REVIEW 6 cited by
Supermassive black holes in cosmological simulations I: M_BH-M_star relation and black hole mass function
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
abstract
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 M_BH-M_star relation and the BH mass function. All simulations predict tight M_BH-M_star relations, and struggle to produce the lowest (M_BH< 10^7.5 Msun) in galaxies of M_star~10^10.5-10^11.5 Msun. While the time evolution of the mean M_BH-M_star relation is mild (<1 dex in BH mass 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_star<10^10.5 Msun. 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 the observations of the local universe, we find an excess of BHs with M_BH>10^9 Msun in most of the simulations. The BH mass function is dominated by efficiently accreting BHs (log10 f_Edd >-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.
Forward citations
Cited by 6 Pith papers
-
The mass-dependent interplay of active galacitc nuclei and supernova feedback in shaping the $L_{\rm X}$--$T$ relation of early-type galaxies
Mass-dependent coupling of AGN winds and supernovae, including a metal-lifting fountain in dwarfs, explains the steep L_X-T relation of early-type galaxies.
-
A prevalent population of normal-mass central black holes in high-redshift massive galaxies
A galaxy-based JWST search finds 13 broad-line AGNs in massive galaxies at z~3-5 with normal black hole-to-stellar mass ratios near the local value, indicating that overmassive black holes are not the only early pathway.
-
Tracing black hole and galaxy growth across environments since cosmic noon
Central black holes in ASTRID and TNG300 follow a tight, redshift-invariant M_BH–M_⋆ relation from z=2 to 0.5; departures mark merger-driven high-mass quenchers, tidally stripped overmassive satellites, and undermassi...
-
Comparing gravitational wave background predictions from cosmological simulations to pulsar timing observations
FABLE simulation predictions for the nanohertz gravitational wave background are statistically consistent with NANOGrav 15-year data at 1–2.5σ tension, with physically motivated population modifications further improv...
-
Large-scale dual AGN in large-scale cosmological hydrodynamical simulations
Across nine cosmological simulations, dual AGN number densities range from 1e-8 to 1e-3 cMpc^-3 at z = 0-7, with fractions of 0-6% and a redshift peak at z = 1-3.
-
Cosmological Simulations of Galaxies
A comprehensive introductory review of cosmological galaxy simulation methods, covering initial conditions, numerical solvers, star formation and feedback, analysis, and validation.
Discussion (0). Continue with ORCID to comment.