with increasing galaxy density before peaking and then decreasing at the highest local densities. These results are not reproduced by a SAM using the Millennium simulation. In the SAM, there is never a reversal of the SFR-density relation, just a gradual flattening (it is not flat by $z$$=$1). When only examining galaxies with 5$\times$10$^{10}$ $<$ M$_*$/M$_{\odot}$ $<$ 5$\times$10$^{11}$, E07 finds that the sSFR increases with increasing local density. They claim that the increase of $<$SFR$>$ with local density is due to increases of both M$_*$ and sSFR with galaxy density. Because in general sSFR decreases with increasing M$_*$ (e.g. Blanton et al. 2003; Baldry et al. 2004), they find it likely that the environment enhances the SFR of massive galaxies.

In order to examine comparable galaxy samples, we examine galaxies from our $z$=1 and $z$=0 outputs and use the same magnitude cut as E07 (M$_{\mathrm{B}}$ $\le$ -20). As discussed in Section \[sec:galaxyselection\], we also only include galaxies with M$_*$ $>$ 5$\times$10$^{9}$ M$_{\odot}$. All galaxies that fulfill our magnitude and mass criteria are included in our sample. Recall that the M$_{\mathrm{B}}$ cut in E07 is equivalent to an M$_*$ cutoff of 10$^9$ M$_\odot$ and 10$^{10}$ M$_\odot$ at $z$$=$0.8 and $z$$=$1.2, respectively, 