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We employ a flexible Bayesian technique to estimate the black hole mass and Eddington ratio functions for Type 1 (i. e. , broad line) quasars from a uniformly-selected data set of ~58, 000 quasars from the SDSS DR7. We find that the SDSS becomes significantly incomplete at M₁₇ < 3 x 10⁸ Mₒₔ₍ or L / L₄₃₃ < 0. 07, and that the number densities of Type 1 quasars continue to increase down to these limits. Both the mass and Eddington ratio functions show evidence of downsizing, with the most massive and highest Eddington ratio black holes experiencing Type 1 quasar phases first, although the Eddington ratio number densities are flat at z < 2. We estimate the maximum Eddington ratio of Type 1 quasars in the observable Universe to be L / L₄₃₃ ~ 3. Consistent with our results in Paper I, we do not find statistical evidence for a so-called "sub-Eddington boundary" in the mass-luminosity plane of broad line quasars, and demonstrate that such an apparent boundary in the observed distribution can be caused by selection effect and errors in virial BH mass estimates. Based on the typical Eddington ratio in a given mass bin, we estimate typical growth times for the black holes in Type 1 quasars and find that they are typically comparable to or longer than the age of the universe, implying an earlier phase of accelerated (i. e. , with higher Eddington ratios) and possibly obscured growth. The large masses probed by our sample imply that most of our black holes reside in what are locally early type galaxies, and we interpret our results within the context of models of self-regulated black hole growth.
Kelly et al. (Thu,) studied this question.