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Black hole evolution - I. Supernova-regulated black hole growth

Dubois, Yohan ; Volonteri, Marta ; Silk, Joseph ; Devriendt, Julien ; Slyz, Adrianne ; Teyssier, Romain

In: Monthly Notices of the Royal Astronomical Society, 2015, vol. 452, no. 2, p. 1502-1518

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    Titel
    • Black hole evolution - I. Supernova-regulated black hole growth
    Autor
    • Dubois, Yohan. Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75014, Paris, France
    • Volonteri, Marta. Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75014, Paris, France
    • Silk, Joseph. Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75014, Paris, France
    • Devriendt, Julien. Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
    • Slyz, Adrianne. Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
    • Teyssier, Romain. Institute für Theoretische Physik, Universität Zürich, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland
    Dokumententyp
    • Postprint
    Sprache
    • Englisch
    Veröffentlicht in
    • Monthly Notices of the Royal Astronomical Society, 2015, vol. 452, no. 2, p. 1502-1518. Oxford University Press
    Andere elektronische Ausgabe
    OAI-PMH-ID
    • oai:doc.rero.ch:298994
    Summary
    The growth of a supermassive black hole (BH) is determined by how much gas the host galaxy is able to feed it, which in turn is controlled by the cosmic environment, through galaxy mergers and accretion of cosmic flows that time how galaxies obtain their gas, and also by internal processes in the galaxy, such as star formation and feedback from stars and the BH itself. In this paper, we study the growth of a 1012 M⊙ halo at z=2, which is the progenitor of a group of galaxies at z=0, and of its central BH by means of a high-resolution zoomed cosmological simulation, the Seth simulation. We study the evolution of the BH driven by the accretion of cold gas in the galaxy, and explore the efficiency of the feedback from supernovae (SNe). For a relatively inefficient energy input from SNe, the BH grows at the Eddington rate from early times, and reaches self-regulation once it is massive enough. We find that at early cosmic times z>3.5, efficient feedback from SNe forbids the formation of a settled disc as well as the accumulation of dense cold gas in the vicinity of the BH and starves the central compact object. As the galaxy and its halo accumulate mass, they become able to confine the nuclear inflows provided by major mergers and the BH grows at a sustained near-to-Eddington accretion rate. We argue that this mechanism should be ubiquitous amongst low-mass galaxies, corresponding to galaxies with a stellar mass below ≲ 109 M⊙ in our simulations