The Calorimetric Electron Telescope (CALET) for the JEM Exposure Facility

作     者：S. Torii N. Tateyama T. Tamura T. Ouchi K. Kashiwagi K. Yoshida K. Hibino T. Yamagami Y. Saito H. Murakami T. Kobayashi Y. Komori K. Kasahara T. Yuda M. Ohnishi M. Shibata F. Makino J. Nishimura 

作者机构：1Institute of Physics Department of Industrial Engineering and Management Institute of Computer Science Kanagawa University Yokohama Kanagawa 221-8686 Japan 2Institute of Space and Astronautical Science Sagamihara Kanagawa 229-8510 Japan 3Department of Physics Rikkyo University Tokyo 171-8501 Japan 4Department of Physics Aoyama-gakuin University Tokyo 157-8672 Japan 5Kanagawa Prefectural College of Nursing Yokohama Kanagawa 241 Japan 6Department of System Engineering Shibaura Institute of Technology Omiya Saitama 330-8570 Japan 7Institute for Cosmic Ray Research University of Tokyo Tanashi Tokyo 188-8502 Japan 8Department of Physics Yokahama National University Yokohama Kanagawa 240-0067 Japan 9National Space Development Agency of Japan Tsukuba Ibaraki 305-8505 Japan 10Yamagata Institute of Technology Yamagata 993 Japan 

出 版 物：《AIP Conference Proceedings》 

年 卷 期：2000年第504卷第1期

页      面：187-192页

学科分类：07[理学] 0702[理学-物理学] 

摘      要：The CALET instrument is proposed for the Japanese Experiment Module/Exposure Facility (JEM/EF) on International Space Station (ISS) to resolve the long-term puzzles in high-energy cosmic-ray physics. The ISS gives us a unique opportunity to carry out the measurements of cosmic ray electrons with a relatively heavy and large detector, and for the long exposure. The instrument will be composed of an imaging calorimeter with scintillating fibers and a total absorption calorimeter for detecting the electrons up to 10,000 GeV. The origin of high-energy electrons and the diffusion characteristics in the Galaxy will be revealed by measuring the energy spectrum of electrons and the anisotropy of arrival directions. By the excellent capability of the CALET, both of the gamma-rays over GeV and nucleus component up to 1015 eV might be investigated as additional possibilities of the observation.