Date Published:
July 1, 2015
Abstract:
We utilize ΛCDM halo occupation models of galaxy clustering toinvestigate the evolving stellar mass dependent clustering of galaxiesin the PRIsm MUlti-object Survey (PRIMUS) and DEEP2 Redshift Survey overthe past eight billion years of cosmic time, between 0.2\lt z\lt 1.2.These clustering measurements provide new constraints on the connectionsbetween dark matter halo properties and galaxy properties in the contextof the evolving large-scale structure of the universe. Using both ananalytic model and a set of mock galaxy catalogs, we find a strongcorrelation between central galaxy stellar mass and dark matter halomass over the range {M}
{halo}˜{10}
11-{10}
13 {h}
-1{M}
⊙ , approximately consistent with previousobservations and theoretical predictions. However, the stellar-to-halomass relation and the mass scale where star formation efficiency reachesa maximum appear to evolve more strongly than predicted by other models,including models based primarily on abundance-matching constraints. Wefind that the fraction of satellite galaxies in halos of a given massdecreases significantly from z˜ 0.5 to z˜ 0.9, partly due to thefact that halos at fixed mass are rarer at higher redshift and havelower abundances. We also find that the{M}
1/{M}
{min} ratio, a model parameter thatquantifies the critical mass above which halos host at least onesatellite, decreases from ≈ 20 at z˜ 0 to ≈ 13 at z˜ 0.9.Considering the evolution of the subhalo mass function vis-à-vissatellite abundances, this trend has implications for relations betweensatellite galaxies and halo substructures and for intracluster mass,which we argue has grown due to stripped and disrupted satellitesbetween z˜ 0.9 and z˜ 0.5.
Website
