A Panchromatic Study of the X-ray Binary Population in NGC 300 on Sub-Galactic Scales

The population-wide properties and demographics of extragalactic X-ray binaries (XRBs) correlate with the star formation rates (SFRs), stellar masses (M_⋆), and environmental factors (such as metallicity, Z) of their host galaxy. Although there is evidence that XRB scaling relations (L_X/SFR for high mass XRBs [HMXBs] and L_X/M_⋆ for low mass XRBs [LMXBs]) may depend on metallicity and stellar age across large samples of XRB-hosting galaxies, disentangling the effects of metallicity and stellar age from stochastic effects, particularly on subgalactic scales, remains a challenge. We use archival X-ray through IR observations of the nearby galaxy NGC 300 to self-consistently model the broadband spectral energy distribution and examine radial trends in its XRB population. We measure a current (<100 Myr) SFR of 0.18±0.08 M_⊙ yr^-1 and M_⋆= (2.15^+0.26_-0.14)×10^9 M_⊙. Although we measure a metallicity gradient and radially resolved star formation histories that are consistent with the literature, there is a clear excess in the number of X-ray sources below ∼10^37 erg s^-1 that are likely a mix of variable XRBs and additional background AGN. When we compare the subgalactic L_X/SFR ratios as a function of Z to the galaxy-integrated L_X-SFR-Z relationships from the literature, we find that only the regions hosting the youngest (≲30 Myr) HMXBs agree with predictions, hinting at time evolution of the L_X-SFR-Z relationship.