期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 511, 期 1, 页码 506-535出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stac040
关键词
black holes physics; galaxies: evolution; galaxies: high-redshift; quasars: supermassive black hole
资金
- Swiss National Science Foundation [157591, 194814]
- NSF [AST-2009687, AST-1517491, AST-1715216]
- Flatiron Institute by the Simons Foundation
- CAREER [AST-1652522]
- NASA [17-ATP17-0067]
- Cottrell Scholar Award
- Research Corporation for Science Advancement [26968]
The concurrent growth of supermassive black holes and their host galaxies is explored using cosmological zoom-in simulations. The results show that the growth of supermassive black holes at low redshift can be explained by a gravitational torque-driven accretion model. At high redshift, supermassive black holes are found to be undermassive but start to grow efficiently once their host galaxies reach a certain mass.
The concurrent growth of supermassive black holes (SMBHs) and their host galaxies remains to be fully explored, especially at high redshift. While often understood as a consequence of self-regulation via AGN feedback, it can also be explained by alternative SMBH accretion models. Here, we expand on previous work by studying the growth of SMBHs with the help of a large suite of cosmological zoom-in simulations (MassiveFIRE) that are part of the Feedback in Realistic Environments (FIRE) project. The growth of SMBHs is modelled in post-processing with different black hole accretion models, placements, and merger treatments, and validated by comparing to on-the-fly calculations. Scaling relations predicted by the gravitational torque-driven accretion (GTDA) model agree with observations at low redshift without the need for AGN feedback, in contrast to models in which the accretion rate depends strongly on SMBH mass. At high redshift, we find deviations from the local scaling relations in line with previous theoretical results. In particular, SMBHs are undermassive, presumably due to stellar feedback, but start to grow efficiently once their host galaxies reach M-* similar to 10(10)M(circle dot). We analyse and explain these findings in the context of a simple analytic model. Finally, we show that the predicted scaling relations depend sensitively on the SMBH location and the efficiency of SMBH merging, particularly in low-mass systems. These findings highlight the relevance of understanding the evolution of SMBH-galaxy scaling relations to predict the rate of gravitational wave signals from SMBH mergers across cosmic history.
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