Quiescent Galaxies 1.5 Billion Years after the Big Bang and Their Progenitors

We report two secure (z = 3.775, 4.012) and one tentative (z 3.767) spectroscopic confirmations of massive and quiescent galaxies through K-band observations with Keck/MOSFIRE and Very Large Telescope/X-Shooter. The stellar continuum emission, absence of strong nebular emission lines, and lack of significant far-infrared detections confirm the passive nature of these objects, disfavoring the alternative solution of low-redshift dusty star-forming interlopers. We derive stellar masses of log(M-star/M-circle dot) similar to 11 and ongoing star formation rates placing these galaxies greater than or similar to 1-2 dex below the main sequence at their redshifts. The adopted parameterization of the star formation history suggests that these sources experienced a strong (< SFR > similar to 1200-3500 M-circle dot yr(-1)) and short (similar to 50 Myr) burst of star formation, peaking similar to 150-500 Myr before the time of observation, all properties reminiscent of the characteristics of submillimeter galaxies (SMGs) at z > 4. We investigate this connection by comparing the comoving number densities and the properties of these two populations. We find a fair agreement only with the deepest submillimeter surveys detecting not only the most extreme starbursts but also more normal galaxies. We support these findings by further exploring the Illustris TNG cosmological simulation, retrieving populations of both fully quenched massive galaxies at z similar to 3-4 and SMGs at z similar to 4-5, with number densities and properties in agreement with the observations at z similar to 3 but in increasing tension at higher redshift. Nevertheless, as suggested by the observations, not all of the progenitors of quiescent galaxies at these redshifts shine as bright SMGs in their past, and, similarly, not all bright SMGs quench by z similar to 3, both fractions depending on the threshold assumed to define the SMGs themselves.