redshift for this sample of massive, quiescent galaxies. We note that the scatter is measured from the actual colors of the quiescent sample, not the dust-corrected colors shown in Figure 1, as there are degeneracies in the models that limit the level of accurarcy of $A_{V}$. To interpret this increase we need to correct for the scatter introduced by photometric errors, thereby measuring the intrinsic scatter. For each quiescent galaxy, the observed $u$-8$\mu$m fluxes were each perturbed by a normally-distributed, pseudo-random number from a Gaussian distribution with a mean of zero and a standard deviation of the photometric error for each respective filter. From these perturbed flux values, we generate 50 simulated catalogs and use EAZY to re-determine $U$-$V$, refitting the photometric redshifts. We take the biweight sigma of the $U$-$V$ distribution for each galaxy to signify the uncertainty in the color. The average uncertainty in the colors due to photometric error for all massive ($>$10$^{11}$ M$_{\odot}$) galaxies ranges from 0.008 mag at $z$=0.5 to 0.05 mag at $z$=2[^5].

We calculated the contribution of the photometric error to our measurement in the scatter of $U$-$V$ by creating a sample of mock galaxies with an intrinsic scatter of 0 (in other 