Interacting dark energy from redshift-space galaxy clustering
Interacting dark energy from redshift-space galaxy clustering
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DOI：
10.1088/1475-7516/2021/10/004
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发表时间：
2021-06
影响因子：
6.4
通讯作者：
P. Carrilho;C. Moretti;B. Bose;K. Markovič;A. Pourtsidou
中科院分区：
文献类型：
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作者：
P. Carrilho;C. Moretti;B. Bose;K. Markovič;A. Pourtsidou
相互作用暗能量模型已经被提出作为ΛCDM的有吸引力的替代方案。即将到来的第四阶段星系聚类调查将限制这些模型，但它们需要在轻度非线性尺度上对星系功率谱多极子进行精确建模。在这项工作中，我们考虑了一个简单的1-参数扩展到wCDM的暗散射模型-只添加A，它描述了一个纯粹的暗能量和暗物质之间的动量交换。然后，我们提供了一个全面的比较三种方法的建模非线性，同时包括这种暗区耦合的影响。我们的非线性建模基于两个最流行的扰动理论方法：TNS和EFTofLSS。为了测试建模的有效性和精度，我们使用模拟数据进行MCMC分析，模拟数据对应于ΛCDM基准宇宙学和第四阶段调查规范，在两个红移箱，z=0.5和z=1。我们发现，最复杂的EFTofLSS为基础的模型研究，更适合在这两个，描述模拟数据到较小的规模，并提取最多的信息。使用这个模型，我们预测暗能量状态方程w和相互作用参数A的不确定性，发现在z=0.5时分析的σ w=0.06和σ A =1.1 B/GeV，在z=1时分析的σ w =0.06和σ A =2.0 B/GeV。此外，我们表明，如果非线性建模不正确，将发生高达3σ的奇异暗能量的错误检测，这表明了验证阶段对准确解释测量的重要性。
Interacting dark energy models have been proposed as attractive alternatives to ΛCDM. Forthcoming Stage-IV galaxy clustering surveys will constrain these models, but they require accurate modelling of the galaxy power spectrum multipoles on mildly non-linear scales. In this work we consider a dark scattering model with a simple 1-parameter extension to wCDM — adding only A, which describes a pure momentum exchange between dark energy and dark matter. We then provide a comprehensive comparison of three approaches of modeling non-linearities, while including the effects of this dark sector coupling. We base our modeling of non-linearities on the two most popular perturbation theory approaches: TNS and EFTofLSS. To test the validity and precision of the modelling, we perform an MCMC analysis using simulated data corresponding to a ΛCDM fiducial cosmology and Stage-IV surveys specifications in two redshift bins, z=0.5 and z=1. We find the most complex EFTofLSS-based model studied to be better suited at both, describing the mock data up to smaller scales, and extracting the most information. Using this model, we forecast uncertainties on the dark energy equation of state, w, and on the interaction parameter, A, finding σ_w=0.06 and σ A =1.1 b/GeV for the analysis at z=0.5 and σ w =0.06 and σ A =2.0 b/GeV for the analysis at z=1. In addition, we show that a false detection of exotic dark energy up to 3σ would occur should the non-linear modelling be incorrect, demonstrating the importance of the validation stage for accurate interpretation of measurements.