J/MNRAS/495/1807ivo://CDS.VizieR/J/MNRAS/495/1807doi:10.26093/cds/vizier.74951807CDSArrabal Haro P.Rodriguez Espinosa J.M.Munoz-Tunon C.Sobral D.,Lumbreras-Calle A.Boquien M.Hernan-Caballero A.Rodriguez-Munoz L.,Alcalde Pampliega B.2024-08-21T20:14:28Z2023-09-04T12:13:16ZCDS support team

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

cds-question@unistra.frgalaxiesredshiftedstellar-populationsstellar-agesastronomical-modelsvisible-astronomyinfrared-astronomyLyman alpha emitters (LAEs) and Lyman break galaxies (LBGs) represent the most common groups of star-forming galaxies at high z, and the differences between their inherent stellar populations (SPs) are a key factor in understanding early galaxy formation and evolution. We have run a set of SP burst-like models for a sample of 1558 sources at 3.4<z<6.8 from the Survey for High-z Absorption Red and Dead Sources (SHARDS) over the GOODS-N field. This work focuses on the differences between the three different observational subfamilies of our sample: LAE-LBGs, no-Ly{alpha} LBGs, and pure LAEs. Single and double SP synthetic spectra were used to model the spectral energy distributions, adopting a Bayesian information criterion to analyze under which situations a second SP is required. We find that the sources are well modelled using a single SP in ~79 per cent of the cases. The best models suggest that pure LAEs are typically young low-mass galaxies (t~26^+41^_-25_Myr; M_star_~5.6^+12.0^_-5.5_x10^8^M_{sun}_), undergoing one of their first bursts of star formation. On the other hand, no-Ly{alpha} LBGs require older SPs (t~71+/-12Myr), and they are substantially more massive (M_star_~3.5+/-1.1x10^9^M_{sun}_). LAE-LBGs appear as the subgroup that more frequently needs the addition of a second SP, representing an old and massive galaxy caught in a strong recent star-forming episode. The relative number of sources found from each subfamily at each z supports an evolutionary scenario from pure LAEs and single SP LAE-LBGs to more massive LBGs. Stellar mass functions are also derived, finding an increase of M_*_ with cosmic time and a possible steepening of the low-mass slope from z~6 to z~5 with no significant change to z~4. Additionally, we have derived the SFR-M_star_ relation, finding an SFR{prop.to}M_star_^{beta}^ behaviour with negligible evolution from z~4 to z~6.2020MNRAS.495.1807Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/495/1807CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/478/3740 : High-z LAEs and LBGs in SHARDS survey (Arrabal Haro+, 2018)J/ApJ/762/46 : SHARDS: GOODS-N spectrophotometry surveyII/261 : GOODS initial results (Giavalisco+, 2004)J/ApJ/675/234 : Stellar mass functions for galaxies 0<z<4J/ApJS/218/33 : Spitzer-CANDELS catalog within 5 deep fields (Ashby+, 2015)J/ApJS/193/13 : Spitzer/IRAC sources in the EGS I. SEDs (Barro+, 2011)J/ApJS/193/30 : UV-to-FIR analysis of sources in the EGS. II.https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/495/1807https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/495/1807http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/495/1807https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/495/1807https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/495/1807http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/495/1807GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/495/1807/table2 (Main physical parameters derived from the best models fitted to each source)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/495/1807/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/495/1807/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/495/1807/table2?GETtext/xml+votable180.050000true188.95041762.2006670.0055555555555555566/11252https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/495/1807?format=asciiOpticalInfrareddefaultJ/MNRAS/495/1807/table2Main physical parameters derived from the best models fitted to each sourceSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource name (SHARDSNNNNNNNN)meta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainzRedshiftsrc.redshiftfloate_zError on zstat.error;src.redshiftfloatMstarmMain stellar population mass1e+09solMassphys.massfloate_MstarmError on Mstarm1e+09solMassstat.errorfloatAgemMain stellar population ageMyrtime.age;meta.maininte_AgemError on AgemMyrstat.errorinttau0Main stellar population e-folding time stellar populationsMyrtime.epoch;meta.main;meta.modelledfloate_tau0Error on tau0Myrstat.errorfloatMstarb? Burst stellar mass (1)1e+09solMassphys.massfloatnullablee_Mstarb? Error on Mstarb1e+09solMassstat.errorfloatnullableAgeb? Burst age (1)Myrtime.ageintnullablee_Ageb? Error on AgebMyrstat.errorintnullabletau1? Burst e-folding time (1)Myrtime.epoch;meta.main;meta.modelledfloatnullablee_tau1? Error on tau1Myrstat.errorfloatnullable