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In this paper we use an RXTE library of spectral models from 10 black-holeand 9 pulsar X-ray binaries, as well as model spectra available in theliterature from 13 extra-galactic Ultra-luminous X-ray sources (ULXs). Wecompute average bolometric corrections (BC=$\mathrm{L_{band}/L_{bol}}$) for oursample as a function of different accretion rates. We notice the same behaviourbetween black-hole and pulsars BCs only when ULX pulsars are included. Thesemeasurements provide a picture of the energetics of the accretion flow for anX-ray binary based solely on its observed luminosity in a given band. Moreoverit can be a powerful tool in X-ray binary population synthesis models.Furthermore we calculate the X-ray (2-10 keV) to optical (V-band) flux ratiosat different Eddington ratios for the black-hole X-ray binaries in our sample.This provides a metric of the maximum contribution of the disk to the opticalemission of a binary system and better constraints on its nature (donor typeetc). We find that the optical to X-ray flux ratio shows very little variationas a function of accretion rate, but testing for different disk geometriesscenarios we find that the optical contribution of the disk increases as the$p$ value decreases ($T(r)\sim r^{-p}$). Moreover observational data are inagreement with a thicker disk scenario ($p<0.65$), which could also possiblyexplain the lack of observed high-inclination systems.

Average bolometric corrections and optical to X-ray flux measurements as a function of accretion rate for X-ray binaries