VERITAS Phase I: A Cherenkov Telescope Array For Gamma-Ray Astrophysics

VERITAS 第一阶段：用于伽马射线天体物理学的切伦科夫望远镜阵列

• 批准号: 0234268
• 负责人: Wystan Benbow
• 金额: $ 664.31万
• 依托单位: Smithsonian Institution Astrophysical Observatory
• 依托单位国家: 美国
• 项目类别: Cooperative Agreement
• 财政年份: 2003
• 资助国家: 美国
• 起止时间: 2003-10-01 至 2011-09-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0234268&HistoricalAwards=false
• 关键词: VERITAS; Phase; Cherenkov; Telescope; Array

AST 0234268WeekesThe Smithsonian Astrophysical Observatory will manage the construction of the Very Energetic Radiation Imaging Telescope Array System (VERITAS), an array of four 12m aperture telescopes for gamma-ray astronomy in the 50 GeV to 50 TeV energy range. These atmospheric Cherenkovtelescopes will use the imaging concept developed by the Whipple Observatory Gamma-Ray Collaboration and used to detect the first galactic and extragalactic sources of TeV gamma-rays. VERITAS will achieve an order of magnitude better flux sensitivity than existing telescopes. It will be the only gamma-ray telescope array in the northern hemisphere and will complement the HESS and CANGAROO observatories in the southern hemisphere.Each VERITAS telescope will have an effective mirror area of 100 sq m (equivalent to a telescope of aperture ~12m) and a long focal length (12 m) with the optical design optimized for good angular resolution, a large field of view, and minimum wavefront distortion. Each telescope camera will have 499 pixels covering a 3.5 degree field of view with 0.15 degree resolution. VERITAS will have appreciable sensitivity at 80 GeV (where it will overlap with the next generation space telescopes) and at 10 TeV (where it will overlap with particle air shower detectors). With stereoscopic imaging, the array will achieve unprecedented angular resolution, energy resolution and background rejection over three decades of energy. The minimum detectable flux sensitivity will be 1% of the Crab Nebula at 200 GeV, a factor of 20 improvement over the most sensitive telescopes currently operating in this energy range. The primary scientific objectives of VERITAS will be the study of active galactic nuclei, supernova remnants, pulsars, the galactic plane, and gamma-ray bursts; in addition a sky survey will be made to search for new astrophysical sources. VERITAS will also explore new physics in areas such as neutralino annihilation, quantum gravity and primordial black hole evaporation. VERITAS will effectively complement GLAST, the next major high energy gamma-ray telescope in space; they will overlap in the 50 GeV to 300 GeV energy range allowing important cross correlations. Together, VERITAS and GLAST may solve the problem of the origin of the cosmic radiation as well as probing fundamental questions in physics and cosmology. The VERITAS Collaboration consists of groups from ten institutions: Iowa State University, McGill University, National University of Ireland, Purdue University, Smithsonian Astrophysical Observatory, University of California at Los Angeles, University of Chicago, University of Leeds, University of Utah, and Washington University. The array will be built at a dark site on Kitt Peak in southern Arizona. VERITAS is a unique scientific endeavor which offers unusual opportunities for education and outreach. Because the project falls in the interface between high energy physics and astronomy, between particle astrophysics and high energy astrophysics, it is inherently multi-disciplinary. The VERITAS Outreach program will capitalize on the experience of the Smithsonian Astrophysical Observatory, as well as that of the university groups involved in VERITAS. The project is funded by the Department of Energy and the National Science Foundation, in approximately equal shares. Within NSF, the funding partners are Division of Astronomical Sciences, Division of Physics, and Office of Multidisciplinary Activities in the Directorate for Mathematical and Physical Sciences. ***

AST 0234268 Weeks史密森天体物理天文台将管理甚高能辐射成像望远镜阵列系统（VERITAS）的建设，这是一个由四个12米口径望远镜组成的阵列，用于50 GeV至50 TeV能量范围内的伽马射线天文学。这些大气切伦科夫望远镜将使用维普莱伽马射线合作天文台开发的成像概念，用于探测TeV伽马射线的第一个银河系和河外源。VERITAS的通量灵敏度将比现有望远镜高一个数量级。它将是北方唯一的伽马射线望远镜阵列，并将补充南半球的HESS和CANGAROO天文台，每个VERITAS望远镜的有效镜面面积为100平方米（相当于口径~ 12米的望远镜）和长焦距（12米），光学设计优化，具有良好的角分辨率，大视场，和最小的波前失真。 每个望远镜相机将有499个像素，覆盖3.5度的视场，分辨率为0.15度。 VERITAS将在80 GeV（与下一代空间望远镜重叠）和10 TeV（与粒子空气簇射探测器重叠）处具有可观的灵敏度。通过立体成像，该阵列将在三十年的能量中实现前所未有的角度分辨率，能量分辨率和背景抑制。在200 GeV时，最小可探测通量灵敏度将是蟹状星云的1%，比目前在这个能量范围内运行的最灵敏的望远镜提高了20倍。 VERITAS的主要科学目标将是研究活动星系核、超新星遗迹、超新星、银道面和伽马射线爆发;此外，还将进行巡天以寻找新的天体物理来源。VERITAS还将在中性伴子湮灭、量子引力和原始黑洞蒸发等领域探索新的物理学。 VERITAS将有效地补充GLAST，这是太空中下一个主要的高能伽马射线望远镜;它们将在50 GeV至300 GeV的能量范围内重叠，从而允许重要的互相关。VERITAS和GLAST一起可以解决宇宙辐射的起源问题，并探索物理学和宇宙学中的基本问题。VERITAS协作组由来自十个机构的小组组成：爱荷华州州立大学、麦吉尔大学、爱尔兰国立大学、普渡大学、史密森天体物理观测站、洛杉矶的加州大学、芝加哥大学、利兹大学、犹他州大学和华盛顿大学。 该阵列将建在亚利桑那州南部基特峰的一个黑暗地点。 VERITAS是一项独特的科学奋进，为教育和推广提供了不同寻常的机会。由于该项目福尔斯处于高能物理与天文学、粒子天体物理与高能天体物理之间的交界处，因此它本质上是多学科的。VERITAS外联方案将利用史密森天体物理观测站以及参与VERITAS的大学团体的经验。该项目由能源部和国家科学基金会资助，大约各占一半。 在NSF内部，资助伙伴是天文科学部，物理部和数学和物理科学理事会多学科活动办公室。 ***