  It has been assumed that intermediate-mass black holes (IMBHs) in globular
clusters can only reside in the most centrally concentrated clusters, with a
so-called `core-collapsed' density profile. While this would be a natural
guess, it is in fact wrong. We have followed the evolution of star clusters
containing IMBHs with masses between 125 \le M_{BH} \le 1000 M_{\odot} through
detailed N-body simulations, and we find that a cluster with an IMBH, in
projection, appears to have a relatively large `core' with surface brightness
only slightly rising toward the center. This makes it highly unlikely that any
of `core-collapsed' clusters will harbor an IMBH. On the contrary, the places
to look for an IMBH are those clusters that can be fitted well by
medium-concentration King models.
  The velocity dispersion of the visible stars in a globular cluster with an
IMBH is nearly constant well inside the apparent core radius. For a cluster of
mass M_C containing an IMBH of mass M_{BH}, the influence of the IMBH becomes
significant only at a fraction 2.5 M_{BH}/M_C of the half-mass radius, deep
within the core, where it will affect only a small number of stars. In
conclusion, observational detection of an IMBH may be possible, but will be
challenging.
