of Table 2.

![Left: The rest-frame  lag in days is shown as a function of the AGN luminosity $L_{\rm AGN}(5100\,{\rm \AA})$ in . The host-galaxy starlight contribution has been removed by using unsaturated [[*HST*]{}]{} images [see @Bentz13]. Right: The  lag in days is shown as a function of the broad  luminosity $L({\mbox{\rm H$\beta$}}_{\rm broad})$ in . The narrow component of  has been removed in each case where it was sufficiently strong (i.e., easily identifiable) to isolate. In both panels, the solid line shows the best-fit to the data using equation (\[eq:powerlaw\]) with coefficients given in Table 2. The short dashed lines show the $\pm1\,\sigma$ uncertainty (equivalent to enclosing 68% of the values for a Gaussian distribution) and the long dashed lines show the $2.6\sigma$ uncertainties (equivalent to enclosing 99% of the values for a Gaussian distribution). []{data-label="Figure:HbRL"}](Figure1.eps)

[llccccc]{} $\log L_{\scriptsize\rm AGN}(5100\,{\rm \AA})$ & $\log \tau({\mbox{\rm H$\beta$}})$ & $1.228 \pm 0.025$ & $0.482 \pm 0.029$ & $43.444$ & $0.213 \pm 0.021$ & $0.241$\
$\log L({\mbox{\rm H$\beta$}}_{\scriptsize\rm broad})$ & $\log \tau({\mbox{\rm H$\beta$}})$ & $1.200\pm 0.025$ & $0.492 \pm 0.030$ & $41.746$ & $0.218 \pm 0.022$ & $0.244$\
$\log L(1350\,{\rm \AA})$ & $\log \tau({\mbox{\rm C\,{\sc iv}}})$ & $1.915 \pm 0.047$ & $0.517 \pm 