AMANDA 2004

这是一项延长建议，将在2004-2006年期间继续在南极站运行南极μ介子和中微子阵列。阿曼达使用1.5英里深的南极冰作为切伦科夫探测器。该望远镜的有效面积已达到40，000平方米。m用于探测宇宙中微子的点源，并超过50，000平方米。m代表所有天顶角的伽马射线爆发。阿曼达探测器已经运行了三年多，其最终配置为部署19个字符串上的677个光学模块。探测器每年收集大约4 TB的数据。这些数据在南极进行高级别过滤，并通过地球静止卫星系统以每天约3千兆字节的速度传回威斯康星大学麦迪逊分校，并存储以供进一步分析和分发给阿曼达协作。还存储了分析实验数据所需的模拟数据。目前，6 TB的阿曼达数据在线保存在大型高可用性RAID阵列上。为了提高数据管理的质量，UW-AMANDA正在带头使DIF元数据标准适用于天体物理学。阿曼达中的科学分析可分为以下几类：（a）大气μ介子通量：宇宙射线μ介子通量已被用于对探测器进行高精度的统计校准;（B）大气中微子：阿曼达的性能已通过重建大气μ介子中微子产生的上行μ介子进行校准。该探测器在稳定运行中，每天使用快速在线分析软件收集大约4个中微子。大气中的中微子光谱现在测量到高达100 TeV;（c）由电子和τ中微子引发的次级电磁和强子簇射产生的级联。通量水平正在接近可以观测到低得多的大气中微子通量以及可以测量重夸克衰变产生的瞬发通量的水平;（d）寻找宇宙中微子的点源，如超新星遗迹、小型类星体、活动星系;（e）寻找宇宙中微子的扩散通量;（f）寻找伽马射线爆发;（f）寻找宇宙中微子的扩散通量。（g）来自宇宙学遗迹或微型黑洞、磁单极子、冷暗物质粒子的极高能量事件。UW在所有分析中起着重要作用，除了最后一个。与特拉华州大学合作，华盛顿大学的研究小组通过研究阿曼达对地面部署的SPASE阵列探测到的空气簇射的μ子响应，确定了宇宙射线通量中重元素的比例随着膝关节区域能量的增加而增加。UW阿曼达集团开创了许多项目，这些项目现在是广泛的IceCube教育和推广计划的一部分，包括涉及高中教师和学生的冰中科学课程，以及TEA（南极洲教师体验）计划的参与者。

This is a renewal proposal to continue operating the Antarctic Muon and Neutrino Array (AMANDA) at the South Pole Station through 2004-2006. The AMANDA uses natural 1.5-mile deep Antarctic ice as a Cerenkov detector. The telescope's effective area has reached 40,000 sq. m for the detection of point sources of cosmic neutrinos and exceeds 50,000 sq. m for gamma ray bursts at all zenith angles. The AMANDA detector has now operated for more than three years in its final configuration of 677 optical modules on deployed 19 strings. The detector collects approximately 4 terabytes of data yearly. These data are filtered at a high level at the South Pole and transmitted back to UW-Madison at a rate of about 3 gigabytes per day via the geostationary satellite systems and stored for further analysis and distribution to the AMANDA collaboration. Also stored are simulation data needed to analyze the experimental data. Presently 6 TB of AMANDA data is held online on large high availability RAID arrays. To enhance the quality of data management UW-AMANDA is taking the lead in adapting the DIF metadata standard to astrophysics. The scientific analyses in AMANDA can be classified as follows: (a) Atmospheric muon flux: the cosmic ray muon flux has been used to do a precision calibration of the detector with high statistics; (b) Atmospheric neutrinos: AMANDA's performance has been calibrated by reconstructing upward-going muons produced by atmospheric muon neutrinos. The detector, in steady operation, collects roughly four neutrinos per day using fast on-line analysis software. The atmospheric neutrino spectrum is now measured up to 100 TeV; (c) Cascades produced by the secondary electromagnetic and hadronic showers initiated by electron and tau neutrinos. The flux level is approaching where the much lower atmospheric neutrino fluxes should be observed, as well as the prompt flux from the decay of heavy quarks can be measured; (d) Search for point sources of cosmic neutrinos such as supernova remnants, mini-quasars, active galaxies; (e) Search for a diffuse flux of cosmic neutrinos; (f) Search for gamma ray bursts; and (g) Extremely high energy events from cosmological remnants or mini-black holes, magnetic monopoles, cold dark matter particles. The UW plays a major role in all analyses except for the last one. With the University of Delaware, the UW group determined that the fraction of heavy elements in the cosmic ray flux increases with energy in the region of the knee, by studying the muon response of AMANDA to air showers detected by the SPASE array deployed at the surface. The UW AMANDA group has pioneered many of the programs that are now part of the extensive IceCube education and outreach program including the Science in the Ice course that involves high school teachers and their students, as well as participants in the TEA (Teacher Experience in Antarctica) program.