优化法拉第背景网格
Optimizing Faraday Background Grids
摘要：
从HII区到宇宙学大尺度结构的天体中的磁场强度可以用来自极化背景射电结构的旋转测度（RM）的密集网格来估计。即将进行的对SKA及其前兆的调查将大大增加背景源的数量N。然而，对于天空固定区域上的积分时间$t$，可检测的磁场强度将仅按$t^{-0.15}$缩放，因此需要优化分析技术。一个关键因素是不同人群内在RM的分散性差异，必须仔细考虑以达到科学所需的准确性。
英文摘要：
Magnetic field strengths in objects ranging from HII regions to cosmological large scale structure can be estimated using dense grids of Rotation Measures (RMs) from polarized background radio structures. Upcoming surveys on the SKA and its precursors will dramatically increase the number N of background sources. However, detectable magnetic field strengths will scale only as $t^{-0.15}$, for an integration time $t$ on a fixed area of sky, so the analysis techniques need to be optimized. A key factor is the difference in the dispersion of intrinsic RMs for different populations, which must be carefully accounted for to achieve the scientifically needed accuracies.
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