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| Format: | Preprint |
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2025
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| Accès en ligne: | https://arxiv.org/abs/2510.07389 |
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| _version_ | 1866916997826084864 |
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| author | Ugolini, Cristiano |
| author_facet | Ugolini, Cristiano |
| contents | Intermediate-mass black holes (IMBHs) occupy the $ 10^2 - 10^5\,M_\odot $ range, but their existence remains poorly constrained. Only a few candidates have been suggested in dwarf galaxies, globular clusters, and LIGO-Virgo-Kagra detections. To investigate their formation and demographics, we adopt two complementary approaches. We first analyze the \textsc{dragonii} direct $N$-body simulations, which follow clusters with up to $ 10^6 $ stars, capture IMBHs growth. We then employ the semi-analytic code \textsc{bpop}, calibrated on \textsc{dragonii}, to explore a broad range of cluster and cosmological conditions.
Our models reproduce merger rates consistent with GWTC-3, with $\sim30 - 60\%$ of BBHs forming dynamically, mainly in globular and nuclear clusters. About 2-3\% of mergers involve an IMBH, producing intermediate-mass ratio inspirals. The IMBH mass distribution spans $2.5 \times 10^2 - 4 \times 10^4\,M_\odot $, with rare growth beyond $10^6\,M_\odot$. Formation efficiency rises with initial binary fraction but declines in metal-rich environments. IMBHs thus emerge as a distinct population bridging stellar and supermassive black holes. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_07389 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The assembly of intermediate black holes with complementary approaches: Dragon II and BPop Ugolini, Cristiano Astrophysics of Galaxies Solar and Stellar Astrophysics Intermediate-mass black holes (IMBHs) occupy the $ 10^2 - 10^5\,M_\odot $ range, but their existence remains poorly constrained. Only a few candidates have been suggested in dwarf galaxies, globular clusters, and LIGO-Virgo-Kagra detections. To investigate their formation and demographics, we adopt two complementary approaches. We first analyze the \textsc{dragonii} direct $N$-body simulations, which follow clusters with up to $ 10^6 $ stars, capture IMBHs growth. We then employ the semi-analytic code \textsc{bpop}, calibrated on \textsc{dragonii}, to explore a broad range of cluster and cosmological conditions. Our models reproduce merger rates consistent with GWTC-3, with $\sim30 - 60\%$ of BBHs forming dynamically, mainly in globular and nuclear clusters. About 2-3\% of mergers involve an IMBH, producing intermediate-mass ratio inspirals. The IMBH mass distribution spans $2.5 \times 10^2 - 4 \times 10^4\,M_\odot $, with rare growth beyond $10^6\,M_\odot$. Formation efficiency rises with initial binary fraction but declines in metal-rich environments. IMBHs thus emerge as a distinct population bridging stellar and supermassive black holes. |
| title | The assembly of intermediate black holes with complementary approaches: Dragon II and BPop |
| topic | Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2510.07389 |