Merger and Accretion History of Massive Black Holes

Details Merger and Accretion History of Massive Black Holes Merger and Accretion History of Massive Black Holes

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...203.8708v&link_type=abstract

American Astronomical Society Meeting 203, #87.08; Bulletin of the American Astronomical Society, Vol. 36, p.582

Astronomy and Astrophysics

Astronomy

Scientific paper

We investigate a hierarchical structure formation scenario describing the evolution of a Super Massive Black Holes (SMBHs) population.
The seeds of the local SMBHs are assumed to be 'pregalactic' black holes, remnants of the first POPIII stars. As these pregalactic holes become incorporated through a series of mergers into larger and larger halos, they sink to the center owing to dynamical friction, accrete a fraction of the gas in the merger remnant to become supermassive, form a binary system, and eventually coalesce. Binaries decay efficiently both as a result of stellar slingshots and, at very high redshifts, due to triple BH interactions.
A simple model in which the damage done to a stellar cusps by decaying BH pairs is cumulative is able to reproduce the observed scaling relation between galaxy luminosity and core size. An accretion model connecting quasar activity with major mergers and the observed BH mass-velocity dispersion correlation reproduces remarkably well the observed luminosity function of optically-selected quasars in the redshift range 1 < z < 5.
Support for this work was provided by NASA grant NAG5-11513 and NSF grant AST-0205738 (P.M.)

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