or color-density relations (E07; Cucciati et al. 2006; 2012).

In this paper we present the SFR-density, sSFR-density, and quiescent fraction of galaxies at $z$ = 0 and $z$ $=$ 1 in a hydrodynamic cosmological simulation. We choose these redshifts in order to compare our results to recent work, specifically E07, C08, and Q12. We focus on one region centered around a cluster within a large simulation with box side of 120 $h^{-1}$ Mpc, with size 21$\times$ 24$\times$20 $h^{-3}$ Mpc$^3$, which gives us a broad range of local environments to study. Our goal is to gain physical insight into what sets galaxy SFRs by comparing the SFR, sSFR, and quiescent fraction as a function of environmental density on the same galaxy sample.

After a brief description of our simulations (Section \[sec:boxes\]), we discuss our galaxy selection technique and our method for determining quantities for each galaxy in Section \[sec:galaxyselection\]. In Section \[sec:localdensity\] we define our local density parameter. In Section \[sec:obscomparisons\] we compare our results to E07 (Section \[sec:E07\]), C08 (Section \[sec:C08\]) and Q12 (Section \[sec:Q12\]). We then discuss and interpret our results in terms of the halo mass (§\[sec:story\]), and highlight why our results differ from those based on semi-analytic 