星系团中CMB的康普顿化。蒙特卡罗计算
Comptonization of CMB in galaxy clusters. Monte Carlo computations
摘要：
我们考虑的问题是确定由于热Sunyaev-Zeldovich效应引起的宇宙微波背景（CMB）谱形的变化。我们数值模拟了宇宙微波背景辐射在热的星系际麦克斯韦等离子体压缩下的光谱强度。为此，我们开发了一个带光子权重的相对论蒙特卡罗程序。该程序使我们能够在较宽的能量范围内构造康普顿化CMB谱。将结果与已知的解析解和以前的数值模拟进行比较。我们还计算了从云中出现的辐射强度的角分布，这表明tSZ效应的光谱形状对于不同方向的逃逸光子是不通用的。该数值方法可以模拟不同光学深度、温度、光子源初始光谱及其空间分布的康普顿化过程，所得结果对研究星系团的轮廓有一定的意义。
英文摘要：
The problem under consideration is to determine the change of the Cosmic Microwave Background (CMB) spectral shape due to the thermal Sunyaev-Zeldovich effect. We numerically model the spectral intensity of the CMB radiation Comptonized by the hot intergalactic Maxwellian plasma. To this aim, a relativistic Monte Carlo code with photon weights is developed. The code enables us to construct the Comptonized CMB spectrum in a wide energy range. The results are compared with known analytical solutions and previous numerical simulations. We also calculate the angular distributions of the intensity of radiation emerging from the cloud, which show that the spectral shape of the tSZ effect is not universal for different directions of escaping photons. The numerical method can be applied to simulate the processes of Comptonization for different optical depths, temperatures, initial spectra of photon sources and their spatial distributions, the obtained results may have implications on investigating the profiles of galaxy clusters.
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