A Pan-Chromatic View of Clusters of Galaxies and the Large-Scale Structure
A Pan-Chromatic View of Clusters of Galaxies and the Large-Scale Structure
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星系团和大尺度结构的全色视图
DOI：
10.1007/978-1-4020-6941-3_8
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发表时间：
2008
期刊：
影响因子：
--
通讯作者：
Birkinshaw M
中科院分区：
文献类型：
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作者：
Birkinshaw M
丰富的星系团包含大量的热气体大气。这种气体在X射线中的发射是第一代X射线望远镜的重大发现之一。钱德拉和XMM-牛顿卫星现在可以提供星团X射线的高质量图像和光谱。第二种成像这些大气层的方法是由Sunyaev-Zel'dovich（SZ）效应提供的[35]。当宇宙微波背景辐射（CMB）穿过星系团向我们传播时，光子被星系团气体中的电子逆康普顿散射的概率很小。由于微波背景辐射的温度约为2.7 K，而星系团中的气体温度可能高达108 K，散射往往会增加光子能量，从而导致微波背景辐射强度和光谱向星系团的变化。SZ效应的威力是因为该效应是由散射而不是发射引起的，因此与散射电子的密度成比例。因此，星系团的X射线和SZ效应结构可能会有很大的不同，这些结构的比较可以提供有关星系团及其大气物理学的有趣信息。这介绍使用SZ效应描述了基本物理的热，运动学，和其他方面的影响（第2节），用于观察效应产生的小信号的技术（第3节），可以从数据中获得的星系团信息（第4节），和宇宙学的信息可通过这样的工作（第5节），然后描述了一些新一代的仪器设计的详细工作的SZ效应，带我们超越探索阶段的SZ效应科学。关于该效应的更多细节可以在Rephaeli [33]、Birkinshaw [4]和Carlstrom等人的最新综述中找到。[9]，但是
Rich clusters of galaxies contain extensive atmospheres of hot gas. Emission from this gas in X-rays was one of the major discoveries of the first generation of X-ray telescopes. High-quality images and spectra of the X-rays from clusters are now available from the Chandra and XMM-Newton satellites. A second method of imaging these atmospheres is provided by the Sunyaev-Zel’dovich (SZ) effect [35]. As the cosmic microwave background (CMB) radiation propagates through a cluster of galaxies towards us, photons have a small probability of being inverse-Compton scattered by electrons in the cluster gas. Since the microwave background radiation has a temperature of about 2.7 K, while the gas in a cluster of galaxies may have a temperature as high as 108 K, scatterings tend to increase the photon energies, so causing a change in the microwave background radiation intensity and spectrum towards the cluster.The power of the SZ effect comes about because the effect is caused by scattering, rather than emission, and so scales with the density of the scattering electrons. A cluster of galaxies may therefore appear quite different in its X-ray and SZ effect structures, and a comparison of those structures can provide interesting information on the physics of clusters and their atmospheres. This introduction to the use of the SZ effect describes the underlying physics of the thermal, kinematic, and other aspects of the effect (Sect. 2), the techniques used for observing the small signal produced by the effect (Sect. 3), the information on clusters of galaxies that can be obtained from the data (Sect. 4), and the cosmological information available by such work (Sect. 5), and then describes some of the coming generation of instruments designed for detailed work on the SZ effect, to take us beyond the exploratory phase of SZ effect science. More details about the effect can be found in recent reviews by Rephaeli [33], Birkinshaw [4], and Carlstrom et al.[9], but