magnitudes and $R$ values, we calculate [$L_{5100}$]{} assuming an intrinsic AGN continuum spectrum of $f_{\nu} \propto \nu^{-0.45}$ (Vanden Berk [et al.]{} 2001). Brotherton’s sample is, on average, about an order of magnitude more luminous than ours. The entire Brotherton sample (open symbols in Fig. 4) is displaced by +0.1 dex from the fiducial line of radio-quiet objects, increasing to +0.14 dex for the core-dominated systems (defined as those with core-to-lobe ratios $\geq 1$; open triangles). We conclude that BH masses based on [$L_{5100}$]{}can be systematically overestimated in radio-loud objects, but the effect is only serious for relatively luminous, core-dominated sources. While the systematic enhancement of the optical continuum relative to Balmer line emission in the most radio-loud, core-dominant sources can be attributed reasonably to jet contamination, we cannot rule out the possibility that this effect is due to changes in the ionizing spectrum or covering factor of the line-emitting gas.

A New Formalism for Estimating BH Virial Masses
-----------------------------------------------

The existence of the tight empirical correlations described above (Eqs. 1 and 3) implies that we can transform the virial mass expression of Kaspi et al. (2000), which makes use of [$L_{5100}$]{} and [$\mathrm{FWHM}_\mathrm{H{\beta}}$]{}, into a new formalism that depends solely 