magnitude is $I<19.5$ mag; [*Cut 2.*]{} $\ln L_{\rm best}>\ln L_{\rm noise}+2$; [*Cut 3.*]{} The SF slope $0.1<\gamma<0.9$ (e.g., see @2010ApJ...714.1194S); [*Cut 4.*]{} The $I$-band amplitude $A<0.4$ mag (this removes large amplitude variable stars); [@2010ApJ...721.1014M] report that some of $\sim$9000 SDSS quasars occupy areas outside the $\tau$–$\hat{\sigma}$ cut of [@2010ApJ...708..927K], therefore we decided to loosen the cut on the $\tau$ parameter and to ignore $\hat{\sigma}$ parameter, so [*Cut 5*]{} is $1<\log(\tau)<5$. When simply applied to the OGLE light curve database, this process yields $\sim 24,000$ candidates. The vast majority are due to two known systematic issues. First, bright variable stars typically generate several fake, fainter variable stars in their wings, and these “ghost” variables show long term irregular variability. Second, there can be small magnitude shifts between seasons, and (for one field in particular) the shifts were being misinterpreted as quasar-like variability. We carried out a quick visual inspection of all candidates, but this was over kill and would certainly be automated in any subsequent analysis. We were left with 1063 variability-selected candidates.

![Venn diagram for all 2434 LMC MQS quasar candidates. The upper numbers give the number of candidates in each selection region. Priority 9 is given to AGN candidates 