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 \sigma _ { kick } \sim 150 km s ^ { -1 } , 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 .