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Date and Time of the Query: 2019-06-25 T03:44:19 PDT
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For refcode 2004ApJ...614...91W:
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2004ApJ...614...91W Black Hole Mass and Accretion Rate of Active Galactic Nuclei with Double-peaked Broad Emission Lines Xue-Bing Wu and F. K. Liu Abstract. Using an empirical relation between the broad-line region size and optical continuum luminosity, we estimated the black hole mass and accretion rate for 135 active galactic nuclei (AGNs) with double-peaked broad emission lines in two samples, one from the Sloan Digital Sky Survey (SDSS) and the other from a survey of radio-loud broad emission line AGNs. With black hole masses ranging from 3x10^7^M_sun_ to 5x10^9^M_sun_, these AGNs have dimensionless accretion rates (Eddington ratios) between 0.001 and 0.1 and bolometric luminosity between 10^43^ and 10^46^ ergs s^-1^, both values being significantly larger than those of several previously known low-luminosity (L_bol_<10^43^ ergs s^-1^) double-peaked AGNs. The optical - X-ray spectra indices, {alpha}_OX_, of these high-luminosity double-peaked AGNs are between 1 and 1.9, systematically larger than those of low-luminosity objects, which are around 1. Modest correlations (with a Spearman rank correlation coefficient of 0.60) of the {alpha}_OX_ value with the Eddington ratio and bolometric luminosity have been found, indicating that double-peaked AGNs with higher Eddington ratios or higher luminosity tend to have larger {alpha}_OX_ values. Based on these results, we suggested that the accretion process in the central region of some high-luminosity double-peaked emission line AGNs (especially those with Eddington ratios larger than 0.01) is probably different from that of low-luminosity objects, in which a well-known ADAF-like accretion flow was thought to exist. It is likely that the accretion physics in some high-luminosity double-peaked AGNs is similar to that in normal type 1 AGNs, which is also supported by the presence of possible big blue bumps in the spectra of some double-peaked AGNs with higher Eddington ratios. We note that the prototype double-peaked emission line AGN, Arp 102B, which has a black hole mass of 10^8^ M_sun_ and a dimensionless accretion rate of 0.001, may be an "intermediate" object between the high- and low-luminosity double-peaked AGNs. In addition, we found an apparent strong anticorrelation (with a Spearman rank correlation coefficient of -0.79) between the peak separation of double-peaked profiles and Eddington ratios. However, such an anticorrelation is probably induced by a strong correlation between the peak separation and emission-line widths and needs to be confirmed by future work. If it is real, it may provide us another clue to understanding why double-peaked broad emission lines were hardly found in luminous AGNs with Eddington ratios larger than 0.1. Keywords: Accretion, Accretion Disks, Black Hole Physics, Galaxies: Active, Galaxies: Nuclei, Galaxies: Quasars: Emission Lines, Galaxies: Quasars: General
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