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

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Published 2020 July 8 © 2020. The American Astronomical Society. All rights reserved.
, , Citation Marcin Marculewicz and Marek Nikolajuk 2020 ApJ 897 117 DOI 10.3847/1538-4357/ab9597

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0004-637X/897/2/117

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.

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10.3847/1538-4357/ab9597