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- W2090880925 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 , 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•–(MGσ2)/c2 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 χ2 obtained by using the M•–MGσ2 relation are better than the corresponding ones obtained from the M•–σ or the M•–MG relation." @default.
- W2090880925 created "2016-06-24" @default.
- W2090880925 creator A5068446562 @default.
- W2090880925 creator A5090456074 @default.
- W2090880925 date "2009-09-10" @default.
- W2090880925 modified "2023-09-24" @default.
- W2090880925 title "A HERTZSPRUNG-RUSSELL-LIKE DIAGRAM FOR GALAXIES: THE<i>M</i><sub>•</sub>VERSUS<i>M</i><sub>G</sub>σ<sup>2</sup>RELATION" @default.
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- W2090880925 doi "https://doi.org/10.1088/0004-637x/703/2/1502" @default.
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