Planck 2018 results: VI. Cosmological parameters
Planck 2018 results: VI. Cosmological parameters
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DOI：
10.1051/0004-6361/201833910
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发表时间：
2020-09-11
影响因子：
6.5
通讯作者：
Zonca, A.
中科院分区：
文献类型：
--
作者：
Aghanim, N.;Akrami, Y.;Zonca, A.
我们结合来自温度和偏振图以及透镜重建的信息，展示了宇宙微波背景（CMB）各向异性的最终全任务普朗克测量的宇宙学参数结果。与 2015 年的结果相比，大尺度偏振测量的改进使得再电离光学深度的测量精度更高，从而导致其他相关参数的精度显着提高。改进的小尺度极化建模对许多参数产生了更稳健的约束，估计残余建模不确定性仅在 0.5 西格玛水平上影响它们。我们发现与标准空间平坦 6 参数 Lambda CDM 宇宙学具有良好的一致性，该宇宙学具有绝热标量扰动的幂律谱（在本文中表示为“基础 Lambda CDM”），分别来自偏振、温度和透镜效应，无论是单独还是组合。综合分析得出暗物质密度 Omega (c)h(2)=0.120 +/- 0.001，重子密度 Omega (b)h(2)=0.0224 +/- 0.0001，标量光谱指数 n(s)=0.965 +/- 0.004，光学深度 tau =0.054 +/- 0.007（在本摘要中，我们引用 68% 置信度）测量参数的区域和 上限为 95%）。角度声学刻度的测量精度为 0.03%，其中 100 theta (*)=1.0411 +/- 0.0003。这些结果仅微弱地依赖于宇宙学模型，并且在许多通常考虑的扩展中保持稳定，但误差有所增加。假设基础-Lambda CDM宇宙学，推断的（模型相关的）晚宇宙参数为： 哈勃常数 H-0=(67.4 +/- 0.5) km s(-1) Mpc(-1)；物质密度参数Omega(m)=0.315+/-0.007；物质波动幅度西格玛(8)=0.811+/-0.006。我们没有发现令人信服的证据可以扩展基本 Lambda CDM 模型。结合重子声振荡（BAO）测量（并考虑单参数扩展），我们将有效的额外相对论自由度限制为 N-eff=2.99 +/- 0.17，与标准模型预测 N-eff=3.046 一致，并发现中微子质量严格限制在 Sigma m(nu)< 0.12 eV。 CMB 光谱继续倾向于比基础 CDM 中预测的更高的透镜振幅（超过 2 sigma），这将影响透镜振幅的一些参数从 Lambda CDM 模型中拉开；然而，透镜重建或（在也改变背景几何形状的模型中）BAO 数据不支持这一点。 BAO 测量对空间曲率的联合约束与平坦宇宙一致，Omega (K)=0.001 +/- 0.002。结合Ia型超新星（SNe），测得暗能量状态方程参数为w(0)=-1.03+/-0.03，与宇宙学常数一致。我们没有发现任何偏离纯幂律原初谱的证据，并结合 BAO、BICEP2 和 Keck 阵列数据的数据，我们对张量与标量之比 r(0.002)< 0.06 进行了限制。基本 CDM 宇宙学中氦和氘丰度的标准大爆炸核合成预测与观测结果非常一致。普朗克基本 Lambda CDM 结果与 BAO、超新星和一些星系透镜观测结果非常一致，但与暗能量巡天的组合探测结果（包括星系团簇（更喜欢较低的波动幅度或 物质密度参数），以及显着的 3.6 sigma 张力以及哈勃常数的局部测量（更喜欢更高的值）。普朗克数据不支持可以部分解决这些紧张局势的简单模型扩展。
We present cosmological parameter results from the final full-mission Planck measurements of the cosmic microwave background (CMB) anisotropies, combining information from the temperature and polarization maps and the lensing reconstruction. Compared to the 2015 results, improved measurements of large-scale polarization allow the reionization optical depth to be measured with higher precision, leading to significant gains in the precision of other correlated parameters. Improved modelling of the small-scale polarization leads to more robust constraints on many parameters, with residual modelling uncertainties estimated to affect them only at the 0.5 sigma level. We find good consistency with the standard spatially-flat 6-parameter Lambda CDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted "base Lambda CDM" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density Omega (c)h(2)=0.120 +/- 0.001, baryon density Omega (b)h(2)=0.0224 +/- 0.0001, scalar spectral index n(s)=0.965 +/- 0.004, and optical depth tau =0.054 +/- 0.007 (in this abstract we quote 68% confidence regions on measured parameters and 95% on upper limits). The angular acoustic scale is measured to 0.03% precision, with 100 theta (*)=1.0411 +/- 0.0003. These results are only weakly dependent on the cosmological model and remain stable, with somewhat increased errors, in many commonly considered extensions. Assuming the base-Lambda CDM cosmology, the inferred (model-dependent) late-Universe parameters are: Hubble constant H-0=(67.4 +/- 0.5) km s(-1) Mpc(-1); matter density parameter Omega (m)=0.315 +/- 0.007; and matter fluctuation amplitude sigma (8)=0.811 +/- 0.006. We find no compelling evidence for extensions to the base-Lambda CDM model. Combining with baryon acoustic oscillation (BAO) measurements (and considering single-parameter extensions) we constrain the effective extra relativistic degrees of freedom to be N-eff=2.99 +/- 0.17, in agreement with the Standard Model prediction N-eff=3.046, and find that the neutrino mass is tightly constrained to Sigma m(nu)< 0.12 eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base CDM at over 2 sigma, which pulls some parameters that affect the lensing amplitude away from the Lambda CDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. The joint constraint with BAO measurements on spatial curvature is consistent with a flat universe, Omega (K)=0.001 +/- 0.002. Also combining with Type Ia supernovae (SNe), the dark-energy equation of state parameter is measured to be w(0)=-1.03 +/- 0.03, consistent with a cosmological constant. We find no evidence for deviations from a purely power-law primordial spectrum, and combining with data from BAO, BICEP2, and Keck Array data, we place a limit on the tensor-to-scalar ratio r(0.002)< 0.06. Standard big-bang nucleosynthesis predictions for the helium and deuterium abundances for the base-CDM cosmology are in excellent agreement with observations.The Planck base-Lambda CDM results are in good agreement with BAO, SNe, and some galaxy lensing observations, but in slight tension with the Dark Energy Survey's combined-probe results including galaxy clustering (which prefers lower fluctuation amplitudes or matter density parameters), and in significant, 3.6 sigma, tension with local measurements of the Hubble constant (which prefer a higher value). Simple model extensions that can partially resolve these tensions are not favoured by the Planck data.