Decomposing The X-ray Emission From The M31 Bulge

Details Decomposing The X-ray Emission From The M31 Bulge Decomposing The X-ray Emission From The M31 Bulge

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.3904l&link_type=abstract

American Astronomical Society Meeting 208, #39.04; Bulletin of the American Astronomical Society, Vol. 38, p.114

Astronomy and Astrophysics

Astronomy

Scientific paper

We map out the bulge of M 31 using 40 Chandra ACIS observations. We are able to isolate discrete X-ray sources down to 5×1034 erg/s in the 0.5-8 keV band and study the remaining diffuse emission. We find that the 2-8 keV diffuse emission closely traces the K-band light in the bulge region, indicating an origin primarily in the old stellar populations, analogous to the recently proposed origin of the Galactic ridge X-ray emission by Revnivtsev et al. (2005). The 0.5-2 keV diffuse emission is also found to well follow the K-band light, but only at large radii (r > 1.4 kpc); the prominent excess at smaller radii presumably arises from hot gas, which is likely regulated by stellar feedbacks.

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