median value of the photometric scatter and the horizontal black error bars are the bin size. The grey filled region indicates the range of $\sigma_{U-V}$ values we measure when we raise and lower the horizontal limit in Figure 1 by 0.2 magnitudes, thereby changing the number of quiescent galaxies selected. Regardless of the selection limit, we find an increasing intrinsic scatter with redshift. We compare our measurements to work done by @Bower92 in the Coma Cluster, as well as a study of the massive (M$_{\mathrm{dyn}}\!>$10$^{11}$ M$_{\odot}$) early-type galaxies in 7 clusters from $z$=0.18 to 0.84 [@vanDokkum08b]. We find that the scatter at $z$=0.5 is similar to the intrinsic scatter of field galaxies recently measured by @Ruhland09[^6], but a factor of 2 higher than that measured previously in clusters at these redshifts. This may reflect a systematic difference between field and cluster galaxies or some unrecognizable error contribution within our data. We note that if we limit the quiescent sample to the 75 galaxies with a spectroscopic redshift between $0.2<z<0.9$, we find a very similar (somewhat larger) scatter. @vanDokkum07 found that the massive red sequence galaxies in clusters are typically $\sim$0.4$\pm$0.2 Gyr older than field galaxies. If quenching in the cluster 