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Fig. 14.

image

Best fit specific SFR (sSFR) as a function of stellar mass for galaxies at 3 < z < 4, as derived from their UV-to-NIR SEDs. The whole ZFOURGE sample (in COSMOS and UDS) is shown as small dots, and the z > 3 quiescent galaxies observed with MOSFIRE are shown as red stars with gray error bars. Filled and open symbols refer to galaxies with and without a zspec, respectively (values are listed in Table 3). The locus of the main sequence for the ZFOURGE galaxies is shown with a blue line. Different definitions for “quiescence” are shown in gray: the one we adopted in this paper, sSFR = sSFRQ = 0.15 Gyr−1 (dashed), sSFR = 1/(3 tH (dot-dashed, tH being the age of the Universe), and sSFR = 0.01 Gyr−1 (dotted). The sSFR measured in stacks of ALMA imaging at z ∼ 4 is shown with yellow squares (Schreiber et al. 2017), and was corrected down by a factor 1.3 to account for redshift evolution of the sSFR between z  =  3.5 and z  =  4. As in Fig. 13, for display purposes we place a limit on the minimum sSFR of 10−3 Gyr−1, which is indicated with the dashed pink line. The hashed region on the bottom left shows the region of this parameter space where the ZFOURGE catalogs are incomplete because of the Ks magnitude limit.

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