\times 4$ deg$^2$ area of the LMC disk. We will also identify any bright quasars suitable for absorption studies of the LMC’s interstellar medium (ISM), as we expect 1, 10, and 74 quasars brighter than $I<17$, 18, and 19 mag in the four observed fields.

The goal of our Magellanic Quasars Survey (MQS) is to identify and characterize all these quasars, where we estimate a final sample of roughly $700$ quasars in a complete survey of the OGLE-III project regions. Spectroscopy is essential not only for confirmation of the candidates but also to determine the luminosity, rest-wavelength and black hole masses (through the emission line widths) of the quasars, so that the variability parameters can be related to other physical properties. Relatively large numbers of quasars will be needed to explore this (minimally) three dimensional parameter space quantitatively. While the sample will be smaller than the $\sim 9000$ quasars we considered in [@2010ApJ...721.1014M], the longer, more densely sampled light curves should let us examine the physical correlations with less “blurring” from the noisy parameter estimates obtained from the sparsely sampled Sloan Digital Sky Survey (SDSS) light curves, making it far easier to determine the intrinsic parameter distributions. In this paper, 