2017MNRAS.467.3775P

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 disc of OB stars extending to ∼0.5 pc. 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 disc 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 time-scale. 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_☉, 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 an ∼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.