Development of an atmospheric Cherenkov imaging camera for the CANGAROO-III experiment

被引：31
|
作者：
Kabuki, S
Tsuchiya, K
Okumura, K
Enomoto, R
Uchida, T
Tsunoo, H
Hayashi, S
Hayashi, S
Kajino, F
Maeshiro, A
Tada, I
Itoh, C
Asahara, A
Bicknell, GV
Clay, RW
Edwards, PG
Gunji, S
Hara, S
Hara, T
Hattori, T
Katagiri, H
Kawachi, A
Kifune, T
Kubo, H
Kushida, J
Matsubara, Y
Mizumoto, Y
Mori, M
Moro, H
Muraishi, H
Muraki, Y
Naito, T
Nakase, T
Nishida, D
Nishijima, K
Ohishi, M
Patterson, JR
Protheroe, RJ
Sakurazawa, K
Swaby, DL
Tanimori, T
Tokanai, F
Watanabe, A
Watanabe, S
Yanagita, S
Yoshida, T
Yoshikoshi, T
机构：
[1] Univ Tokyo, Inst Cosm Ray Res, Chiba 2778582, Japan
[2] Konan Univ, Dept Phys, Hyogo 6588501, Japan
[3] Ibaraki Univ, Fac Sci, Ibaraki 3108512, Japan
[4] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan
[5] Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Weston, ACT 2611, Australia
[6] Univ Adelaide, Dept Phys & Math Phys, Adelaide, SA 5005, Australia
[7] Inst Space & Astronaut Sci, Kanagawa 2298510, Japan
[8] Yamagata Univ, Dept Phys, Yamagata 9908560, Japan
[9] Tokyo Inst Technol, Dept Phys, Tokyo 1528551, Japan
[10] Yamanashi Gakuin Univ, Fac Management Informat, Yamanashi 4008575, Japan
[11] Tokai Univ, Dept Phys, Kanagawa 2591292, Japan
[12] Shinshu Univ, Fac Engn, Nagano 3808553, Japan
[13] Nagoya Univ, STE Lab, Aichi 4648601, Japan
[14] Natl Astron Observ Japan, Tokyo 1818588, Japan
[15] Ibaraki Prefectural Univ Hlth Sci, Dept Radiol Sci, Ibaraki 3000394, Japan
[16] Osaka City Univ, Dept Phys, Osaka 5588585, Japan
来源：
NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT | 2003年 / 500卷 / 1-3期
关键词：
gamma-ray telescopes; imaging atmospheric Cherenkov technique; photomultiplier; camera; cosmic ray;
D O I：
10.1016/S0168-9002(03)00331-0
中图分类号：
TH7 [仪器、仪表];
学科分类号：
0804 ; 080401 ; 081102 ;
摘要：
A Cherenkov imaging camera for the CANGAROO-III experiment has been developed for observations of gamma-ray-induced air showers at energies from 10(11) to 10(14) eV. The camera consists of 427 pixels, arranged in a hexagonal shape at 0.17degrees intervals, each of which is a 3/4in. diameter photomultiplier module with a Winston-cone-shaped light guide. The camera was designed to have a large dynamic range of signal linearity, a wider field of view, and an improvement in photon-collection efficiency compared with the CANGAROO-II camera. The camera, and a number of the calibration experiments made to test its performance, are described in detail in this paper. (C) 2003 Elsevier Science B.V. All rights reserved.
引用
收藏
页码：318 / 336
页数：19
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