Massive Black Holes in Star Clusters. II. Realistic Cluster Models
  We have followed the evolution of multi-mass star clusters containing massive central black holes through collisional N-body simulations done on GRAPE6. Each cluster is composed of between 16,384 to 131,072 stars together with a black hole with an initial mass of M_BH=1000 Msun. We follow the evolution of the clusters under the combined influence of two-body relaxation, stellar mass-loss and tidal disruption of stars.   The (3D) mass density profile follows a power-law distribution \rho \sim r^{-\alpha} with slope \alpha=1.55. This leads to a constant density profile of bright stars in projection, which makes it highly unlikely that core collapse clusters contain intermediate-mass black holes (IMBHs). Instead globular clusters containing IMBHs can be fitted with standard King profiles.   The disruption rate of stars is too small to form an IMBH out of a M_BH \approx 50 Msun progenitor black hole, unless a cluster starts with a central density significantly higher than what is seen in globular clusters.   Kinematical studies can reveal 1000 Msun IMBHs in the closest clusters. IMBHs in globular clusters are only weak X-ray sources since the tidal disruption rate of stars is low and the star closest to the IMBH is normally another black hole. For globular clusters, dynamical evolution can push compact stars near the IMBH to distances small enough that they become detectable through gravitational radiation. If 10% of all globular clusters contain IMBHs, extragalactic globular clusters could be one of the major sources for {\it LISA}. (abridged) 
Holger Baumgardt, Junichiro Makino, Toshikazu Ebisuzaki