correlation between the [H$\alpha$]{} and [H$\beta$]{} line width (Fig. 3), which we parameterize[^3] by the FWHM. In this case, neither [$\mathrm{FWHM}_\mathrm{H{\alpha}}$]{} nor [$\mathrm{FWHM}_\mathrm{H{\beta}}$]{} can be regarded as the independent variable, so we calculate the ordinary least-squares bisector, again accounting for errors in both parameters (Akritas & Bershady 1996). Whereas for the line-continuum correlations we were forced to include lower-S/N spectra in order to increase the dynamic range in luminosity, in this case we can span the entire range in line width without considering the full sample. To minimize errors resulting from profile decomposition, we concentrate on spectra with strong [H$\beta$]{} lines by excluding objects with [H$\beta$]{}EWs less than 50 Å. For this restricted sample of 162 objects, we find

$${\ensuremath{\mathrm{FWHM}_\mathrm{H{\beta}}}}= (1.07 \pm 0.07) \times 10^3 
\left(\frac{{\ensuremath{\mathrm{FWHM}_\mathrm{H{\alpha}}}}}{10^3~\mathrm{{km~s\ensuremath{^{-1}}}}}\right)^{(1.03 \pm
0.03)}~\mathrm{{km~s\ensuremath{^{-1}}}}.$$

+0.35cm

The rms scatter around the best-fit line is $\sim 0.1$ dex. We note that when we include the entire sample, or look at the radio-loud subset separately, [H$\beta$]{} is still on average broader than [H$\alpha$]{}, but the scatter is larger and the slope of the correlation changes slightly.

Radio-loud Sources
------------------

If the optical continuum of radio-loud sources is significantly boosted by nonthermal emission from a jet, their [$L_{5100}$]{}, and hence 