possible, we obtain similar completeness estimates. As expected from filling the fibers with targets, most targets are peculiar stars of various types, particularly at the brighter magnitudes. Unclassifiable spectra dominate at the fainter magnitudes, and with the weather-limited integration times, there was an effective magnitude limit of roughly $19.5$–$20$ mag.

![Cumulative distributions of MQS targets. The upper solid curve shows the distribution of all the targets, which is then decomposed into stars (dashed), unclassified spectra (dotted), and quasars (solid, divided into $z<0.5$ and $z>0.5$ sources). The red solid (dashed) curves show the distribution of $z>0.5$ AGES (SDSS $0.3 < z < 2.2$) quasars for comparison. Our selection methods and bands are more comparable to AGES than to SDSS. []{data-label="fig:cumul"}](MQS_fig8.eps){width="8cm"}

![$V-I$ colors of the MQS LMC quasars (filled squares) and other confirmed LMC and SMC quasars (open circles) as a function of redshift. Overplotted is the color for a pure AGN spectrum from [@2001AJ....122..549V] convolved with the $V$ and $I$ filters (solid line). The same spectrum was also convolved with the $i$ and $I$ filters in order to convert OGLE magnitudes into SDSS $i$-band magnitudes—the $(i-I)$ color is shown as dotted line.[]{data-label="fig:AGNcolor"}](MQS_fig9.eps){width="8cm"}

Figure \[fig:AGNcolor\] shows the colors of the confirmed quasars 