Abstract
The evolution of halos with masses around M h ≈ 1011 M ⊙ and M h ≈ 1012 M ⊙ at redshifts z > 9 is examined using constrained N-body simulations. The average specific mass accretion rates, Ṁh/Mh , exhibit minimal mass dependence and generally agree with existing literature. Individual halo accretion histories, however, vary substantially. About one-third of simulations reveal an increase in Ṁh around z ≈ 13. Comparing simulated halos with observed galaxies having spectroscopic redshifts, we find that for galaxies at z ≳ 9, the ratio between observed star formation rate and Ṁh is approximately 2%. This ratio remains consistent for the stellar-to-halo mass ratio (SHMR) but only for z ≳ 10. At z ≃ 9, the SHMR is notably lower by a factor of a few. At z ≳ 10, there is an agreement between specific star formation rates (sSFRs) and Ṁh/Mh . However, at z ≃ 9, observed sSFRs exceed simulated values by a factor of 2. It is argued that the mildly elevated SHMR in high-z halos with M h ≈ 1011 M ⊙ can be achieved by assuming the applicability of the local Kennicutt–Schmidt law and a reduced effectiveness of stellar feedback due to deeper gravitational potential of high-z halos of a fixed mass.
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