Black Hole Masses of Weak Emission Line Quasars Based on the Continuum Fit Method

We studied optical-ultraviolet spectral energy distribution of 10 weak emission-line quasars (WLQs) that lie at redshifts z = 0.19 and 1.43 z < 3.48. The theoretical models of their accretion disk continua are created based on the Novikov-Thorne equations. It allows us to estimate masses of their supermassive black holes (M-BH) and accretion rates. We determined the virial factor for WLQs and note its anticorrelation with the FWHM of the H beta emission line (f proportional to FWHM alpha, alpha = -134 +/- 0.37). By comparison with the previously estimated factor of 4-5, which depends on the measured full width. We proposed a new formula to estimate in WLQs based on their observed (H beta) and luminosities at 5100 A. In our opinion, WLQs are also normal quasars visible in a reactivation stage.