Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing
Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing
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DOI：
10.1103/physrevd.105.023520
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发表时间：
2022-01-13
影响因子：
5
通讯作者：
Zuntz, J.
中科院分区：
文献类型：
--
作者：
Abbott, T. M. C.;Aguena, M.;Zuntz, J.
我们使用来自暗能量巡天（DES）数据发布1的完整5000 deg（2）成像数据展示了大尺度结构的第一个宇宙学结果。我们进行了分析的大尺度结构相结合的三个两点相关函数（3 × 2 pt）：（i）宇宙剪切使用1亿个源星系，（ii）星系聚类，和（iii）交叉相关的源星系剪切与透镜星系的位置，星系星系透镜。为了实现这些测量所实现的宇宙学精度，需要更新DES第一年的几乎每一个分析部分，包括使用两个独立的星系团样本，建模进展，以及在引力剪切和光度红移推断的校准方面的一些新的改进。分析是在严格的条件下进行的，以减轻确认或观察者的偏见;我们描述了对透镜星系样本的具体变化后，揭盲的结果和我们的结果的稳健性测试，这一决定。我们模型的数据在平坦的Lambda CDM和wCDM宇宙模型，边缘化超过25个讨厌的参数。我们发现三个两点相关函数之间的宇宙学结果是一致的;它们的组合产生了聚类幅度S-8 = 0.776（-0.017）（+0.017）和物质密度Ω（m）= 0.339（-0.031）（+0.032）在Lambda CDM中，均值，置信限为68%;在wCDM中，S-8 = 0.775（-0.024）（+0.026），Omega（m）= 0.352（-0.041）（+0.035），暗能量状态方程参数w = -0.98（-0.02）（+0.32）。这些限制对应于DES第33年x 2 pt数据相对于DES第1年的信噪比提高了2.1倍，比仅观察面积增加的预期高出约20%。DES数据的这种组合与普朗克2018年宇宙微波背景（CMB）主要各向异性数据所支持的模型预测一致，该数据被量化为超过p = 0.13-0.48的概率。我们发现DES 3 x 2 pt和普朗克之间比DES Y1更好的协议，尽管两者的精度显着提高。当结合DES 3 x 2 pt数据与现有的重子声学振荡，红移空间失真，和Ia型超新星的数据，我们发现p = 0.34。将所有这些数据集与普朗克CMB透镜相结合，得到S-8 = 0.812（-0.008）（+0.008），Omega（m）= 0.306（-0.005）（+0.004），h = 0.680（-0.003）（+0.004）和Sigma m（nu）< 0.13 eV（95% C.L.）在λ CDM中，S-8 = 0.812（-0.008）（+0.008），Ω（m）= 0.302（-0.006）（+0.006），h = 0.687（-0.007）（+0.006），w = -1.031（-0.027）（+0.030）。
We present the first cosmology results from large-scale structure using the full 5000 deg(2) of imaging data from the Dark Energy Survey (DES) Data Release 1. We perform an analysis of large-scale structure combining three two-point correlation functions (3 x 2pt): (i) cosmic shear using 100 million source galaxies, (ii) galaxy clustering, and (iii) the cross-correlation of source galaxy shear with lens galaxy positions, galaxy-galaxy lensing. To achieve the cosmological precision enabled by these measurements has required updates to nearly every part of the analysis from DES Year 1, including the use of two independent galaxy clustering samples, modeling advances, and several novel improvements in the calibration of gravitational shear and photometric redshift inference. The analysis was performed under strict conditions to mitigate confirmation or observer bias; we describe specific changes made to the lens galaxy sample following unblinding of the results and tests of the robustness of our results to this decision. We model the data within the flat Lambda CDM and wCDM cosmological models, marginalizing over 25 nuisance parameters. We find consistent cosmological results between the three two-point correlation functions; their combination yields clustering amplitude S-8 = 0.776(-0.017)(+0.017) and matter density Omega(m) = 0.339(-0.031)(+0.032) in Lambda CDM, mean with 68% confidence limits; S-8 = 0.775(-0.024)(+0.026), Omega(m) = 0.352(-0.041)(+0.035), and dark energy equation-of-state parameter w = -0.98(-0.02)(+0.32) in wCDM. These constraints correspond to an improvement in signal-to-noise of the DES Year 33 x 2pt data relative to DES Year 1 by a factor of 2.1, about 20% more than expected from the increase in observing area alone. This combination of DES data is consistent with the prediction of the model favored by the Planck 2018 cosmic microwave background (CMB) primary anisotropy data, which is quantified with a probability-to-exceed p = 0.13-0.48. We find better agreement between DES 3 x 2pt and Planck than in DES Y1, despite the significantly improved precision of both. When combining DES 3 x 2pt data with available baryon acoustic oscillation, redshift-space distortion, and type la supernovae data, we find p = 0.34. Combining all of these datasets with Planck CMB lensing yields joint parameter constraints of S-8 = 0.812(-0.008)(+0.008), Omega(m) = 0.306(-0.005)(+0.004), h = 0.680(-0.003)(+0.004), and Sigma m(nu) < 0.13 eV (95% C.L.) in Lambda CDM; S-8 = 0.812(-0.008)(+0.008), Omega(m) = 0.302(-0.006)(+0.006), h = 0.687(-0.007)(+0.006), and w = -1.031(-0.027)(+0.030) in wCDM.