The coupled evolution of nuclear star clusters and intermediate-mass black holes in a dwarf-galaxy merger

@misc{partmann2026coupled,
  title = {{The coupled evolution of nuclear star clusters and intermediate-mass black holes in a dwarf-galaxy merger}},
  author = {Christian Partmann and Rachel S. Somerville and Michaela Hirschmann and Antti Rantala and Natalia Lahén},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.38767},
  eprint = {2610.38767},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.38767},
  note = {CC BY 4.0},
}

TY  - UNPB
TI  - The coupled evolution of nuclear star clusters and intermediate-mass black holes in a dwarf-galaxy merger
AU  - Christian Partmann
AU  - Rachel S. Somerville
AU  - Michaela Hirschmann
AU  - Antti Rantala
AU  - Natalia Lahén
PY  - 2026
DA  - 2026/10/28
PB  - arXiv
DO  - 10.48550/arxiv.2610.38767
UR  - https://arxiv.org/abs/2610.38767
AB  - Nuclear star clusters (NSCs) and intermediate-mass black holes (IMBHs) are expected to coexist in low-mass galaxies and might together facilitate the coalescence and growth of IMBHs. We simulate an equal-mass, gas-rich dwarf-galaxy merger in which each progenitor hosts a 10^3 M_⊙ IMBH embedded in a 10^6 M_⊙ NSC to study their co-evolution. The simulation model combines the multiphase interstellar medium and fully sampled initial stellar mass function of GRIFFIN at 4 M_⊙ gas resolution with the regularised post-Newtonian black hole dynamics of KETJU. Black holes are modelled as accreting sink particles without feedback. Without NSCs, 10^3-10^4 M_⊙ IMBHs sink only to separations of $50−200\,\rm pc$ and capture no gas. With NSCs, the clusters coalesce within ∼ 500 Myr, the IMBHs form a binary within a few Myr, and scattering of mainly old NSC stars drives them to merger ∼ 340 Myr later. The NSCs also promote gas capture, growing the black holes to 1.1×10^5 and 4.1×10^4 M_⊙. Gas capture is suppressed during the merger-induced starburst by stellar feedback and the motion of the NSCs relative to the gas, and proceeds in brief supernova-regulated episodes once the NSCs have settled in the centre. Scattering by the IMBH binary and the merger recoil of ∼ 175 km s^−1, which removes the remnant from the NSC but not from the galaxy, leave a larger, rotating NSC with a flat core. The stellar tidal disruption rate rises towards coalescence, and the merger is detectable with LISA out to high redshift. NSCs thus remove the delivery and hardening bottlenecks of IMBH mergers in low-mass galaxies.
ER  -