Song, MimiMimiSongFinkelstein, Steven L.Steven L.FinkelsteinAshby, Matthew L. N.Matthew L. N.AshbyGRAZIAN, AndreaAndreaGRAZIANLu, YuYuLuPapovich, CaseyCaseyPapovichSalmon, BrettBrettSalmonSomerville, Rachel S.Rachel S.SomervilleDICKINSON, MARKMARKDICKINSONDuncan, K.K.DuncanFaber, Sandy M.Sandy M.FaberFazio, Giovanni G.Giovanni G.FazioFerguson, Henry C.Henry C.FergusonFONTANA, AdrianoAdrianoFONTANAGuo, YichengYichengGuoHathi, NimishNimishHathiLee, Seong-KookSeong-KookLeeMERLIN, EmilianoEmilianoMERLINWillner, S. P.S. P.Willner2020-05-202020-05-2020160004-637Xhttp://hdl.handle.net/20.500.12386/25014We present galaxy stellar mass functions (GSMFs) at z = 4-8 from a rest-frame ultraviolet (UV) selected sample of ∼4500 galaxies, found via photometric redshifts over an area of ∼280 arcmin<SUP>2</SUP> in the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS)/Great Observatories Origins Deep Survey (GOODS) fields and the Hubble Ultra Deep Field. The deepest Spitzer/IRAC data to date and the relatively large volume allow us to place a better constraint at both the low- and high-mass ends of the GSMFs compared to previous space-based studies from pre-CANDELS observations. Supplemented by a stacking analysis, we find a linear correlation between the rest-frame UV absolute magnitude at 1500 Å ({M}<SUB>{{UV</SUB>}}) and logarithmic stellar mass ({log}{M}<SUB>* </SUB>) that holds for galaxies with {log}({M}<SUB>* </SUB>/{M}<SUB>☉ </SUB>)≲ 10. We use simulations to validate our method of measuring the slope of the {log}{M}<SUB>* </SUB>-M <SUB>UV</SUB> relation, finding that the bias is minimized with a hybrid technique combining photometry of individual bright galaxies with stacked photometry for faint galaxies. The resultant measured slopes do not significantly evolve over z = 4-8, while the normalization of the trend exhibits a weak evolution toward lower masses at higher redshift. We combine the {log}{M}<SUB>* </SUB>-M <SUB>UV</SUB> distribution with observed rest-frame UV luminosity functions at each redshift to derive the GSMFs, finding that the low-mass-end slope becomes steeper with increasing redshift from α =-{1.55}<SUB>-0.07</SUB><SUP>+0.08</SUP> at z = 4 to α =-{2.25}<SUB>-0.35</SUB><SUP>+0.72</SUP> at z = 8. The inferred stellar mass density, when integrated over {M}<SUB>* </SUB>={10}<SUP>8</SUP>-10<SUP>13</SUP> M <SUB>☉</SUB>, increases by a factor of {10}<SUB>-2</SUB><SUP>+30</SUP> between z = 7 and z = 4 and is in good agreement with the time integral of the cosmic star formation rate density.STAMPAenArticle10.3847/0004-637X/825/1/52-s2.0-84978194621000381930000005https://iopscience.iop.org/article/10.3847/0004-637X/825/1/52016ApJ...825....5SFIS/05 - ASTRONOMIA E ASTROFISICA