  Recent Chandra observations of interacting and starburst galaxies have led us
to investigate the apparent correlation between the positions of young star
clusters and Chandra point sources. Assumed to be X-ray binaries (XRBs), these
point sources do not seem to coincide with the massive (~1e5 Msun), young (1-50
Myr) stellar clusters that can easily form systems capable of such emission. We
use a sophisticated binary evolution and population synthesis code (StarTrack)
and a simplified cluster model to track both the X-ray luminosity and position
of XRBs as a function of time. These binaries are born within the cluster
potential with self-consistent positions and velocities and we show that a
large fraction (~70%) can be ejected from the parent due to supernova
explosions and associated systemic velocities. For brighter sources and cluster
masses below ~1e6 Msun, we find that the average number of bright XRBs per
cluster remains near or below unity, consistent with current observations.
