2002 Fiscal Year Final Research Report Summary
Dark Matter Search Experiment with Double Phase Xenon Detector at Kamioka Underground Laboratory
| Project/Area Number |
13304021
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| Research Category |
Grant-in-Aid for Scientific Research (A)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
素粒子・核・宇宙線
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| Research Institution | Waseda University |
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Principal Investigator |
SUZUKI Satoshi Waseda University, Advanced Research Institute for Science and Engineering, Associate Professor, 理工学総合研究センター, 助教授 (30318828)
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| Co-Investigator(Kenkyū-buntansha) |
TAKIZAWA Kyoko Waseda University, Adv.Res.Inst.Sci. & Eng., Lecture, 理工学総合研究センター, 助手 (80339746)
TERASAWA Kazuhiro Waseda University, Adv.Res.Inst.Sci. & Eng., Lecture, 理工学総合研究センター, 講師 (10329138)
OKADA Hiroyuki Waseda University, Adv.Res.Inst.Sci. & Eng., Lecture, 理工学総合研究センター, 講師 (20308258)
OOTANI Wataru University of Tokyo, ICEPP, Assistant, 素粒子物理国際センター, 助手 (30311335)
MORIYAMA Sigetaka University of Tokyo, ICRR, Assistant, 宇宙線研究所, 助手 (50313044)
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| Project Period (FY) |
2001 – 2002
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| Keywords | Dark Matter / Liquid Xenon / Proportional Scintillation / WIMPs / Double Phase Detector / Kamioka mine |
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| Research Abstract |
We built the detector with 0.3-liter fiducial volume and measured its basic performance. We succeeded to utilize a PTFE reflector for liquid Xenon scintillation light and have been able to distinguish nuclear recoil from electron recoil using the direct scintillation and the proportional scintillation. From 2001, we started an underground experiment using a prototype detector in Kamioka mine. The background study, the radioactivity of all the materials used for this detector, was carried out using high purity Ge detector in the mine. Low background PMTs were developed by our group. The result of the prototype detector was 1 order of magnitude worse than the current limit in the WIMP-nucleon cross section. However, the origin of the radioactive source has been identified and the background level is understood quantitatively. The expected results with a 15 kg detector in the next phase will be three orders of magnitude better than the current limit.
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[Publications] M.Yamashita, T.Doke, K.Kawasaki, J.Kikuchi, S.Suzuki, S.Fukuda, Y.Fukuda, T.Itow, Y.Koshio, M.Miura, S.Moriyama, M.Nakahata, T.Namba, M.Shiozawa, Y.Suzuki, Y.Takeuchi, M.Ishitsuka, T.Kajita, K.Kaneyuki, A.Okada, Y.Iimori, T.Tsukamoto, R.Ohsumi, K.Ito, K.Miyano, T.Hashimoto, K.Nishijima, S.Tasaka, K.Ishino, Y.Watanabe, I.Kang, S.Kim, O.Ponkratenko, Y.Zdesenko, M.Smy, K.Sobel, M.Vagins: "XMASS Experiment II"Technique and Application of Xenon Detectors, World Scientific. (Proceeding). 136-141 (2002)
Description
「研究成果報告書概要(欧文)」より
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[Publications] K.Kawasaki, M.Yamashita, S.Suzuki, J.Kikuchi, T.Doke, Y.Fukuda, T.Itow, Y.Koshio, M.Miura, S.Moriyama, E.Nakahata, M.Shiozawa, Y.Suzuki, Y.Takeuchi, T.Kajita, K.Kaneyuki, A.Okada: "XMASS (Xenon) II"Low Energy Solar Neutrino Detection, World Scientific. (Proceeding). 91-97 (2001)
Description
「研究成果報告書概要(欧文)」より
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