The Halo Mass Function: High‐Redshift Evolution and Universality

Abstract

We study the formation of dark matter halos in the concordance ΛCDM model over a wide range of redshifts, from z = 20 to the present. Our primary focus is the halo mass function, a key probe of cosmology. By performing a large suite of nested-box N-body simulations with careful convergence and error controls (60 simulations with box sizes from 4 to 256 h −1 Mpc), we determine the mass function and its evolution with excellent statistical and systematic errors, reaching a few percent over most of the considered redshift and mass range. Across the studied redshifts, the halo mass is probed over 6 orders of magnitude (10 7 -10 13.5 h −1 M ⊙ ). Historically, there has been considerable variation in the high redshift mass function as obtained by different groups. We have made a concerted effort to identify and correct possible systematic errors in computing the mass function at high-redshift and to explain the discrepancies between some of the previous results. We discuss convergence criteria for the required force resolution, simulation box size, halo mass range, initial and final redshifts, and time stepping. Because of conservative cuts on the mass range probed by individual boxes, our results are relatively insensitive to simulation volume, the remaining sensitivity being consistent with extended Press-Schechter theory. Previously obtained mass function fits near z = 0, when scaled by linear theory, are in good agreement with our results at all redshifts, although a mild redshift dependence consistent with that found by Reed et al. may exist at low redshifts. Overall, our results are consistent with a "universal" form for the mass function at high redshifts.

Probing the first galaxies with the Square Kilometer Array

“…Our halo mass functions are in very good agreement with other recent work (e.g. Reed et al 2007;Lukic et al 2007;Cohn & White 2008). The second step produces a hydrodynamic + RT simulation with moderate resolution, but incorporating subgrid physics modeled using the high-resolution information from the large N-body simulation.…”

The Cosmogrid Simulation: Statistical Properties of Small Dark Matter Halos

“…Here, we examine the mass function of mass below 10 10 M down to 10 7 M . The mass function of this range has been studied only in high redshift (e.g., Reed et al 2007;Lukić et al 2007). Figure 4 shows the halo mass functions at three different redshifts for the CG2048 run and the prediction of the Sheth & Tormen formula (ST, Sheth & Tormen 1999).…”

The evolution of the star formation rate function in the EAGLE simulations: a comparison with UV, IR and Hα observations from z ∼ 8 to z ∼ 0

“…In the following paragraphs we will see that at this era higher mass haloes (M halo = 10 11-12 M ) dominate the CSFRD. From z ∼ 5 to z ∼ 1 the total number of haloes with masses M halo = 10 9-10 M slightly increases, while from z ∼ 1 to z ∼ 0 it is kept almost constant (Warren et al 2006;Lukić et al 2007). At z ∼ 0 only 0.6 per cent of them are able to form stars, with their efficiency being onlyṀ /M gas ∼ 6.6 × 10 −12 yr −1 .…”