Cosmological-parameter determination with microwave background maps.
Cosmological-parameter determination with microwave background maps.
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用微波背景图确定宇宙学参数。
DOI：
10.1103/physrevd.54.1332
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发表时间：
1995
期刊：
影响因子：
--
通讯作者：
D. Spergel
中科院分区：
文献类型：
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作者：
G. Jungman;M. Kamionkowski;A. Kosowsky;D. Spergel
宇宙微波背景辐射（CMB）的角功率谱包含了几乎所有感兴趣的宇宙学参数的信息，包括宇宙的几何结构（Ω）、重子密度、哈勃常数（h）、宇宙学常数（Λ）、轻中微子的数量、电离历史以及原始标量和张量微扰谱的振幅和谱指数。我们检查CMB上每个参数的印记。仅假设原始扰动是绝热的，我们使用协方差矩阵的方法来估计这些参数可以由CMB温度图确定为天空映射的分数，像素噪声水平和角分辨率的函数的精度。例如，在没有任何关于宇宙学参数的先验信息的情况下，一张具有0.5°角分辨率和每像素15 μK噪声水平的全天空CMB图可以确定Ω、h和Λ，标准误差为±0.1或更好，并提供传统观测无法获得的其他参数的确定。较小的光束尺寸或来自其他观测的关于其他参数中的一些的先验信息提高了灵敏度。对基本的宇宙学模型的依赖进行了讨论。
The angular power spectrum of the cosmic microwave background (CMB) contains information on virtually all cosmological parameters of interest, including the geometry of the Universe (Ω), the baryon density, the Hubble constant (h), the cosmological constant (Λ), the number of light neutrinos, the ionization history, and the amplitudes and spectral indices of the primordial scalar and tensor perturbation spectra. We review the imprint of each parameter on the CMB. Assuming only that the primordial perturbations were adiabatic, we use a covariance-matrix approach to estimate the precision with which these parameters can be determined by a CMB temperature map as a function of the fraction of sky mapped, the level of pixel noise, and the angular resolution. For example, with no prior information about any of the cosmological parameters, a full-sky CMB map with 0.5° angular resolution and a noise level of 15 μK per pixel can determine Ω, h, and Λ with standard errors of ±0.1 or better, and provide determinations of other parameters which are inaccessible with traditional observations. Smaller beam sizes or prior information on some of the other parameters from other observations improves the sensitivity. The dependence on the underlying cosmological model is discussed.