On intracluster Faraday rotation. II - Statistical analysis
On intracluster Faraday rotation. II - Statistical analysis
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关于簇内法拉第旋转。
DOI：
10.1086/159536
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发表时间：
1982
期刊：
影响因子：
--
通讯作者：
B. Dennison
中科院分区：
文献类型：
--
作者：
J. M. Lawler;B. Dennison
通过丰富的星系团看到的射电源法拉第旋转测量的可靠样本与通过星系团外部看到的源进行比较，因此具有很小的团内法拉第旋转，表明旋转分布在前群体中被拓宽，但仅在80%的统计置信度水平上。采用一个物理模型的intracluster介质中的磁场强度/湍流细胞每气体核心半径数比的平方根等于约0.07微高斯，蒙特卡罗模拟是能够重现所观察到的增宽。磁场强度/湍流胞比的上限分析图小于0.20微高斯，结合康普顿散射通量限制所施加的磁场强度下限，表明团内磁场必须在大于约20 kpc的尺度上纠缠。
The comparison of a reliable sample of radio source Faraday rotation measurements seen through rich clusters of galaxies, with sources seen through the outer parts of clusters and therefore having little intracluster Faraday rotation, indicates that the distribution of rotation in the former population is broadened, but only at the 80% level of statistical confidence. Employing a physical model for the intracluster medium in which the square root of magnetic field strength/turbulent cell per gas core radius number ratio equals approximately 0.07 microgauss, a Monte Carlo simulation is able to reproduce the observed broadening. An upper-limit analysis figure of less than 0.20 microgauss for the field strength/turbulent cell ratio, combined with lower limits on field strength imposed by limitations on the Compton-scattered flux, shows that intracluster magnetic fields must be tangled on scales greater than about 20 kpc.