SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION
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DOI：
10.1088/0067-0049/192/2/18
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发表时间：
2011-02-01
影响因子：
8.7
通讯作者：
Wright, E. L.
中科院分区：
文献类型：
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作者：
Komatsu, E.;Smith, K. M.;Wright, E. L.
来自WMAP的七年数据和改进的天体物理学数据相结合，严格测试了标准宇宙学模型，并对其基本参数和扩展提出了新的限制。结合WMAP数据和最近的星系分布中重子声振荡（BAO）距离测量以及哈勃常数（H-0）测量，我们确定了最简单的六参数Lambda CDM模型的参数。对于该数据组合，原始功率谱的幂律指数为n（s）= 0.968 +/- 0.012（68% CL），该测量结果排除了Harrison-Zel'dovich-Peebles谱的99.5% CL。其他参数，包括超出最低限度的参数，也与五年结果一致，并有所改进。我们没有发现令人信服的偏离最小模型。七年的温度功率谱给出了一个更好的确定的第三声峰，这导致在一个更好的确定红移的物质辐射平等的时代。改进参数的显著例子是中微子的总质量，Sigma m（nu）< 0.58 eV（95%CL），以及中微子种类的有效数量，N-eff = 4.34（-0.88）（+0.86）（68%CL），这得益于更好地确定第三个峰和H-0。在没有高红移Ia型超新星的情况下，WMAP+BAO+H-0的恒定暗能量状态方程参数的极限是w = -1.10 +/- 0.14（68%CL）。我们通过测量γ-p = 0.326 +/- 0.075（68%CL），探测了原初氦对温度功率谱的影响，并提供了一个新的大爆炸核合成实验。我们检测，并显示在地图上的第一次，切向和径向偏振模式周围的热点和冷点的温度波动，一个重要的测试物理过程在z = 1090和绝热标量波动的主导地位。七年的偏振数据有显着改善：我们现在检测到的温度E模式偏振交叉功率谱在21西格玛，相比之下，13西格玛从五年的数据。利用七年温度-B模式互功率谱，由于潜在的宇称违反效应，对偏振平面旋转的限制提高了38%，达到Δ a = -1度.1 +/- 1度. 4（统计）+/- 1度. 5（系统）（68% CL）。我们报告显着的Sunyaev-Zel'dovich（SZ）效应在已知的星系团的位置检测。所测量的SZ信号与来自X射线数据的预期信号在逐簇的基础上吻合得很好。然而，它是Arnaud等人的“通用概况”预测的0.5-0.7倍，分析模型和流体动力学模拟。我们发现，第一次在SZ效应，冷却流和非冷却流集群（或放松和非放松集群）之间的显着差异，这可以解释一些差异。这一较低的振幅与南极望远镜合作组织最近测量的低于理论预期的SZ功率谱一致。
The combination of seven-year data from WMAP and improved astrophysical data rigorously tests the standard cosmological model and places new constraints on its basic parameters and extensions. By combining the WMAP data with the latest distance measurements from the baryon acoustic oscillations (BAO) in the distribution of galaxies and the Hubble constant (H-0) measurement, we determine the parameters of the simplest six-parameter Lambda CDM model. The power-law index of the primordial power spectrum is n(s) = 0.968 +/- 0.012 (68% CL) for this data combination, a measurement that excludes the Harrison-Zel'dovich-Peebles spectrum by 99.5% CL. The other parameters, including those beyond the minimal set, are also consistent with, and improved from, the five-year results. We find no convincing deviations from the minimal model. The seven-year temperature power spectrum gives a better determination of the third acoustic peak, which results in a better determination of the redshift of the matter-radiation equality epoch. Notable examples of improved parameters are the total mass of neutrinos, Sigma m(nu) < 0.58 eV (95% CL), and the effective number of neutrino species, N-eff = 4.34(-0.88)(+0.86) (68% CL), which benefit from better determinations of the third peak and H-0. The limit on a constant dark energy equation of state parameter from WMAP+BAO+H-0, without high-redshift Type Ia supernovae, is w = -1.10 +/- 0.14 (68% CL). We detect the effect of primordial helium on the temperature power spectrum and provide a new test of big bang nucleosynthesis by measuring Y-p = 0.326 +/- 0.075 (68% CL). We detect, and show on the map for the first time, the tangential and radial polarization patterns around hot and cold spots of temperature fluctuations, an important test of physical processes at z = 1090 and the dominance of adiabatic scalar fluctuations. The seven-year polarization data have significantly improved: we now detect the temperature-E-mode polarization cross power spectrum at 21 sigma, compared with 13 sigma from the five-year data. With the seven-year temperature-B-mode cross power spectrum, the limit on a rotation of the polarization plane due to potential parity-violating effects has improved by 38% to Delta a = -1 degrees.1 +/- 1 degrees.4(statistical) +/- 1 degrees.5(systematic) (68% CL). We report significant detections of the Sunyaev-Zel'dovich (SZ) effect at the locations of known clusters of galaxies. The measured SZ signal agrees well with the expected signal from the X-ray data on a cluster-by-cluster basis. However, it is a factor of 0.5-0.7 times the predictions from "universal profile" of Arnaud et al., analytical models, and hydrodynamical simulations. We find, for the first time in the SZ effect, a significant difference between the cooling-flow and non-cooling-flow clusters (or relaxed and non-relaxed clusters), which can explain some of the discrepancy. This lower amplitude is consistent with the lower-than-theoretically expected SZ power spectrum recently measured by the South Pole Telescope Collaboration.