Black Hole Masses of Weak Emission Line Quasars Based on the Continuum Fit Method
Abstract
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 ( ${M}_{\mathrm{BH}}$ ) and accretion rates. We determined the virial factor for WLQs and note its anticorrelation with the FWHM of the Hβ emission line $(f\propto {\mathrm{FWHM}}^{\alpha },\alpha =-1.34\pm 0.37$ ). By comparison with the previously estimated BH masses, the underestimation of ${M}_{\mathrm{BH}}$ is noticed with a mean factor of 4-5, which depends on the measured full width. We proposed a new formula to estimate ${M}_{\mathrm{BH}}$ in WLQs based on their observed $\mathrm{FWHM}$ (Hβ) and luminosities at 5100 Å. In our opinion, WLQs are also normal quasars visible in a reactivation stage.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- July 2020
- DOI:
- 10.3847/1538-4357/ab9597
- arXiv:
- arXiv:1910.06175
- Bibcode:
- 2020ApJ...897..117M
- Keywords:
-
- Active galactic nuclei;
- Black holes;
- Quasars;
- 1319;
- 16;
- 162;
- Astrophysics - High Energy Astrophysical Phenomena;
- Astrophysics - Astrophysics of Galaxies
- E-Print:
- 13 pages, 15 figures, accepted for publication in the Astrophysical Journal