Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth

Rosas-Guevara, Yetli; Bower, Richard G.; Schaye, Joop; McAlpine, Stuart; Vecchia, Claudio Dalla; Frenk, Carlos S.; Schaller, Matthieu; Theuns, Tom

doi:10.1093/mnras/stw1679

Cited by 122 publications

(122 citation statements)

References 85 publications

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“…Sijacki et al (2015) also predict that average Eddington ratios are roughly constant over a broad range of black hole mass (at a given redshift) but drop very rapidly for the very highest mass black holes (MBH 10 9 − 10 10 M⊙, depending on redshift). This mass dependence differs from the much more gradual decrease in average Eddington ratio with increasing black hole mass found by Rosas-Guevara et al (2016) in the EAGLE simulation and the changes in the duty cycle and λsBHAR with stellar mass that we measure. Direct comparisons of the Illustis predictions of p(λsBHAR) as a function of M * are required to explore this issue.…”

Section: Agn Accretion Rate Distributions In Cosmological Simulationscontrasting

confidence: 99%

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

Aird

Coil

Georgakakis

2017

Monthly Notices of the Royal Astronomical Society

161

266

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We use deep Chandra X-ray imaging to measure the distribution of specific black hole accretion rates (L X relative to the stellar mass of the galaxy) and thus trace AGN activity within star-forming and quiescent galaxies, as a function of stellar mass (from 10 8.5 -10 11.5 M ⊙ ) and redshift (to z ∼ 4). We adopt near-infrared selected samples of galaxies from the CANDELS and UltraVISTA surveys, extract X-ray data for every galaxy, and use a flexible Bayesian method to combine these data and to measure the probability distribution function of specific black hole accretion rates, λ sBHAR . We identify a broad distribution of λ sBHAR in both starforming and quiescent galaxies-likely reflecting the stochastic nature of AGN fuelling-with a roughly power-law shape that rises toward lower λ sBHAR , a steep cutoff at λ sBHAR 0.1−1 (in Eddington equivalent units), and a turnover or flattening at λ sBHAR 10 −3 − 10 −2 . We find that the probability of a star-forming galaxy hosting a moderate λ sBHAR AGN depends on stellar mass and evolves with redshift, shifting toward higher λ sBHAR at higher redshifts. This evolution is truncated at a point corresponding to the Eddington limit, indicating black holes may self-regulate their growth at high redshifts when copious gas is available. The probability of a quiescent galaxy hosting an AGN is generally lower than that of a star-forming galaxy, shows signs of suppression at the highest stellar masses, and evolves strongly with redshift. The AGN duty cycle in high-redshift (z 2) quiescent galaxies thus reaches ∼20 per cent, comparable to the duty cycle in star-forming galaxies of equivalent stellar mass and redshift.

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Section: Agn Accretion Rate Distributions In Cosmological Simulationscontrasting

confidence: 99%

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

Aird

Coil

Georgakakis

2017

Monthly Notices of the Royal Astronomical Society

161

266

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“…The black solid line shows the BHMD to SMD ratio of the Illustris simulation with a resolution of 1820 3 (Sijacki et al 2015). The black dashed line shows the BHMD to SMD ratio of the EAGLE simulation (Furlong et al 2015;Rosas-Guevara et al 2016).…”

Section: Resultsmentioning

confidence: 99%

Stellar and Black Hole Mass Densities as Empirical Tracers of Co-Evolution Show Lock-Step Growth Since Z ∼ 3

Schindler

Fan

Duschl

2016

ApJ

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At redshifts beyondz 1, measuring the black hole (BH) galaxy relations proves to be a difficult task. The bright light of the active galactic nuclei aggravates the deconvolution of BH and galaxy properties. However, highredshift data on these relations are vital to understand the ways in which galaxies and BHs co-evolve and the ways in which they do not. In this work we use BH and stellar mass densities (BHMDs and SMDs) to constrain the possible co-evolution of BHs with their host galaxies sincez 5. The BHMDs are calculated from quasar luminosity functions using the Soltan argument, while we use integrals over stellar mass functions or the starformation rate density to obtain values for the SMD. We find that both quantities grow in lock-step below redshifts ofz 3 with a non-evolving BHMD to SMD ratio. A fit to the data assuming a power-law relation between the BHMD and the SMD yields exponents around unity (1.0-1.5). Up toz 5 the BHMD to SMD ratio does not show a strong evolution given the larger uncertainty in the completeness of high-redshift data sets. Our results, always applying the same analysis technique, seem to be consistent across all adopted data sets.

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“…Our typical SMBH mass is 10 7 M in a M * = 10 10.3 M galaxy, and is representative of EAGLE cosmological volumes (Rosas-Guevara et al 2016). The observed Häring & Rix (2004) SMBH mass-galaxy mass relation predicts about ≈ 2× more massive SMBH in their local sample, but it should be noted that this is a bulge-dominated sample.…”

Section: Agn Luminosities and Duty Cycles In Star-forming Galaxiesmentioning

confidence: 99%

Flickering AGN can explain the strong circumgalactic O viobserved by COS-Halos

Oppenheimer¹,

Segers

Schaye

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Proximity zone fossils (PZFs) are ionization signatures around recently active galactic nuclei (AGN) where metal species in the circumgalactic medium remain overionized after the AGN has shut-off due to their long recombination timescales. We explore cosmological zoom hydrodynamic simulations using the EAGLE model paired with a non-equilibrium ionization and cooling module including time-variable AGN radiation to model PZFs around star-forming, disk galaxies in the z ∼ 0.2 Universe. Previous simulations typically under-estimated the O vi content of galactic haloes, but we show that plausible PZF models increase O vi column densities by 2 − 3× to achieve the levels observed around COS-Halos star-forming galaxies out to 150 kpc. Models with AGN bolometric luminosities 10 43.6 erg s −1 , duty cycle fractions 10%, and AGN lifetimes 10 6 yr are the most promising, because their supermassive black holes grow at the cosmologically expected rate and they mostly appear as inactive AGN, consistent with COS-Halos. The central requirement is that the typical star-forming galaxy hosted an active AGN within a timescale comparable to the recombination time of a high metal ion, which for circumgalactic O vi is ≈ 10 7 years. H i, by contrast, returns to equilibrium much more rapidly due to its low neutral fraction and does not show a significant PZF effect. O vi absorption features originating from PZFs appear narrow, indicating photo-ionization, and are often well-aligned with lower metal ion species. PZFs are highly likely to affect the physical interpretation of circumgalactic high ionization metal lines if, as expected, normal galaxies host flickering AGN.

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Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth

Cited by 122 publications

References 85 publications

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

X-rays across the galaxy population – II. The distribution of AGN accretion rates as a function of stellar mass and redshift

Stellar and Black Hole Mass Densities as Empirical Tracers of Co-Evolution Show Lock-Step Growth Since Z ∼ 3

Flickering AGN can explain the strong circumgalactic O viobserved by COS-Halos

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