# Infalling Young Clusters in the Galactic Centre: implications for IMBHs and young stellar populations

## TL;DR

This study investigates whether migrating young star clusters can explain the young stellar populations near the Galactic Centre, concluding that such migration is unlikely and in-situ formation is more plausible.

## Contribution

The paper uses N-body simulations to show that migrating clusters cannot produce the observed young stars or IMBHs, challenging previous migration-based theories.

## Key findings

- Massive star mergers produce stars collapsing into black holes of 20-400 solar masses.
- Migrating clusters do not form IMBHs capable of explaining the young populations.
- The presence of a 2 pc ring of massive stars is inconsistent with the migration scenario.

## Abstract

The central parsec of the Milky Way hosts two puzzlingly young stellar populations, a tight isotropic distribution of B stars around SgrA* (the S-stars) and a disk of OB stars extending to ~0.5pc. Using a modified version of Sverre Aarseth's direct summation code NBODY6 we explore the scenario in which a young star cluster migrates to the Galactic Centre within the lifetime of the OB disk population via dynamical friction. We find that star clusters massive and dense enough to reach the central parsec form a very massive star via physical collisions on a mass segregation timescale. We follow the evolution of the merger product using the most up to date, yet conservative, mass loss recipes for very massive stars. Over a large range of initial conditions, we find that the very massive star expels most of its mass via a strong stellar wind, eventually collapsing to form a black hole of mass 20 - 400 M_Sun, incapable of bringing massive stars to the Galactic Centre. No massive intermediate mass black hole can form in this scenario. The presence of a star cluster in the central ~10 pc within the last 15 Myr would also leave a ~2 pc ring of massive stars, which is not currently observed. Thus, we conclude that the star cluster migration model is highly unlikely to be the origin of either young population, and in-situ formation models or binary disruptions are favoured.