our analysis. The ratio of broad [H$\alpha$]{} to [H$\beta$]{} strengths has been found to vary quite significantly from the value of 3.1 predicted by Case B recombination. For instance, while Seyfert 1 galaxies have typical [H$\alpha$]{}/[H$\beta$]{} ratios of $\sim 3.5-5$ (Adams & Weedman 1975; Osterbrock 1977), in both broad-line radio galaxies and Seyfert 1.9 galaxies values as high as 7–10 are seen (Osterbrock 1981). Interestingly, we find $\langle$[H$\alpha$]{}/[H$\beta$]{}$\rangle=3.5$ (for the combined broad and narrow components; Fig. 5), which is virtually identical to the value seen in the SDSS quasar composite spectrum of Vanden Berk et al. (2001). \[The mean [H$\alpha$]{}/[H$\beta$]{} ratio for the radio-loud group is slightly higher ($\sim$4), but given the smaller sample, this is only a marginally significant difference.\] Since this value is only mildly larger than the theoretical limit of 3.1, it implies that processes that enhance the Balmer decrement, such as collisional excitation or self-absorption (e.g., Netzer 1975), are generally not that important. We can also place a stringent limit on the amount of internal reddening by dust: for an intrinsic Balmer decrement of 3.1, the extinction law of Cardelli et al. (1989) would allow at most $E(B-V)$ = 0.12 mag. Most likely our selection of 