virial mass, will be systematically overestimated. We can empirically test the magnitude of this effect by examining the correlation between [$L_{5100}$]{}and Balmer-line luminosity for our auxiliary radio-loud sample. If jet contamination is important, we would expect the -1mm +5mm radio-loud objects to lie systematically to the right of the best-fit relations shown in Figure 2. However, as shown in Figure 4, the radio-loud sources (filled points) do not show a significant offset with respect to the main sample. Their mean displacement from our best-fit [$L_{\mathrm{H{\beta}}}$]{}-[$L_{5100}$]{} line is only +0.02 dex in [$L_{5100}$]{}, and for the strongest radio sources ($R \geq
100$) the mean displacement is in fact $-$0.04; neither result is statistically significant. Instead of the degree of radio-loudness, the more important parameter may be the amount of beaming, which can be guaged roughly by the degree of core dominance of the radio emission. Unfortunately, the resolution of FIRST (5 or 10 kpc at $z=0.1$) is inadequate to distinguish truly core-dominated objects from objects with intrinsically compact jets. We thus additionally consider objects from the sample of Brotherton (1996), which is composed entirely of radio-loud objects with tabulated core-to-lobe radio luminosity ratios. For the 37 Brotherton objects with measured $V$-band 