line-width measures motivated a broader effort to produce easy-to-use prescriptions for computing [*accurate*]{} black hole masses using  and  emission lines and nearby continuum fluxes measurements for each line. We note that we do not discuss  RM results in this contribution as the present situation has been addressed rather thoroughly by [@Bahk19] and new SDSS-RM results will be published soon [@Homayouni20]. In §[2]{}, the data used in this investigation are described. In §[3]{}, the relationship between the  reverberation lag and different measures of the AGN luminosity are considered, and we identify the physical parameters to lead to accurate black-hole mass determinations. In §[4]{}, we will similarly discuss masses based on . In §[5]{}, we present simple empirical formulae for estimating black hole masses from  or . The results of this investigation and our future plans to improve this method are outlined in §[6]{}. Our results are briefly summarized in §[7]{}. Throughout this work, we assume $H_0 = 72$Mpc$^{-1}$, $\Omega_{\rm matter} =0.3$ and $\Omega_\Lambda = 0.7$.

Observational Database and Methodology
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Data {#section:Data}
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We use two high-quality databases for this investigation:

1.  Spectra and measurements for previously reverberation-mapped AGNs, for  (Table A1) and for  (Table A2). These are mostly taken from 