  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.
