Formation of the First Stars and Black Holes

Haemmerlé, L.; Mayer, Lucio; Klessen, Ralf S.; Hosokawa, Takashi; Madau, Piero; Bromm, Volker

doi:10.1007/s11214-020-00673-y

Cited by 64 publications

(48 citation statements)

References 264 publications

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“…Only few astrophysical scenarios can lead to such high accretion rates. In scenarios relying on seed black holes of only tens to hundreds of solar masses formed by the collapse of metal-free Population III stars at z > 20, this cannot be sustained due to the ionising bubbles that easily stifle accretion (Haemmerlé et al 2020). In direct collapse scenarios, a significantly more massive black hole seed results from the collapse of a precursor object assembled via high inflow rates (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…In direct collapse scenarios, a significantly more massive black hole seed results from the collapse of a precursor object assembled via high inflow rates (e.g. Woods et al 2019;Haemmerlé et al 2020). The most studied of these scenarios relies on inflows driven by the gravitational collapse of protogalaxies hosted in primordial, atomically cooled halos, reaching temperatures of ∼10 4 K (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…The formation of the black hole seed represents a critical step in the formation of the earliest SMBHs (e.g. Woods et al 2019;Haemmerlé et al 2020). The most important parameter is its mass, which is key for the efficiency of further accretion (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Maximum accretion rate of supermassive stars

Haemmerlé

Klessen

Mayer

et al. 2021

A&A

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Context. The formation of the most massive quasars observed at high redshifts requires extreme inflows of gas down to the length scales of the central compact object. Aims. Here we estimate the maximum inflow rate allowed by gravity down to the surface of supermassive stars, the possible progenitors of these supermassive black holes. Methods. We use the continuity equation and the assumption of spherical symmetry and free fall to derive the maximum allowed inflow rates for various density profiles. We apply our approach to the mass–radius relation of rapidly accreting supermassive stars to estimate an upper limit to the accretion rates allowed during the formation of these objects. Results. We find that, as long as the density of the accreted gas is smaller than or equal to the average density of the accretor, the maximum allowed rate, Ṁmax, is given uniquely by the compactness of the accretor. We argue that a density inversion between accreting matter and the accretor is inconsistent with gravitational collapse. For the compactness of rapidly accreting supermassive stars, Ṁmax is related to the stellar mass, M, by a power law, Ṁmax ∝ M3/4. The rates of atomically cooled halos (0.1−10 M⊙ yr−1) are allowed as soon as M ≳ 1 M⊙. The largest rates expected in galaxy mergers (104 − 105 M⊙ yr−1) become accessible once the accretor is supermassive (M ≳ 104 M⊙). Conclusions. These results suggest that supermassive stars can accrete up to masses > 106 M⊙ before they collapse via the general-relativistic instability. At such masses, the collapse is expected to lead to the direct formation of a supermassive black hole, even within metal-rich gas, resulting in a black hole seed that is significantly heavier than in conventional direct collapse models for atomic cooling halos.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Maximum accretion rate of supermassive stars

Haemmerlé

Klessen

Mayer

et al. 2021

A&A

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“…Lodato & Natarajan 2006;Gallo et al 2008;Bonoli, Mayer & Callegari 2014;Miller et al 2015) or the death of the first stars (f occ > 60 per cent; e.g. Volonteri, Lodato & Natarajan 2008;van Wassenhove et al 2010;Volonteri 2010Volonteri , 2012Volonteri & Bellovary 2012;Reines & Comastri 2016;Haemmerlé et al 2020;Inayoshi, Visbal & Haiman 2020;).…”

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confidence: 99%

The MBHBM⋆ Project – II. Molecular gas kinematics in the lenticular galaxy NGC 3593 reveal a supermassive black hole

Nguyen

Bureau

Thater

et al. 2021

Monthly Notices of the Royal Astronomical Society

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As part of the Measuring Black Holes in below Milky Way-mass (M⋆) galaxies (MBHBM⋆) Project, we present a dynamical measurement of the supermassive black hole (SMBH) mass in the nearby lenticular galaxy NGC 3593, using cold molecular gas 12CO(2-1) emission observed at an angular resolution of ≈0${_{.}^{\prime\prime}}$3 (≈10 pc) with the Atacama Large Millimeter/submillimeter Array (ALMA). Our ALMA observations reveal a circumnuclear molecular gas disc (CND) elongated along the galaxy major axis and rotating around the SMBH. This CND has a relatively low-velocity dispersion (≲10 km s−1) and is morphologically complex, with clumps having higher integrated intensities and velocity dispersions (≲25 km s−1). These clumps are distributed along the ridges of a two-arm/bi-symmetric spiral pattern surrounded by a larger ring-like structure (radius r ≈ 10 arcsec or ≈350 pc). This pattern likely plays an important role to bridge the molecular gas reservoirs in the CND and beyond (10 ≲ r ≲ 35 arcsec or 350 pc ≲ r ≲ 1.2 kpc). Using dynamical modelling, the molecular gas kinematics allow us to infer an SMBH mass $M_{\rm BH}=2.40_{-1.05}^{+1.87}\times 10^6$ M⊙ (only statistical uncertainties at the 3σ level). We also detect a massive core of cold molecular gas (CMC) of mass MCMC = (5.4 ± 1.2) × 106 M⊙ and effective (half-mass) radius rCMC,e = 11.2 ± 2.8 pc, co-spatial with a nuclear star cluster (NSC) of mass MNSC = (1.67 ± 0.48) × 107 M⊙ and effective radius rNSC,e = 5.0 ± 1.0 pc (or 0${_{.}^{\prime\prime}}$15 ± 0${_{.}^{\prime\prime}}$03). The mass profiles of the CMC and NSC are well described by Sérsic functions with indices 1−1.4. Our MBH and MNSC estimates for NGC 3593 agree well with the recently compiled MBH–MNSC scaling relation. Although the MNSC uncertainty is twice the inferred MBH, the rapid central rise of the rotation velocities of the CND (as the radius decreases) clearly suggests an SMBH. Indeed, our dynamical models show that even if MNSC is at the upper end of its allowed range, the evidence for a BH does not vanish, but remains with a lower limit of MBH > 3 × 105 M⊙.

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“…Lodato & Natarajan 2006;Gallo et al 2008;Bonoli et al 2014;Miller et al 2015) or the death of the first stars ( 𝑓 occ > 60%; e.g. Volonteri et al 2008;van Wassenhove et al 2010;Volonteri 2010Volonteri , 2012Volonteri & Bellovary 2012;Reines & Comastri 2016;Inayoshi et al 2020;Haemmerlé et al 2020).…”

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The MBHBM$^{\star}$ Project -- II. Molecular Gas Kinematics in the Lenticular Galaxy NGC 3593 Reveal a Supermassive Black Hole

Nguyen,

Bureau,

Thater

et al. 2021

Preprint

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As part of the Measuring Black Holes in Below Milky Way-mass (M ★ ) galaxies (MBHBM ★ ) Project, we present a dynamical measurement of the supermassive black hole (SMBH) mass in the nearby lenticular galaxy NGC 3593, using cold molecular gas 12 CO(2-1) emission observed at an angular resolution of ≈ 0. 3 (≈ 10 pc) with the Atacama Large Millimeter/submillimeter Array (ALMA). Our ALMA observations reveal a circumnuclear molecular gas disc (CND) elongated along the galaxy major axis and rotating around the SMBH. This CND has a relatively low velocity dispersion ( 10 km s −1 ) and is morphologically complex, with clumps having higher integrated intensities and velocity dispersions ( 25 km s −1 ). These clumps are distributed along the ridges of a two-arm/bi-symmetric spiral pattern surrounded by a larger ring-like structure (radius 𝑟 ≈ 10 or ≈ 350 pc). This pattern likely plays an important role to bridge the molecular gas reservoirs in the CND and beyond ( 10𝑟 35 or 350 pc 𝑟 1.2 kpc). Using dynamical modelling, the molecular gas kinematics allow us to infer a SMBH mass 𝑀 BH = 2.40 +1.87 −1.05 × 10 6 M (only statistical uncertainties at the 3𝜎 level). We also detect a massive core of cold molecular gas (CMC) of mass 𝑀 CMC = (5.4 ± 1.2) × 10 6 M and effective (half-mass) radius 𝑟 CMC,e = 11.2 ± 2.8 pc, co-spatial with a nuclear star cluster (NSC) of mass 𝑀 NSC = (1.67 ± 0.48) × 10 7 M and effective radius 𝑟 NSC,e = 5.0 ± 1.0 pc (or 0. 15 ± 0. 03). The mass profiles of the CMC and NSC are well described by Sérsic functions with indices 1 − 1.4. Our 𝑀 BH and 𝑀 NSC estimates for NGC 3593 agree well with the recently compiled 𝑀 BH -𝑀 NSC scaling relation. Although the 𝑀 NSC uncertainty is twice the inferred 𝑀 BH , the rapid central rise of the rotation velocities of the CND (as the radius decreases) clearly suggests a SMBH. Indeed, our dynamical models show that even if 𝑀 NSC is at the upper end of its allowed range, the evidence for a black hole does not vanish, but remains with a lower limit of 𝑀 BH > 3 × 10 5 M .

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Formation of the First Stars and Black Holes

Cited by 64 publications

References 264 publications

Maximum accretion rate of supermassive stars

Maximum accretion rate of supermassive stars

The MBHBM⋆ Project – II. Molecular gas kinematics in the lenticular galaxy NGC 3593 reveal a supermassive black hole

The MBHBM$^{\star}$ Project -- II. Molecular Gas Kinematics in the Lenticular Galaxy NGC 3593 Reveal a Supermassive Black Hole

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