  Using an updated population synthesis code initially developed by Hurley et
al. we modeled the synthetic X-ray binary (XRB) populations for direct
comparison with the universal, featureless X-ray luminosity function (XLF) of
high mass X-ray binaries (HMXBs) in star-forming galaxies. Our main goal is to
use the universal XLF to constrain the model parameters, given the current
knowledge of binary evolution. We find that the one-dimensional (1D) Maxwellian
velocity dispersion of the natal kick can be constrained to be of the order of
~150km/s, supporting earlier findings that neutron stars (NSs) formed in
binaries seem to receive significantly smaller natal kicks than the velocities
of Galactic single pulsars would indicate. The super-Eddington accretion factor
is further confirmed in the framework of stellar mass black holes (BHs),
revealing the true origin of the most of the ultraluminous X-ray sources (ULXs)
may indeed be the high-luminosity extension of ordinary HMXBs which harbor
stellar-mass BHs rather than exotic intermediate-mass BHs or ones. We present
the detail properties of the model-predicted present-day HMXBs, which may be
investigated by future high-resolution X-ray and optical observations of
sources in nearby star-forming galaxies.
