High energy electron observation by polar patrol balloon flight in Antarctica

Shoji Torii; Tadahisa Tamura; Kenji Yoshida; Hisashi Kitamura; Takamasa Yamagami; Hiroyuki Murakami; Nobuhito Tateyama; Jun Nishimura; Yoshitaka Saito; Shigeo Ohta; Michiyoshi Namiki; Yukihiko Matsuzaka; Issei Iijima; Masaki Ejiri; Hisao Yamagishi; Akira Kadokura; Makio Shibata; Yusaku Katayose; Katsuaki Kasahara; Kohei Mizutani; Tadashi Kobayashi; Yoshiko Komori; Toshinori Yuda; Jin Chang

High energy electron observation by polar patrol balloon flight in Antarctica

Shoji Torii^*, Tadahisa Tamura, Kenji Yoshida, Hisashi Kitamura, Takamasa Yamagami, Hiroyuki Murakami, Nobuhito Tateyama, Jun Nishimura, Yoshitaka Saito, Shigeo Ohta, Michiyoshi Namiki, Yukihiko Matsuzaka, Issei Iijima, Masaki Ejiri, Hisao Yamagishi, Akira Kadokura, Makio Shibata, Yusaku Katayose, Katsuaki Kasahara, Kohei MizutaniTadashi Kobayashi, Yoshiko Komori, Toshinori Yuda, Jin Chang

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

11 Citations (Scopus)

Abstract

We accomplished a balloon observation of the high-energy cosmic-ray electrons in 10-1000 GeV to reveal the origin and the acceleration mechanism. The observation was carried out for 13 days at an average altitude of 35km by the Polar Patrol Balloon (PPB) around Antarctica in January 2004. The detector is an imaging calorimeter composed of scintillating-fiber belts and plastic scintillation counters sandwiched between lead plates. The geometrical factor is about 600 cm ²sr, and the total thickness of lead absorber is 9 radiation lengths. The performance of the detector has been confirmed by a test flight at the Sanriku Balloon Center and by an accelerator beam test using the CERN-SPS (Super Proton Synchrotron at CERN). The new telemetry system using the Iridium satellite, the power system supplied by solar panels and the automatic flight level control operated successfully during the flight. We collected 5.7 × 10 ³ events over 100 GeV, and selected the electron candidates by a preliminary data analysis of the shower images. We report here an outline of both detector and observation, and the first result of the electron energy spectrum over 100 GeV obtained by an electronic counter.

Original language	English
Pages (from-to)	52-62
Number of pages	11
Journal	Advances in Polar Upper Atmosphere Research
Issue number	20
Publication status	Published - 2006 Aug

Keywords

Antarctica
Balloon observation
Cosmic ray
High energy electron

ASJC Scopus subject areas

Atmospheric Science
Earth-Surface Processes

Cite this

Torii, S., Tamura, T., Yoshida, K., Kitamura, H., Yamagami, T., Murakami, H., Tateyama, N., Nishimura, J., Saito, Y., Ohta, S., Namiki, M., Matsuzaka, Y., Iijima, I., Ejiri, M., Yamagishi, H., Kadokura, A., Shibata, M., Katayose, Y., Kasahara, K., ... Chang, J. (2006). High energy electron observation by polar patrol balloon flight in Antarctica. Advances in Polar Upper Atmosphere Research, (20), 52-62.

Torii, S, Tamura, T, Yoshida, K, Kitamura, H, Yamagami, T, Murakami, H, Tateyama, N, Nishimura, J, Saito, Y, Ohta, S, Namiki, M, Matsuzaka, Y, Iijima, I, Ejiri, M, Yamagishi, H, Kadokura, A, Shibata, M, Katayose, Y, Kasahara, K, Mizutani, K, Kobayashi, T, Komori, Y, Yuda, T & Chang, J 2006, 'High energy electron observation by polar patrol balloon flight in Antarctica', Advances in Polar Upper Atmosphere Research, no. 20, pp. 52-62.

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abstract = "We accomplished a balloon observation of the high-energy cosmic-ray electrons in 10-1000 GeV to reveal the origin and the acceleration mechanism. The observation was carried out for 13 days at an average altitude of 35km by the Polar Patrol Balloon (PPB) around Antarctica in January 2004. The detector is an imaging calorimeter composed of scintillating-fiber belts and plastic scintillation counters sandwiched between lead plates. The geometrical factor is about 600 cm 2sr, and the total thickness of lead absorber is 9 radiation lengths. The performance of the detector has been confirmed by a test flight at the Sanriku Balloon Center and by an accelerator beam test using the CERN-SPS (Super Proton Synchrotron at CERN). The new telemetry system using the Iridium satellite, the power system supplied by solar panels and the automatic flight level control operated successfully during the flight. We collected 5.7 × 10 3 events over 100 GeV, and selected the electron candidates by a preliminary data analysis of the shower images. We report here an outline of both detector and observation, and the first result of the electron energy spectrum over 100 GeV obtained by an electronic counter.",

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AU - Torii, Shoji

AU - Tamura, Tadahisa

AU - Yoshida, Kenji

AU - Kitamura, Hisashi

AU - Yamagami, Takamasa

AU - Murakami, Hiroyuki

AU - Tateyama, Nobuhito

AU - Nishimura, Jun

AU - Saito, Yoshitaka

AU - Ohta, Shigeo

AU - Namiki, Michiyoshi

AU - Matsuzaka, Yukihiko

AU - Iijima, Issei

AU - Ejiri, Masaki

AU - Yamagishi, Hisao

AU - Kadokura, Akira

AU - Shibata, Makio

AU - Katayose, Yusaku

AU - Kasahara, Katsuaki

AU - Mizutani, Kohei

AU - Kobayashi, Tadashi

AU - Komori, Yoshiko

AU - Yuda, Toshinori

AU - Chang, Jin

PY - 2006/8

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N2 - We accomplished a balloon observation of the high-energy cosmic-ray electrons in 10-1000 GeV to reveal the origin and the acceleration mechanism. The observation was carried out for 13 days at an average altitude of 35km by the Polar Patrol Balloon (PPB) around Antarctica in January 2004. The detector is an imaging calorimeter composed of scintillating-fiber belts and plastic scintillation counters sandwiched between lead plates. The geometrical factor is about 600 cm 2sr, and the total thickness of lead absorber is 9 radiation lengths. The performance of the detector has been confirmed by a test flight at the Sanriku Balloon Center and by an accelerator beam test using the CERN-SPS (Super Proton Synchrotron at CERN). The new telemetry system using the Iridium satellite, the power system supplied by solar panels and the automatic flight level control operated successfully during the flight. We collected 5.7 × 10 3 events over 100 GeV, and selected the electron candidates by a preliminary data analysis of the shower images. We report here an outline of both detector and observation, and the first result of the electron energy spectrum over 100 GeV obtained by an electronic counter.

AB - We accomplished a balloon observation of the high-energy cosmic-ray electrons in 10-1000 GeV to reveal the origin and the acceleration mechanism. The observation was carried out for 13 days at an average altitude of 35km by the Polar Patrol Balloon (PPB) around Antarctica in January 2004. The detector is an imaging calorimeter composed of scintillating-fiber belts and plastic scintillation counters sandwiched between lead plates. The geometrical factor is about 600 cm 2sr, and the total thickness of lead absorber is 9 radiation lengths. The performance of the detector has been confirmed by a test flight at the Sanriku Balloon Center and by an accelerator beam test using the CERN-SPS (Super Proton Synchrotron at CERN). The new telemetry system using the Iridium satellite, the power system supplied by solar panels and the automatic flight level control operated successfully during the flight. We collected 5.7 × 10 3 events over 100 GeV, and selected the electron candidates by a preliminary data analysis of the shower images. We report here an outline of both detector and observation, and the first result of the electron energy spectrum over 100 GeV obtained by an electronic counter.

KW - Antarctica

KW - Balloon observation

KW - Cosmic ray

KW - High energy electron

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High energy electron observation by polar patrol balloon flight in Antarctica

Abstract

Keywords

ASJC Scopus subject areas

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