and increase more quickly with increasing local density. We speculate that rerunning our simulation with a lower star formation efficiency might lower early SFRs, producing lower-mass galaxies.

Comparing the SFR-density and sSFR-density relations {#sec:C08}
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We next use a galaxy sample matched to that in C08 to compare the SFR-density relation to the sSFR-density relation. As in C08, in this section at each redshift we use the same galaxy sample when we measure the SFR and sSFR as a function of density. C08 used SDSS galaxies at low redshift and the DEEP2 sample at $z$$\sim$1. The color-independent completeness limit of the DEEP2 survey at $z$ = 1.05 is M$_{\mathrm{B}}$ $\le$ -20.6, so in their DEEP2-C sample they use a redshift-dependent magnitude cut that is M$_{\mathrm{B}}$ $\le$ -20.53 at $z$=1 and M$_{\mathrm{B}}$ $\le$ -19.16 at $z$=0 (SDSS-B sample). We choose to compare to this magnitude-limited observed sample because the magnitude limit acts to remove the lowest-mass galaxies from their sample (see C08 Figure 7). This results in a closer match to the mass range in our simulated sample, which, as discussed in Section \[sec:galaxyselection\], has a minimum stellar mass of 5$\times$10$^{9}$ M$_{\odot}$.

Our median sSFR and SFR as a function of 