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Title:
Direct Cosmological Simulations of the Growth of Black Holes and Galaxies
Authors:
Di Matteo, Tiziana; Colberg, Jörg; Springel, Volker; Hernquist, Lars; Sijacki, Debora
Affiliation:
AA(Physics Department, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213.), AB(Physics Department, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213.), AC(Max-Planck-Institut für Astrophysik, Karl-Schwarzchild-Strasse 1, 85740 Garching bei München, Germany.), AD(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.), AE(Max-Planck-Institut für Astrophysik, Karl-Schwarzchild-Strasse 1, 85740 Garching bei München, Germany.)
Publication:
The Astrophysical Journal, Volume 676, Issue 1, pp. 33-53. (ApJ Homepage)
Publication Date:
03/2008
Origin:
UCP
ApJ Keywords:
Cosmology: Theory, Galaxies: Active, Galaxies: Evolution, Galaxies: Formation, Hydrodynamics, Galaxies: Quasars: General
DOI:
10.1086/524921
Bibliographic Code:
2008ApJ...676...33D

Abstract

We investigate the coupled formation and evolution of galaxies and their embedded supermassive black holes using state-of-the-art hydrodynamic simulations of cosmological structure formation. For the first time, we self-consistently follow the dark matter dynamics, radiative gas cooling, and star formation, as well as BH growth and associated feedback processes, starting directly from initial conditions appropriate for the ΛCDM cosmology. Our modeling of the black hole physics is based on an approach that we have developed in simulations of isolated galaxy mergers. Here we examine (1) the predicted global history of BH mass assembly, (2) the evolution of the local black hole-host mass correlations, and (3) the conditions that allow rapid growth of the first quasars, and the properties of their hosts and descendants today. We find a total BH mass density in good agreement with observational estimates. The BH accretion rate density peaks at lower redshift and evolves more strongly at high redshift than the star formation rate density, but the ratio of black hole to stellar mass density shows only a moderate evolution at low redshifts. We find strong correlations between BH masses and properties of the stellar systems, agreeing well with the measured local MBH-σ and MBH-M* relationships, but also suggesting (dependent on the mass range) a weak evolution with redshift in the normalization and the slope. Our simulations also produce massive black holes at high redshift, due to extended periods of exponential growth in regions that collapse early and exhibit strong gas inflows. These first supermassive BH systems, however, are not necessarily the most massive ones today, since they are often overtaken in growth by quasars that form later.
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