Observation of high-energy atmospheric neutrinos with the Antarctic Muon and Neutrino Detector Array
Observation of high-energy atmospheric neutrinos with the Antarctic Muon and Neutrino Detector Array
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DOI：
10.1103/physrevd.66.012005
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发表时间：
2002-05
影响因子：
5
通讯作者：
A. C. Ahrens;E. al.
中科院分区：
文献类型：
--
作者：
A. C. Ahrens;E. al.
南极μ子和中微子探测器阵列（阿曼达）于1997年开始收集十串数据。结果从第一年的操作。从北方半球穿过地球的中微子被向上移动通过阵列的次级μ子识别。大气中的宇宙射线产生了向下运动的μ子的背景，其丰度比向上运动的μ子高出约106倍。在130多天的暴露中，我们总共观察到大约300个中微子事件。在同一时期，记录了1.05 × 109宇宙射线μ子事件的背景。观测到的中微子通量与大气中微子的预测是一致的。Monte Carlo模拟表明，这些事件的90%位于能量范围66 GeV至3.4 TeV。对大气中微子的观测与预期一致，使AMANDA-B10成为一台工作中的中微子望远镜。
The Antarctic muon and neutrino detector array (AMANDA) began collecting data with ten strings in 1997. Results from the first year of operation are presented. Neutrinos coming through the Earth from the Northern Hemisphere are identified by secondary muons moving upward through the array. Cosmic rays in the atmosphere generate a background of downward moving muons, which are about 106 times more abundant than the upward moving muons. Over 130 days of exposure, we observed a total of about 300 neutrino events. In the same period, a background of 1.05 × 109 cosmic ray muon events was recorded. The observed neutrino flux is consistent with atmospheric neutrino predictions. Monte Carlo simulations indicate that 90% of these events lie in the energy range 66 GeV to 3.4 TeV. The observation of atmospheric neutrinos consistent with expectations establishes AMANDA-B10 as a working neutrino telescope.