scatter introduced by photometric and systematic errors at $z\!\sim$2.[]{data-label="scatter"}](fig3_sm.eps)

From Figure \[scatter\], we see that the intrinsic scatter in the colors of quiescent galaxies increases out to $z\!\sim1$ and likely continues to increase to $z\!\sim$2, although there may exist selection biases in this regime. It seems likely that the trend at $1<z<2$ is real given the recent results of @Hilton09, who measure an intrinsic $z_{\mathrm{850}}$-$J$ scatter (close to the rest-frame $U$-$V$) of 0.123$\pm$0.049 magnitudes for a cluster at $z=1.46$, and @Papovich10, who find $\sigma_{\mathrm{U-B}}$=0.136$\pm$0.024 magnitudes for a cluster at $z=1.62$. Furthermore, the color scatter is in qualitative agreement with the predictions of simple passive evolution models that the scatter in color should decrease as the galaxies evolve.

Origin of the Intrinsic Scatter in Quiescent Galaxies
-----------------------------------------------------

To understand the origin of the intrinsic scatter in $U$-$V$, we consider the properties of these stellar populations through spectral synthesis modeling. The scatter in the red sequence is thought to be determined by the scatter in both the age and metallicity, where the scatter in relative ages is generally thought to be the dominant driver [e.g. @Bower92; @Gallazzi06]. The range of metallicities observed for local red sequence ellipticals from SDSS DR2 is $\sim$0.8-1.6 