γ射线和宇宙μ子的单探测器分析
Analysis of Gamma Rays and Cosmic Muons with a Single Detector
摘要：
我们报告劳伦斯伯克利国家实验室宇宙μ子探测器的建设和升级。我们修改了电子和机械，以实现高效的伽马射线和宇宙射线探测器。每个探测器模块使用一个一英寸厚的闪烁体，连接到一个光电倍增管（PMT），并安装在一个固体铝框架。探测器使用闪烁将通过的辐射转换成可检测的光子，这些光子被引导向PMT的光电阴极表面，触发光电子的释放，然后光电子被放大以产生可测量的电子信号。这些模块连接到电子部分，该电子部分比较来自两个PMT的信号并逻辑地确定它们是否是重合事件。增加了一个数据收集装置，以实现更快和更长的计数率。产生两种伽马射线和一种β粒子的钴-60被用作校准源。为了研究辐射的各向同性行为，将两个检测模块调节到相对于彼此的不同旋转角度，并且测量符合计数。在整个角谱范围内，以不同角度设置的模块的符合计数是一致的，只有铅屏蔽明显减少了放射源的计数。还考虑了辐射的平方反比律行为。结果是，计数的数量随着与源的距离的增加而减少。此外，将探测器定位为以不同的方向指向天空，我们测量了宇宙射线μ子通量，因为与垂直的角度减小。在这样做的过程中，我们扫描了不同的大气层。为了在检测阶段实现最佳操作，我们使两个PMT达到平稳状态，以挑选出它们的最佳操作增益电压，同时消除虚假背景噪声信号。
英文摘要：
We report on the construction and upgrade of a Lawrence Berkeley National Laboratory Cosmic Muons Detector. We modify the electronics and mechanics to achieve a highly efficient gamma-ray and cosmic-ray detector. Each detector module uses a one-inch-thick scintillator, attached to a photomultiplier tube (PMT) and mounted on a solid aluminum frame. The detector uses scintillation to transform passing radiation into detectable photons that are guided toward a photocathode surface of the PMT, triggering the release of photoelectrons that are then amplified to yield measurable electronic signals. The modules were connected to an electronics section that compared the signals from the two PMTs and logically determined if they were coincidence events. A data-collection device was added for faster and prolonged count rates. A cobalt-60, which produced two gamma rays and a beta particle has been used as a calibration source. To investigate the isotropic behavior of radiation, two detection modules were adjusted to different angles of rotation with respect to each other, and the coincidence counts were measured. The coincidence counts from the modules set at various angles were consistent throughout the angular spectrum, and only lead shielding visibly reduced the number of counts from the radioactive source. The inverse-square-law behavior of radiation has also been considered. The results were such that the number of counts decreased as a function of increasing distance from the source. Furthermore, positioning the detector to point toward the sky in different orientations, we measured cosmic ray muon flux as the angle from the vertical was decreased. In doing so, we scanned different patches of the atmosphere. For the optimum operation during the detection phase, we plateaued both PMTs to single out their best operating gain voltage while eliminating false background noise signals.
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