Table 2.

In the right panel of Figure \[Figure:HbRL\], we show the  lag as a function of the luminosity of the broad component of , with the narrow component removed whenever possible. We give the best-fit values to the equation (\[eq:powerlaw\]) in the second row of Table 2, which shows that the slope of this relationship is nearly identical to the slope of the $R$–$L$ relationship using the AGN continuum. The luminosity of the  broad component is thus an excellent proxy for the AGN luminosity and requires only removal of the narrow component (at least when it is significant) which is much easier than estimating the starlight contribution to the continuum luminosity at 5100Å. Moreover, by using the line flux instead of the continuum flux, we can include core-dominated radio sources where the continuum may be enhanced by the jet component [@Greene05]. This is therefore the $R$–$L$ relationship we prefer for the purpose of estimating single-epoch masses and we will focus on this relationship through the remainder of this contribution.

![The relationship between the broad  emission line luminosity and the starlight-corrected AGN luminosity for the sources in Table A1. The black solid line is the regression of $L({\mbox{\rm H$\beta$}}_{\rm broad})$ 