the modeling in §3.3, as the average uncertainty is much smaller than what we expect given our assumptions in the modeling due to degeneracies between age and metallicity. Additionally, we plot the typical random and systematic errors in the $U$-$V$ color as a function of redshift in Figure \[agecolor\]. At $z\!<$1.5, the red and blue quartiles have the same low-level of dust reddening, whereas at $z\!>$1.5 the red quiescent galaxies have $\sim$0.2 magnitudes more extinction.

Rest-Frame SEDs of Quiescent Galaxies
-------------------------------------

We note that the general trends in Figure \[agecolor\] do not prove that we are measuring age differences, as bluer $U$-$V$ colors will force a lower age in the fit, even if the range in $U$-$V$ is due to photometric scatter only (see Appendix B for more details on the effects of photometric scatter). In the previous section we just considered the $U$-$V$ colors, we will now investigate the shape of the full observed rest-frame SEDs of these galaxies to see if there is a fundamental difference between the reddest and bluest galaxies on the red sequence.

![The effect of resolution can be seen in this figure, where the thin black line is the average best-fit model to the 