2020ApJ...897..117M

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 Hβ emission line (f∝FWHM^α^,α=-1.34±0.37). By comparison with the previously estimated BH masses, the underestimation of M_BH is noticed with a mean factor of 4-5, which depends on the measured full width. We proposed a new formula to estimate M_BH in WLQs based on their observed FWHM(Hβ) and luminosities at 5100 Å. In our opinion, WLQs are also normal quasars visible in a reactivation stage.