affect these properties (Cen 2011c). This is done by summing the dark matter mass directly, not demanding that it is within the virial radius of any galaxy. We randomly select 27 000 positions within the refined region (with a 2 $h^{-1}$ Mpc buffer at each edge) to be the center of the spheres. Thus we oversample our box and end up with a total of 27 000 environments that we probe, which we differentiate by the dark matter mass in the sphere, M$_{\mathrm{sph}}$. However, not every r=1 $h^{-1}$ Mpc sphere will contain a galaxy, so when we determine galaxy properties as a function of environment, we only consider those spheres that contain galaxies. This technique of choosing random spheres in space rather than spheres centered on galaxies differs from that used by many observers, however, E07 compare average SFRs found in regions centered on galaxies to those found in regions centered on grid points independent of galaxy positions, and find negligible difference between the two techniques.

Results {#sec:obscomparisons}
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The reversal of the $<$SFR$>$-density relation {#sec:E07}
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We first determine whether our SFR-density relation evolves from $z$$=$0 to $z$$=$1. To facilitate comparisons to E07 we use similar galaxy selection criteria 