techniques developed for extragalactic surveys (@2005ApJ...631..163S) could also be applied to dense stellar regions, albeit with some contamination from the relatively rare dusty stars (e.g., young stellar objects (YSOs), planetary nebulae (PNe), etc.). In [@2010ApJ...708..927K], we showed that the DRW variability parameters of quasars differed from those of variable stars, providing a more quantitative approach to variability-selecting quasars that has been expanded on in [@2011ApJ...728...26M] and [@2011AJ....141...93B]. In a single test observation under poor conditions, [@2011ApJS..194...22K] doubled the number of known quasars behind the SMC from 28 to 57.

Apart from studying variability, quasars in these fields are important tools for deriving more precise proper motions of the LMC, SMC and, potentially, the Galactic Bulge using the [*Hubble Space Telescope (HST)*]{} or, in the future, the [*James Webb Space Telescope (JWST)*]{}. [@2006ApJ...638..772K] and [@2008AJ....135.1024P] based their LMC proper motions on 21 quasars. Further improvements require better measuring the internal motions of the Clouds, and this requires larger numbers of quasars well-distributed over the LMC disk. Based on [@2008AJ....135.1024P], the newly confirmed LMC quasars we discuss here could be used to reduce the proper motion uncertainties by a factor of three, since our new quasars are distributed over a large $6 