The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample
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DOI：
10.1093/mnras/stx721
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发表时间：
2017-09-01
影响因子：
4.8
通讯作者：
Zhao, Gong-Bo
中科院分区：
文献类型：
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作者：
Alam, Shadab;Ata, Metin;Zhao, Gong-Bo
我们展示了重子振荡光谱巡天最终星系聚类数据集的宇宙学结果，该巡天是斯隆数字巡天 III 的一部分。我们的组合星系样本包含 120 万个大质量星系，有效面积为 9329 deg(2)，体积为 18.7 Gpc(3)，分为三个部分重叠的红移切片，中心有效红移为 0.38、0.51 和 0.61。在应用重建以减少对 BAO 特征的非线性影响之后，我们结合声视界尺度上的宇宙微波背景，通过重子声振荡 (BAO) 方法测量角直径距离 DM 和哈勃参数 H。利用重建前密度场的各向异性聚类，我们测量了 Alcock-Paczynski (AP) 效应的乘积 DMH 和红移空间扭曲 (RSD) 的结构生长，通过 f sigma(8(z)) 进行量化。我们将七篇配套论文中提出的单独测量结果组合成一组共识值和可能性，获得比任何一种方法更严格、更稳健的约束；特别是，子 BAO 尺度的 AP 测量通过打破 D-M 和 H 之间的简并性，锐化了重建后 BAO 的约束。结合普朗克 2016 年宇宙微波背景测量，我们的距离尺度测量同时意味着曲率 Omega(K) = 0.0003 +/- 0.0026 和暗能量状态方程参数 w = -1.01 +/- 0.06，强烈肯定了具有宇宙学常数 (Lambda CDM) 的空间平坦冷暗物质 (CDM) 模型。我们对 f sigma(8) 的 RSD 测量精度为 6%，同样与该模型一致。当与超新星 Ia 数据结合时，我们发现 H-0 = 67.3 +/- 1.0 km s(-1) Mpc(-1)，即使对于我们最一般的暗能量模型来说，在一些直接测量的张力下也是如此。添加额外的相对论物种作为自由度仅稍微放松约束，达到 H-0 = 67.8 +/- 1.2 km s(-1) Mpc(-1)。假设平坦的 Lambda CDM，我们发现 Omega(m) = 0.310 +/- 0.005 和 H-0 = 67.6 +/- 0.5 km s(-1) Mpc(-1)，并且我们发现中微子质量和的 95% 上限为 0.16 eV c(-2)。
We present cosmological results from the final galaxy clustering data set of the Baryon Oscillation Spectroscopic Survey, part of the Sloan Digital Sky Survey III. Our combined galaxy sample comprises 1.2 million massive galaxies over an effective area of 9329 deg(2) and volume of 18.7 Gpc(3), divided into three partially overlapping redshift slices centred at effective redshifts 0.38, 0.51 and 0.61. We measure the angular diameter distance DM and Hubble parameter H from the baryon acoustic oscillation (BAO) method, in combination with a cosmic microwave background prior on the sound horizon scale, after applying reconstruction to reduce non-linear effects on the BAO feature. Using the anisotropic clustering of the pre-reconstruction density field, we measure the product DMH from the Alcock-Paczynski (AP) effect and the growth of structure, quantified by f sigma(8(z)), from redshift-space distortions (RSD). We combine individual measurements presented in seven companion papers into a set of consensus values and likelihoods, obtaining constraints that are tighter and more robust than those from any one method; in particular, the AP measurement from sub-BAO scales sharpens constraints from post-reconstruction BAOs by breaking degeneracy between D-M and H. Combined with Planck 2016 cosmic microwave background measurements, our distance scale measurements simultaneously imply curvature Omega(K) = 0.0003 +/- 0.0026 and a dark energy equation-of-state parameter w = -1.01 +/- 0.06, in strong affirmation of the spatially flat cold dark matter (CDM) model with a cosmological constant (Lambda CDM). Our RSD measurements of f sigma(8), at 6 per cent precision, are similarly consistent with this model. When combined with supernova Ia data, we find H-0 = 67.3 +/- 1.0 km s(-1) Mpc(-1) even for our most general dark energy model, in tension with some direct measurements. Adding extra relativistic species as a degree of freedom loosens the constraint only slightly, to H-0 = 67.8 +/- 1.2 km s(-1) Mpc(-1). Assuming flat Lambda CDM, we find Omega(m) = 0.310 +/- 0.005 and H-0 = 67.6 +/- 0.5 km s(-1) Mpc(-1), and we find a 95 per cent upper limit of 0.16 eV c(-2) on the neutrino mass sum.