only MgII in the region of the dichroic split. We show ten selected spectra of the newly confirmed AGNs in Figure \[fig:spectra1\] and also show several spectra of common contaminating sources in Figure \[fig:contamination\]. The remaining spectra are discussed in Section \[sec:contamination\], and are either not quasars or quasars with too low S/N for clear detection. As we discuss in Section \[sec:discussion\], a fair number of the fainter sources ($I \gtrsim 19$ mag) should be quasars.

![Redshift distribution of the confirmed quasars in $z=0.1$ bins.[]{data-label="fig:hist"}](MQS_fig3.eps){width="8cm"}

![image](MQS_fig4.eps){width="15cm"}

![image](MQS_fig5.eps){width="15cm"}

One target, MQS J050155.46$-$700210.1, shows emission lines corresponding to redshifts of $z=0.228$ and $0.341$, as shown in Figure \[fig:doubleAGN\]. This could be a chance coincidence or a gravitational lens. In the OGLE-III reference image (Figure \[fig:doubleAGNchart\]), we find that the AGN candidate was a faint source ($V=21.3$, $I=20.5$) in the wings of a brighter extended source. The standard OGLE catalogs may not include all extended sources, so it is likely that the faint source was mistargeted and the brighter galaxy is the AGN candidate. If we assume the bright galaxy is acting as a gravitational lens, then we estimate that it has an Einstein radius of $R_{\rm E}<0.4$ arcsec, which is very small 