A CMB polarization primer
A CMB polarization primer
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DOI：
10.1016/s1384-1076(97)00022-5
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发表时间：
1997-01-01
期刊：
影响因子：
2
通讯作者：
White, M
中科院分区：
文献类型：
--
作者：
Hu, W;White, M
我们对宇宙微波背景（CMB）偏振的研究进行了教学和现象学介绍，以建立对其探测所面临的前景和挑战的直觉。最后一个散射表面上的温度各向异性的汤姆逊散射在天空上产生线性偏振图案，可以从它们的四极矩中简单地读出该图案。这些反过来又直接对应于宇宙扰动的基本标量（压缩）、矢量（涡旋）和张量（引力波）模式。我们根据所谓的电和磁宇称模式以及它们与温度模式的相关性来解释这些模式之间几何区别的起源和现象学。通过对最后一个散射表面和各种扰动模式的隔离，偏振为宇宙学模型的唯象重建提供了独特的信息。最后我们对理论与实验数据的比较进行了评论，并对未来 CMB 偏振探测进行了展望。 (C) 1997 Elsevier Science B.V.
We present a pedagogical and phenomenological introduction to the study of cosmic microwave background (CMB) polarization to build intuition about the prospects and challenges facing its detection. Thomson scattering of temperature anisotropies on the last scattering surface generates a linear polarization pattern on the sky that can be simply read off from their quadrupole moments. These in turn correspond directly to the fundamental scalar (compressional), vector (vortical), and tensor (gravitational wave) modes of cosmological perturbations. We explain the origin and phenomenology of the geometric distinction between these patterns in terms of the so-called electric and magnetic parity modes, as well as their correlation with the temperature pattern. By its isolation of the last scattering surface and the various perturbation modes, the polarization provides unique information for the phenomenological reconstruction of the cosmological model. Finally we comment on the comparison of theory with experimental data and prospects for the future detection of CMB polarization. (C) 1997 Elsevier Science B.V.