Globular Cluster (GC) cores have long been speculated to contain
Intermediate-Mass Black Holes (IMBHs). Claims stemming from indirect
detection methods abound, however there are still no definitive
detections of radio or X-ray emission from accreting matter on IMBHs
in GCs. Due to the high mass of IMBHs, an important criterium for
distinguishing an IMBH candidate from other sources is based on how
central the source is. I will briefly discuss analytical predictions
and numerical simulation results about how far an IMBH can wander from
the center of a typical GC, and the consequences in terms of potential
false negatives in direct detection attempts.