color-color plane (see @2004ApJS..154..166L and @2004ApJS..154...48E, and also @2010ApJ...713..970A, @2008ApJ...679.1040G, and @2010ApJ...716..530K for the mid-IR colors of X-ray and variability selected AGNs). The red mid-IR colors of a typical AGN are not due to dust emission, so mid-IR-selected AGNs are generally normal $z\gtorder 1$ broad-line quasars (see @2010ApJ...713..970A, @2011ApJ...728...56A). There is also no significant tendency for them to be Type II quasars. This is particularly true with the addition of a magnitude limit for the optical spectroscopy, since at most redshifts the emission from the disk is required to render the source bright enough to be observed.

In [@2009ApJ...701..508K], we used this approach to identify quasars in the LMC and SMC from the [*Spitzer/IRAC*]{} four-band photometry (i.e., 3.6, 4.5, 5.8, and 8.0$\micron$) of the Surveying the Agents of a Galaxy’s Evolution project (SAGE; @2006AJ....132.2268M). The 5000 AGN candidates were divided into several categories. First, all the objects must be located inside the “Stern AGN wedge” (@2005ApJ...631..163S). The locus of cool blackbodies passes through the wedge so the quasar sample is divided into group “A” if they are far from the blackbody locus, and “B” if they can be contaminated with cold stars. Second, the mid-IR color-magnitude diagram (CMD) was divided 