Spectral Energy Distributions of Companion Galaxies to z ∼ 6 Quasars

Abstract

Massive, quiescent galaxies are already observed at redshift z similar to 4, i.e., similar to 1.5 Gyr after the big bang. Current models predict them to be formed via massive, gas-rich mergers at z > 6. Recent ALMA observations of the cool gas and dust in z greater than or similar to 6 quasars have discovered [C II]- and far-infrared-bright galaxies adjacent to several quasars. In this work, we present sensitive imaging and spectroscopic follow-up observations, with HST/WFC3, Spitzer/IRAC, VLT/MUSE, Magellan/FIRE, and LBT/LUCI-MODS, of ALMA-detected, dust-rich companion galaxies of four quasars at z greater than or similar to 6, specifically acquired to probe their stellar content and unobscured star formation rate. Three companion galaxies do not show significant emission in the observed optical/IR wavelength range. The photometric limits suggest that these galaxies are highly dust-enshrouded, with unobscured star formation rates SFRUV < few M-circle dot yr(-1), and a stellar content of M-* < 10(10) M(circle dot)yr(-1). However, the companion to PJ167-13 shows bright rest-frame UV emission (F140W AB = 25.48). Its spectral energy distribution resembles that of a star-forming galaxy with a total SFR similar to 50 M-circle dot yr(-1) and M-* similar to 9 x 10(9) M-circle dot. All the companion sources are consistent with residing on the galaxy main sequence at z similar to 6. Additional, deeper data from future facilities, such as the James Webb Space Telescope, are needed in order to characterize these gas-rich sources in the first gigayear of cosmic history.