N-body modeling of globular clusters: Masses, mass-to-light ratios and
  intermediate-mass black holes
  We have determined the masses and mass-to-light ratios of 50 Galactic
globular clusters by comparing their velocity dispersion and surface brightness
profiles against a large grid of 900 N-body simulations of star clusters of
varying initial concentration, size and central black hole mass fraction. Our
models follow the evolution of the clusters under the combined effects of
stellar evolution and two-body relaxation allowing us to take the effects of
mass segregation and energy equipartition between stars self-consistently into
account. For a subset of 16 well observed clusters we also derive their
kinematic distances. We find an average mass-to-light ratio of Galactic
globular clusters of $<M/L_V>=1.98 \pm 0.03$, which agrees very well with the
expected M/L ratio if the initial mass function of the clusters was a standard
Kroupa or Chabrier mass function. We do not find evidence for a decrease of the
average mass-to-light ratio with metallicity. The surface brightness and
velocity dispersion profiles of most globular clusters are incompatible with
the presence of intermediate-mass black holes (IMBHs) with more than a few
thousand $M_\odot$ in them. The only clear exception is $\omega$ Cen, where the
velocity dispersion profile provides strong evidence for the presence of a
$\sim$40,000 $M_\odot$ IMBH in the centre of the cluster.
