  We present the first results of a series of Monte-Carlo simulations
investigating the imprint of a central black hole on the core structure of a
globular cluster. We investigate the three-dimensional and the projected
density profile of the inner regions of idealized as well as more realistic
globular cluster models, taking into account a stellar mass spectrum, stellar
evolution and allowing for a larger, more realistic, number of stars than was
previously possible with direct N-body methods. We compare our results to other
N-body simulations published previously in the literature.
