local density (M$_{\mathrm{sph}}$) are shown in Figure \[fig-Cooper\]. As in C08, we simply take the median SFR or sSFR of all galaxies that fall into a bin of local density (M$_{\mathrm{sph}}$) (rather than the median of the average SFR or sSFR in each M$_{\mathrm{sph}}$ as in Section \[sec:E07\]). As in the previous figures, the $z$=0 LR is blue $\bigcirc$, $z$=1 LR is orange $\bigtriangleup$, and $z$=1 HR is red $\nabla$. The horizontal lines denote the M$_{\mathrm{sph}}$ bin sizes. The shaded regions enclose the region between the 25th and 75th percentiles of the $z$=1 HR (red) and $z$=0 LR (blue) samples. Our bins are selected to include at least 100 galaxies. We overplot estimates of the values from Figures A1 & A2 in C08. As in Sec. 3.1, we re-scale the observed density measure to compare directly with our own density measure, M$_{\mathrm{sph}}$. The DEEP2 survey does not probe clusters, but includes somewhat larger groups at $z$$\sim$1 than the GOODS fields (Gerke et al. 2005), so we align M$_{\mathrm{sph}}$ with the density measure in C08 such that the highest local density measurement in DEEP2 is in a DM sphere of 2$\times$10$^{13}$ M$_{\odot}$. We again assume that there is a one-to-one relationship 