a galaxy contribution of $\leq 20 \%$. Thus, our primary sample was chosen to satisfy EW(Ca K) $\leq 1.5$ Å. In order to increase the dynamic range of the sample at the lowest luminosities, we included $\sim 30$ more galaxies, including the 19 objects from Greene & Ho (2004), which have a mean S/N $\approx$ 17 and EW(Ca K) as high as 10 Å. The total sample consists of 229 objects.

To investigate the possible influence of jet emission on [$L_{5100}$]{}, we also consider an auxiliary sample of 59 radio-loud objects, selected using the standard criterion for radio-loudness, $R \geq 10$, where $R$ is the ratio of the flux densities at 6 cm and 4400 Å (Kellermann et al. 1989). The radio flux densities were obtained from the Faint Images of the Radio Sky at Twenty-cm (FIRST; Becker, White, & Helfand 1995) survey, which covers all the objects in our sample. We corrected the flux densities from 20 cm to 6 cm assuming a spectrum $f_{\nu} \propto \nu^{-0.46}$ (Ho & Ulvestad 2001). The derived $R$ values for the radio-loud sample range from 10 to $10^4$.

Spectral Fitting
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Below we discuss our method to measure the AGN continuum and the 