Measurement of TeV electrons on ISS/JEM

Journal Article · Fri Jan 22 00:00:00 EST 1999 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.57681· OSTI ID:21202499

Torii, S; Tateyama, N; Tamura, T; Ouchi, T; Kashiwagi, K; Yoshida, K; Hibino, K ^[1]; Yamagami, T; Saito, Y ^[2]; Murakami, H ^[3]; Kobayashi, T ^[4]; Komori, Y ^[5]; Kasahara, K ^[6]; Yuda, T; Ohnishi, M ^[7]; Shibata, M ^[8]; Nishimura, J ^[9]

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

By using the JEM (Japanese Experiment Module) facility on ISS, we are planning to carry out a precise measurement of the flux and energy spectrum of cosmic-ray electrons of 10 GeV to several TeV. Since the electrons over several 100 GeV could be contributed only from the nearby sources within a distance less than 1 kpc, it is expected in the high energy region that the energy spectrum has a structural component and the distribution of the arrival directions presents anisotropy. By helping to localize and identify the nearest cosmic ray sources, these data should help to resolve the long-term puzzle. The instrument used for the observation is a kind of scintilating-fiber/lead imaging calorimeter that has been used for the balloon observations. We are developing an improved detector having a geometrical factor of 0.5 m{sup 2}sr and a higher rejection power against the background protons ({>=}10{sup 4}). It is expected to observe nearly 500 electrons over 1 TeV during the one-year observation.

• OSTI ID: 21202499
• Journal Information: AIP Conference Proceedings, Vol. 458, Issue 1; Conference: Space technology and applications international forum - 1999, Albuquerque, NM (United States), 31 Jan - 4 Feb 1999; Other Information: DOI: 10.1063/1.57681; (c) 1999 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

46 INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY
ANISOTROPY
COSMIC ELECTRONS
COSMIC RAY DETECTION
COSMIC RAY FLUX
COSMIC RAY PROPAGATION
COSMIC RAY SOURCES
DESIGN
ELECTRON DETECTION
ENERGY SPECTRA
GEV RANGE
INTERNATIONAL SPACE STATION
OPTICAL FIBERS
SHOWER COUNTERS
SOLID SCINTILLATION DETECTORS
TEV RANGE