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Design and operation of the Wide-angle Air Cherenkov Telescope array.

机译：广角切伦科夫空中望远镜阵列的设计和操作。

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摘要

Much has been learned about cosmic rays since their discovery near the beginning of the twentieth century. One of the mysteries that still remains is the nature of their source. While theories exist, the ability to observe in the energy range necessary to test the models has been unreachable by cosmic ray instruments until the last few years. Balloon and space based instruments have not been able to measure high enough energies and ground based instruments have not been able to measure low enough energies. In the last few years this gap has narrowed until the energy ranges covered by the balloon and space instruments and the ground instruments just touch. However, no instrument as of yet has been able to bridge the gap and cross over into the other energy range.; In this dissertation I will present the design and first observations of the Wide-angle Air Cherenkov Telescope (WACT) array. The WACT array is a ground based cosmic ray detector capable of measuring cosmic ray particles with energies down to a few TeV well below the upper limit of modern space and balloon based instruments. It consists of six 2 meter telescopes arranged around the Milagro Gamma Ray Observatory in Fenton Hill, NM at an altitude of 2666 meters above sea level. The instrument design, characteristics and response are presented. Additionally, I present the method used to reconstruct the energy and species of the primary cosmic ray particle.; Finally, I will present the data from the first observations made with the WACT array. With these first observations we measured the primary cosmic ray proton flux and present our cosmic ray spectrum along with a comparison other published results. The primary cosmic ray spectrum measured with the initial WACT array data is dNdE H=&parl0;1.27+0.93-0.54&parr0;× 10-1E-2.80±0.11m-2sr -1s-1TeV-1 .
机译：自从二十世纪初发现宇宙射线以来，人们已经学到了很多东西。其来源的本质仍然是一个谜。尽管存在理论，但宇宙射线仪器直到近几年才具备在测试模型所需的能量范围内进行观察的能力。气球和太空仪器无法测量足够高的能量，而地面仪器无法测量足够低的能量。在最近几年中，这种差距一直在缩小，直到气球，太空仪器和地面仪器所覆盖的能量范围完全接触为止。但是，到目前为止，还没有一种仪器能够弥合差距并跨越其他能量范围。在本文中，我将介绍广角空气切伦科夫望远镜（WACT）阵列的设计和初步观察。 WACT阵列是一种基于地面的宇宙射线探测器，能够以低至几个TeV的能量测量远低于现代太空和基于气球的仪器的上限的宇宙射线粒子。它由六只2米长的望远镜组成，它们绕着新墨西哥州芬顿山（Menton Hill）的米拉格罗伽玛射线天文台（Milagro Gamma Ray Observatory）海拔2666米。介绍了仪器的设计，特性和响应。另外，我介绍了用于重建主要宇宙射线粒子的能量和种类的方法。最后，我将展示来自WACT阵列的最初观察的数据。通过这些最初的观察，我们测量了主要的宇宙射线质子通量，并给出了我们的宇宙射线光谱以及其他已发表结果的比较。使用初始WACT阵列数据测量的主要宇宙射线光谱为 dN dE H =＆parl0; 1.27 +0.93 -0.54 ＆parr0;×10 - 1 E -2.80±0.11 m -2 sr -1 s -1 TeV -1 。

著录项

  • 作者

    Stephens, Thomas Edward, Jr.;

  • 作者单位

    New Mexico State University.;

  • 授予单位 New Mexico State University.;
  • 学科 Physics Astronomy and Astrophysics.; Engineering Electronics and Electrical.
  • 学位 Ph.D.
  • 年度 2003
  • 页码 158 p.
  • 总页数 158
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类 天文学;无线电电子学、电信技术;
  • 关键词

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