J/ApJ/876/135ivo://CDS.VizieR/J/ApJ/876/135doi:10.26093/cds/vizier.18760135CDSAlcalde Pampliega B.Perez-Gonzalez P.G.Barro G.Dominguez Sanchez H.,Eliche-Moral M.C.Cardiel N.Hernan-caballero A.Rodriguez-Munoz L.,Sanchez Blazquez P.Esquej P.2022-08-29T10:16:22Z2022-08-24T07:17:27ZCDS support team

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

cds-question@unistra.frgalaxiesphotometryredshiftedtwo-color-diagramsextinctionWe present a sample of 33 Balmer break galaxies (BBGs) selected as Hubble Space Telescope/F160W dropouts in the deepest CANDELS/GOODS fields (H>=27.3mag) but relatively bright in Spitzer/IRAC ([3.6], [4.5] <24.5mag), implying red colors (median and quartiles: <H-[3.6]>=3.1_2.8_^3.4^mag). Half of these BBGs are newly identified sources. Our BBGs are massive (<log(M/M_{sun}_)>=10.8_10.4_^11.0^), high-redshift (<z>=4.8_4.4_^5.1^), dusty (<A(V)>=2.0_1.5_^2.0^mag) galaxies. The spectral energy distributions (SEDs) of half of our sample indicate that they are star-forming galaxies with typical specific star formation rates (SFRs) of 0.5-1.0Gyr^-1^, qualifying them as main-sequence (MS) galaxies at 3<z<6. One-third of these SEDs indicate the presence of prominent emission lines (H{beta}+[OIII], H{alpha}+[NII]) boosting the IRAC fluxes and red colors. Approximately 20% of the BBGs are very dusty (A(V)~2.5mag) starbursts with strong mid-to-far-infrared detections and extreme SFRs (SFR>10^3^M_{sun}_/yr) that place them above the MS. The rest, 30%, are post-starbursts or quiescent galaxies located >2{sigma} below the MS with mass-weighted ages older than 700Myr. Only two of the 33 galaxies are X-ray-detected active galactic nuclei (AGNs) with optical/near-infrared SEDs dominated by stellar emission, but the presence of obscured AGNs in the rest of the sources cannot be discarded. Our sample accounts for 8% of the total number density of log(M/M_{sun}_)>10 galaxies at z>3, but it is a significant contributor (30%) to the general population of red log(M/M_{sun}_)> 11 galaxies at 4<z<6. Finally, our results point out that one of every 30 massive log(M/M_{sun}_)> 11 galaxies in the local universe was assembled in the first 1.5Gyr after the big bang, a fraction that is not reproduced by state-of-the-art galaxy formation simulations.2019ApJ...876..135Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/876/135CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/876/135https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/876/135http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/876/135https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/876/135https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/876/135http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/876/135GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/876/135/table (Galaxy properties for the 33 galaxies (table1 and table3))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/876/135/table?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/876/135/table?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/876/135/table?GETtext/xml+votable180.050000true189.23577562.202069440.0055555555555555566/11252 359351.1796835550914393e-19 1.4053184620945436e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/876/135?format=asciidefaultJ/ApJ/876/135/tableGalaxy properties for the 33 galaxies (table1 and table3)e_AgeError on age (lower value)Gyrstat.error;time.agefloatE_AgeError on age (upper value)Gyrstat.error;stat.maxfloatAgeBest-fitting ageGyrtime.agefloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDID (BBG_GDNNN or BBG_GDSNN)meta.id;meta.maincharRAJ2000Rigth ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainzPhotometric redshiftsrc.redshiftfloatF160WPhotometry HST/WFC3_F160W (AB)magphot.mag;em.UV.100-200nmfloate_F160WPhotometric error in HST/WFC3_F160W (AB)magstat.errorfloat[3.6]Photometry IRAC CH1 (AB)magphot.mag;em.IR.3-4umfloate_[3.6]Photometric error in IRAC CH1 (AB)magstat.errorfloat[4.5]Photometry IRAC CH2 (AB)magphot.mag;em.IR.4-8umfloate_[4.5]Photometric error in IRAC CH2 (AB)magstat.errorfloat[5.8]? Photometry IRAC CH3 (AB)magphot.flux.density;em.IR.4-8umfloatnullablee_[5.8]? Photometric error in IRAC CH3 (AB)magstat.errorfloatnullable[8.0]? Photometry IRAC CH4 (AB)magphot.flux.density;em.IR.8-15umfloatnullablee_[8.0]? Photometric error in IRAC CH4 (AB)magstat.errorfloatnullableSFRSFR_total if IR-detected: SFRUV+SFRIR, otherwise: SFRsedsolMass/yrphys.SFRdoubleSFRsedSFR from SED fittingsolMass/yrphys.SFRfloatSimbadNameSimbad column added by the CDSmeta.idcharnullablelogMStellar masslog(solMass)phys.massfloatSFRUVSFR UV, computed from rest-frame UV luminosity, uncorrected for attenuationsolMass/yrphys.SFRdoubleSFRIR? SFR IR, computed from IR luminositysolMass/yrphys.SFRdoublenullablee_logMError on logM (lower value)log(solMass)stat.errorfloatE_logMError on logM (upper value)log(solMass)stat.error;stat.maxfloatZMetallicitylog(Sun)phys.abund.ZfloatTauStar formation time-scaleMyrtime.scalefloate_TauError on tau (lower value)Myrstat.errorfloatE_TauError on tau (upper value)Myrstat.error;stat.maxfloatAvDust attenuationmagphys.absorptionfloate_AvError on Av (lower value)magstat.errorfloatE_AvError on Av (upper value)magstat.error;stat.maxfloat