First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: The Angular Power Spectrum-猫眼课题宝

DOI：

10.1086/377225

发表时间：

2003-02

期刊：

The Astrophysical Journal Supplement Series

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

G. Hinshaw;D. Spergel;L. Verde;R. Hill;S. Meyer;C. Barnès;C. Bennett;M. Halpern;N. Jarosik;A. Kogut;E. Komatsu;M. Limon;L. Page;G. Tucker;J. Weiland;Edward J. Wollack;E. L. W. N. Gsfc;Princeton;Ssai;U. Chicago;Ubc;Brown;Ucla

本文给出了从威尔金森微波各向异性探测器（WMAP）第一年的天图中得到的角功率谱。我们研究了各种功率谱估计方法和数据组合，并证明了结果是稳健的。这些数据受到弥漫的银河系前景发射的适度污染，但我们表明，一个简单的银河系模板模型足以消除信号。点源在低频数据中产生适度的污染。在从地图上屏蔽了大约700个已知的亮源之后，我们估计剩余源在41 GHz和94 GHz分别对功率谱[<$（<$+ 1）C <$/2π]贡献了大约3500 μK2和大约130 μK2。与前景发射的（适度）水平相比，系统误差可以忽略不计。我们的最佳估计的功率谱是来自28个统计独立的通道的交叉功率谱。最终的光谱基本上是独立的噪声特性的一个单独的辐射计。由此产生的光谱提供了一个确定的测量宇宙微波背景（CMB）功率谱，与宇宙方差的不确定性限制，高达350万。频谱清楚地显示出在λ = 220处的第一声峰和在λ = 540处的第二声峰（Page和同事），并且它为绝热初始条件提供了强有力的支持（Spergel和同事）。Kogut和同事分析了C功率谱，并提出了相对较高的光学深度和宇宙再电离早期的证据。除此之外，这意味着温度功率谱在角度尺度上被抑制了30%，这是二次散射的结果。

We present the angular power spectrum derived from the first-year Wilkinson Microwave Anisotropy Probe (WMAP) sky maps. We study a variety of power spectrum estimation methods and data combinations and demonstrate that the results are robust. The data are modestly contaminated by diffuse Galactic foreground emission, but we show that a simple Galactic template model is sufficient to remove the signal. Point sources produce a modest contamination in the low-frequency data. After masking ∼700 known bright sources from the maps, we estimate that residual sources contribute ∼3500 μK2 at 41 GHz and ∼130 μK2 at 94 GHz to the power spectrum [ℓ(ℓ + 1)Cℓ/2π] at ℓ = 1000. Systematic errors are negligible compared to the (modest) level of foreground emission. Our best estimate of the power spectrum is derived from 28 cross-power spectra of statistically independent channels. The final spectrum is essentially independent of the noise properties of an individual radiometer. The resulting spectrum provides a definitive measurement of the cosmic microwave background (CMB) power spectrum, with uncertainties limited by cosmic variance, up to ℓ ∼ 350. The spectrum clearly exhibits a first acoustic peak at ℓ = 220 and a second acoustic peak at ℓ ∼ 540 (Page and coworkers), and it provides strong support for adiabatic initial conditions (Spergel and coworkers). Kogut and coworkers analyze the C power spectrum and present evidence for a relatively high optical depth and an early period of cosmic reionization. Among other things, this implies that the temperature power spectrum has been suppressed by ∼30% on degree angular scales, as a result of secondary scattering.

First-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: The Angular Power Spectrum

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