The impact of reionization on the formation of supermassive black hole seeds

Johnson, Jarrett L.; Whalen, Daniel J.; Agarwal, Bhaskar; Paardekooper, Jan‐Pieter; Khochfar, Sadegh

doi:10.1093/mnras/stu1676

Cited by 54 publications

(47 citation statements)

References 101 publications

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“…Here M cloud = 10 6 M ⊙ is the typical mass of the central gas cloud collapsing in an atomic cooling halo (e.g. Wise et al 2008;Johnson et al 2011Johnson et al , 2014Latif et al 2013;Choi et al 2013). Assuming a uniform cloud density, which is appropriate for our simplified one-zone calculations, this implies a cloud radius of r cloud = 30 pc (n/10 2 cm −3 ) −1/3 where n is the number density of hydrogen nuclei.…”

Section: Feedback From Lyman α Cooling Radiationmentioning

confidence: 99%

Enhanced direct collapse due to Lyman α feedback

Johnson

Dijkstra

2017

A&A

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We assess the impact of trapped Lyman α cooling radiation on the formation of direct collapse black holes (DCBHs). We apply a one-zone chemical and thermal evolution model, accounting for the photodetachment of H − ions, precursors to the key coolant H 2 , by Lyman α photons produced during the collapse of a cloud of primordial gas in an atomic cooling halo at high redshift. We find that photodetachment of H − by trapped Lyman α photons may lower the level of the H 2 -dissociating background radiation field required for DCBH formation substantially, dropping the critical flux by up to a factor of a few. This translates into a potentially large increase in the expected number density of DCBHs in the early Universe, and supports the view that DCBHs may be the seeds for the BHs residing in the centers of a significant fraction of galaxies today. We find that detachment of H − by Lyman α has the strongest impact on the critical flux for the relatively high background radiation temperatures expected to characterize the emission from young, hot stars in the early Universe. This lends support to the DCBH origin of the highest redshift quasars.

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Section: Feedback From Lyman α Cooling Radiationmentioning

confidence: 99%

Enhanced direct collapse due to Lyman α feedback

Johnson

Dijkstra

2017

A&A

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“…To form a massive POPIII star cluster thus requires a massive primordial gas cloud that can fragment and form POPIII stars in one go. One way to achieve this is by photo-ionization heating (Johnson et al 2014;Visbal et al 2016). The mean UV background (UVB) is not sufficiently high enough to ionize haloes at z > 7 (Faucher-Giguère et al 2009).…”

Section: Modelmentioning

confidence: 99%

Upper limits on the mass and luminosity of Population III-dominated galaxies

Yajima

Khochfar

2016

Monthly Notices of the Royal Astronomical Society: Letters

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We here derive upper limits on the mass and luminosity of Population III (POPIII) dominated proto-galaxies based on the collapse of primordial gas under the effect of angular momentum loss via Lyα radiation drag and the gas accretion onto a galactic centre. Our model predicts that POPIII-dominated galaxies at z ∼ 7 are hosted by haloes with M h ∼ 1.5 × 10 8 − 1.1 × 10 9 M ⊙ , that they have Lyα luminosities of L Lyα ∼ 3.0 × 10 42 − 2.1 × 10 43 erg s −1 , stellar mass of M star ∼ 0.8 × 10 5 − 2.5 × 10 6 M ⊙ , and outflowing gas with velocities V out ∼ 40 km s −1 due to Lyα radiation pressure. We show that the POPIII galaxy candidate CR7 violates the derived limits on stellar mass and Lyα luminosity and thus is unlikely to be a POPIII galaxy. POPIII-dominated galaxies at z ∼ 7 have Heii line emission that is ∼ 1 − 3 orders of magnitude lower then that of Lyα, they have high Lyα equivalent width of 300Å and should be found close to bright star forming galaxies. The Heii 1640Å line is in comfortable reach of next generation telescopes, like the JWST or TMT.

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“…In addition, the gas in this halo must remain atomic (with a temperature on the order of 10 4 K), because the formation of molecular hydrogen will enable further cooling (and thus fragmentation). To prevent the formation of H 2 , it is suggested that the halo may be irradiated by a nearby burst of star formation, producing UV light which dissociates any H 2 (Dijkstra et al 2008;Shang et al 2010;Latif et al 2013a,b;Johnson et al 2014;Regan et al 2014;Choi et al 2015;Dunn et al 2018). The resulting collapsing object may first form a "quasi-star" (Begelman et al 2006), or possibly collapse directly into a black hole (Lodato & Natarajan 2006).…”

Section: Introductionmentioning

confidence: 99%

Multimessenger Signatures of Massive Black Holes in Dwarf Galaxies

Bellovary

Cleary

Munshi

et al. 2018

Monthly Notices of the Royal Astronomical Society

175

174

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Recent discoveries of massive black holes (MBHs) in dwarf galaxies suggest that they may have a more common presence than once thought. Systematic searches are revealing more candidates, but this process could be accelerated by predictions from simulations. We perform a study of several high-resolution, cosmological, zoom-in simulations focusing on dwarf galaxies that host massive black holes at z = 0, with the aim of determining when the black holes are most observable. Larger dwarf galaxies are more likely to host MBHs than those of lower mass. About 50% of the MBHs in dwarfs are not centrally located, but rather are wandering within a few kpc of the galaxy center. The accretion luminosities of MBHs in dwarfs are low throughout cosmic time, rendering them extremely difficult to detect. However, the merger history of these MBHs is optimal for gravitational wave detection by LISA.

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The impact of reionization on the formation of supermassive black hole seeds

Cited by 54 publications

References 101 publications

Enhanced direct collapse due to Lyman α feedback

Enhanced direct collapse due to Lyman α feedback

Upper limits on the mass and luminosity of Population III-dominated galaxies

Multimessenger Signatures of Massive Black Holes in Dwarf Galaxies

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