Galaxy population constraints on cosmology and star formation in the early Universe

We present the first post-cosmic-microwave-background early-Universe observational constraints on $σ_8$, $Ω_{\rm m}$, mean galaxy star-forming efficiency and galaxy UV magnitude scatter at redshifts $z = 4-10$. We perform a simultaneous 11-parameter cosmology and star-formation physics fit using the new code GalaxyMC, with redshift $z>4$ galaxy UV luminosity and correlation function data. Consistent with previous studies, we find evidence for redshift-independent star formation physics, regulated by halo assembly. For a flat $Λ$CDM universe with a low-redshift Hubble constant and a Type Ia supernovae $Ω_{\rm m}$ prior, we constrain $σ_8 = 0.81 \pm 0.03$, and a mean star-forming efficiency peaking at $\log_{10} {\rm SFE} = -[(0.09 \pm 0.20) + (0.58 \pm 0.29) \times \log_{10} (1+z)]$ for halo mass $\log_{10} M_{\rm p} / h^{-1} M_{\odot} = 11.48 \pm 0.09$. The suppression of star formation due to feedback is given by a double power law in halo mass with indices $α= 0.56 \pm 0.08, β= -1.03 \pm 0.07$. The scatter in galaxy UV magnitude for fixed halo mass is $σ_M = 0.56 \pm 0.08$. Without a prior on $Ω_{\rm m}$ we obtain $σ_8 = 0.78 \pm 0.06$, $Ω_{\rm m} = 0.33 \pm 0.07$ and at most $1σ$ differences in all other parameter values. Our best-fit galaxy luminosity functions yield a reionization optical depth $τ\approx 0.048$, consistent with the Planck 2018 value.