The AMIGA underground muon detector of the Pierre Auger Observatory - performance and event reconstruction
The AMIGA underground muon detector of the Pierre Auger Observatory - performance and event reconstruction
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皮埃尔奥格天文台的 AMIGA 地下 μ 介子探测器 - 性能和事件重建
DOI：
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发表时间：
2019
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影响因子：
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通讯作者：
A. Botti
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作者：
A. Botti
俄歇μ子和地面阵列填充（AMIGA）的目标是将皮埃尔俄歇天文台的探测阈值降低到$sim 10^{16.5}$ eV的能量，并直接测量广泛的空气簇射的μ子含量。AMIGA由一个耦合水切伦科夫和掩埋闪烁探测器阵列组成，部署在两个重叠的三角形网格中，间距为433米和750米。每个地下探测器的总面积为30平方米，埋深为2.3米，以屏蔽簇射电磁分量。闪烁平面被分割成塑料闪烁体条，其中嵌入式波长移位光纤耦合到共同的光学传感器。在开始建造全尺寸阵列之前，工程阵列一直运行到2017年11月，以验证和优化设计，并评估检测系统的性能。在此阶段，测试了5 $mathrm{m}^2$和10 $mathrm{m}^2$的闪烁面积以及两个光学传感器，光电倍增管和硅光电倍增管。在这项工作中，我们目前的状态和性能的阵列目前配备了硅光电倍增管，沿着的定时性能和几何重建模块配备了光电倍增管。分析和结果基于实验室和现场测量。选择闪烁面积为10平方米，硅光电倍增管作为读出器作为AMIGA阵列的基线设计。
The Auger Muons and Infill for the Ground Array (AMIGA) aims to both lower the detection threshold of the Pierre Auger Observatory down to energies of $sim 10^{16.5}$ eV and to directly measure the muon content of extensive air showers. AMIGA consists of an array of coupled water-Cherenkov and buried scintillation detectors deployed in two superimposed triangular grids of 433 m and 750 m spacings. Each underground detector has a total area of 30 $mathrm{m}^2$ buried at a depth of 2.3 m, to shield it from the shower electromagnetic component. The scintillation plane is segmented in plastic-scintillator strips with embedded wavelength-shifter optical fibers coupled to a common optical sensor. Before proceeding to the construction of the full-size array, an engineering array was operated until November 2017 to validate and optimize the design, and to evaluate the performance of the detection system. During this phase, scintillation areas of 5 $mathrm{m}^2$ and 10 $mathrm{m}^2$ and two optical sensors, photomultiplier tubes and silicon photomultipliers, were tested. In this work, we present the status and performance of the array currently equipped with silicon photomultipliers, along with the timing performance and geometry reconstruction of modules equipped with photomultiplier tubes. Analyses and results are based on both laboratory and field measurements. Scintillation areas of 10 $mathrm{m}^2$ and silicon photomultipliers as readout have been selected as the baseline design for the full-scale AMIGA array.