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Black hole masses of weak emission line quasars based on continuum fit method

We studied optical-ultraviolet spectral energy distribution of 10 weak emission-line quasars (WLQs) which 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 (MBH) and accretion rates. We determined the virial factor for WLQs and note its anti-correlation with the full width at half maximum (FWHM) of Hbeta emission-line (f propto FWHM^(alpha), alpha = (-1.34 +/- 0.37)). By comparison with the previously estimated BH masses, the underestimation of MBH is noticed with a mean factor 4-5 which depends on the measured full width. We proposed the new formula to estimate MBH in WLQs based on their observed FWHM (H beta) and luminosities at 5100 A. In our opinion, WLQs are also normal quasars visible in a reactivation stage.