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A Spatial Study of X-ray Properties in Superbubble 30 Dor C with XMM-Newton

Published online by Cambridge University Press:  27 October 2016

Y. Babazaki ,
I. Mitsuishi ,
H. Sano ,
S. Yoshiike ,
T. Fukuda ,
S. Maruyama ,
K. Fujii ,
Y. Fukui ,
Y. Tawara  and
H Matsumoto
Y. Babazaki
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan; email: y_babazaki@u.phys.nagoya-u.ac.jp
I. Mitsuishi
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan; email: y_babazaki@u.phys.nagoya-u.ac.jp
H. Sano
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan; email: y_babazaki@u.phys.nagoya-u.ac.jp
S. Yoshiike
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan; email: y_babazaki@u.phys.nagoya-u.ac.jp
T. Fukuda
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan; email: y_babazaki@u.phys.nagoya-u.ac.jp
S. Maruyama
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan; email: y_babazaki@u.phys.nagoya-u.ac.jp
K. Fujii
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan; email: y_babazaki@u.phys.nagoya-u.ac.jp
Y. Fukui
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan; email: y_babazaki@u.phys.nagoya-u.ac.jp
Y. Tawara
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan; email: y_babazaki@u.phys.nagoya-u.ac.jp
H Matsumoto
Affiliation:
Kobayashi-Maskawa Institute (KMI), Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, Japan464-8602
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Abstract

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The superbubble (SB) 30 Dor C with the strong non-thermal X-ray emission is one of the best targets for study of the cosmic-ray (CR) acceleration. We investigated X-ray spectral properties of the SB with a high spatial resolution of ~10 pc. Consequently, the spectra in the east regions can be described with a combination of absorbed thermal and non-thermal models while the spectra in the west regions can be fitted with an absorbed non-thermal model. We found that the observed photon index and intensity in 2-10 keV show variations of 2.0-3.5 and (0.6-8.0) × 10−7 erg s−1 cm−2 str−1, respectively. The results are possibly caused by the spatial variation of the CR acceleration efficiency and/or the circumstellar environment.

Keywords

cosmic rays - ISM: supernova remnants - ISM: bubbles - X-rays: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 737
Copyright
Copyright © International Astronomical Union 2016 

References

Sano, H. et al. 2015, ApJ, 799, 175S CrossRefGoogle Scholar
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