The Illustris simulation: the evolving population of black holes across cosmic time

By D. Sijacki, M. Vogelsberger, Shy Genel, Volker Springel, P. Torrey, Gregory F. Snyder, D. Nelson, Lars Hernquist IoAKICC, Cambridge, Mit and 7 more. 2014

444 citations recorded by the source corpus.

We study the properties of black holes and their host galaxies across cosmic time in the Illustris simulation. Illustris is a large-scale cosmological hydrodynamical simulation which resolves a (106.5 Mpc)^3 volume with more than 12 billion resolution elements and includes state-of-the-art physical models relevant for galaxy formation. We find that the black hole mass density for redshifts z = 0–5 and the black hole mass function at z = 0 predicted by Illustris are in very good agreement with the most recent observational constraints. We show that the bolometric and hard X-ray luminosity functions of active galactic nuclei (AGN) at z = 0 and 1 reproduce observational data very well over the full dynamic range probed. Unless the bolometric corrections are largely underestimated, this requires radiative efficiencies to be on average low, ϵ_r ≲ 0.1, noting however that in our model radiative efficiencies are degenerate with black hole feedback efficiencies. Cosmic downsizing of the AGN population is in broad agreement with the findings from X-ray surveys, but we predict a larger number density of faint AGN at high redshifts than currently inferred. We also study black hole–host galaxy scaling relations as a function of galaxy morphology, colour and specific star formation rate. We find that black holes and galaxies co-evolve at the massive end, but for low mass, blue and star-forming galaxies there is no tight relation with either their central black hole masses or the nuclear AGN activity.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/9794a6a544bd50479dcda64d2fa2f839072f4165

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Citations in the corpus

Eccentric Black Hole Gravitational-wave Capture Sources in Galactic Nuclei: Distribution of Binary Parameters (2017, background): “However, these massive GN are expected to be subdominant, in terms of EBBH rates, because the rates per single GN approximately do not depend on the SMBH mass and lowmass SMBHs are more common (see Sijacki et al. 2015 and references therein).”
The impact of angular momentum on black hole accretion rates in simulations of galaxy formation (2013, methodology): “This approach along with a radiative mode, that includes the effects of a strong ionizing radiation emerging from active BHs in the net gas cooling rates, is used in the recent large volume cosmological simulations of the ILLUSTRIS project (Vogelsberger et al. 2014; Sijacki et al. 2015).”
Gravitational torque-driven black hole growth and feedback in cosmological simulations (2016, methodology): “…ratios (Anglés-Alcázar et al. 2015) and the typical densities, metallicities, and SFR properties in galactic nuclei, it is plausible that T (hence the black hole–host scalings) could evolve (see, e.g., Hopkins et al. 2007a; Di Matteo et al. 2008; DeGraf et al. 2015; Sijacki et al. 2015).”
The Romulus cosmological simulations: a physical approach to the formation, dynamics and accretion models of SMBHs (2016, methodology): “For example, a common treatment of SMBH dynamics is to assume they are always stable at the center of their host galaxies, often obtained by shifting a SMBH towards the nearest potential minimum (Sijacki et al. 2015), a process we refer to as ‘advection’.”
The cosmic evolution of massive black holes in the Horizon-AGN simulation (2016, methodology): “The overestimate of the faint end of the LF is a common problem in cosmological simulations; for instance Sijacki et al. (2015) find a similar behaviour in the Illustris simulations.”
Simulating galaxy formation with black hole driven thermal and kinetic feedback (2016, methodology): “The fact that the burstiness of the feedback has such a dramatic impact is in agreement with other works (e.g. Le Brun et al. 2014; Sijacki et al. 2015) and can in our case be explained by the fact that the velocity kicks directly determine the strength of the resulting shocks as well as the post…”
Massive Black Hole Binary Mergers in Dynamical Galactic Environments (2016, methodology): “For detailed descriptions of the general results of the Illustris simulations, and comparisons of their properties with the observed universe, see e.g., Vogelsberger et al. (2014a), Genel et al. (2014), and Sijacki et al. (2015).”
THE SINFONI BLACK HOLE SURVEY: THE BLACK HOLE FUNDAMENTAL PLANE REVISITED AND THE PATHS OF (CO)EVOLUTION OF SUPERMASSIVE BLACK HOLES AND BULGES (2016, background): “Thus, we would expect the MBH/MBu ratio to increase with increasing redshift (Sijacki et al. 2015).”
RELATIONS BETWEEN CENTRAL BLACK HOLE MASS AND TOTAL GALAXY STELLAR MASS IN THE LOCAL UNIVERSE (2015, background): “In most cosmological simulations that produce statistical samples of BHs and AGNs, i.e., large uniform-volume simulations (e.g., MassiveBlack I and II, Di Matteo et al. (2012); DeGraf et al. (2014); Illustris, Sijacki et al. (2015); Eagle, Schaye et al. (2015); Horizon-AGN, Dubois et al. (2014)) the”
The illustris simulation: Public data release (2015, background): “Any investigation of the black hole population should cite if appropriate Sijacki et al. (2014).”
The star formation activity of IllustrisTNG galaxies: main sequence, UVJ diagram, quenched fractions, and systematics (2018, background): “…build and improve upon the original Illustris project (Vogelsberger et al. 2013; Torrey et al. 2014; Vogelsberger et al. 2014b; Genel et al. 2014; Sijacki et al. 2015; Nelson et al. 2015) by including, among others, a new black-hole feedback model, magnetohydrodynamics, and a new scheme for…”
The IllustrisTNG simulations: public data release (2018, methodology): “The IllustrisTNG project a is the successor of the original Illustris simulation b (Genel et al. 2014; Sijacki et al. 2015; Vogelsberger et al. 2014b, 2014a) and its associated galaxy formation model (Vogelsberger et al. 2013; Torrey et al. 2014).”
First results from the IllustrisTNG simulations: the galaxy colour bimodality (2017, methodology): “The emergence of cosmological hydrodynamical simulations as powerfully predictive theoretical models is embodied in the recent Illustris (Vogelsberger et al. 2014a,b; Genel et al. 2014; Sijacki et al. 2015) and EAGLE (Schaye et al. 2015; Crain et al. 2015) simulations.”
First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies (2017, unknown): “Still, projects like Illustris (Vogelsberger et al. 2014b,a; Genel et al. 2014; Sijacki et al. 2015) and EAGLE (Schaye et al. 2015; Crain et al. 2015) have shown that hydrodynamical simulations with sub-grid models tailored to such resolutions can reproduce many structural properties and scaling…”
The dark nemesis of galaxy formation : why hot haloes trigger black hole growth and bring star formation to an end (2016, background): “Such observations have motivated the inclusion of black hole feedback in cosmological galaxy formation models (eg., Di Matteo et al. 2005; Croton et al. 2006; Bower et al. 2006; Sijacki et al. 2007; Booth & Schaye 2009; Dubois et al. 2013; Sijacki et al. 2015; Dubois et al. 2016).”
Theoretical Challenges in Galaxy Formation (2016, methodology): “…rates, dark matter fractions, gas fractions as well as stellar and black hole masses, from well defined initial conditions, for a direct comparison to observational galaxy surveys (e.g. Davé et al. 2013, Hirschmann et al. 2014, Khandai et al. 2015, Schaye et al. 2015, Sijacki et al. 2015).”