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Date and Time of the Query: 2019-03-26 T05:43:27 PDT
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For refcode 2009ApJ...703.1502F:
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Copyright by American Astronomical Society. Reproduced by permission
2009ApJ...703.1502F A Hertzsprung-Russell-like Diagram for Galaxies: The M_blackhole_ Versus M_G_{sigma}^2^ Relation Feoli, A.; Mancini, L. Abstract. We show that the relation between the mass of supermassive black holes located in the center of the host galaxies and the kinetic energy of random motions of the corresponding bulges is a useful tool to study the evolution of galaxies. In the form log_{10}_(M_{bullet}_)=b+m log_{10}_(M_G{sigma}^2/c^2), the best-fitting results for a sample of 64 galaxies of various morphological types are the slope m = 0.80 +/- 0.03 and the normalization b = 4.53 +/- 0.13. We note that, in analogy with the Hertzsprung-Russell diagram for stars, each morphological type of galaxy generally occupies a different area in the M_blackhole_-(M_G_{sigma}^2^)/c^2^ plane. In particular, we find elliptical galaxies in the upper part of the line of best fit, the lenticular galaxies in the middle part, and the late-type galaxies in the lower part, the mass of the central black hole giving an estimate of the age, whereas the kinetic energy of the stellar bulges is directly connected with the temperature of each galactic system. Finally, the values of the linear correlation coefficient, the intrinsic scatter, and the chi^2^ obtained by using the M_blackhole_-M_G_{sigma}^2^ relation are better than the corresponding ones obtained from the M_blackhole_-{sigma} or the M_blackhole_-M_G_ relation. Key words: black hole physics, galaxies: general, galaxies: kinematics and dynamics, galaxies: statistics
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