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Title:
Evolution of Supermassive Black Holes
Authors:
Volonteri, M.
Affiliation:
AA(Institute of Astronomy, University of Cambridge)
Publication:
Relativistic Astrophysics Legacy and Cosmology - Einstein's, ESO Astrophysics Symposia, Volume . ISBN 978-3-540-74712-3. Springer-Verlag Berlin Heidelberg, 2008, p. 174
Publication Date:
00/2008
Origin:
SPRINGER
Bibliographic Code:
2008ralc.conf..174V

Abstract

Supermassive black holes (SMBHs) are nowadays believed to reside in most local galaxies, and the available data show an empirical correlation between bulge luminosity - or stellar velocity dispersion - and black hole mass, suggesting a single mechanism for assembling black holes and forming spheroids in galaxy halos. The co-evolution between galaxies and quasars is indicated by the observation of quiescent SMBHs in nearby normal (i.e. not active) galactic centers. The inferred mass density of the inactive black holes is in good agreement with the estimate of the total mass accreted by quasars, through integration of their luminosity function over time. In hierarchical models of galaxy formation major mergers are responsible for forming bulges and elliptical galaxies. Galactic interactions also trigger gas inflows, and the cold gas may be eventually driven into the very inner regions, fueling an accretion episode and the growth of the nuclear SMBH. In cold dark matter cosmogonies, small-mass subgalactic systems form first to merge later into larger and larger structures. In this paradigm galaxy halos experience multiple mergers during their lifetime. If every galaxy with a bulge hosts a SMBH in its center, and a local galaxy has been made up by multiple mergers, then a BH binary is a natural evolutionary stage. The evolution of the supermassive black hole population clearly has to be investigated taking into account both the cosmological framework and the dynamical evolution of SMBHs and their hosts.
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