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X-ray Emission from G359.1-0.5

Published online by Cambridge University Press:  12 April 2016

Roland Egger  and
Xuejun Sun
Roland Egger
Affiliation:
Max–Planck–Institut für extraterrestrische Physik, Giessenbachstrasse, D-85740 Garching, Germany
Xuejun Sun
Affiliation:
Beijing Astronomical Observatory, Chinese Academy of Sciences, 100080 Beijing, P.R.China

Abstract

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We report on the detection of X-ray emission from the supernova remnant (SNR) G359.1-0.5 in a deep ROSAT PSPC pointed observation. The diffuse emission is well confined within the radio shell of the SNR. Its spectrum can be represented by a thermal plasma model at T ~ 1 keV and Fx ~ 2×10−11 erg cm−2 s−1 (0.1–2.0 keV) modified by the column absorption of NH ~ 3 × 1022 cm−2. This result supports the view that the source is at a large distance consistent with that from radio observation, and helps to resolve a puzzle about the SNR in previous observations.

Type
Part VII Gas in Superbubbles and in the Galactic Halo
Information
International Astronomical Union Colloquium , Volume 166: The Local Bubble and Beyond , 1997 , pp. 417 - 420
Copyright
Copyright © Springer-Verlag 1998

References

Reich, W., Schlickeiser, R., (1992): A&A 256, 408 Google Scholar
Uchida, K., Morris, M., Yusef-Zadeh, F., (1992): AJ 104, 1533 Google Scholar
Zimmermann, H. et al., (1994): “EXSAS User’s Guide”, MPE Report 257Google Scholar