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Title:
Discovery of Interacting Molecular Gas toward the TeV Gamma-Ray Peak of the SNR G 347.3--0.5
Authors:
Fukui, Yasuo; Moriguchi, Yoshiaki; Tamura, Keisuke; Yamamoto, Hiroaki; Tawara, Yuzuru; Mizuno, Norikazu; Onishi, Toshikazu; Mizuno, Akira; Uchiyama, Yasunobu; Hiraga, Junko; Takahashi, Tadayuki; Yamashita, Koujin; Ikeuchi, Satoru
Affiliation:
AA(Department of Astrophysics, Nagoya University), AB(Department of Astrophysics, Nagoya University), AC(Department of Astrophysics, Nagoya University), AD(Department of Astrophysics, Nagoya University), AE(Center for Integrated Research in Science and Engineering, Nagoya University), AF(Department of Astrophysics, Nagoya University), AG(Department of Astrophysics, Nagoya University), AH(Department of Astrophysics, Nagoya University), AI(The Institute of Space and Astronautical Science), AJ(The Institute of Space and Astronautical Science), AK(The Institute of Space and Astronautical Science), AL(Department of Astrophysics, Nagoya University), AM(Department of Astrophysics, Nagoya University)
Publication:
Publications of the Astronomical Society of Japan, Vol.55, No.5, pp. L61-L64 (PASJ Homepage)
Publication Date:
10/2003
Origin:
PASJ
Keywords:
cosmic rays, ISM: cloud, molecules, supernova remnants
Bibliographic Code:
2003PASJ...55L..61F

Abstract

Supernova remnants ( = SNR) are suggested to be sites of cosmic-ray acceleration. In particular, it has been an issue of keen interest whether cosmic ray protons are being accelerated in a SNR which emits TeV γ-rays. A crucial observational test for this is to find dense molecular gas towards the SNR, because such molecular gas can best verify the existence of cosmic-ray protons via pion decay to γ-rays. Here, we show that new high-resolution mm-wave observations of interstellar CO molecule have revealed molecular gas at 1kpc distance interacting with the TeV γ-ray SNR G 347.3 - 0.5, and that a molecular cloud of ˜ 200 solar masses is clearly associated with the TeV γ-ray peak, providing strong evidence for proton acceleration. We have estimated the total energy of accelerated protons to be ˜ 1048 erg, which corresponds to an acceleration efficiency of ˜ 0.001, posing an observational constraint on the proton acceleration.
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