the UVJ diagram. The majority of our lowest-mass galaxies (M_*_~10^10.5^M_{sun}_) are consistent with formation in recent (z<2), intense starburst events, with time-scales of =<500Myr. A second class of objects experience extended star-formation epochs before rapidly quenching, passing through both green-valley and post-starburst phases. The most massive galaxies in our sample are extreme systems: already old by z=1, they formed at z~5 and quenched by z=3. However, we find evidence for their continued evolution through both AGN and rejuvenated star-formation activity.2019MNRAS.490..417Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/490/417CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toV/151 : VANDELS High-Redshift Galaxy Evolution (McLure+, 2017)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/490/417https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/490/417http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/490/417https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/490/417https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/490/417http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/490/417GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/490/417/table1 (Details of the 75 VANDELS objects considered in this work)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/490/417/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/490/417/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/490/417/table1?GETtext/xml+votable180.050000true53.0296-27.96860.0055555555555555566/17679 17688 17690 35935https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/490/417?format=asciiUVOpticalInfrareddefaultJ/MNRAS/490/417/table1Details of the 75 VANDELS objects considered in this workSimbadNameSimbad column added by the CDSmeta.idcharnullablere? Effective radii in arcseconds, taken from van der Wel et al. (2014ApJ...788...28V)arcsecphysfloatnullableSNRAverage SNR over the spectral range from 7450-7550{AA}0.1nm**-1stat.snrfloatb_logM*16th percentile of the posterior probability distribution for the stellar masslog(solMass)phys.mass;stat.minfloatlogM*50th percentile of the posterior probability distribution for the stellar masslog(solMass)phys.massfloatB_logM*84th percentile of the posterior probability distribution for the stellar masslog(solMass)phys.mass;stat.maxfloatb_zform16th percentile of the posterior probability distribution for the formation redshiftsrc.redshift;stat.minfloatzform50th percentile of the posterior probability distribution for the formation redshiftsrc.redshift;pos.heliocentricfloatB_zform84th percentile of the posterior probability distribution for the formation redshiftsrc.redshift;stat.maxfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameVANDELS unique galaxy identificationmeta.id;meta.maincharRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainimagi-band AB magnitudemagphot.mag;em.opt.IfloatHmagH-band AB magnitudemagphot.mag;em.IR.HfloatzpecSpectroscopic redshift, measured by the VANDELS team in Pentericci et al. (2018A&A...616A.174P, Cat. V/151)src.redshift;pos.heliocentricfloat