标题： 用AMANDA寻找高能中微子的点源 显示英文标题

标题： Search for Point Sources of High Energy Neutrinos with AMANDA

摘要： 本文描述了利用位于南极冰层深处的 AMANDA-B10 探测器（一个包含 302 个光电倍增管的阵列，用于探测由向上行进的中微子诱导μ子产生的切伦科夫光）搜寻高能中微子天文源的工作。 通过使用 AMANDA 探测器与两个独立的地表望远镜（GASP 空气切伦科夫望远镜和 SPASE 广延大气簇射阵列）之间的共向事件，研究了绝对指向精度和角分辨率。 利用 1997 年 4 月至 10 月期间收集的数据（有效运行时间为 130.1 天），对北半球的一般巡天未发现任何方向有统计显著的事件过量。 μ 子中微子的灵敏度基于贯穿μ子的有效探测面积。 在北天平均后，对于 E_{μ} ≈ 10 TeV 的能量，有效探测面积超过 10,000 平方米。 通过宇宙线与大气相互作用生成的大气中微子被用来验证探测器的预测性能。 对于具有 E_{ν}^{-2}能谱指数和赤纬大于 +40° 的源，我们得到 E^2(dN_{ν}/dE) <= 10^{-6}GeVcm^{-2}s^{-1}（对于 10 GeV 的能量阈值）。 显示英文摘要

摘要： This paper describes the search for astronomical sources of high-energy neutrinos using the AMANDA-B10 detector, an array of 302 photomultiplier tubes, used for the detection of Cherenkov light from upward traveling neutrino-induced muons, buried deep in ice at the South Pole. The absolute pointing accuracy and angular resolution were studied by using coincident events between the AMANDA detector and two independent telescopes on the surface, the GASP air Cherenkov telescope and the SPASE extensive air shower array. Using data collected from April to October of 1997 (130.1 days of livetime), a general survey of the northern hemisphere revealed no statistically significant excess of events from any direction. The sensitivity for a flux of muon neutrinos is based on the effective detection area for through-going muons. Averaged over the Northern sky, the effective detection area exceeds 10,000 m^2 for E_{mu} ~ 10 TeV. Neutrinos generated in the atmosphere by cosmic ray interactions were used to verify the predicted performance of the detector. For a source with a differential energy spectrum proportional to E_{nu}^{-2} and declination larger than +40 degrees, we obtain E^2(dN_{nu}/dE) <= 10^{-6}GeVcm^{-2}s^{-1} for an energy threshold of 10 GeV.