The ratio in number between unobscured (type 1) and obscured (type 2) active galactic nuclei (AGNs) is often used to explore the structure of the torus in the unified scheme for AGNs. Oh et al. (2015) investigated the type 1 AGN fraction on two-dimensional space in terms of black hole mass (MBH) and bolometric luminosity (Lbol) and found that the fraction changes depending on both MBH and Lbol, forming a ridge-shaped distribution. In this study, based on the up-to-date type 1 AGN catalog of Oh et al. (2015), we examine how the trend of the type 1 AGN fraction in the MBH-Lbol plane is affected by the different methods used to derive MBH and Lbol, and suggest an analytic model to explain the observations. We use galaxies from the Sloan Digital Sky Survey Data Release 7 in the redshift range 0.01 0.2 z . In estimating Lbol, we employ two different methods using [O III ] and/or [O I ] emission lines, and find that the Lbol values obtained from the two methods agree well. We consider the MBH-s∗ relation, the MBH-Lbulge relation, and the single-epoch Ha-based MBH estimate in calculating MBH. We find that the trends of the type 1 AGN fraction with respect to MBH and Lbol are similar for the different methods of deriving Lbol but different when using different methods to derive MBH. We present a model based on the clumpy-torus scheme that reproduces the ridge-shaped distribution of the fraction parallel to the iso-Eddington ratio lines.
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science