Planck 2013 results. XVI. Cosmological parameters
Planck 2013 results. XVI. Cosmological parameters
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DOI：
10.1051/0004-6361/201321591
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发表时间：
2014-11-01
影响因子：
6.5
通讯作者：
Zonca, A.
中科院分区：
文献类型：
--
作者：
Ade, P. A. R.;Aghanim, N.;Zonca, A.
本文介绍了第一个宇宙学结果的基础上普朗克测量的宇宙微波背景（CMB）温度和透镜势功率谱。我们发现，普朗克光谱在高多极（l大于或接近40）是非常好的描述标准的空间平坦的六参数ACDM宇宙学与幂律谱的绝热标量扰动。在这种宇宙学的背景下，普朗克数据以高精度确定了宇宙学参数：复合时声视界的角尺寸、重子和冷暗物质的物理密度以及标量谱指数估计为θ * =（1.04147 +/- 0.00062）× 10（-2），Ω（B）h（2）= 0.02205 +/- 0.00028，Ω（c）h（2）= 0.1199 +/- 0.0027，n（s）= 0.9603 +/- 0.0073，（注意，在本摘要中，我们引用了测量参数的68%误差和其他参数的95%上限）。对于这种宇宙学，我们发现哈勃常数H-0 =（67.3 +/- 1.2）km s（-1）Mpc（-1）的低值，以及物质密度参数Omega（m）= 0.315 +/- 0.017的高值。这些值与最近直接测量的H-0和Ia型超新星的星等-红移关系存在紧张关系，但与重子声学振荡（BAO）调查的几何约束非常一致。包括曲率，我们发现，宇宙是一致的空间平坦度的百分比级精度仅使用普朗克CMB数据。我们使用高分辨率的CMB数据与普朗克一起提供更大的控制河外前景组件的调查扩展到六参数ACDM模型。我们目前选定的结果，从一个大网格的宇宙学模型，使用一系列额外的天体物理数据集，除了普朗克和高分辨率CMB数据。这些模型中没有一个比标准的六参数ACDM宇宙学更受欢迎。标量谱指数与单位的偏差对张量模的增加和宇宙物质含量的变化不敏感。我们发现张量标量比的上限r（0.002）< 0.11。除了标准模型中的三个中微子族之外，没有其他类似中微子的相对论性粒子的证据。使用BAO和CMB数据，我们发现N-eff = 3.30 +/- 0.27的相对论自由度的有效数量，和上限为0.23 eV的中微子质量的总和。我们的结果与大爆炸核合成和N-eff = 3.046的标准值非常一致。我们没有发现动力学暗能量的证据;使用BAO和CMB数据，暗能量状态方程参数被约束为w = -1.13（-0.10）（+0.13）。我们还使用普朗克数据来限制精细结构常数、暗物质湮灭和原始磁场的可能变化。尽管成功的六参数ACDM模型在描述普朗克数据在高多极，我们注意到，这种宇宙学不提供一个很好的适合在低多极的温度功率谱。不寻常的形状的频谱在多极范围20小于或类似于l小于或类似于40以前看到的WMAP数据，是一个真实的功能的原始CMB各向异性。在低多极的频谱拟合差是没有决定性的意义，但在普朗克温度数据的自洽分析，否则是一个“异常”。
This paper presents the first cosmological results based on Planck measurements of the cosmic microwave background (CMB) temperature and lensing-potential power spectra. We find that the Planck spectra at high multipoles (l greater than or similar to 40) are extremely well described by the standard spatially-flat six-parameter ACDM cosmology with a power-law spectrum of adiabatic scalar perturbations. Within the context of this cosmology, the Planck data determine the cosmological parameters to high precision: the angular size of the sound horizon at recombination, the physical densities of baryons and cold dark matter, and the scalar spectral index are estimated to be theta* = (1.04147 +/- 0.00062) x 10(-2), Omega(b)h(2) = 0.02205 +/- 0.00028, Omega(c)h(2) = 0.1199 +/- 0.0027, and n(s) = 0.9603 +/- 0.0073, respectively (note that in this abstract we quote 68% errors on measured parameters and 95% upper limits on other parameters). For this cosmology, we find a low value of the Hubble constant, H-0 = (67.3 +/- 1.2) km s(-1) Mpc(-1), and a high value of the matter density parameter, Omega(m) = 0.315 +/- 0.017. These values are in tension with recent direct measurements of H-0 and the magnitude-redshift relation for Type Ia supernovae, but are in excellent agreement with geometrical constraints from baryon acoustic oscillation (BAO) surveys. Including curvature, we find that the Universe is consistent with spatial flatness to percent level precision using Planck CMB data alone. We use high-resolution CMB data together with Planck to provide greater control on extragalactic foreground components in an investigation of extensions to the six-parameter ACDM model. We present selected results from a large grid of cosmological models, using a range of additional astrophysical data sets in addition to Planck and high-resolution CMB data. None of these models are favoured over the standard six-parameter ACDM cosmology. The deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the Universe. We find an upper limit of r(0.002) < 0.11 on the tensor-to-scalar ratio. There is no evidence for additional neutrino-like relativistic particles beyond the three families of neutrinos in the standard model. Using BAO and CMB data, we find N-eff = 3.30 +/- 0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.23 eV for the sum of neutrino masses. Our results are in excellent agreement with big bang nucleosynthesis and the standard value of N-eff = 3.046. We find no evidence for dynamical dark energy; using BAO and CMB data, the dark energy equation of state parameter is constrained to be w = -1.13(-0.10)(+0.13). We also use the Planck data to set limits on a possible variation of the fine-structure constant, dark matter annihilation and primordial magnetic fields. Despite the success of the six-parameter ACDM model in describing the Planck data at high multipoles, we note that this cosmology does not provide a good fit to the temperature power spectrum at low multipoles. The unusual shape of the spectrum in the multipole range 20 less than or similar to l less than or similar to 40 was seen previously in the WMAP data and is a real feature of the primordial CMB anisotropies.The poor fit to the spectrum at low multipoles is not of decisive significance, but is an "anomaly" in an otherwise self-consistent analysis of the Planck temperature data.