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Unresolved X-ray Emission and Hot ISM in the bulge of M 31

Published online by Cambridge University Press:  17 September 2012

Á. Bogdán  and
M. Gilfanov
Á. Bogdán
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str.1, 85741 Garching bei München, Germany
M. Gilfanov
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str.1, 85741 Garching bei München, Germany Space Research Institute, Russian Academy of Sciences, Profsoyuznaya 84/32, 117997 Moscow, Russia
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Abstract

We investigate the unresolved X-ray emission originating from the bulge of M 31. We show that a part of this emission is due to a large number of faint sources – mainly accreting white dwarfs and active binaries, associated with the old stellar population, similar to the Galactic ridge X-ray emission of the Milky Way. We also detect soft X-ray emission from ionized gas. It has a temperature of about ∼300 eV and total mass of ∼2 × 106Msun. The gas distribution is extended along the minor axis of the galaxy suggesting that it may be outflowing in the direction perpendicular to the disk of M 31. The outflow can be maintained from the mass and energy supply from evolved stars and type Ia supernovae respectively.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 56: The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall? , 2012 , pp. 239 - 242
Copyright
© EAS, EDP Sciences, 2012

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References

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