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The evolution of high-redshift massive black holes

Published online by Cambridge University Press:  17 August 2016

Marta Volonteri
Affiliation:
Institut dAstrophysique de Paris, Sorbonne Universitès, UPMC Univ Paris 6 et CNRS, UMR 7095, 98 bis bd Arago, 75014 Paris, France email: martav@iap.fr, habouzit@iap.fr
Melanie Habouzit
Affiliation:
Institut dAstrophysique de Paris, Sorbonne Universitès, UPMC Univ Paris 6 et CNRS, UMR 7095, 98 bis bd Arago, 75014 Paris, France email: martav@iap.fr, habouzit@iap.fr
Fabio Pacucci
Affiliation:
Scuola Normale Superiore, Piazza dei Cavalieri, 7 56126 Pisa, Italy email: fabio.pacucci@sns.it
Michael Tremmel
Affiliation:
Department of Astronomy, University of Washington, Seattle, WA email: mjt29@astro.washington.edu
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Abstract

Massive black holes (MBHs) are nowadays recognized as integral parts of galaxy evolution. Both the approximate proportionality between MBH and galaxy mass, and the expected importance of feedback from active MBHs in regulating star formation in their host galaxies point to a strong interplay between MBHs and galaxies. MBHs must form in the first galaxies and be fed by gas in these galaxies, with continuous or intermittent inflows that, at times, can be larger than the Eddington rate. Feedback from supernovae and from the MBHs themselves modulates the growth of the first MBHs. While current observational data only probe the most massive and luminous MBHs, the tip of the iceberg, we will soon be able to test theoretical models of MBH evolution on more “normal” MBHs: the MBHs that are indeed relevant in building the population that we observe in local galaxies, including our own Milky Way.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2016 

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