Dark Energy Survey year 1 results: Constraints on extended cosmological models from galaxy clustering and weak lensing
Dark Energy Survey year 1 results: Constraints on extended cosmological models from galaxy clustering and weak lensing
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DOI：
10.1103/physrevd.99.123505
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发表时间：
2018-10
影响因子：
5
通讯作者：
T. Abbott;F. Abdalla;S. Ávila;M. Banerji;E. Baxter;K. Bechtol;M. Becker;E. Bertin;J. Blazek-J.-Blaze
中科院分区：
文献类型：
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作者：
T. Abbott;F. Abdalla;S. Ávila;M. Banerji;E. Baxter;K. Bechtol;M. Becker;E. Bertin;J. Blazek-J.-Blaze
作者：Abbott， TMC；阿布达拉,FB;阿维拉,年代;纳杰,M;巴克斯特,E;Bechtol K;贝克先生;贝尔坦公司E;Blazek J;缰绳,SL;布鲁克斯,D;Brout D;伯克,DL;坎波斯,;Carnero Rosell， A；卡拉斯科·金德，M；Carretero J;Castander FJ;Cawthon R;常,C;陈;Crocce, M;达,CE;Da Costa， LN；戴维斯,C;De Vicente， J；Derose J;德赛,年代;迪·瓦伦蒂诺，E；发,HT;迪特里希,摩根;Dodelson年代;德尔,了P;Drlica-Wagner,;Eifler特遣部队;Elvin-Poole J;AE分离出来;费尔南德斯,E;Ferte,;Flaugher, B;Fosalba P;Frieman J;Garcia-Bellido J;Gaztanaga E;格迪斯,DW;Giannantonio T;格伦,D;Gruendl,类风湿性关节炎;Gschwend J;古铁雷斯,G;哈特利,描写;Hollowood DL;Honscheid K;霍伊尔,B;huter D;耆那教徒,B;Jeltema T;约翰逊,MWG;约翰逊博士;金、银;Krause, E;期,K;Kuropatkin N;阿,Lahav表示;李,年代;Lemos P;伦纳德,CD;李,TS;Liddle,基于“增大化现实”技术;利马M;林,H;玛雅,杂志;马歇尔,杰;马提尼,P;Menanteau F;米勒,CJ;纳斯,R;米兰达,V;莫尔,JJ;穆尔,J;Nichol RC;北方,B;Ogando RLC;广场、AA;摘要：©2019美国物理学会。通过对暗能量调查（DES Y1）第一年数据的星系群集和弱引力透镜的综合分析，结合外部数据，我们提出了以暗物质和暗能量（ΛCDM和wCDM）为主导的最小宇宙学模型的扩展约束。我们考虑了最小暗能量占主导的四种情形的扩展：(1)非零曲率ωk，(2)不同于标准值3.046的相对论性种数Neff，(3)由参数w0和wa描述的时变暗能量状态方程（或由枢轴红移值wp和wa引用），以及(4)由参数μ0和ρ 0描述的修正引力，修改度量势。我们还考虑了来自普朗克宇宙微波背景测量的外部信息；SDSS、6dF和BOSS的重子声学振荡测量；BOSS红移空间畸变测量；以及来自万神殿汇编数据集的Ia型超新星信息。曲率和相对论种数的约束由外部数据主导；当这些与DES Y1结合时，我们发现ωk=0.0020-0.0032+0.0037在68%置信度下，上限Neffl3.28（3.55）在68%（95%）置信度下，假设硬先验Neffg3.0。对于时变状态方程，我们发现单独DES在枢轴红移zp=0.27处的枢轴值(wp,wa)=(-0.91-0.23+0.19,-0.57-1.11+0.93)，而结合外部数据的DES Y1在zp=0.20处的枢轴值(wp,wa)=(-1.01-0.04+0.04,-0.28-0.48+0.37)；在这两种情况下，我们都找不到状态方程随时间变化的证据。对于修正重力，我们发现DES Y1单独得到的相关参数的现今值为0.43-0.29+0.28，DES Y1结合外部数据得到的相关参数的现今值为(0,0,μ0)=(0.06-0.07+0.08,-0.11-0.46+0.42)。这些修正的引力约束与广义相对论的预测是一致的。
Author(s): Abbott, TMC; Abdalla, FB; Avila, S; Banerji, M; Baxter, E; Bechtol, K; Becker, MR; Bertin, E; Blazek, J; Bridle, SL; Brooks, D; Brout, D; Burke, DL; Campos, A; Carnero Rosell, A; Carrasco Kind, M; Carretero, J; Castander, FJ; Cawthon, R; Chang, C; Chen, A; Crocce, M; Cunha, CE; Da Costa, LN; Davis, C; De Vicente, J; Derose, J; Desai, S; Di Valentino, E; Diehl, HT; Dietrich, JP; Dodelson, S; Doel, P; Drlica-Wagner, A; Eifler, TF; Elvin-Poole, J; Evrard, AE; Fernandez, E; Ferte, A; Flaugher, B; Fosalba, P; Frieman, J; Garcia-Bellido, J; Gaztanaga, E; Gerdes, DW; Giannantonio, T; Gruen, D; Gruendl, RA; Gschwend, J; Gutierrez, G; Hartley, WG; Hollowood, DL; Honscheid, K; Hoyle, B; Huterer, D; Jain, B; Jeltema, T; Johnson, MWG; Johnson, MD; Kim, AG; Krause, E; Kuehn, K; Kuropatkin, N; Lahav, O; Lee, S; Lemos, P; Leonard, CD; Li, TS; Liddle, AR; Lima, M; Lin, H; Maia, MAG; Marshall, JL; Martini, P; Menanteau, F; Miller, CJ; Miquel, R; Miranda, V; Mohr, JJ; Muir, J; Nichol, RC; Nord, B; Ogando, RLC; Plazas, AA; Raveri, M | Abstract: © 2019 American Physical Society. We present constraints on extensions of the minimal cosmological models dominated by dark matter and dark energy, ΛCDM and wCDM, by using a combined analysis of galaxy clustering and weak gravitational lensing from the first-year data of the Dark Energy Survey (DES Y1) in combination with external data. We consider four extensions of the minimal dark energy-dominated scenarios: (1) nonzero curvature ωk, (2) number of relativistic species Neff different from the standard value of 3.046, (3) time-varying equation-of-state of dark energy described by the parameters w0 and wa (alternatively quoted by the values at the pivot redshift, wp, and wa), and (4) modified gravity described by the parameters μ0 and ς0 that modify the metric potentials. We also consider external information from Planck cosmic microwave background measurements; baryon acoustic oscillation measurements from SDSS, 6dF, and BOSS; redshift-space distortion measurements from BOSS; and type Ia supernova information from the Pantheon compilation of datasets. Constraints on curvature and the number of relativistic species are dominated by the external data; when these are combined with DES Y1, we find ωk=0.0020-0.0032+0.0037 at the 68% confidence level, and the upper limit Neffl3.28(3.55) at 68% (95%) confidence, assuming a hard prior Neffg3.0. For the time-varying equation-of-state, we find the pivot value (wp,wa)=(-0.91-0.23+0.19,-0.57-1.11+0.93) at pivot redshift zp=0.27 from DES alone, and (wp,wa)=(-1.01-0.04+0.04,-0.28-0.48+0.37) at zp=0.20 from DES Y1 combined with external data; in either case we find no evidence for the temporal variation of the equation of state. For modified gravity, we find the present-day value of the relevant parameters to be ς0=0.43-0.29+0.28 from DES Y1 alone, and (ς0,μ0)=(0.06-0.07+0.08,-0.11-0.46+0.42) from DES Y1 combined with external data. These modified-gravity constraints are consistent with predictions from general relativity.