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Building on recent work by Chandar et al. (2020), we construct X-rayluminosity functions (XLFs) for different classes of X-ray binary (XRB) donorsin the nearby star-forming galaxy M83 through a novel methodology: rather thanclassifying low- vs. high-mass XRBs based on the scaling of the number of X-raysources with stellar mass and star formation rate, respectively, we utilizemulti-band Hubble Space Telescope imaging data to classify eachChandra-detected compact X-ray source as a low-mass (i.e. donor mass <~ 3 solarmasses), high-mass (donor mass >~ 8 solar masses) or intermediate-mass XRBbased on either the location of its candidate counterpart on opticalcolor-magnitude diagrams or the age of its host star cluster. In addition tothe the standard (single and/or truncated) power-law functional shape, weapproximate the resulting XLFs with a Schechter function. We identify amarginally significant (at the 1-to-2 sigma level) exponential downturn for thehigh-mass XRB XLF, at logLx ~ 38.48^{+0.52}_{-0.33} (in log CGS units). Incontrast, the low- and intermediate-mass XRB XLFs, as well as the total XLF ofM83, are formally consistent with sampling statistics from a single power-law.Our method suggests a non-negligible contribution from low- and possiblyintermediate-mass XRBs to the total XRB XLF of M83, i.e. between 20 and 50%, inbroad agreement with X-ray based XLFs. More generally, we caution againstconsiderable contamination from X-ray emitting supernova remnants to thepublished, X-ray based XLFs of M83, and possibly all actively star-forminggalaxies.

Calibrating X-ray binary luminosity functions via optical reconnaissance I. The case of M83