LERGs have order-of-magnitude lower average X-ray luminosities (a proxy for accretion rate) than HERGs and RQ-AGN across 0.3<z≤2.
The cosmic evolution of massive black holes in the Horizon-AGN simulation
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
abstract
We analyse the demographics of black holes (BHs) in the large-volume cosmological hydrodynamical simulation Horizon-AGN. This simulation statistically models how much gas is accreted onto BHs, traces the energy deposited into their environment and, consequently, the back-reaction of the ambient medium on BH growth. The synthetic BHs reproduce a variety of observational constraints such as the redshift evolution of the BH mass density and the mass function. Strong self-regulation via AGN feedback, weak supernova feedback, and unresolved internal processes result in a tight BH-galaxy mass correlation. Starting at z~2, tidal stripping creates a small population of BHs over-massive with respect to the halo. The fraction of galaxies hosting a central BH or an AGN increases with stellar mass. The AGN fraction agrees better with multi-wavelength studies, than single-wavelength ones, unless obscuration is taken into account. The most massive halos present BH multiplicity, with additional BHs gained by ongoing or past mergers. In some cases, both a central and an off-centre AGN shine concurrently, producing a dual AGN. This dual AGN population dwindles with decreasing redshift, as found in observations. Specific accretion rate and Eddington ratio distributions are in good agreement with observational estimates. The BH population is dominated in turn by fast, slow, and very slow accretors, with transitions occurring at z=3 and z=2 respectively.
representative citing papers
Unresolved massive black hole binaries will create a stochastic foreground in LISA that can raise the minimum detectable amplitude of a cosmological gravitational wave background by up to a factor of about 40 near a spectral index of one.
A fully connected network trained on millions of simulated quads predicts SIE lens mass and ellipticity from four image positions, cutting optimisation time for real and simulated quadruply lensed quasars to minutes.
FIRE-3 cosmological simulations of Seyfert galaxies produce episodic AGN feedback and gas clearing but no clear anti-correlation between nuclear gas concentration and AGN luminosity, highlighting timing mismatches with observations.
Horizon-AGN shows galaxy and black hole merger rates both rise with stellar mass and fall with redshift, peaking near z=2-3, establishing a direct evolutionary link from galaxy interactions to black hole coalescences.
citing papers explorer
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Fundamental differences in the X-ray accretion properties of low and high-excitation radio galaxies
LERGs have order-of-magnitude lower average X-ray luminosities (a proxy for accretion rate) than HERGs and RQ-AGN across 0.3<z≤2.
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A Fog Over the Cosmological SGWB: Unresolved Massive Black Hole Binaries in the LISA Band
Unresolved massive black hole binaries will create a stochastic foreground in LISA that can raise the minimum detectable amplitude of a cosmological gravitational wave background by up to a factor of about 40 near a spectral index of one.
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Speeding up Gravitational Lens Mass Models with Machine Learning: Applications in X-ray Astronomy
A fully connected network trained on millions of simulated quads predicts SIE lens mass and ellipticity from four image positions, cutting optimisation time for real and simulated quadruply lensed quasars to minutes.
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Investigating black hole accretion and feedback self-regulation in Seyfert galaxies using the FIRE-3 cosmological hydrodynamic simulations
FIRE-3 cosmological simulations of Seyfert galaxies produce episodic AGN feedback and gas clearing but no clear anti-correlation between nuclear gas concentration and AGN luminosity, highlighting timing mismatches with observations.
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One Merge to Rule Them All: From Galaxy Interactions to Black Hole Mergers Using Horizon-AGN
Horizon-AGN shows galaxy and black hole merger rates both rise with stellar mass and fall with redshift, peaking near z=2-3, establishing a direct evolutionary link from galaxy interactions to black hole coalescences.