\] which would be expected from UV34. In the LoBAL composite, this same excess may still persist, but more significant is a decrement of flux at the centroid of \].

No strong absorption from is seen in the HiBAL composite, but the LoBAL composite exhibits two prominent absorption troughs near $1804\,{\rm \AA}$ and $1835\,{\rm \AA}$, with a peak near $1819\,{\rm
\AA}$. A third depression is found near $1750\,{\rm \AA}$ and may have a weaker counterpart in the HiBAL composite. The absorption lines are quite strong in the LoBAL composite, whereas the troughs which were used to define the LoBALs are relatively absent, suggesting perhaps that is a better indicator of LoBALs or that absorption has a more consistent velocity distribution from quasar to quasar.

In the composite spectra shown in Figure \[fig:fig1\], $\lambda1640$ emission appears to be slightly weaker in BALQSOs than in nonBALQSOs. The difference spectra in Figures \[fig:fig3\] and \[fig:fig4\] also exhibit this weakness.

At the location of we see some interesting differences in the spectra. First, we confirm the reality of the “droop” in the difference spectrum that was reported by (1991). This “droop” occurs between the emission peak and $\sim1600\,{\rm \AA}$ and is seen in both 