0.036$ & $45.351$ & $0.336 \pm 0.041$ & $0.361$\
$\log L_{\scriptsize\rm AGN}(5100\,{\rm \AA})$ & $\log L({\mbox{\rm H$\beta$}}_{\rm broad})$ & $41.797 \pm 0.017$ & $0.960 \pm 0.020$ & $43.444$ & $0.158 \pm 0.014$ &$0.171$\
$\log L({\mbox{\rm H$\beta$}}_{\rm broad})$ &$\log L_{\scriptsize\rm AGN}(5100\,{\rm \AA})$ & $43.396 \pm 0.018$ & $1.003 \pm 0.022$ & $41.746$ & $0.161 \pm 0.015$ & $0.174$ \[table:RL\]

Accounting for the host-galaxy contribution in the same way for large number of AGNs, such as those in SDSS-RM (not to mention the entire SDSS catalog), is simply not feasible. It is well-known, however, that there is a tight correlation between the AGN continuum luminosity and the luminosity of [e.g., @Yee80; @Ilic17], and it has indeed been argued that the  emission-line luminosity can be used as a proxy for the AGN continuum luminosity for reverberation studies [@Vestergaard06; @Greene10a]. However, in some of the reverberation-mapped sources, narrow-line contributes significantly to the total  flux; NGC 4151 is an extreme example [e.g., @Antonucci83; @Bentz06a; @Fausnaugh17]. Whenever the narrow-line component can be isolated, it has been subtracted from the total  flux. In Figure \[Figure:LAGNLHb\], we show the tight relationship between $L_{\rm AGN}(5100\,{\rm \AA})$ and $L({\mbox{\rm H$\beta$}}_{\rm broad})$; the best-fit coefficients for this relationship are given in 