  We have developed a set of dynamically evolving Fokker-Planck models for the
collapsed-core globular star cluster M15, which directly address the issue of
whether a central black hole is required to fit Hubble Space Telescope (HST)
observations of the stellar spatial distribution and kinematics. As in our
previous work reported by Dull et al., we find that a central black hole is not
needed. Using local mass-function data from HST studies, we have also inferred
the global initial stellar mass function. As a consequence of extreme mass
segregation, the local mass functions differs from the global mass function at
every location. In addition to reproducing the observed mass functions, the
models also provide good fits to the star-count and velocity-dispersion
profiles, and to the millisecond pulsar accelerations. We address concerns
about the large neutron star populations adopted in our previous Fokker-Planck
models for M15. We find that good model fits can be obtained with as few as
1600 neutron stars; this corresponds to a retention fraction of 5% of the
initial population for our best fit initial mass function. The models contain a
substantial population of massive white dwarfs, that range in mass up to 1.2
solar masses. The combined contribution by the massive white dwarfs and neutron
stars provides the gravitational potential needed to reproduce HST measurements
of the central velocity dispersion profile.
