The Brightest Galaxies in the Dark Ages: Galaxies' Dust Continuum Emission during the Reionization Era

Though half of cosmic starlight is absorbed by dust and reradiated at long wavelengths (3 μm-3 mm), constraints on the infrared through the millimeter galaxy luminosity function (or the "IRLF") are poor in comparison to the rest-frame ultraviolet and optical galaxy luminosity functions, particularly at z 2.5. Here, we present a backward evolution model for interpreting number counts, redshift distributions, and cross-band flux density correlations in the infrared and submillimeter sky, from 70 μm-2 mm, using a model for the IRLF out to the epoch of reionization. Mock submillimeter maps are generated by injecting sources according to the prescribed IRLF and flux densities drawn from model spectral energy distributions that mirror the distribution of SEDs observed in 0 < z < 5 dusty star-forming galaxies (DSFGs). We explore two extreme hypothetical case studies: a dust-poor early universe model, where DSFGs contribute negligibly (<10%) to the integrated star formation rate density at z > 4; and an alternate dust-rich early universe model, where DSFGs dominate ∼90% of z > 4 star formation. We find that current submm/mm data sets do not clearly rule out either of these extreme models. We suggest that future surveys at 2 mm will be crucial to measuring the IRLF beyond z ∼ 4. The model framework developed in this paper serves as a unique tool for the interpretation of multiwavelength IR/submm extragalactic data sets, and will enable more refined constraints on the IRLF than can be made from direct measurements of individual galaxies' integrated dust emission.