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We have examined resolved stellar photometry from HST imaging surrounding 18high-mass X-ray binary (HMXB) candidates in NGC 300 and NGC 2403 as determinedfrom combined Chandra/HST analysis. We have fit the color-magnitudedistribution of the surrounding stars with stellar evolution models. All butone region in NGC 300 and two in NGC 2403 contain a population with an agebetween 20 and 70 Myr. One of the candidates is the ultraluminous X-ray source(ULX) in NGC 2403, which we associate with a 60 Myr old population. These agedistributions provide additional evidence that 16 of these 18 candidates areHMXBs. Furthermore, our results suggest that the most common HMXB age in thesegalaxies is 40-55 Myr. This preferred age is similar to observations of HMXBsin the Small Magellanic Cloud, providing new evidence of this formationtimescale, but in higher metallicity populations. We suggest that thispreferred HMXB age is the result of the fortuitous combination of two physicaleffects. First, this is the age of a population when the greatest rate ofcore-collapse events should be occurring, maximizing neutron star production.Second, this is the age when B stars are most likely to be actively losingmass. We also discuss our results in the context of HMXB feedback in galaxies,confirming HMXBs as a potentially important source of energy for theinterstellar medium in low-mass galaxies.

The Ages of High Mass X-ray Binaries in NGC 2403 and NGC 300