arXiv 0704.03032007-04astro-phphysics.ao-ph

俄歇天文台气溶胶相函数的测量

Measurement of the Aerosol Phase Function at the Pierre Auger Observatory

S. Y. BenZvi, B. M. Connolly, J. A. J. Matthews, M. Prouza, E. F. Visbal, S. Westerhoff

备注：: 19 pages, 10 figures (4 in color), replaced with version accepted for publication in Astroparticle Physics
发表信息：: Astropart.Phys.28:312-320,2007
DOI：: 10.1016/j.astropartphys.2007.06.005

摘要：

空气荧光探测器通过收集氮分子沿着广泛的空气簇射级联发射的荧光来测量超高能宇宙射线的能量。为了确保可靠的能量确定，光信号需要针对大气效应进行校正，大气效应不仅使信号衰减，而且由于散射的切伦科夫光和多重散射光而产生不可忽略的背景分量。校正需要定期测量气溶胶衰减长度和气溶胶相函数，定义为光在给定方向上散射的概率。在阿根廷马拉格的皮埃尔·俄歇天文台，相位函数是使用两个气溶胶相位函数（APF）光源每小时测量一次的。这些光源引导UV光束穿过荧光检测器的视场;相位函数可以从荧光检测器相机中的拍摄图像中提取。本文介绍了皮埃尔俄歇天文台有源滤波器系统的设计、现状、标准操作程序和性能。

英文摘要：

Air fluorescence detectors measure the energy of ultra-high energy cosmic rays by collecting fluorescence light emitted from nitrogen molecules along the extensive air shower cascade. To ensure a reliable energy determination, the light signal needs to be corrected for atmospheric effects, which not only attenuate the signal, but also produce a non-negligible background component due to scattered Cherenkov light and multiple-scattered light. The correction requires regular measurements of the aerosol attenuation length and the aerosol phase function, defined as the probability of light scattered in a given direction. At the Pierre Auger Observatory in Malargue, Argentina, the phase function is measured on an hourly basis using two Aerosol Phase Function (APF) light sources. These sources direct a UV light beam across the field of view of the fluorescence detectors; the phase function can be extracted from the image of the shots in the fluorescence detector cameras. This paper describes the design, current status, standard operation procedure, and performance of the APF system at the Pierre Auger Observatory.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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