The Assembly of the First Massive Black Holes
By K. Inayoshi, E. Visbal, Zoltán Haiman. 2019
425 citations recorded by the source corpus.
The existence of $\approx$10^9 Msun supermassive black holes (SMBHs) within the first billion year of the universe has stimulated numerous ideas for the prompt formation and rapid growth of BHs in the early universe. Here we review ways in which the seeds of massive BHs may have first assembled, how they may have subsequently grown as massive as $\approx$10^9 Msun, and how multi-messenger observations could distinguish between different SMBH assembly scenarios. We conclude the following: (1) The ultra-rare $\approx$10^9 Msun SMBHs represent only the tip of the iceberg. Early BHs likely fill a continuum from stellar-mass (approx. 10 Msun) to the super-massive ($\approx$10^9 Msun) regime, reflecting a range of initial masses and growth histories. (2) Stellar-mass BHs were likely left behind by the first generation of stars at redshifts as high as z=30, but their initial growth was typically stunted due to the shallow potential wells of their host galaxies. (3) Conditions in some larger, metal-poor galaxies soon became conducive to the rapid formation and growth of massive `seed' holes, via gas accretion and by mergers in dense stellar clusters. (4) BH masses depend on the environment (such as the number and properties of nearby radiation sources and the local baryonic streaming velocity), and on the metal enrichment and assembly history of the host galaxy. (5) Distinguishing between assembly mechanisms will be difficult, but a combination of observations by LISA (probing massive BH growth via mergers) and by deep multi-wavelength electromagnetic observations (probing growth via gas accretion) is particularly promising.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/0256b7e02b11d70fca92ae9ccb313d03e28e4cb7
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Citations in the corpus
- A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties (2023, background): “…the evolution of the SMBH growth in cosmic history, but previous observations have been limited to bright quasars identified in surveys with ground-based telescopes (e.g., Ba˜nados et al. 2016; Shen et al. 2019, see Inayoshi et al. 2020 for a review) including the most distant quasars at z > 7 .”
- Pōniuā‘ena: A Luminous z = 7.5 Quasar Hosting a 1.5 Billion Solar Mass Black Hole (2020, background): “…(e.g., Mortlock et al. 2011; Wu et al. 2015; Bañados et al. 2018) have already raised the question of how these early SMBHs grew in such a short time (e.g., Volonteri 2012; Smith et al. 2017; Inayoshi et al. 2019), which probably requires massive seed black holes, as illustrated in Figure 2.”
- JWST CEERS and JADES Active Galaxies at z = 4–7 Violate the Local M •–M ⋆ Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models (2023, background): “Seeds are typically categorized into light ( M • ∼ 10 2 M ⊙ ) and heavy ( M • ∼ 10 5 M ⊙ ) seeds (see, e.g., the reviews Woods et al. 2019; Inayoshi et al. 2020; Fan et al. 2023).”
- A Census of Photometrically Selected Little Red Dots at 4 < z < 9 in JWST Blank Fields (2024, methodology): “Previously limited to UV − selected samples at z ≲ 6 (Kashikawa et al. 2015; Ba˜nados et al. 2018; Matsuoka et al. 2018; Inayoshi et al. 2020; Wang et al. 2021; Fan et al. 2022) we are now able to use JWST to reveal the presence of AGN during (e.g. Kocevski et al. 2023; Matthee et al. 2023; ¨Ubler…”
- Nuclear star clusters (2009, background): “Several recent reviews summarise the different proposed formation channels (Volonteri 2010, 2012; Mezcua 2017; Greene et al. 2019; Inayoshi et al. 2019).”