Spectral Energy Distributions of Companion Galaxies to z$\sim$6 Quasars

Abstract

Massive, quiescent galaxies are already observed at redshift $z\sim4$, i.e. $\sim$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\gtrsim$6 quasars have discovered [CII]- 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 $z\gtrsim 6$, 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 SFR$_{\rm UV}<$few M$_{\odot}$ yr$^{-1}$, and a stellar content of $M_{*}<$10$^{10}$ M$_{\odot}$ yr$^{-1}$. However, the companion to PJ167-13 shows bright rest-frame UV emission (F140W AB = 25.48). Its SED resembles that of a star-forming galaxy with a total SFR$\sim$50 M$_{\odot}$ yr$^{-1}$ and $M_{*}\sim 9 \times 10^{9}$ M$_{\odot}$. All the companion sources are consistent with residing on the galaxy main sequence at $z\sim$6. Additional, deeper data from future facilities, such as JWST, are needed in order to characterize these gas-rich sources in the first Gyr of cosmic history.