Stellar-Mass Black Holes in Globular Clusters: Dynamical Consequences
  and Observational Signatures
  Sizeable number of stellar-mass black holes (BHs) in globular clusters (GCs)
can strongly influence the dynamical evolution and observational properties of
their host cluster. Using results from a large set of numerical simulations, we
identify the key ingredients needed to sustain a sizeable population of BHs in
GCs up to a Hubble time. We find that while BH natal kick prescriptions are
essential in determining the initial retention fraction of BHs in GCs, the
long-term survival of BHs is determined by the size, initial central density
and half-mass relaxation time of the GC. Simulated GC models that contain many
BHs are characterized by relatively low central surface brightness, large
half-light and core radii values. We also discuss novel ways to compare
simulated results with available observational data to identify GCs that are
most likely to contain many BHs.
