the red sequence because they have old, evolved stellar populations. At high $z$, where we currently lack morphological information, we must devise a method for selection of dusty, star-forming galaxies masquerading as red, quiescent galaxies.

The Age Spread of Quiescent Galaxies
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Selecting Quiescent Galaxies
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The color-mass relation is shown in the top panels of Figure 1. Clearly, the majority of massive galaxies with masses $>$10$^{11}$ M$_{\odot}$ are red at all redshifts to $z$=2. However, a significant fraction of these galaxies are red because of dust, not because they have old, evolved stellar populations [e.g. @Wyder07; @Cowie08; @Brammer09].

Following @Brammer09, we select quiescent galaxies by requiring, $$(U-V)'-\Delta_{UV}-(2.03-0.77\cdot t_{LB}/t_{H})>-0.4,$$

where ($U$-$V$)$'$ is the rest-frame $U$-$V$ color with the slope of the color-magnitude relation removed using the non-evolving slope from @Bell04 and $\Delta_{UV}$ is dust reddening correction factor of $0.47\cdot A_{V}$ (the visual extinction) as derived using the @Calzetti00 exinction law. The final term accounts for a mean linear color evolution with time, where $t_{\mathrm{LB}}$ is the lookback time and $t_{\mathrm{H}}$ is the Hubble time. The average selection given by Equation 1 corresponds to the dashed horizontal line at each redshift interval. The selection method removes dusty, star forming galaxies based 