we show two example SEDs from the highest redshift bin normalized at 1$\mu$m to highlight both the improved sampling of the SED as well as the fundamental differences between the SEDs of the quiescent and dusty galaxies. Although both galaxies have red observed $U$-$V$ colors, we see clear distinctions in the continuum shapes of the SEDs. The dusty galaxy (right panel) has a more gradual slope than the instrinsically red, older stellar population (left panel), which shows a well-defined 4000Å break with a peaked SED. With the increased resolution of the medium-band data, we are able to distinguish the continuum shapes and properties of galaxies residing on the red sequence to remove dusty contaminants such as the galaxy in the right panel.

![image](fig2_sm.eps)

The issue of the ongoing star-formation in these galaxies is ambiguous, as this depends on the definition of a “quiescent” galaxy and is very model-dependent: for an individual quiescent galaxy the 1$\sigma$ range of specific star formation rates (sSFR) from the SED modeling described in §2 is on average 0 to 0.004 Gyr$^{-1}$ out to $z$=2 [see also @Kriek08]. Degeneracies between the age, dust, and mass in models complicate matters when selecting “quiescent” galaxies based on their 