which point the $<$SFR$>$ increases. We compare the $<$SFR$>$ in the lowest and highest M$_{\mathrm{sph}}$ bins, and find that the comparison is quite different in the $z$$=$1 and $z$$=$0 samples. At $z$=1 the $<$SFR$>$ in the highest M$_{\mathrm{sph}}$ bin is nearly an order of magnitude more than the $<$SFR$>$ in the lowest M$_{\mathrm{sph}}$ bin, while at $z$=0 the $<$SFR$>$ in the highest M$_{\mathrm{sph}}$ bin is three times that in the lowest M$_{\mathrm{sph}}$ bin.

In Figure \[fig-elbaz\] we include all galaxies that fulfill our luminosity and mass criteria, including both star-forming and passive galaxies. However, our result that the $<$SFR$>$-density relation is much steeper at $z$=1 than at $z$=0 is robust to whether or not we include only star-forming galaxies. If we limit our sample to galaxies with SFR $>$ 0.5 M$_{\odot}$ yr$^{-1}$ (at both $z$=0 and $z$=1), the median $<$SFR$>$ is unchanged up to M$_{\mathrm{sph}}$ $=$ 3$\times$10$^{12}$ M$_{\odot}$, and the median $<$SFR$>$ in our five highest density bins increases by at most 33% in the $z$=1 (HR or LR) outputs, and by as much as a factor of two in our $z$=0 output. The $z$=1 $<$SFR$>$ remains universally higher than the $z$=0 $<$SFR$>$.

For comparison, we also plot values from 