the BALQSO parent sample. Using what we have learned about the colors of BALQSOs we present an analysis of the BALQSO fraction in § \[sec:balfractions\]. Finally, §\[sec:conclusions\] summarizes our results. Cosmology dependent parameters (e.g., absolute magnitude) are used in this paper only in a relative sense, thus throughout this paper we will use a cosmology where $H_o
={\rm50\,km\,s^{-1}\,Mpc^{-1}}$, $\Omega_M = 1$, and $\Omega_\Lambda =
0$. We also adopt a convention for optical spectral index such that $\alpha=\alpha_{\lambda}$ unless stated otherwise, where $f_{\lambda}
\propto \lambda^{\alpha_{\lambda}}$.

The Data \[sec:data\]
=====================

Our analysis is based upon the 224 SDSS BALQSOs cataloged by (2003). This catalog includes 185 BALQSOs from a complete sample between $z=1.7$ and $z=4.2$, of which 131 quasars also form a relatively homogeneous sample of objects that were selected as quasar candidates using the SDSS’s adopted quasar target selection algorithm as described by (2002a). This catalog was constructed from the 3814 bona fide quasars ($M_{i^*}\,<\,-23$, with at least one line broader than $1000\,{\rm km\,s^{-1}}$) from the SDSS EDR quasar sample ([Schneider]{} [et al.]{} 2002). The EDR quasars were selected for spectroscopic follow-up from the SDSS imaging survey, which uses a wide-field five filter ([Fukugita]{} [et al.]{} 1996) multi-CCD camera ([Gunn]{} [et 