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Title:
Evidence for TeV gamma-ray emission from the shell type SNR RX J1713.7-3946
Authors:
Muraishi, H.; Tanimori, T.; Yanagita, S.; Yoshida, T.; Moriya, M.; Kifune, T.; Dazeley, S. A.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Kawachi, A.; Kubo, H.; Matsubara, Y.; Mizumoto, Y.; Mori, M.; Muraki, Y.; Naito, T.; Nishijima, K.; Patterson, J. R.; Rowell, G. P.; Sako, T.; Sakurazawa, K.; Susukita, R.; Tamura, T.; Yoshikoshi, T.
Affiliation:
AA(Ibaraki University, Faculty of Science, Mito, Ibaraki 310-8521, Japan), AB(Tokyo Institute of Technology, Department of Physics, Meguro, Tokyo 152-8551, Japan), AC(Ibaraki University, Faculty of Science, Mito, Ibaraki 310-8521, Japan), AD(Ibaraki University, Faculty of Science, Mito, Ibaraki 310-8521, Japan), AE(Tokyo Institute of Technology, Department of Physics, Meguro, Tokyo 152-8551, Japan), AF(University of Tokyo, Institute for Cosmic Ray Research, Tanashi, Tokyo 188-8502, Japan), AG(University of Adelaide, Department of Physics and Mathematical Physics, South Australia 5005, Australia), AH(Institute of Space and Astronautical Science, Sagamihara, Kanagawa 229-8510, Japan), AI(Yamagata University, Department of Physics, Yamagata 990-8560, Japan), AJ(Tokyo Institute of Technology, Department of Physics, Meguro, Tokyo 152-8551, Japan), AK(Yamanashi Gakuin University, Faculty of Management Information, Kofu, Yamanashi 400-8575, Japan), AL(University of Tokyo, Institute for Cosmic Ray Research, Tanashi, Tokyo 188-8502, Japan), AM(Tokyo Institute of Technology, Department of Physics, Meguro, Tokyo 152-8551, Japan), AN(Nagoya University, STE Laboratory, Nagoya, Aichi 464-8601, Japan), AO(National Astronomical Observatory, Tokyo 181-8588, Japan), AP(University of Tokyo, Institute for Cosmic Ray Research, Tanashi, Tokyo 188-8502, Japan), AQ(Nagoya University, STE Laboratory, Nagoya, Aichi 464-8601, Japan), AR(Yamanashi Gakuin University, Faculty of Management Information, Kofu, Yamanashi 400-8575, Japan), AS(Tokai University, Department of Physics, Hiratsuka, Kanagawa 259-1292, Japan), AT(University of Adelaide, Department of Physics and Mathematical Physics, South Australia 5005, Australia), AU(University of Tokyo, Institute for Cosmic Ray Research, Tanashi, Tokyo 188-8502, Japan; University of Adelaide, Department of Physics and Mathematical Physics, South Australia 5005, Australia), AV(Nagoya University, STE Laboratory, Nagoya, Aichi 464-8601, Japan; LPNHE, Ecole Polytechnique. Palaiseau CEDEX 91128, France), AW(Tokyo Institute of Technology, Department of Physics, Meguro, Tokyo 152-8551, Japan), AX(Institute of Physical and Chemical Research, Computational Science Laboratory, Wako, Saitama 351-0198, Japan), AY(Kanagawa University, Faculty of Engineering, Yokohama, Kanagawa 221-8686, Japan), AZ(University of Tokyo, Institute for Cosmic Ray Research, Tanashi, Tokyo 188-8502, Japan)
Publication:
Astronomy and Astrophysics, v.354, p.L57-L61 (2000) (A&A Homepage)
Publication Date:
02/2000
Origin:
A&A
A&A Keywords:
STARS: SUPERNOVAE: INDIVIDUAL: RX J1713.7-3946, GAMMA RAYS: OBSERVATIONS
Bibliographic Code:
2000A&A...354L..57M

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 ~ 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 Čerenkov telescope and obtained evidence for TeV gamma-ray emission from the NW rim of the remnant with the significance of ~ 5.6 sigma . The observed TeV gamma-ray flux from the NW rim region was estimated to be (5.3 +/- 0.9[statistical] +/- 1.6[systematic]) x 10-12 photons cm-2 s-1 at energies >= 1.8 +/- 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 ~ 11 mu G is deduced for the remnant from our observation.

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