  We use direct N-body simulations to study the inspiral and internal evolution
of dense star clusters near the Galactic center. These clusters sink toward the
center due to dynamical friction with the stellar background, and may go into
core collapse before being disrupted by the Galactic tidal field. If a cluster
reaches core collapse before disruption, its dense core, which has become rich
in massive stars, survives to reach close to the Galactic center. When it
eventually dissolves, the cluster deposits a disproportionate number of massive
stars in the innermost parsec of the Galactic nucleus. Comparing the spatial
distribution and kinematics of the massive stars with observations of IRS 16, a
group of young He I stars near the Galactic center, we argue that this
association may have formed in this way.
