暗能量巡天第一年结果：来自星系成团性与弱引力透镜的宇宙学约束
宇宙学与河外天体物理
2019-03-04 v3
摘要
我们展示了基于星系成团性与弱引力透镜联合分析的宇宙学结果，使用了来自暗能量巡天（DES）第一年1321平方度的griz成像数据。我们结合了三种两点相关函数：(i) 四个红移区间内2600万个源星系的宇宙剪切相关函数，(ii) 五个红移区间内65万个亮红星系的星系角自相关函数，以及 (iii) 亮红星系位置与源星系剪切的互相关函数。为证明这些结果的稳健性，我们使用了独立的星系形态、测光红移估计与验证以及似然分析管线对。为防止确认偏误，大部分分析在盲法状态下进行；我们描述了在此盲法阶段执行并通过的一系列广泛的系统误差检验。数据在平坦ΛCDM和wCDM宇宙学模型下建模，边缘化了20个多余参数，变化了6个（对于ΛCDM）或7个（对于wCDM）宇宙学参数（包括中微子质量密度），并包含了457×457元素的解析协方差矩阵。我们从这三种两点相关函数中得到了一致的宇宙学结果，并且通过它们的联合分析，对于ΛCDM模型得到S₈ ≡ σ₈(Ωₘ/0.3)⁰·⁵ = 0.783⁺⁰·⁰²¹₋₀.₀₂₅ 和 Ωₘ = 0.264⁺⁰·⁰³²₋₀.₀₁₉；对于wCDM模型，我们在68%置信水平下得到S₈ = 0.794⁺⁰·⁰²⁹₋₀.₀₂₇，Ωₘ = 0.279⁺⁰·⁰⁴³₋₀.₀₂₂，以及w = -0.80⁺⁰·²⁰₋₀.₂₂。这些DES第一年结果的精度可与普朗克宇宙微波背景测量相媲美，从而允许在同等条件下比较极早期和晚期宇宙的结构。尽管DES第一年对S₈和Ωₘ的最佳拟合值低于普朗克中心值……
引用
@article{arxiv.1708.01530,
title = {Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing},
author = {DES Collaboration and T. M. C. Abbott and F. B. Abdalla and A. Alarcon and J. Aleksić and S. Allam and S. Allen and A. Amara and J. Annis and J. Asorey and S. Avila and D. Bacon and E. Balbinot and M. Banerji and N. Banik and W. Barkhouse and M. Baumer and E. Baxter and K. Bechtol and M. R. Becker and A. Benoit-Lévy and B. A. Benson and G. M. Bernstein and E. Bertin and J. Blazek and S. L. Bridle and D. Brooks and D. Brout and E. Buckley-Geer and D. L. Burke and M. T. Busha and D. Capozzi and A. Carnero Rosell and M. Carrasco Kind and J. Carretero and F. J. Castander and R. Cawthon and C. Chang and N. Chen and M. Childress and A. Choi and C. Conselice and R. Crittenden and M. Crocce and C. E. Cunha and C. B. D'Andrea and L. N. da Costa and R. Das and T. M. Davis and C. Davis and J. De Vicente and D. L. DePoy and J. DeRose and S. Desai and H. T. Diehl and J. P. Dietrich and S. Dodelson and P. Doel and A. Drlica-Wagner and T. F. Eifler and A. E. Elliott and F. Elsner and J. Elvin-Poole and J. Estrada and A. E. Evrard and Y. Fang and E. Fernandez and A. Ferté and D. A. Finley and B. Flaugher and P. Fosalba and O. Friedrich and J. Frieman and J. García-Bellido and M. Garcia-Fernandez and M. Gatti and E. Gaztanaga and D. W. Gerdes and T. Giannantonio and M. S. S. Gill and K. Glazebrook and D. A. Goldstein and D. Gruen and R. A. Gruendl and J. Gschwend and G. Gutierrez and S. Hamilton and W. G. Hartley and S. R. Hinton and K. Honscheid and B. Hoyle and D. Huterer and B. Jain and D. J. James and M. Jarvis and T. Jeltema and M. D. Johnson and M. W. G. Johnson and T. Kacprzak and S. Kent and A. G. Kim and A. King and D. Kirk and N. Kokron and A. Kovacs and E. Krause and C. Krawiec and A. Kremin and K. Kuehn and S. Kuhlmann and N. Kuropatkin and F. Lacasa and O. Lahav and T. S. Li and A. R. Liddle and C. Lidman and M. Lima and H. Lin and N. MacCrann and M. A. G. Maia and M. Makler and M. Manera and M. March and J. L. Marshall and P. Martini and R. G. McMahon and P. Melchior and F. Menanteau and R. Miquel and V. Miranda and D. Mudd and J. Muir and A. Möller and E. Neilsen and R. C. Nichol and B. Nord and P. Nugent and R. L. C. Ogando and A. Palmese and J. Peacock and H. V. Peiris and J. Peoples and W. J. Percival and D. Petravick and A. A. Plazas and A. Porredon and J. Prat and A. Pujol and M. M. Rau and A. Refregier and P. M. Ricker and N. Roe and R. P. Rollins and A. K. Romer and A. Roodman and R. Rosenfeld and A. J. Ross and E. Rozo and E. S. Rykoff and M. Sako and A. I. Salvador and S. Samuroff and C. Sánchez and E. Sanchez and B. Santiago and V. Scarpine and R. Schindler and D. Scolnic and L. F. Secco and S. Serrano and I. Sevilla-Noarbe and E. Sheldon and R. C. Smith and M. Smith and J. Smith and M. Soares-Santos and F. Sobreira and E. Suchyta and G. Tarle and D. Thomas and M. A. Troxel and D. L. Tucker and B. E. Tucker and S. A. Uddin and T. N. Varga and P. Vielzeuf and V. Vikram and A. K. Vivas and A. R. Walker and M. Wang and R. H. Wechsler and J. Weller and W. Wester and R. C. Wolf and B. Yanny and F. Yuan and A. Zenteno and B. Zhang and Y. Zhang and J. Zuntz},
journal= {arXiv preprint arXiv:1708.01530},
year = {2019}
}
备注
Matches published version. Results essentially unchanged, except updated covariance matrix leads to improved chi^2 (colored text removed)