银河系ISM λ~ 0.86 m的WSRT法拉第层析成像
WSRT Faraday tomography of the Galactic ISM at λ~ 0.86 m
摘要：
我们调查的银河系ISM的属性，通过应用法拉第层析成像的射电偏振数据集的银河系反中心的方向。我们解决了数据中缺少大尺度结构的问题，并表明这对我们提出的结果并不起重要作用。在我们的数据集中，法拉第深度谱的主峰在8%的视线范围内无法测量。一个未分辨的峰表示法拉第旋转和同步辐射区域之间的分离。然而，宇宙射线遍布ISM，因此在法拉第旋转的地方也会产生同步辐射。我们认为，磁场的方向可以分开这两种效果。通过模拟热电子对法拉第深度的贡献，我们绘制了沿视线的磁场分量的强度。在我们的数据集中的偏振点源的旋转措施，是在我们的数据中的漫射发射的法拉第深度相媲美。我们的法拉第深度图显示了低极化强度的狭窄通道。我们的结论是，望远镜光束的去偏振至少会产生一些这样的运河。最后，我们调查的一个显着的区域在这个数据集中的属性，并认为它是由减少视线去极化相比，其周围环境。
英文摘要：
We investigate the properties of the Galactic ISM by applying Faraday tomography to a radio polarization data set in the direction of the Galactic anti-centre. We address the problem of missing large-scale structure in our data, and show that this does not play an important role for the results we present. The main peak of the Faraday depth spectra in our data set is not measurably resolved for about 8% of the lines of sight. An unresolved peak indicates a separation between the regions with Faraday rotation and synchrotron emission. However, cosmic rays pervade the ISM, and synchrotron emission would therefore also be produced where there is Faraday rotation. We suggest that the orientation of the magnetic field can separate the two effects. By modelling the thermal electron contribution to the Faraday depth, we map the strength of the magnetic field component along the line of sight. Polarized point sources in our data set have rotation measures that are comparable to the Faraday depths of the diffuse emission in our data. Our Faraday depth maps show narrow canals of low polarized intensity. We conclude that depolarization over the telescope beam produces at least some of these canals. Finally, we investigate the properties of one conspicuous region in this data set and argue that it is created by a decrease in line-of-sight depolarization compared to its surroundings.
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