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The aim of this work is to study the imprints that different models for blackhole (BH) and neutron star (NS) formation have on the Galactic distribution ofX-ray binaries (XRBs) which contain these objects. We find that the root meansquare of the height above the Galactic plane of BH- and NS-XRBs is a powerfulproxy to discriminate among different formation scenarios, and that binaryevolution following the BH/NS formation does not significantly affect theGalactic distributions of the binaries. We find that a population model inwhich at least some BHs receive a (relatively) high natal kick fits theobserved BH-XRBs best. For the NS case, we find that a high NK distribution,consistent with the one derived from the measurement of pulsar proper motion,is the most preferable. We also analyse the simple method we previously used toestimate the minimal peculiar velocity of an individual BH-XRB at birth. Wefind that this method may be less reliable in the bulge of the Galaxy forcertain models of the Galactic potential, but that our estimate is excellentfor most of the BH-XRBs.

The Galactic distribution of X-ray binaries and its implications for compact object formation and natal kicks