| Project/Area Number |
61460016
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| Research Category |
Grant-in-Aid for General Scientific Research (B)
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| Allocation Type | Single-year Grants |
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| Research Field |
核・宇宙線・素粒子
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| Research Institution | The University of Tokyo |
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Principal Investigator |
KASAHARA Katsuaki Institute for Cosmic Ray Research, Univ. of Tokyo, assistant, 宇宙線研究所, 助手 (00013425)
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| Co-Investigator(Kenkyū-buntansha) |
TORII Shoji Faculty of Engineering, Kanagawa Univ., assistant, 工学部, 助手 (90167536)
YUDA Toshinori Institute for Cosmic Ray Research, Univ. of Tokyo, assistant Prof., 宇宙線研究所, 助教授 (60092368)
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| Project Period (FY) |
1986 – 1987
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| Project Status |
Completed (Fiscal Year 1988)
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| Budget Amount *help |
¥6,700,000 (Direct Cost: ¥6,700,000)
Fiscal Year 1987: ¥600,000 (Direct Cost: ¥600,000)
Fiscal Year 1986: ¥6,100,000 (Direct Cost: ¥6,100,000)
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| Keywords | Gamma ray astronomy / 10^<15>eV / Gamma ray point source / Fast timing / 到来角決定精度 / 宇宙線 / 空気シャワー / 到来方向決定 / FT / 【10^(15)】eV / CAMAC |
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| Research Abstract |
The array constructed in 1986 has been updated in 1987 to have the final system used for test experiment as follows: 16 fast timing detectors are placed in a 4x4 matrix with 15 m separation. Each consists of a plastic scintillater of 500x 500x35 size and a fast photomultiplier accomodated in a steinless steal box of whcih inner surface is painted white. A lead plate of 0.5 cm thick is placed on the top of the box to have better time resolution by converting high energy gamma rays into election pairs. A cammac system is used for the data taking which is controlled by a micor-computer. The data is recorded in an optical disk with a frequency of about 1 Hz. In addition to these, 8 detectors dedicated to the electron number measurement are distributed in the center and peripheral part of the array.
The two main purposes of the test experiment, i.e., 1) establishing the stability for a long time (especially for heavy weather conditions) and 2) acquiring the augular resolution better then 1゜, have been achieved successfully. The angular resolution is estimated and its dependence on the shower size, the number of detector and the timing accuracy of the detectors has been clarified. The present system give -0.7゜ for 10^<15>eV cosmic rays where means that the estimated arrival direction falls in within from the true direction for 50 % cases. Increasing the number of detectors and upgrading the quality of scintillaters will give us better resuolution than the present one; better than 1゜ for 10^<14>eV region showers better than 0.3゜ for 10^<15>eV showers.
Thus we have established the basis for a full scale experiment at Yambatin (4300m) in Tibet and expect that a reliable gamma-ray astronomy in the 10^<15>eV region can be explored.
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