AI 中文总结
该研究结合 DESI DR2 等观测数据，约束与非冷暗物质耦合的 Barrow 全息暗能量模型，发现暗物质近无压强、暗能量高于幻像分界，且数据集未偏好该模型与 $\boldsymbol{\tau}$CDM 中的任一者。
AI 中文摘要
我们在空间平坦的 Friedmann-Lemaître-Robertson-Walker 宇宙中研究 Barrow 全息暗能量的宇宙学可行性，该宇宙中暗物质分量允许具有非零压强，由常数状态方程参数 $w_{m}$ 表征。通过将未来事件视界作为红外截断，我们推导了描述背景空间宇宙动力学的主方程。我们结合 DESI DR2 的重子声学振荡数据、三类不同的 Ia 型超新星测量星表以及宇宙计时器数据，对该模型进行晚宇宙学数据约束。对于 PantheonPlus、Union3.0 和 DES-Dovekie 超新星数据集，暗物质状态方程分别被约束为 $w_{m}=0.033_{-0.030}^{+0.045}$、$0.009_{-0.041}^{+0.047}$ 和 $0.033_{-0.029}^{+0.042}$，因此在 $2\boldsymbol{\tau}$ 范围内恢复了无压强极限。另一方面，由于 $\boldsymbol{\tau}-w_{m}$ 简并，Barrow 指数仅受到弱约束。暗能量状态方程在探测到的整个红移范围内始终高于幻像分界。最后，与 $\boldsymbol{\tau}$CDM 模型的统计参数比较显示，$\boldsymbol{\tau}\text{AIC}$ 分别为 +2.23、+0.75 和 +1.38，而贝叶斯证据的 $\boldsymbol{\tau}\text{ln}Z$ 分别为 -0.63、+0.47 和 -0.13，表明本分析中使用的数据集未表现出对任一模型的偏好。最后讨论了其与对应 Tsalis 全息暗能量模型的关系。
英文摘要
We investigate the cosmological viability of Barrow holographic dark energy in a spatially flat Friedmann--Lema\^ıtre--Robertson--Walker universe in which the dark matter component is allowed to have a non-zero pressure, characterized by a constant equation-of-state parameter $w_{m}$. By considering the future event horizon as the infrared cutoff, we derive the master equation, which describes the cosmological dynamics for the background space. We constrain the model against late-time data, combining the baryon acoustic oscillation from DESI DR2 with three different catalogues for the Type Ia Supernova measurements and the Cosmic Chronometers. The dark matter equation of state is constrained to $w_{m}=0.033_{-0.030}^{+0.045}$, $0.009_{-0.041}^{+0.047}$, and $0.033_{-0.029}^{+0.042}$, for the PantheonPlus, the Union3.0 and the DES-Dovekie supernova datasets respectively. Therefore, the pressureless limit is recovered within the $2σ$ regime. On the other hand, the Barrow exponent is weakly constrained, due to the $Δ-w_{m}$ degeneracy. The dark energy equation of state remains above the phantom divide throughout the redshift range probed. Finally, in the comparison of the statistical parameters with that of $Λ$CDM, it follows $Δ\mathrm{AIC}=+2.23$, $+0.75$, and $+1.38$, $\ $while for the Bayesian evidence we find $Δ\ln Z=-0.63$, $+0.47$, and $-0.13$, which suggest that the datasets considered in this analysis do not have a preferred model. Finally the relation with the corresponding Tsalis holographic dark energy model is discussed.
Comments11 pages, 4 figures, 3 tables, Comments welcome
