共形相互作用暗能量与早期和晚期测量
Conformally Interacting Dark Energy with Early and Late-Time Measurements
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中文总结 AI 辅助
本研究通过共形相互作用暗能量模型，结合早期和晚期宇宙学数据，探讨其缓解哈勃常数和结构增长张力问题的潜力。
中文摘要 AI 辅助
研究了共形相互作用暗能量（CIDE）模型，该模型通过共形变换引入一个标量场来表示暗能量（DE）与暗物质（DM）的耦合，从而产生一类标量-张量理论。相互作用项 $Q$ 表示暗区之间的能量流动，其与 DM 流体的能量动量张量的迹成正比，即 $Q = \frac{C'(\phi)}{2C(\phi)} g^{\mu\nu} T^{\mathrm{DM}}_{\mu\nu}$，其中 $C(\phi)$ 是标量势（耦合）场的共形函数。我们假设幂律参数化 $C(\phi) \propto (1+\phi)^m$，其中 $m$ 是耦合参数，并确定 DM 和 DE 组分之间能量流动的方向和大小。DE 的动态性质通过两种共形相互作用情景建模：CIDE 和 $w$CIDE，其中 $w$ 是 DE 的状态方程参数。为了测试每个模型的可行性，我们使用早期和晚期宇宙学数据的组合对其进行约束，即：来自南极望远镜、普朗克 2018 和阿塔卡马宇宙学望远镜（DR6）的 CMB 测量（\texttt{CMB SPA}）；来自暗能量巡天（\texttt{DESI DR2 BAO}）的 BAO 数据；以及 Ia 型超新星距离汇编（\texttt{PantheonPlus, PantheonPlus + SH0ES, Union3} 和 \texttt{DES Dovekie}）。参数推断使用蒙特卡洛马尔可夫链（\texttt{MCMC}）模拟，采用 \texttt{COBAYA} 和修改后的 \texttt{CLASS}。进一步使用赤池信息准则（AIC）和贝叶斯信息准则（BIC）进行统计分析，以评估模型相对于标准宇宙学模型的可行性，并研究该模型缓解 $H_0$ 和 $S_8$ 张力的潜力。
英文摘要
The conformal interacting dark energy (CIDE) model is investigated by introducing a scalar field representing dark energy (DE) coupled to dark matter (DM) via a conformal transformation, thereby yielding a class of scalar-tensor theories. The interaction term ${Q}$, that indicts the flow of energy between the dark sectors is proportional to the trace of the energy momentum tensor of the DM fluid, $T^{\mathrm{DM}}_{μν}$, as ${Q}=\frac{C'(ϕ)}{2C(ϕ)}g^{μν}T^{\mathrm{DM}}_{μν}$, where $C(ϕ)$ is the conformal function of a scalar potential (coupling) field. We assume the power-law parametrization $C(ϕ)\propto (1+ϕ)^m$, with $m$ a coupling parameter, and determine the direction and magnitude of the energy flow between the DM and DE components. The dynamical nature of DE is modeled by the two conformal interacting scenarios, CIDE and $w$CIDE, with $w$ the DE equation of state parameter. To test the viability of each model, we constrain them using a combination of early- and late-time cosmological data, namely: CMB measurements from the South Pole Telescope, Planck 2018, and the Atacama Cosmology Telescope (DR6) (\texttt{CMB SPA}); BAO data from the Dark Energy Survey (\texttt{DESI DR2 BAO}); and Supernova Type Ia distance compilations (\texttt{PantheonPlus, PantheonPlus + SH0ES, Union3}, and \texttt{DES Dovekie}). Parameter inference is performed with Monte Carlo Markov Chain (\texttt{MCMC}) simulations using \texttt{COBAYA} and a modified \texttt{CLASS}. Further statistical analysis using the Akaike information criterion (AIC) and the Bayesian information criterion (BIC) is summarized to assess the viability of the model in comparison with the standard cosmological model, investigating the model's potential to alleviate the $H_0$ and $S_8$ tensions.
发表机构
- North-West University（西北大学）
- National Institute for Theoretical and Computational Sciences (NITheCS)（国家理论与计算科学研究所）
- Entoto Observatory and Research Center, Space Science and Geospatial Institute（恩托多观测与研究中心，空间科学与地理空间研究所）
- Instituto de Física Corpuscular (IFIC), CSIC-Universitat de València（粒子物理研究所（IFIC），西班牙科学院-瓦伦西亚大学）
- Departamento de Física Teórica and IPARCOS, Universidad Complutense de Madrid（理论物理系和IPARCOS，马德里康普顿斯大学）
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