TY - JOUR
T1 - Black holes on FIRE
T2 - Stellar feedback limits early feeding of galactic nuclei
AU - Anglés-Alcázar, Daniel
AU - Faucher-Giguère, Claude André
AU - Quataert, Eliot
AU - Hopkins, Philip F.
AU - Feldmann, Robert
AU - Torrey, Paul
AU - Wetzel, Andrew
AU - Kereš, Dušan
N1 - Publisher Copyright:
© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2017/11/21
Y1 - 2017/11/21
N2 - We introduce massive black holes (BHs) in the Feedback In Realistic Environments (FIRE) project and perform high-resolution cosmological hydrodynamic simulations of quasar-mass haloes [Mhalo(z = 2) ≈ 1012.5M⊙] down to z = 1. These simulations model stellar feedback by supernovae, stellar winds and radiation, and BH growth using a gravitational torque-based prescription tied to the resolved properties of galactic nuclei.We do not include BH feedback. We show that early BH growth occurs through short (≲1Myr) accretion episodes that can reach or even exceed the Eddington rate. In this regime, BH growth is limited by bursty stellar feedback continuously evacuating gas from galactic nuclei, and BHs remain undermassive in low-mass galaxies relative to the local MBH-Mbulgerelation. BH growth is more efficient at later times, when the nuclear stellar potential retains a significant gas reservoir, star formation becomes less bursty and galaxies settle into a more ordered state. BHs rapidly converge on to the observed scaling relations when the host reaches Mbulge ~1010M⊙. We show that resolving the effects of stellar feedback on the gas supply in the inner ~100 pc of galaxies is necessary to accurately capture the growth of central BHs. Our simulations imply that bursty stellar feedback has important implications for BH-galaxy relations, AGN demographics and time variability, the formation of early quasars and massive BH mergers.
AB - We introduce massive black holes (BHs) in the Feedback In Realistic Environments (FIRE) project and perform high-resolution cosmological hydrodynamic simulations of quasar-mass haloes [Mhalo(z = 2) ≈ 1012.5M⊙] down to z = 1. These simulations model stellar feedback by supernovae, stellar winds and radiation, and BH growth using a gravitational torque-based prescription tied to the resolved properties of galactic nuclei.We do not include BH feedback. We show that early BH growth occurs through short (≲1Myr) accretion episodes that can reach or even exceed the Eddington rate. In this regime, BH growth is limited by bursty stellar feedback continuously evacuating gas from galactic nuclei, and BHs remain undermassive in low-mass galaxies relative to the local MBH-Mbulgerelation. BH growth is more efficient at later times, when the nuclear stellar potential retains a significant gas reservoir, star formation becomes less bursty and galaxies settle into a more ordered state. BHs rapidly converge on to the observed scaling relations when the host reaches Mbulge ~1010M⊙. We show that resolving the effects of stellar feedback on the gas supply in the inner ~100 pc of galaxies is necessary to accurately capture the growth of central BHs. Our simulations imply that bursty stellar feedback has important implications for BH-galaxy relations, AGN demographics and time variability, the formation of early quasars and massive BH mergers.
KW - Black hole physics
KW - Cosmology: Theory
KW - Galaxies: Active
KW - Galaxies: Evolution
KW - Galaxies: Formation
KW - Quasars: Supermassive black holes
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U2 - 10.1093/mnrasl/slx161
DO - 10.1093/mnrasl/slx161
M3 - Article
AN - SCOPUS:85042556215
SN - 1745-3925
VL - 472
SP - L109-L114
JO - Monthly Notices of the Royal Astronomical Society: Letters
JF - Monthly Notices of the Royal Astronomical Society: Letters
IS - 1
ER -