AI 中文总结
该研究利用宇宙计时器、超新星、BAO和RSD增长测量等晚期观测，对HDE、ADE和RDE三种全息暗能量模型进行限制，通过贝叶斯马尔可夫链蒙特卡罗参数估计和AIC、BIC比较模型，结果显示三种模型均未显著缓解哈勃张力，HDE现象学行为最平衡。
AI 中文摘要
我们使用宇宙计时器、Ia型超新星（SNe Ia）、DESI DR2重子声学振荡（BAO）和红移空间畸变（RSD）增长测量的晚期观测，对三种全息启发的暗能量模型进行限制，即全息暗能量（HDE）、年龄图暗能量（ADE）和里奇暗能量（RDE）。考虑了五种数据组合。我们进行贝叶斯马尔可夫链蒙特卡罗参数估计，并通过AIC和BIC比较模型。在包含BAO的组合中，HDE给出了一些参数值，表明其膨胀历史接近德西特边界而非稳健的幻像区域。ADE产生了稳定的年龄图参数，而RDE给出了一些参数值并持续支持低物质密度。将$r_d$视为自由参数揭示了$H_0$与$r_d$之间的强负相关，包含RSD的组合通过$f\sigma_8(z)$提供了增长水平的一致性检查。这三种模型都没有显著缓解哈勃张力。总体而言，HDE在三种模型中表现出最平衡的现象学行为，尽管当前的晚期数据并没有决定性地偏好它超过ΛCDM。
英文摘要
We constrain three holographic-inspired dark energy models, namely holographic dark energy (HDE), agegraphic dark energy (ADE), and Ricci dark energy (RDE), using late-time observations from cosmic chronometers, Type Ia supernovae (SNe Ia), DESI DR2 baryon acoustic oscillations (BAO), and {redshift-space distortion (RSD) growth measurements}. Five data combinations are considered: $H(z)+$Pantheon+, $H(z)+$DESI DR2+Pantheon+, $H(z)+$DESI DR2+DES-Dovekie, $H(z)+$DESI DR2+DESY5, and {$H(z)+$DESI DR2+DES-Dovekie+RSD}. We perform Bayesian Markov chain Monte Carlo parameter estimation and compare the models with AIC and BIC. In the BAO-included combinations, HDE gives $H_0\simeq67.3$--$68.0~\mathrm{~km~s^{-1}~Mpc^{-1}}$, $Ω_{m0}\simeq0.270$--$0.272$, and $c\simeq1$, indicating an expansion history close to the de Sitter boundary rather than a robust phantom regime. ADE yields a stable agegraphic parameter $n\simeq2.78$--$2.81$, while RDE gives $γ\simeq0.53$--$0.55$ and persistently favors a low matter density, $Ω_{m0}\simeq0.215$--$0.219$. {Treating $r_d$ as a free parameter reveals a strong negative correlation between $H_0$ and $r_d$, and the RSD-included combination provides a growth-level consistency check through $fσ_8(z)$ without constituting a full perturbative stability analysis.} None of the three models significantly alleviates the Hubble tension. Overall, HDE shows the most balanced phenomenological behavior among the three models, although current late-time data do not decisively prefer it over $Λ\text{CDM}$.
Comments15 pages, 6 figures, submitted to EPJC
Journal refEuropean Physical Journal C, 86, 1042 (2026)
DOI：10.1140/epjc/s10052-026-16300-z
