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Astron. Astrophys. 354, L57-L61 (2000)

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Letter to the Editor

Evidence for TeV gamma-ray emission from the shell type SNR RX J1713.7-3946

H. Muraishi 1, T. Tanimori 2, S. Yanagita 1, T. Yoshida 1, M. Moriya 2, T. Kifune 3, S. A. Dazeley 4, P. G. Edwards 5, S. Gunji 6, S. Hara 2, T. Hara 7, A. Kawachi 3, H. Kubo 2, Y. Matsubara 8, Y. Mizumoto 9, M. Mori 3, Y. Muraki 8, T. Naito 7, K. Nishijima 10, J. R. Patterson 4, G. P. Rowell 3,4, T. Sako 8,11, K. Sakurazawa 2, R. Susukita 12, T. Tamura 13 and T. Yoshikoshi 3

1 Ibaraki University, Faculty of Science, Mito, Ibaraki 310-8521, Japan
2 Tokyo Institute of Technology, Department of Physics, Meguro, Tokyo 152-8551, Japan
3 University of Tokyo, Institute for Cosmic Ray Research, Tanashi, Tokyo 188-8502, Japan
4 University of Adelaide, Department of Physics and Mathematical Physics, South Australia 5005, Australia
5 Institute of Space and Astronautical Science, Sagamihara, Kanagawa 229-8510, Japan
6 Yamagata University, Department of Physics, Yamagata 990-8560, Japan
7 Yamanashi Gakuin University, Faculty of Management Information, Kofu, Yamanashi 400-8575, Japan
8 Nagoya University, STE Laboratory, Nagoya, Aichi 464-8601, Japan
9 National Astronomical Observatory, Tokyo 181-8588, Japan
10 Tokai University, Department of Physics, Hiratsuka, Kanagawa 259-1292, Japan
11 LPNHE, Ecole Polytechnique. Palaiseau CEDEX 91128, France
12 Institute of Physical and Chemical Research, Computational Science Laboratory, Wako, Saitama 351-0198, Japan
13 Kanagawa University, Faculty of Engineering, Yokohama, Kanagawa 221-8686, Japan

Received 1 December 1999 / Accepted 23 December 1999

Abstract

We report the results of TeV gamma-ray observations of the shell type SNR RX J1713.7-3946 (G347.3-0.5). The discovery of strong non-thermal X-ray emission from the northwest part of the remnant strongly suggests the existence of electrons with energies up to [FORMULA] 100 TeV in the remnant, making the SNR a good candidate TeV gamma-ray source. We observed RX J1713.7-3946 from May to August 1998 with the CANGAROO 3.8m atmospheric imaging erenkov telescope and obtained evidence for TeV gamma-ray emission from the NW rim of the remnant with the significance of [FORMULA]. The observed TeV gamma-ray flux from the NW rim region was estimated to be (5.3 [FORMULA] 0.9[statistical] [FORMULA] 1.6[systematic]) [FORMULA] 10-12 photons cm-2 s-1 at energies [FORMULA] 1.8 [FORMULA] 0.9 TeV. The data indicate that the emitting region is much broader than the point spread function of our telescope. The extent of the emission is consistent with that of hard X-rays observed by ASCA. This TeV gamma-ray emission can be attributed to the Inverse Compton scattering of the Cosmic Microwave Background Radiation by shock accelerated ultra-relativistic electrons. Under this assumption, a rather low magnetic field of [FORMULA]G is deduced for the remnant from our observation.

Key words: stars: supernovae: individual: RX J1713.7-3946 – gamma rays: observations

Send offprint requests to: yanagita@mito.ipc.ibaraki.ac.jp

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Online publication: January 31, 2000
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