The Origin of Supermassive Black Holes from Pop III.1 Seeds
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arXiv
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| Autores principales: | , , , , , , |
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| Formato: | Preprint |
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2024
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| _version_ | 1866929610733649920 |
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| author | Tan, Jonathan C. Singh, Jasbir Cammelli, Vieri Sanati, Mahsa Petkova, Maya Nandal, Devesh Monaco, Pierluigi |
| author_facet | Tan, Jonathan C. Singh, Jasbir Cammelli, Vieri Sanati, Mahsa Petkova, Maya Nandal, Devesh Monaco, Pierluigi |
| contents | The origin of supermassive black holes (SMBHs) is a key open question for contemporary astrophysics and cosmology. Here we review the features of a cosmological model of SMBH formation from Pop III.1 seeds, i.e., remnants of metal-free stars forming in locally-isolated minihalos, where energy injection from dark matter particle annihilation alters the structure of the protostar allowing growth to supermassive scales (Banik et al. 2019; Singh et al. 2023; Cammelli et al. 2024). The Pop III.1 model explains the paucity of intermediate-mass black holes (IMBHs) via a characteristic SMBH seed mass of $\sim10^5\:M_\odot$ that is set by the baryonic content of minihalos. Ionization feedback from supermassive Pop III.1 stars sets the cosmic number density of SMBHs to be $n_{\rm SMBH}\lesssim 0.2\:{\rm Mpc}^{-3}$. The model then predicts that all SMBHs form by $z\sim20$ with a spatial distribution that is initially unclustered. SMBHs at high redshifts $z\gtrsim7$ should all be single objects, with SMBH binaries and higher order multiples emerging only at lower redshifts. We also discuss the implications of this model for SMBH host galaxy properties, occupation fractions, gravitational wave emission, cosmic reionization, and the nature of dark matter. These predictions are compared to latest observational results, especially from HST, JWST and pulsar timing array observations. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2412_01828 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Origin of Supermassive Black Holes from Pop III.1 Seeds Tan, Jonathan C. Singh, Jasbir Cammelli, Vieri Sanati, Mahsa Petkova, Maya Nandal, Devesh Monaco, Pierluigi Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics The origin of supermassive black holes (SMBHs) is a key open question for contemporary astrophysics and cosmology. Here we review the features of a cosmological model of SMBH formation from Pop III.1 seeds, i.e., remnants of metal-free stars forming in locally-isolated minihalos, where energy injection from dark matter particle annihilation alters the structure of the protostar allowing growth to supermassive scales (Banik et al. 2019; Singh et al. 2023; Cammelli et al. 2024). The Pop III.1 model explains the paucity of intermediate-mass black holes (IMBHs) via a characteristic SMBH seed mass of $\sim10^5\:M_\odot$ that is set by the baryonic content of minihalos. Ionization feedback from supermassive Pop III.1 stars sets the cosmic number density of SMBHs to be $n_{\rm SMBH}\lesssim 0.2\:{\rm Mpc}^{-3}$. The model then predicts that all SMBHs form by $z\sim20$ with a spatial distribution that is initially unclustered. SMBHs at high redshifts $z\gtrsim7$ should all be single objects, with SMBH binaries and higher order multiples emerging only at lower redshifts. We also discuss the implications of this model for SMBH host galaxy properties, occupation fractions, gravitational wave emission, cosmic reionization, and the nature of dark matter. These predictions are compared to latest observational results, especially from HST, JWST and pulsar timing array observations. |
| title | The Origin of Supermassive Black Holes from Pop III.1 Seeds |
| topic | Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2412.01828 |