Development of a 30 cm-cube Electron-Tracking Compton Camera for the SMILE-II Experiment
Development of a 30 cm-cube Electron-Tracking Compton Camera for the SMILE-II Experiment
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DOI：
10.1088/1748-0221/9/05/c05045
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发表时间：
2013-12
影响因子：
1.3
通讯作者：
Y. Mizumura;T. Tanimori;H. Kubo;A. Takada;J. Parker;T. Mizumoto;S. Sonoda;D. Tomono;T. Sawano;K. Nakamura;Y. Matsuoka;S. Komura;S. Nakamura;M. Oda;K. Miuchi;S. Kabuki;Yuji Kishimoto;Shunsuke Kurosawa;S. Iwaki
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文献类型：
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作者：
Y. Mizumura;T. Tanimori;H. Kubo;A. Takada;J. Parker;T. Mizumoto;S. Sonoda;D. Tomono;T. Sawano;K. Nakamura;Y. Matsuoka;S. Komura;S. Nakamura;M. Oda;K. Miuchi;S. Kabuki;Yuji Kishimoto;Shunsuke Kurosawa;S. Iwaki
为了探索亚MeV/MeV伽马射线天文窗口，我们研制了电子跟踪康普顿相机（ETCC），并在实验室条件下使用几个亚MeV能带伽马射线源进行了首次性能测试。使用一个简单的跟踪分析的性能进行快速的第一次测试，伽马射线成像能力证明了清晰的图像和5.3度的角分辨率测量（ARM）在662 keV。作为这项工作的最大影响，在亚MeV伽马射线波段实现了10−4量级的伽马射线探测效率，比我们以前的实验高出一个数量级。这种角分辨率和探测效率使我们能够在中纬度气球高度上用几个小时的观测在5σ水平上探测到蟹状星云。此外，这种性能测试和仅包括物理过程的模拟之间效率的良好一致性非常重要;这意味着我们实现了近100%的康普顿反冲电子检测，并意味着我们对未来升级导致的性能增强的预测更加现实。我们计划通过SMILE-II（Sub-MeV伽马射线成像装载在气球上的实验II）中观测天体来确认ETCC的成像能力。SMILE-II和后续的SMILE-III计划将是亚MeV/MeV γ射线天文学的重要关键。
To explore the sub-MeV/MeV gamma-ray window for astronomy, we have developed the Electron-Tracking Compton Camera (ETCC), and carried out the first performance test in laboratory conditions using several gamma-ray sources in the sub-MeV energy band. Using a simple track analysis for a quick first test of the performance, the gamma-ray imaging capability was demonstrated with clear images and 5.3 degrees of angular resolution measure (ARM) measured at 662 keV. As the greatest impact of this work, a gamma-ray detection efficiency on the order of 10−4 was achieved at the sub-MeV gamma-ray band, which is one order of magnitude higher than our previous experiment. This angular resolution and detection efficiency enables us to detect the Crab Nebula at the 5σ level with several hours observation at balloon altitude in middle latitude. Furthermore, good consistency of efficiencies between this performance test and simulation including only physical processes is very important; it means we achieve nearly 100% detection of Compton recoil electrons and means that our predictions of performance enhancement resulting from future upgrades are more realistic. We are planning to confirm the imaging capability of the ETCC by observation of celestial objects in the SMILE-II (Sub-MeV gamma ray Imaging Loaded-on-balloon Experiment II). The SMILE-II and following SMILE-III project will be an important key of sub-MeV/MeV gamma-ray astronomy.