star-forming galaxies, and the dust complicates the measurements of the intrinsic color scatter of red, old galaxies. This complication is less important at low redshift because $\sim\!$70-80% of red galaxies have very little dust [@Bell04a; @Wolf05]. Furthermore, dusty contaminants can be visually identified using morphological information out to $z\!\sim$1 [e.g. @McIntosh05b; @Ruhland09], whereas at higher redshifts the galaxies are too faint to resolve with current technology. However, these dusty systems can be identified using additional information: e.g. $UVJ$ rest-frame colors [@Williams09], the visual dust extinction from SED modeling [@Brammer09], or mid-IR imaging [@Papovich05; @Franx08; @Fontana09].

Currently the best estimates for the ages of stellar populations in massive high redshift galaxies comes from @Kriek08, who combine broadband multiwavelength imaging with NIR spectroscopy for a $K$-selected sample. They find that red sequence galaxies at $z\!\sim$2.3 typically have 0.5-1 Gyr populations with moderate amounts of dust. However, older galaxies may have been missed due to the magnitude limits of the $K$-selection. To understand the properties of quiescent galaxies, a large systematic study is required to connect and confirm the limited knowledge we have of galaxies at $z\!\sim$2 with the observed properties of local early-type galaxies.

High redshift studies of galaxies are either based 