J/ApJS/270/12ivo://CDS.VizieR/J/ApJS/270/12doi:10.26093/cds/vizier.22700012CDSWang B.Leja J.Labbe I.Bezanson R.Whitaker K.E.Brammer G.,Furtak L.J.Weaver J.R.Price S.H.Zitrin A.Atek H.Coe D.,Cutler S.E.Dayal P.van Dokkum P.Feldmann R.Marchesini D.,Franx M.Forster Schreiber N.Fujimoto S.Geha M.Glazebrook K.,de Graaff A.Greene J.E.Juneau S.Kassin S.Kriek M.Khullar G.,Maseda M.Mowla L.A.Muzzin A.Nanayakkara T.Nelson E.J.Oesch P.A.,Pacifici C.Pan R.Papovich C.Setton D.J.Shapley A.E.Smit R.,Stefanon M.Suess K.A.Taylor E.N.Williams C.C.2024-11-06T20:30:43Z2024-05-13T12:08:04ZCDS support team

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

cds-question@unistra.frgalaxy-clustershst-photometryinfrared-photometrytwo-color-diagramsspectral-energy-distributionredshiftedvisible-astronomyThe recent UNCOVER survey with the James Webb Space Telescope (JWST) exploits the nearby cluster A2744 to create the deepest view of our Universe to date by leveraging strong gravitational lensing. In this work, we perform photometric fitting of more than 50000 robustly detected sources out to z~15. We show the redshift evolution of stellar ages, star formation rates, and rest- frame colors across the full range of 0.2<~z<~15. The galaxy properties are inferred using the Prospector Bayesian inference framework using informative Prospector-{beta} priors on the masses and star formation histories to produce joint redshift and stellar populations posteriors. Additionally, lensing magnification is performed on the fly to ensure consistency with the scale-dependent priors. We show that this approach produces excellent photometric redshifts with {sigma}_NMAD_~0.03, of a similar quality to the established photometric redshift code EAzY. In line with the open-source scientific objective of this Treasury survey, we publicly release the stellar population catalog with this paper, derived from our photometric catalog adapting aperture sizes based on source profiles.2024ApJS..270...12Whttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/270/12CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AJ/125/1107 : Ultra-deep near-IR observation in HDF-S (Labbe+, 2003)J/ApJ/621/673 : Line indices for 124 early-type galaxies (Thomas+, 2005)J/MNRAS/371/703 : MILES library of empirical spectra (Sanchez-Blazquez+, 2006)J/ApJ/812/114 : Grism Lens-Amplified Survey from Space. I. (Treu+, 2015)J/ApJ/801/44 : HST lensing analysis of the CLASH sample (Zitrin+, 2015)J/A+A/646/A83 : 12 massive lensing clusters MUSE obs. (Richard+, 2021)J/AJ/165/248 : COSMOS2020; 230 quiescent galaxies at 3<z<5 (Gould+, 2023)J/ApJS/270/7 : The UNCOVER phot. cat. of A2744 wiht HST+JWST (Weaver+, 2024)http://zenodo.org/records/10223792 : Most recent versions of UNCOVER DR2https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJS/270/12https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJS/270/12http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJS/270/12https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJS/270/12https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJS/270/12http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJS/270/12GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJS/270/12/spscat (Stellar population catalog based on the DR2 SUPER photometric catalog)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJS/270/12/spscat?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJS/270/12/spscat?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJS/270/12/spscat?GETtext/xml+votable180.050000true3.61533009655-30.461230316550.0055555555555555566/16486https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJS/270/12?format=asciiOpticalInfrareddefaultJ/ApJS/270/12/spscatStellar population catalog based on the DR2 SUPER photometric catalogrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[1/61648] Running sequence number as in UNCOVER DR2 phot. cat. (Weaver+ 2024, J/ApJS/270/7) (id)meta.recordintRAJ2000[3.4/3.7] Right ascension (J2000) (ra)degpos.eq.ra;meta.mainindexedDEJ2000[-30.5/-30.2] Declination (J2000) (dec)degpos.eq.dec;meta.mainindexedUsePhot1 if photometry is reliable (use_phot)meta.codeintzsp[2e-6/6.4]? Spectroscopic redshift (z_spec)src.redshiftdoublenullablez16[0.0017/18.8] Redshift posterior, 16% (z_16)src.redshift;pos.heliocentricdoublez50[0.0018/19.6] Redshift posterior, 50% (z_50)src.redshift;pos.heliocentricdoublez84[0.002/20] Redshift posterior, 84% (z_84)src.redshift;pos.heliocentricdoublelogMs16[5.7/11.4] Log of stellar mass, 16% (mstar_16)log(solMass)phys.massfloatlogMs50[5.7/11.4] Log of stellar mass, 50% (mstar_50)log(solMass)phys.massfloatlogMs84Log of stellar mass, 84% (mstar_84)log(solMass)phys.massfloatlogZ16[-2/0.2] Stellar metallicity, 16% (met_16)log(Sun)phys.abund.ZfloatlogZ50[-2/0.2] Stellar metallicity, 50% (met_50)log(Sun)phys.abund.ZfloatlogZ84Stellar metallicity, 84% (met_84)log(Sun)phys.abund.ZfloatwAge16[0.01/12.6] Mass-weighted age, 16% (mwa_16)Gyrtime.agefloatwAge50[0.017/13] Mass-weighted age, 50% (mwa_50)Gyrtime.agefloatwAge84Mass-weighted age, 84% (mwa_84)Gyrtime.agefloatdustd16[7.5e-5/4] Optical depth of diffuse dust, 16% (dust2_16)phys.absorption.opticalDepthdoubledustd50[0.00029/4] Optical depth of diffuse dust, 50% (dust2_50)phys.absorption.opticalDepthdoubledustd84Optical depth of diffuse dust, 84% (dust2_84)phys.absorption.opticalDepthdoubledusti16[-1/0.4] Power law index for a Calzetti+2000 attenuation curve, 16% (dust_index_16)spect.indexfloatdusti50[-1/0.4] Power law index for a Calzetti+ 2000ApJ...533..682C attenuation curve, 50% (dust_index_50)spect.indexfloatdusti84Power law index for a Calzetti+2000 attenuation curve, 84% (dust_index_84)spect.indexfloatdustf16[0.001/1.8] Ratio between the optical depth of birth cloud dust and diffuse dust, 16% (dust1_fraction_16)phys.absorption.opticalDepth;arith.ratiofloatdustf50[0.006/2] Ratio between the optical depth of birth cloud dust and diffuse dust, 50% (dust1_fraction_50)phys.absorption.opticalDepth;arith.ratiofloatdustf84Ratio between the optical depth of birth cloud dust and diffuse dust, 84% (dust1_fraction_84)phys.absorption.opticalDepth;arith.ratiofloatlogfagn16[-5/0.5] Logarithm of the ratio between the object's AGN luminosity and its bolometric luminosity, 16% (logfagn_16)phys.luminosity;arith.ratiofloatlogfagn50[-4.8/0.5] Log of the ratio between the object's AGN luminosity and its bolometric luminosity, 50% (logfagn_50)phys.luminosity;arith.ratiofloatlogfagn84Logarithm of the ratio between the object's AGN luminosity and its bolometric luminosity, 84% (logfagn_84)phys.luminosity;arith.ratiofloatsfr10p16[1.4e-9/1972] Star formation rate averaged over 10Myr, 16% (sfr10_16)solMass/yrphys.SFRdoublesfr10p50[4.9e-8/2776] Star formation rate averaged over 10Myr, 50% (sfr10_50)solMass/yrphys.SFRdoublesfr10p84[6.3e-7/4020] Star formation rate averaged over 10Myr, 84% (sfr10_84)solMass/yrphys.SFRdoublesfr30p16Star formation rate averaged over 30Myr, 16% (sfr30_16)solMass/yrphys.SFRdoublesfr30p50[7e-8/2047] Star formation rate averaged over 30Myr, 50% (sfr30_50)solMass/yrphys.SFRdoublesfr30p84Star formation rate averaged over 30Myr, 84% (sfr30_84)solMass/yrphys.SFRdoublesfr100p16[6.5e-9/694] Star formation rate averaged over 100Myr, 16% (sfr100_16)solMass/yrphys.SFRdoublesfr100p50[1e-7/793] Star formation rate averaged over 100Myr, 50% (sfr100_50)solMass/yrphys.SFRdoublesfr100p84Star formation rate averaged over 100Myr, 84% (sfr100_84)solMass/yrphys.SFRdoublessfr10p16[8e-17/3e-8] Specific star formation rate averaged over 10Myr, 16% (ssfr10_16)yr**-1phys.SFRdoublessfr10p50[3.6e-15/3.5e-8] Specific star formation rate averaged over 10Myr, 50% (ssfr10_50)yr**-1phys.SFRdoublessfr10p84Specific star formation rate averaged over 10Myr, 84% (ssfr10_84)yr**-1phys.SFRdoublessfr30p16Specific star formation rate averaged over 30Myr, 16% (ssfr30_16)yr**-1phys.SFRdoublessfr30p50[4e-15/3e-8] Specific star formation rate averaged over 30Myr, 50% (ssfr30_50)yr**-1phys.SFRdoublessfr30p84Specific star formation rate averaged over 30Myr, 84% (ssfr30_84)yr**-1phys.SFRdoublessfr100p16Specific star formation rate averaged over 100Myr, 16% (ssfr100_16)yr**-1phys.SFRdoublessfr100p50[6.5e-15/9.3e-9] Specific star formation rate averaged over 100Myr, 50% (ssfr100_50)yr**-1phys.SFRdoublessfr100p84[9e-14/9.5e-9] Specific star formation rate averaged over 100Myr, 84% (ssfr100_84)yr**-1phys.SFRdoublemuz16[0.1/3546] Magnification based z16, calculated from the public maps (mu_num_16)phot.mag;arith.ratiodoublemuz50[0.06/3689] Magnification based z50, calculated from the public maps (mu_num_50)phot.mag;arith.ratiodoublemuz84Magnification based z84, calculated from the public maps (mu_num_84)phot.mag;arith.ratiodoublerestU16[17.6/38] Rest-frame U-band AB mag, 16% (rest_U_16)magphot.mag;em.opt.UfloatrestU50[17.6/39] Rest-frame U-band AB mag, 50% (rest_U_50)magphot.mag;em.opt.UfloatrestU84[17.7/40.1] Rest-frame U-band AB mag, 84% (rest_U_84)magphot.mag;em.opt.UfloatrestV16[17.4/36.4] Rest-frame V-band AB mag, 16% (rest_V_16)magphot.mag;em.opt.VfloatrestV50[17.4/37.1] Rest-frame V-band AB mag, 50% (rest_V_50)magphot.mag;em.opt.VfloatrestV84Rest-frame V-band AB mag, 84% (rest_V_84)magphot.mag;em.opt.VfloatrestJ16[17/35.1] Rest-frame J-band AB mag, 16% (rest_J_16)magphot.mag;em.IR.JfloatrestJ50[17.2/35.7] Rest-frame J-band AB mag, 50% (rest_J_50)magphot.mag;em.IR.JfloatrestJ84Rest-frame J-band AB mag, 84% (rest_J_84)magphot.mag;em.IR.Jfloatrestu16[17.6/41] Rest-frame u-band AB mag, 16% (rest_up_16)magphot.mag;em.opt.Ufloatrestu50[17.7/42] Rest-frame u-band AB mag, 50% (rest_up_50)magphot.mag;em.opt.Ufloatrestu84[17.7/43] Rest-frame u-band AB mag, 84% (rest_up_84)magphot.mag;em.opt.Ufloatrestg16[17.2/37] Rest-frame g-band AB mag, 16% (rest_g_16)magphot.mag;em.opt.Bfloatrestg50[17.2/37.8] Rest-frame g-band AB mag, 50% (rest_g_50)magphot.mag;em.opt.Bfloatrestg84Rest-frame g-band AB mag, 84% (rest_g_84)magphot.mag;em.opt.Bfloatresti16[17.6/35.8] Rest-frame i-band AB mag, 16% (rest_i_16)magphot.mag;em.opt.Ifloatresti50[17.6/36.4] Rest-frame i-band AB mag, 50% (rest_i_50)magphot.mag;em.opt.Ifloatresti84Rest-frame i-band AB mag, 84% (rest_i_84)magphot.mag;em.opt.IfloatU-V16[-0.8/6.3] Rest-frame U-V color, 16% (UV_16)magphot.color;em.opt.U;em.opt.VfloatU-V50[-0.7/6.4] Rest-frame U-V color, 50% (UV_50)magphot.color;em.opt.U;em.opt.VfloatU-V84Rest-frame U-V color, 84% (UV_84)magphot.color;em.opt.U;em.opt.VfloatV-J16[-1.4/4] Rest-frame V-J color, 16% (VJ_16)magphot.color;em.opt.V;em.IR.JfloatV-J50[-1.4/4.1] Rest-frame V-J color, 50% (VJ_50)magphot.color;em.opt.V;em.IR.JfloatV-J84Rest-frame V-J color, 84% (VJ_84)magphot.color;em.opt.V;em.IR.Jfloatg-i16[-0.7/5.4] Rest-frame synthetic g-i, 16% (gi_16)magphot.color;em.opt.B;em.opt.Ifloatg-i50[-0.7/5.5] Rest-frame synthetic g-i, 50% (gi_50)magphot.color;em.opt.B;em.opt.Ifloatg-i84Rest-frame synthetic g-i, 84% (gi_84)magphot.color;em.opt.B;em.opt.Ifloatu-g16[-0.3/8] Rest-frame synthetic u-g, 16% (ug_16)magphot.color;em.opt.U;em.opt.Bfloatu-g50[-0.3/8.1] Rest-frame synthetic u-g, 50% (ug_50)magphot.color;em.opt.U;em.opt.Bfloatu-g84Rest-frame synthetic u-g, 84% (ug_84)magphot.color;em.opt.U;em.opt.Bfloatchi2[6e-7/4502] Best-fit chi^2^, assuming a minimum error of 5% (chi2)stat.fit.chi2;meta.modelleddoubleNb[2/15] Number of bands used in the fit (nbands)meta.numberintzEazy[0.01/20]? Peak of p(z) from fitting with eazy-sfhz-corr (z_eazy)src.redshift.photdoublenullablezEazy16? P(z), 16% (z_eazy_16)src.redshift.photdoublenullablezEazy50[0.01/19.8]? P(z), 50% (z_eazy_50)src.redshift.photdoublenullablezEazy84? P(z), 84% (z_eazy_84)src.redshift.photdoublenullableIDDR1[1/50365]? ID of the source in the DR1 cat. (id_DR1)meta.idintnullableMSA[2008/60157]? ID of the source in the team internal MSA catalog (Price+ 2023arXiv231002500P); all within <0.24" radius (id_msa)meta.id.crossintnullableALMA[1/69]? ID of ALMA source from Fujimoto+ 2023, in prep. (id_alma)meta.id.crossintnullableUseAper[0.3/1.4] Diameter adopted for color aperture (use_aper)arcsecphys.angSizefloatf_kron[0/1]? 1 for systematically underestimated photometry (i.e., the kron radius is not robust,thus the total photometry assumes point-lke light distribution) (flag_kron)meta.codeintnullable