(e.g., $g^*-r^*\lesssim0$) are greatly underrepresented among the BALQSOs. This result is [*not*]{} simply because of absorption from the BAL troughs themselves. The trough absorption can make the broad-band color of BALQSOs bluer as well as redder, depending on where the redshift of the quasar places the troughs with respect to the filters. Instead, it is the overall flux deficit which spans the entire width of a filter that causes BALQSOs to be redder than nonBALQSOs.

In the bottom right-hand panel, we show that BALQSOs are redder than nonBALQSOs in yet another way. Here we use relative colors ([Richards]{} [et al.]{} 2001; [Richards et al.]{} 2003), which are colors corrected by the median color as a function of redshift and thus are independent of redshift. From these distributions of relative $g^*-i^*$ color, we find that BALQSOs have an even more pronounced tail of red colors than do nonBALQSOs.

BALQSO/nonBALQSO Continuum Comparison \[sec:continuum\]
=======================================================

Extending the broad-band results, using spectral analysis, we now investigate the finding of previous authors that LoBALs are redder than both nonBALs and HiBALs (e.g., [Weymann]{} [et al.]{} 1991) and that even HiBALs are redder than nonBALs (e.g., [Brotherton]{} [et al.]{} 2001). We examine the continuum (i.e., color) 