X-ray Emission Line Gas in M81

Details X-ray Emission Line Gas in M81 X-ray Emission Line Gas in M81

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hrxs.confe..30p&link_type=abstract

High Resolution X-ray Spectroscopy with XMM-Newton and Chandra, Proceedings of the international workshop held at the Mullard Sp

Computer Science

Scientific paper

The soft X-ray spectrum of the LINER galaxy M81, from a long observation with the XMM-Newton RGS, contains emission lines from Fe-L, H-like and He-like N, O, and Ne. The emission lines are significantly broader than the RGS line spread function and are found adjacent to as well as coincident with the active nucleus. This implies that they originate in a region of a few arcminutes (kpc) extent. The flux ratios of the O VII triplet suggest that the gas is collisionally ionized. A good fit to the whole RGS spectrum can be obtained with an absorbed power law from the active nucleus and a 3-temperature optically thin thermal plasma. Two of the thermal plasma components have temperatures of 0.18 and 0.64 keV, consistent with a hot interstellar medium produced by supernovae. The third thermal plasma component has a higher temperature (1.7 keV); we argue that this emission is likely to come from low-mass X-ray binaries in the bulge of M81.

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