Spin orientation of supermassive black holes in active galaxies

Abstract

Accretion of gas onto a central supermassive black hole is generally accepted to be the source of the emitted energy in active galactic nuclei.The broad emission lines we observe in their optical spectra are probably formed in the wind of an accretion disk at distances of light days to light years from the central black hole. The variable fraction of the emission lines originates at typical distances of only 1 to 50 light days from the central supermassive black hole. We derived a central black hole mass of M_orbital = 1.8 +/-0.4 x 10^7 M_sun in the Seyfert galaxy Mrk110 assuming the broad emission lines are generated in gas clouds orbiting within an accretion disk. This figure depends on the inclination angle of the accretion disk. Here we report on the detection of gravitational redshifted emission in the variable fraction of the broad emission lines. We derive a central black hole mass of M_grav = 14.0 +/-3.0 x 10^7 M_sun. These measurements are independent on the orientation of the accretion disk. The comparison of both black hole mass estimates allows to determine the projection of the central accretion disk angle i to 21 +/-5 deg. in Mrk110 and therefore the orientation of the spin axis of the central black hole.

4 pages, 6 figures, in press in Astronomy and Astrophysics Letters

References in corpus (6)

• Broad Emission Line Shifts in Quasars: An Orientation Measure for Radio-Quiet Quasars?
• Systematic Errors in the Estimation of Black Hole Masses by Reverberation Mapping
• Accretion disk wind in the AGN broad-line region: Spectroscopically resolved line profile variations in Mrk110
• Variability of Active Galactic Nuclei
• Short-term emission line and continuum variations in Mrk110
• Geometry and Kinematics in the Central Broad-Line Region of a Seyfert 1 Galaxy

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