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First Detection of Photons with Energy beyond 100 TeV from an Astrophysical Source.
Amenomori, M; Bao, Y W; Bi, X J; Chen, D; Chen, T L; Chen, W Y; Chen, Xu; Chen, Y; Cui, S W; Ding, L K; Fang, J H; Fang, K; Feng, C F; Feng, Zhaoyang; Feng, Z Y; Gao, Qi; Gou, Q B; Guo, Y Q; He, H H; He, Z T; Hibino, K; Hotta, N; Hu, Haibing; Hu, H B; Huang, J; Jia, H Y; Jiang, L; Jin, H B; Kajino, F; Kasahara, K; Katayose, Y; Kato, C; Kato, S; Kawata, K; Kozai, M; Le, G M; Li, A F; Li, H J; Li, W J; Lin, Y H; Liu, B; Liu, C; Liu, J S; Liu, M Y; Lou, Y-Q; Lu, H; Meng, X R; Mitsui, H; Munakata, K; Nakamura, Y.
Afiliação
  • Amenomori M; Department of Physics, Hirosaki University, Hirosaki 036-8561, Japan.
  • Bao YW; School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China.
  • Bi XJ; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Chen D; National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China.
  • Chen TL; Physics Department of Science School, Tibet University, Lhasa 850000, China.
  • Chen WY; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Chen X; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Chen Y; University of Chinese Academy of Sciences, Beijing 100049, China.
  • Cirennima; School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China.
  • Cui SW; Physics Department of Science School, Tibet University, Lhasa 850000, China.
  • Danzengluobu; Department of Physics, Hebei Normal University, Shijiazhuang 050016, China.
  • Ding LK; Physics Department of Science School, Tibet University, Lhasa 850000, China.
  • Fang JH; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Fang K; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Feng CF; University of Chinese Academy of Sciences, Beijing 100049, China.
  • Feng Z; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Feng ZY; Department of Physics, Shandong University, Jinan 250100, China.
  • Gao Q; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Gou QB; Institute of Modern Physics, SouthWest Jiaotong University, Chengdu 610031, China.
  • Guo YQ; Physics Department of Science School, Tibet University, Lhasa 850000, China.
  • He HH; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • He ZT; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Hibino K; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Hotta N; Department of Physics, Hebei Normal University, Shijiazhuang 050016, China.
  • Hu H; Faculty of Engineering, Kanagawa University, Yokohama 221-8686, Japan.
  • Hu HB; Faculty of Education, Utsunomiya University, Utsunomiya 321-8505, Japan.
  • Huang J; Physics Department of Science School, Tibet University, Lhasa 850000, China.
  • Jia HY; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Jiang L; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Jin HB; Institute of Modern Physics, SouthWest Jiaotong University, Chengdu 610031, China.
  • Kajino F; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Kasahara K; National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China.
  • Katayose Y; Department of Physics, Konan University, Kobe 658-8501, Japan.
  • Kato C; Research Institute for Science and Engineering, Waseda University, Tokyo 169-8555, Japan.
  • Kato S; Faculty of Engineering, Yokohama National University, Yokohama 240-8501, Japan.
  • Kawata K; Department of Physics, Shinshu University, Matsumoto 390-8621, Japan.
  • Kozai M; Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan.
  • Labaciren; Institute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, Japan.
  • Le GM; Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS/JAXA), Sagamihara 252-5210, Japan.
  • Li AF; Physics Department of Science School, Tibet University, Lhasa 850000, China.
  • Li HJ; National Center for Space Weather, China Meteorological Administration, Beijing 100081, China.
  • Li WJ; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Lin YH; Department of Physics, Shandong University, Jinan 250100, China.
  • Liu B; School of Information Science and Engineering, Shandong Agriculture University, Taian 271018, China.
  • Liu C; Physics Department of Science School, Tibet University, Lhasa 850000, China.
  • Liu JS; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Liu MY; Institute of Modern Physics, SouthWest Jiaotong University, Chengdu 610031, China.
  • Lou YQ; Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
  • Lu H; University of Chinese Academy of Sciences, Beijing 100049, China.
  • Meng XR; School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China.
Phys Rev Lett ; 123(5): 051101, 2019 Aug 02.
Article em En | MEDLINE | ID: mdl-31491288
ABSTRACT
We report on the highest energy photons from the Crab Nebula observed by the Tibet air shower array with the underground water-Cherenkov-type muon detector array. Based on the criterion of a muon number measured in an air shower, we successfully suppress 99.92% of the cosmic-ray background events with energies E>100 TeV. As a result, we observed 24 photonlike events with E>100 TeV against 5.5 background events, which corresponds to a 5.6σ statistical significance. This is the first detection of photons with E>100 TeV from an astrophysical source.
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Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Tipo de estudo: Diagnostic_studies Idioma: En Ano de publicação: 2019 Tipo de documento: Article
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Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Tipo de estudo: Diagnostic_studies Idioma: En Ano de publicação: 2019 Tipo de documento: Article