Figure \[fig:fig4\], where we see evidence for a broader decrement of flux in the red wing of . We also note that strong, prominent absorption troughs, such as those found blueward of and , are absent blueward of in the LoBAL composite. This absence is not unexpected since the creation of composite spectra tends to wipe out features that are not persistent from spectrum to spectrum. Since the absorption troughs can occur at different velocities from the emission line peak, the apparent strength of the absorption is diminished in the composite spectrum.

Moving to shorter wavelengths, we find that the HiBAL composite shows no excess in the UV48 complex of at $2080\,{\rm \AA}$, but that there may be a slight excess in LoBALs. (1991) reported an excess at this wavelength among their LoBALs and also found that the strength of this feature correlates with the balnicity index for HiBALs as well as LoBALs.

Continuing on to the complex of emission near \] $\lambda1909$, we find a small excess of emission in the and \] region of the HiBAL composite, which (1991) suggested is likely due to or emission. However, we do not see any excess longward of the peak of 