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.
