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| Formato: | Preprint |
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2025
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| Acceso en línea: | https://arxiv.org/abs/2507.06316 |
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| _version_ | 1866911113108520960 |
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| author | Prieto, Elena González Rodriguez, Carl L. Cabrera, Tomás |
| author_facet | Prieto, Elena González Rodriguez, Carl L. Cabrera, Tomás |
| contents | The recent detection of fast-moving stars in the core of Omega Centauri ($ω$ Cen), the most massive globular cluster (GC) in the Milky Way, has provided strong evidence for the presence of an intermediate-mass black hole (IMBH). As $ω$ Cen, is likely the accreted nucleus of a dwarf galaxy, this IMBH also represents a unique opportunity to study BH seeding mechanisms and their potential role in the formation of supermassive BHs. We present Monte Carlo $N$-body models of $ω$ Cen with detailed treatments for the loss cone dynamics involving stars, binaries, and compact objects. Starting with BH seeds of $500-5000 \, M_{\odot}$ (consistent with runaway collisions of massive stars), our cluster models grow IMBHs with masses of $\sim50{,}000 \, M_{\odot}$ after 12 Gyr, while successfully reproducing the present-day surface brightness and velocity dispersion profiles of $ω$ Cen. We find a population of fast stars similar to those observed in the core of $ω$ Cen, with the fastest stars originating from binaries that were tidally disrupted by the IMBH. The IMBH growth is primarily driven by mergers with $30-40 \, M_{\odot}$ BHs, suggesting a present-day IMBH-BH merger rate of $\sim(4-8)\times10^{-8}~\rm{yr}^{-1}$ in $ω$ Cen-like GCs. Our models also predict a similar rate of tidal disruption events ($\sim5\times10^{-8}~\rm{yr}^{-1}$) which, depending on the frequency of $ω$ Cen-like GCs per galaxy, may represent anywhere from $0.1\%$ to $10\%$ of the observed TDE rate. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_06316 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Growing the Intermediate-mass Black Hole in Omega Centauri Prieto, Elena González Rodriguez, Carl L. Cabrera, Tomás High Energy Astrophysical Phenomena Astrophysics of Galaxies The recent detection of fast-moving stars in the core of Omega Centauri ($ω$ Cen), the most massive globular cluster (GC) in the Milky Way, has provided strong evidence for the presence of an intermediate-mass black hole (IMBH). As $ω$ Cen, is likely the accreted nucleus of a dwarf galaxy, this IMBH also represents a unique opportunity to study BH seeding mechanisms and their potential role in the formation of supermassive BHs. We present Monte Carlo $N$-body models of $ω$ Cen with detailed treatments for the loss cone dynamics involving stars, binaries, and compact objects. Starting with BH seeds of $500-5000 \, M_{\odot}$ (consistent with runaway collisions of massive stars), our cluster models grow IMBHs with masses of $\sim50{,}000 \, M_{\odot}$ after 12 Gyr, while successfully reproducing the present-day surface brightness and velocity dispersion profiles of $ω$ Cen. We find a population of fast stars similar to those observed in the core of $ω$ Cen, with the fastest stars originating from binaries that were tidally disrupted by the IMBH. The IMBH growth is primarily driven by mergers with $30-40 \, M_{\odot}$ BHs, suggesting a present-day IMBH-BH merger rate of $\sim(4-8)\times10^{-8}~\rm{yr}^{-1}$ in $ω$ Cen-like GCs. Our models also predict a similar rate of tidal disruption events ($\sim5\times10^{-8}~\rm{yr}^{-1}$) which, depending on the frequency of $ω$ Cen-like GCs per galaxy, may represent anywhere from $0.1\%$ to $10\%$ of the observed TDE rate. |
| title | Growing the Intermediate-mass Black Hole in Omega Centauri |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2507.06316 |