on their extinction thereby leaving us with the red sequence. This selection is similar to and more conservative than the $UVJ$ selection of @Labbe05 and @Williams09 (see Appendix A).

Comparing the observed $U$-$V$ color to the color with an additional dust-correction $\Delta_{\mathrm{UV}}$ (top and bottom panels in Figure 1, respectively), we find that not all massive red galaxies are old, as there is a significant population of dusty and star forming massive galaxies at $z\!>$1 [see @Brammer09]. Those star forming galaxies that are dusty interlopers are marked as green stars in the bottom panels of Figure 1 and removed from the sample through the above selection method. Additionally, those galaxies that have MIPS detections ($>$20$\mu$Jy) are indicated with small red circles, but are not removed from the sample[^4]; these objects likely host active galactic nuclei (AGN) or may be forming stars [see also @Daddi07]. We note that the scatter measured in $U$-$V$ decreases by $\sim\!0.03$ mag at $z\sim\!0.5$ and $\sim\!$0.01-0.02 at higher redshifts when removing all MIPS-detected quiescent galaxies. The extinction correction effectively reduces the number of galaxies in the transition zone between the blue cloud and red sequence, revealing distinct populations with bimodal intrinsic colors up to at least 