AMANDA 2004

这是在2004-2006年期间继续在南极站运行南极μ子和中微子阵列（AMANDA）的更新建议。AMANDA利用1.5英里深的南极冰作为切伦科夫探测器。该望远镜的有效观测面积已达4万平方公里。M用于探测宇宙中微子的点源，并且超过50,000平方英尺。M表示所有天顶角的伽马射线暴。AMANDA探测器现在已经运行了三年多，它的最终配置是677个光模块，部署在19根弦上。探测器每年收集大约4tb的数据。这些数据在南极的高空经过过滤，通过地球同步卫星系统以每天约3gb的速度传回威斯康星大学麦迪逊分校，并储存起来供进一步分析和分发给AMANDA合作项目。还存储了分析实验数据所需的仿真数据。目前，6 TB的AMANDA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正在率先将DIF元数据标准应用于天体物理学。AMANDA的科学分析可分为以下几个方面：(a)大气μ介子通量：利用宇宙射线μ介子通量对探测器进行高精度标定，具有较高的统计量；(b)大气中微子：AMANDA的性能是通过重建大气中微子产生的向上运动的μ子来校准的。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。大气中微子谱现在测量到100 TeV；(c)由电子和中微子引起的二次电磁和强子阵雨产生的级联。通量水平正在接近应该观测到的低得多的大气中微子通量，以及可以测量到的重夸克衰变的迅速通量；(d)寻找宇宙中微子的点源，如超新星残余物、小类星体、活动星系；(e)寻找宇宙中微子的漫射通量；(f)搜寻伽马射线暴；(g)来自宇宙残余物或迷你黑洞、磁单极子、冷暗物质粒子的极高能量事件。UW在所有的分析中都扮演着重要的角色，除了最后一个。特拉华大学的研究小组与特拉华大学合作，通过研究AMANDA对部署在表面的SPASE阵列探测到的空气阵雨的μ子反应，确定了宇宙射线通量中重元素的比例随着膝盖区域能量的增加而增加。UW AMANDA小组开创了许多项目，这些项目现在是广泛的冰立方教育和推广项目的一部分，包括涉及高中教师和学生的“冰中的科学”课程，以及TEA（南极洲教师体验）项目的参与者。

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.