Kinematics of disk galaxies with known masses of their supermassive black holes. Observations

Astronomy Reports (Impact Factor: 0.76). 01/2010; 54(7):578-589. DOI: 10.1134/S1063772910070024

ABSTRACT This is the first paper in a project aimed at analyzing relations between the masses of supermassive black holes or nuclear
clusters in galaxies and the kinematic features of the host galaxies. We present long-slit spectroscopic observations of galaxies
obtained on the 6-m telescope of the Special Astrophysical Observatory using the SCORPIO focal reducer. Radial profiles of
the line-of-sight velocities and velocity dispersions of the stellar populations were obtained for seven galaxies with known
masses of their supermassive black holes (Mkn 79, Mkn 279, NGC 2787, NGC 3245, NGC 3516, NGC 7457, and NGC 7469), and also
for one galaxy with a nuclear cluster (NGC 428). Velocity profiles of the emitting gas were obtained for some of these galaxies
as well. We present preliminary galactic rotation curves derived from these data.

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    ABSTRACT: The statistical relation between the masses of supermassive black holes (SMBHs) in disk galaxies and the kinematic properties of their host galaxies is analyzed. Velocity estimates for several galaxies obtained earlier at the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences and the data for other galaxies taken from the literature are used. The SMBH masses correlate well with the rotational velocities at a distance of R ≈ 1 kpc, V 1, which characterize the mean density of the central region of the galaxy. The SMBH masses correlate appreciably weaker with the asymptotic velocity at large distances from the center and the angular velocity at the optical radius R 25. We have found for the first time a correlation between the SMBH mass and the total mass of the galaxy within the optical radius R 25, M 25, which includes both baryonic and “dark” mass. The masses of the nuclear star clusters in disk galaxies (based on the catalog of Seth et al.) are also related to the dynamical mass M 25; the correlations with the luminosity and rotational velocity of the disk are appreciably weaker. For a given value of M 25, the masses of the central cluster are, on average, an order of magnitude higher in S0-Sbc galaxies than in late-type galaxies, or than the SMBH masses. We suggest that the growth of the SMBH occurs in the forming “classical” bulge of the galaxy over a time < 109 yr, during a monolithic collapse of gas in the central region of the protogalaxy. The central star clusters form on a different time scale, and their stellar masses continue to grow for a long time after the growth of the central black hole has ceased, if this process is not hindered by activity of the nucleus.
    Astronomy Reports 01/2011; 55(7):595-607. · 0.76 Impact Factor
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    ABSTRACT: The present situation in the study of black holes is described. Currently, scientists have little doubt about their existence, and the launch of the Russian Radioastron radio interferometer gives hope for finding conclusive evidence of this in the near future.
    Herald of the Russian Academy of Sciences 03/2013; 83(2). · 0.21 Impact Factor