Using the bulge of M31 as a template for the integrated X-ray emission from low-mass X-ray binaries

We have performed joint ASCA + ROSAT PSPC spectral fitting on the inner 5' of the bulge of M31. We find that single-component spectral models provide an inadequate fit to the spectrum, in contrast to previous studies by Einst ein and Ginga. Although the 2-10 keV spectrum can be fitted adequately with a bremsstrahlung model with kT = 7.4 +/- 0.3 keV, an additional soft compo nent with kT = 0.38 +/- 0.03 keV is required to fit the spectrum below 2 ke V. This soft component comprises 38% +/- 6% of the total emission in the 0. 1-2.0 keV band, and possibly more depending on the absorption value used in the lit. Since previous spatial studies of the bulge of M31 indicate that less than 25% of the X-ray emission from the bulge in this band is from a d iffuse gaseous component, this implies that stellar sources, namely, low-ma ss X-ray binaries (LMXBs), are responsible for some if not all of the soft component. The spectral properties of M31 are very similar to those of the X-ray-faint early-type galaxy NGC 4382. This supports the claim that the un explained soft X-ray emission seen previously in these galaxies also emanat es from LMXBs.