Skip to content
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Menu
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Menu
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Publication Details
AFRICAN RESEARCH NEXUS
SHINING A SPOTLIGHT ON AFRICAN RESEARCH
earth and planetary sciences
Supermassive black holes in cosmological simulations I: MBH − M* relation and black hole mass function
Monthly Notices of the Royal Astronomical Society, Volume 503, No. 2, Year 2021
Notification
URL copied to clipboard!
Description
The past decade has seen significant progress in understanding galaxy formation and evolution using large-scale cosmological simulations. While these simulations produce galaxies in overall good agreement with observations, they employ different sub-grid models for galaxies and supermassive black holes (BHs). We investigate the impact of the sub-grid models on the BH mass properties of the Illustris, TNG100, TNG300, Horizon-AGN, EAGLE, and SIMBA simulations, focusing on the MBH − M* relation and the BH mass function. All simulations predict tight MBH − M* relations, and struggle to produce BHs of MBH ≤ 107.5 M☉ in galaxies of M* ∼ 1010.5-1011.5 M☉. While the time evolution of the mean MBH − M* relation is mild (ΔMBH ≤ 1 dex for 0 ≤ z ≤ 5) for all the simulations, its linearity (shape) and normalization varies from simulation to simulation. The strength of SN feedback has a large impact on the linearity and time evolution for M* ≤ 1010.5 M☉. We find that the low-mass end is a good discriminant of the simulation models, and highlights the need for new observational constraints. At the high-mass end, strong AGN feedback can suppress the time evolution of the relation normalization. Compared with observations of the local Universe, we find an excess of BHs with MBH ≥ 109 M☉ in most of the simulations. The BH mass function is dominated by efficiently accreting BHs (log10 fEdd ≥ −2) at high redshifts, and transitions progressively from the high-mass to the low-mass end to be governed by inactive BHs. The transition time and the contribution of active BHs are different among the simulations, and can be used to evaluate models against observations. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society
Authors & Co-Authors
Somerville, Rachel S.
United States, New York
Simons Foundation
United States, New Brunswick
Rutgers University–new Brunswick
Genel, Shy
United States, New York
Simons Foundation
United States, New York
Columbia University
Pillepich, Annalisa
Germany, Heidelberg
Max Planck Institute for Astronomy
Dav́e, Romeel
United Kingdom, Edinburgh
The University of Edinburgh
Peirani, Sébastien
France, Nice
Laboratoire Joseph-louis Lagrange
Hernquist, Lars E.
United States, Cambridge
Harvard-smithsonian Center for Astrophysics
Anglés-Alcázar, Daniel
United States, New York
Simons Foundation
United States, Storrs
University of Connecticut
Bower, Richard G.
United Kingdom, Durham
Durham University
Dubois, Yohan
France, Paris
Cnrs Centre National de la Recherche Scientifique
Nelson, Dylan
Germany, Garching Bei Munchen
Max Planck Institute for Astrophysics
Pichon, Christophe
France, Paris
Cnrs Centre National de la Recherche Scientifique
Vogelsberger, Mark
United States, Cambridge
Massachusetts Institute of Technology
Statistics
Citations: 57
Authors: 12
Affiliations: 17
Identifiers
Doi:
10.1093/mnras/stab496
ISSN:
00358711