Black hole masses from power density spectra: determinations and consequences
Abstract
We show that the X-ray power density spectra do not simply scale linearly with the mass of the black hole over many decades. Nevertheless, the high frequency tail of the power density spectrum can be successfully used for determination of the black hole mass in an AGN if another AGN is used as a reference. We determine the masses of the black holes in 6 Broad Line Seyfert 1 galaxies, 5 Narrow Line Seyfert 1 galaxies and two QSO using available power density spectra. In all but 1 normal Seyferts the resulting luminosity to the Eddington luminosity ratio is smaller than 0.1, with a source MCG-6-15-30 being an exception. Narrow Line Seyfert 1 galaxies have relatively low masses and high luminosity to the Eddington luminosity ratio, supporting the view of those objects as analogs of galactic sources in their high/soft or very high state based on the overall spectral shape. Bulge masses of their host galaxies are similar to normal Seyfert galaxies so they do not follow the black hole mass - bulge mass relation for Seyfert galaxies, being evolutionary less advanced, as suggested by Mathur (2000).Keywords
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