sSFRs. The observational selection of quiescent galaxies in this work is less model dependent than @Romeo08 for example, who select quiescent galaxies by sSFR $<$0.01 Gyr$^{-1}$ from their simulations. About $\sim$35% of our quiescent galaxies at $1.8<z<2.2$ appear to have sSFRs $>$0.01 Gyr$^{-1}$, with a maximum sSFR of $\sim$0.06 Gyr$^{-1}$ (as determined from SED modeling). This fraction decreases to $\sim$14% by $0.2<z<0.9$, with a maximum sSFR of 0.02 Gyr$^{-1}$. A sample of quiescent galaxies selected solely on best-fit sSFR would be biased against including the blue tail of the distribution of galaxies that may be the most recent additions to the red sequence. In Appendix A, we repeat key parts of the analysis using an alternative selection of quiescent galaxies, the $UVJ$ method of @Labbe05 and @Williams09. This method naturally isolates a distinct sequence of “red and dead” galaxies in the rest-frame $U$-$V$ versus $V$-$J$ diagram. We find that the results remain essentially unchanged when this selection is used, but note that the $UVJ$ selection includes a slightly higher number of blue galaxies at high redshift.

Deriving the Intrinsic Scatter in Quiescent Galaxies
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In Figure \[scatter\], we show that the observed scatter in the $U$-$V$ color (green) increases with 