Formation of supermassive black holes

Volonteri, Marta

doi:10.1007/s00159-010-0029-x

Cited by 780 publications

(744 citation statements)

References 159 publications

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“…The low-mass range is unlikely to form BHs eligible to become central BHs, as they are not sufficiently massive to remain in the galaxy centre (Volonteri 2010). The high-mass range is more favorable.…”

Section: Computing Bh Initial Massesmentioning

confidence: 99%

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Habouzit

Volonteri²,

Dubois³

2017

Monthly Notices of the Royal Astronomical Society

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239

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Massive black holes (BHs) inhabit local galaxies, including the Milky Way and some dwarf galaxies. BH formation, occurring at early cosmic times, must account for the properties of BHs in today's galaxies, notably why some galaxies host a BH, and others do not. We investigate the formation, distribution and growth of BH 'seeds' by using the adaptive mesh refinement code Ramses. We develop an implementation of BH formation in dense, low-metallicity environments, as advocated by models invoking the collapse of the first generation of stars, or of dense nuclear star clusters. The seed masses are computed one-by-one on-the-fly, based on the star formation rate and the stellar initial mass function. This self-consistent method to seed BHs allows us to study the distribution of BHs in a cosmological context and their evolution over cosmic time. We find that all high-mass galaxies tend to host a BH, whereas low-mass counterparts have a lower probability of hosting a BH. After the end of the epoch of BH formation, this probability is modulated by the growth of the galaxy. The simulated BHs connect to low-redshift observational samples, and span a similar range in accretion properties as Lyman-Break Analogs. The growth of BHs in low-mass galaxies is stunted by strong supernova feedback. The properties of BHs in dwarf galaxies thus remain a testbed for BH formation. Simulations with strong supernova feedback, which is able to quench BH accretion in shallow potential wells, produce galaxies and BHs in better agreement with observational constraints.

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Section: Computing Bh Initial Massesmentioning

confidence: 99%

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Habouzit

Volonteri²,

Dubois³

2017

Monthly Notices of the Royal Astronomical Society

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239

223

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“…To make further progress with Chandra, i.e. quantitatively probe the first generation of accreting SMBHs, and place strong constraints on SMBH formation models (Madau & Rees 2001;Lodato & Natarajan 2006Volonteri 2010;Volonteri & Begelman 2010;Begelman 2010), and accretion scenarios (Volonteri & Rees 2005;Dotti et al 2010;Fanidakis et al 2011;King et al 2008), would require to at least a threefold increase in the exposure times, i.e. deep surveys of an additional 30-40 Ms.…”

Section: Future Perspectivesmentioning

confidence: 99%

Faint high-redshift AGN in theChandradeep field south: the evolution of the AGN luminosity function and black hole demography

Fiore

Puccetti²,

Grazian

et al. 2011

A&A

156

172

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Context. We present detection and analysis of faint X-ray sources in the Chandra deep field south (CDFS) using the 4 Ms Chandra observation. Aims. We place constraints on active galactic nuclei (AGN) luminosity functions at z = 3-7, its cosmological evolution, and highredshift black hole and AGN demography. Methods. We use a new detection algorithm, using the entire three-dimensional data-cube (position and energy), and searching for X-ray counts at the position of high-z galaxies in the GOODS-South survey.Results. This optimized technique results in the identification of 54 AGN at z > 3, 29 of which are new detections. Applying stringent completeness criteria, we derive AGN luminosity functions in the redshift bins 3-4, 4-5, and >5.8 and for 42.75 < log L(2-10 keV) < 44.5. We combine this data with the luminous AGN luminosity functions from optical surveys and find that the evolution of the high-z, wide luminosity range luminosity function can be modeled by pure luminosity evolution with L * decreasing from 6.6 × 10 44 erg/s at z = 3 to L * = 2 × 10 44 erg/s at z = 6. We compare the high-z luminosity function with the predictions of theoretical models using galaxy interactions as AGN triggering mechanism. We find that these models are broadly able to reproduce the high-z AGN luminosity functions. Closer agreement is found when we assume a minimum dark matter halo mass for black hole formation and growth. We compare our AGN luminosity functions with galaxy mass functions to derive the high-z AGN duty cycle, using observed Eddington ratio distributions to derive black hole masses. We find that the duty cycle increases with galaxy stellar mass and redshift by a factor of 10-30 from z = 0.25 to z = 4-5. We also report the detection of a large fraction of highly obscured, Compton thick AGN at z > 3 (18 +17 −10 %). Their optical counterparts do not show any reddening and we thus conclude that the size of the X-ray absorber is likely smaller than the dust sublimation radius. We finally report the discovery of a highly star-forming galaxy at z = 3.47, arguing that its X-ray luminosity is likely dominated by stellar sources. If confirmed, this would be one of the farthest objects in which stellar sources have been detected in X-rays.

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“…Several possible scenarios have been suggested for the origin of the SMBHs (Volonteri 2010;Haiman 2013;Johnson & Haardt 2016, references therein). One is remnant BHs of massive Population III (Pop III) stars with ∼ 100 M (Madau & Rees 2001;Haiman & Loeb 2001;Schneider et al 2002;Islam, Taylor & Silk 2003;Volonteri, Haardt & Madau 2003;Tanaka & Haiman 2009).…”

Section: Introductionmentioning

confidence: 99%

Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity

Sakurai

Inayoshi

Haiman

2016

Mon. Not. R. Astron. Soc.

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We perform one-dimensional radiation hydrodynamical simulations to solve accretion flows onto massive black holes (BHs) with a very high rate. Assuming that photon trapping limits the luminosity emerging from the central region to L L Edd , Inayoshi, Haiman & Ostriker (2016) have shown that an accretion flow settles to a "hyper-Eddington" solution, with a steady and isothermal (T 8000 K) Bondi profile reaching 5000 times the Eddington accretion rateṀ Edd ≡ L Edd /c 2 . Here we address the possibility that gas accreting with finite angular momentum forms a bright nuclear accretion disc, with a luminosity exceeding the Eddington limit (1 L/L Edd 100). Combining our simulations with an analytic model, we find that a transition to steady hyper-Eddington accretion still occurs, as long as the luminosity remains below L/L Edd 35 (M BH /10 4 M ) 3/2 (n ∞ /10 5 cm −3 )(T ∞ /10 4 K) −3/2 (r /10 14 cm) −1/2 , where n ∞ and T ∞ are the density and temperature of the ambient gas, and r is the radius of the photosphere, at which radiation emerges. If the luminosity exceeds this value, accretion becomes episodic. Our results can be accurately recovered in a toy model of an optically thick spherical shell, driven by radiation force into a collapsing medium. When the central source is dimmer than the above critical value, the expansion of the shell is halted and reversed by ram pressure of the collapsing medium, and by shell's weight. Our results imply that rapid, unimpeded hyper-Eddington accretion is possible even if the luminosity of the central source far exceeds the Eddington limit, and can be either steady or strongly episodic.

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Formation of supermassive black holes

Cited by 780 publications

References 159 publications

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Blossoms from black hole seeds: properties and early growth regulated by supernova feedback

Faint high-redshift AGN in theChandradeep field south: the evolution of the AGN luminosity function and black hole demography

Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity

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