测量和校准银河系同步辐射
Measuring and calibrating Galactic synchrotron emission
摘要：
我们在银河系中的位置需要全天空的观测来揭示它的大尺度性质。全天空测量的零级校准不同于标准的“相对”测量，其中源相对于其周围环境进行测量。全天巡天的目标是包括超过其角分辨率的所有角尺度的发射结构，包括各向同性发射分量。同步辐射是银河系中最主要的辐射过程，频率高达几GHz，其中存在高达1.4 GHz的总强度的许多地面调查。它的偏振特性最近刚刚在1.4 GHz的整个天空中被绘制出来。WMAP提供的23千兆赫及以上频率的全天总强度和线性极化图已经可用，并补充了现有的天空图。使用大型单碟或综合望远镜进行银河平面巡天具有较高的角分辨率。偏振漫射发射显示出与星际介质中法拉第旋转效应引起的总强度发射无关的结构。这些偏振结构的解释关键取决于斯托克斯U和Q的绝对零度水平的正确设置。
英文摘要：
Our position inside the Galaxy requires all-sky surveys to reveal its large-scale properties. The zero-level calibration of all-sky surveys differs from standard 'relative' measurements, where a source is measured in respect to its surroundings. All-sky surveys aim to include emission structures of all angular scales exceeding their angular resolution including isotropic emission components. Synchrotron radiation is the dominating emission process in the Galaxy up to frequencies of a few GHz, where numerous ground based surveys of the total intensity up to 1.4 GHz exist. Its polarization properties were just recently mapped for the entire sky at 1.4 GHz. All-sky total intensity and linear polarization maps from WMAP for frequencies of 23 GHz and higher became available and complement existing sky maps. Galactic plane surveys have higher angular resolution using large single-dish or synthesis telescopes. Polarized diffuse emission shows structures with no relation to total intensity emission resulting from Faraday rotation effects in the interstellar medium. The interpretation of these polarization structures critically depends on a correct setting of the absolute zero-level in Stokes U and Q.
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