al.]{} 1998) on a dedicated 2.5m telescope. The spectra cover the optical range 3800$-$9200 [$\rm{\AA} \;$]{}at a resolution 1800$-$2100. The spectra are calibrated to spectrophotometric standard F-stars and are thus corrected for Galactic reddening (at the scale of the separation to the nearest calibration star, $\lesssim1\deg$) in the limit that these F stars are behind the dust in the Galaxy. The spectrophotometric calibration is thought to be good to $\sim$20%. Details of the photometric calibrations are given by (2001) and (2002), and details of the astrometric calibration are given by (2003). The spectroscopic tiling algorithm is discussed by (2003).

The (2003) EDR BALQSO catalog includes BALQSOs ($0.892 \le z
\le 4.41$) selected by two automated algorithms, cross-checked and supplemented by a manual inspection. One automated algorithm fitted a composite quasar spectrum created from the entire EDR quasar catalog[^4] to each of the individual quasar spectra in order to define the intrinsic flux level from which broad absorption could be measured ([Reichard]{} [et al.]{} 2003). The algorithm also scaled the emission line associated with the broad absorption (either or ) to create a more accurate continuum where the broad-absorption and emission-line regions overlap. The second, more traditional algorithm, described by (2002), 