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Title:
Observation of an Extended Very High Energy Gamma-Ray Emission from MSH 15-52 with CANGAROO-III
Authors:
Nakamori, T.; Kubo, H.; Yoshida, T.; Tanimori, T.; Enomoto, R.; Bicknell, G. V.; Clay, R. W.; Edwards, P. G.; Gunji, S.; Hara, S.; Hara, T.; Hattori, T.; Hayashi, S.; Higashi, Y.; Hirai, Y.; Inoue, K.; Kabuki, S.; Kajino, F.; Katagiri, H.; Kawachi, A.; Kifune, T.; Kiuchi, R.; Kushida, J.; Matsubara, Y.; Mizukami, T.; Mizumoto, Y.; Mizuniwa, R.; Mori, M.; Muraishi, H.; Muraki, Y.; Naito, T.; Nakano, S.; Nishida, D.; Nishijima, K.; Ohishi, M.; Sakamoto, Y.; Seki, A.; Stamatescu, V.; Suzuki, T.; Swaby, D. L.; Thornton, G.; Tokanai, F.; Tsuchiya, K.; Watanabe, S.; Yamada, Y.; Yamazaki, E.; Yanagita, S.; Yoshikoshi, T.; Yukawa, Y.
Affiliation:
AA(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; .), AB(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; .), AC(Faculty of Science, Ibaraki University, Mito, Ibaraki 310-8512, Japan.), AD(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; .), AE(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan.), AF(Research School of Astronomy and Astrophysics, Australian National University, ACT 2611, Australia.), AG(School of Chemistry and Physics, University of Adelaide, SA 5005, Australia.), AH(CSIRO Australia Telescope National Facility, Narrabri, NSW 2390, Australia.), AI(Department of Physics, Yamagata University, Yamagata, Yamagata 990-8560, Japan.), AJ(Ibaraki Prefectural University of Health Sciences, Ami, Ibaraki 300-0394, Japan.), AK(Faculty of Management Information, Yamanashi Gakuin University, Kofu, Yamanashi 400-8575, Japan.), AL(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan.), AM(Department of Physics, Konan University, Kobe, Hyogo 658-8501, Japan.), AN(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; .), AO(Faculty of Science, Ibaraki University, Mito, Ibaraki 310-8512, Japan.), AP(Department of Physics, Yamagata University, Yamagata, Yamagata 990-8560, Japan.), AQ(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; .), AR(Department of Physics, Konan University, Kobe, Hyogo 658-8501, Japan.), AS(Department of Physical Science, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan.), AT(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan.), AU(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan.), AV(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan.), AW(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan.), AX(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8602, Japan.), AY(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; .), AZ(National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan.), BA(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan.), BB(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan.), BC(School of Allied Health Sciences, Kitasato University, Sagamihara, Kanagawa 228-8555, Japan.), BD(Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Aichi 464-8602, Japan.), BE(Faculty of Management Information, Yamanashi Gakuin University, Kofu, Yamanashi 400-8575, Japan.), BF(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; .), BG(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; .), BH(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan.), BI(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan.), BJ(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan.), BK(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan.), BL(School of Chemistry and Physics, University of Adelaide, SA 5005, Australia.), BM(Faculty of Science, Ibaraki University, Mito, Ibaraki 310-8512, Japan.), BN(School of Chemistry and Physics, University of Adelaide, SA 5005, Australia.), BO(School of Chemistry and Physics, University of Adelaide, SA 5005, Australia.), BP(Department of Physics, Yamagata University, Yamagata, Yamagata 990-8560, Japan.), BQ(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; .), BR(Department of Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan; .), BS(Department of Physics, Konan University, Kobe, Hyogo 658-8501, Japan.), BT(Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan.), BU(Faculty of Science, Ibaraki University, Mito, Ibaraki 310-8512, Japan.), BV(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan.), BW(Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan.)
Publication:
The Astrophysical Journal, Volume 677, Issue 1, pp. 297-305. (ApJ Homepage)
Publication Date:
04/2008
Origin:
UCP
ApJ Keywords:
Gamma Rays: Observations, ISM: individual (MSH 15-52), ISM: individual (G320.4-1.2), Stars: Pulsars: Individual: Alphanumeric: PSR B1509-58, ISM: Supernova Remnants
DOI:
10.1086/529029
Bibliographic Code:
2008ApJ...677..297N

Abstract

We have observed the supernova remnant MSH 15-52 (G320.4-1.2), which contains the gamma-ray pulsar PSR B1509-58, using the CANGAROO-III imaging atmospheric Cerenkov telescope array from 2006 April to June. We detected gamma rays above 810 GeV at the 7 σ level during a total effective exposure of 48.4 hr. We obtained a differential gamma-ray flux at 2.35 TeV of (7.9+/-1.5stat+/-1.7sys)×10-13 cm-2 s-1 TeV-1, with a photon index of 2.21+/-0.39stat+/-0.40sys, which is compatible with that of the H.E.S.S. observation in 2004. The morphology shows extended emission compared to our point spread function. We consider the plausible origin of the high-energy emission based on a multiwavelength spectral analysis and energetics arguments.
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