研究早期暗能量对EDENS套件框架内大尺度结构的影响
Investigating The Effects of Early Dark Energy on Large-scale Structure Within the EDENS Suite
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中文总结 AI 辅助
本文利用EDENS套件开展EDE模拟，推导相关度量并构建星系模型，发现所选EDE模型与标准ΛCDM模型存在显著差异，或可用于区分两类模型，相关模拟数据已通过OpenCosmo门户发布。
中文摘要 AI 辅助
早期暗能量（EDE）模型被认为是解决所谓哈勃张力的可能方案，哈勃张力即早期和晚期哈勃常数测量值之间存在的差异。本文通过EDENS（早期暗能量N体模拟）套件，研究EDE对宇宙学大尺度结构探测的影响。EDENS套件通过增加体积和分辨率，大幅拓展了现有EDE模拟的适用范围。我们推导了多个关键度量，包括晕质量函数、非线性功率谱以及浓度-质量关系。此外，我们构建了一个晕占据分布模型，为模拟填充合成星系，这使我们能够测量星系-星系相关函数和星系偏置。我们选择了一个在多个探测中与观测结果一致、且能提升当前哈勃常数值以解决哈勃张力的EDE模型，该模型在标准ΛCDM模型基础上增加了3个参数，还需要对标准ΛCDM宇宙学参数的最佳拟合值进行小幅调整，以适配现有观测约束。我们发现标准ΛCDM模型与该EDE模型之间存在显著差异，表明部分所选度量或许可用于区分EDE与ΛCDM，未来观测将有助于进一步约束可能的宇宙学模型。我们通过OpenCosmo数据门户发布了模拟的输出结果。
英文摘要
Early Dark Energy (EDE) models have been suggested as a possible solution to the so-called Hubble Tension, a discrepancy of the measurement of the Hubble constant at early and late times. In this paper, we investigate the effects of EDE on large-scale structure probes of cosmology via the EDENS (Early Dark Energy N-body Simulations) suite. The EDENS suite extends the reach of available EDE simulations considerably by adding volume and resolution. We derive several key metrics, such as the halo mass function, the nonlinear power spectrum, and the concentration-mass relation. Furthermore, we implement a halo occupation distribution model to populate the simulations with synthetic galaxies. This allows us to measure the galaxy-galaxy correlation function and galaxy bias. We choose an EDE model that is consistent with observations across several probes and allows for the increase of the present day value of the Hubble constant to resolve the Hubble tension. This model adds three more parameters to the standard $Λ$CDM model. Additionally, it requires small shifts in the best-fit $Λ$CDM cosmological parameters to accommodate existing observational constraints. We find significant differences between the standard $Λ$CDM model and the EDE model, suggesting that some of our chosen metrics may allow us to distinguish EDE from $Λ$CDM, and future observations should help further constrain possible cosmological models. We release outputs from our simulations via the OpenCosmo data portal.
