The Black Hole Masses and Eddington Ratios of Type 2 Quasars

Abstract

Type 2 quasars are an important constituent of active galaxies, possibly representing the evolutionary precursors of traditionally studied type 1 quasars. We characterize the black hole mass ($M_{\mathrm{BH}}$) and Eddington ratio ($L_{\mathrm{bol}}/L_{\mathrm{Edd}}$) for 669 type 2 quasars selected from the Sloan Digital Sky Survey, using black hole masses estimated from the $M_{\mathrm{BH}}-{\sigma }_{\ast }$ relation and bolometric corrections scaled from the extinction-corrected $[\mathrm{O}\mathrm{III}]\lambda 5007$ luminosity. When stellar velocity dispersions cannot be measured directly from the spectra, we estimate them from the core velocity dispersions of the narrow emission lines $[\mathrm{O}\mathrm{II}]\lambda \lambda 3726,3729$, $[\mathrm{S}\mathrm{II}]\lambda \lambda 6716,6731$, and $[\mathrm{O}\mathrm{III}]\lambda 5007$, which are shown to trace the gravitational potential of the stars. Energy input from the active nucleus still imparts significant perturbations to the gas kinematics, especially to high-velocity, blueshifted wings. Nonvirial motions in the gas become most noticeable in systems with high Eddington ratios. The black hole masses of our sample of type 2 quasars range from $M_{\mathrm{BH}}\approx 10^{6.5}$ to $10^{10.4}{M}_{\odot }$ (median $10^{8.2}{M}_{\odot }$). Type 2 quasars have characteristically large Eddington ratios ($L_{\mathrm{bol}}/L_{\mathrm{Edd}}\approx 10^{-2.9}-10^{1.8}$; median $10^{-0.7}$), slightly higher than in type~1 quasars of similar redshift; the luminosities of $\sim$20% of the sample formally exceed the Eddington limit. The high Eddington ratios may be consistent with the notion that obscured quasars evolve into unobscured quasars.

23 pages, 12 figures, ApJ, accepted

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