发表机构
GLA University; IILM University; University of Technology and Applied Sciences（GLA大学; IILM大学; 技术与应用科学大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
利用神经网络对Kaniadakis全息暗能量进行模型无关重建，并用Pantheon+SH0ES数据约束，发现其与ΛCDM相比无统计优势。
AI 中文摘要
我们利用在模拟Ia型超新星上训练的人工神经网络，对采用未来事件视界红外截断的Kaniadakis全息暗能量（KHDE）进行了模型无关重建。基于基准KHDE模型（c=1.15，β=0.30，Ω_m=0.30，H_0=69.6 km/s/Mpc）生成了模拟Pantheon（N=1048）和Pantheon+SH0ES（N=1701，含77个造父变星校准）数据集。Bootstrap深度集成将红移映射到视星等μ(z)并加入固有散射；通过解析导数得到H(z)和w(z)。Pantheon+SH0ES优于Pantheon：散射分别为0.018和0.048星等；H(z)精度在0.1<z<1.2范围内分别为3.2%和6.0%。造父变星校准对H_0至关重要：校准后为72.0±2.0 km/s/Mpc，未校准为64.8±6.0 km/s/Mpc。直接拟合和MCMC恢复了注入的Ω_m和H_0；β不受约束（在μ(z)中信号为0.009星等）。将方法应用于真实Pantheon+SH0ES数据（1657个超新星，包含完整统计和系统协方差），复现了已发表的ΛCDM基准结果。KHDE拟合给出：Ω_m=0.254，H_0=73.12 km/s/Mpc；β<0.63（95%置信水平）。ΔAIC=+3.8，ΔBIC=+14.6：表明KHDE相对于ΛCDM没有优势。计算在Azure ML Studio上运行。
英文摘要
Holographic dark energy ties the dark-energy density to an infrared length. We study new Tsallis holographic dark energy (NTHDE), built on the exponential Tsallis entropy, with the local Granda-Oliveros (GO) cutoff $L^{-2}=αH^2+γ\dot H$ in a spatially curved universe. Writing the background as an autonomous system for $(Ω_d,u,Ω_k)$, we obtain four exact results. (i) In the closed-form solution without the Tsallis deformation, the dark energy splits into a matter-like and a curvature-like part. (ii) Because the GO cutoff lacks the term $k/a^2$ of the Ricci scalar, the coefficient of $(1+z)^2$ in $H^2/H_0^2$ is $R_kΩ_{k0}$ with $R_k=(1-α+γ)^{-1}>1$, while distances and the Clarkson-Bassett-Lu test return $Ω_{k0}$; the Ricci completion restores $R_k=1$. (iii) Big-bang nucleosynthesis locks the matter-era dark-energy fraction to $1/(1+3|w_{\rm GO}|)$, where $w_{\rm GO}$ is the equation of state of the GO mode. (iv) The finite-time fold singularity of the flat model survives curvature. Against Pantheon+SH0ES supernovae, 32 cosmic chronometers and DESI DR2 BAO, curved GO-NTHDE gives $Ω_{k0}=-0.001^{+0.041}_{-0.043}$, consistent with flatness, and $Δχ^2=-2.82$ relative to flat $Λ$CDM, but the Bayesian evidence prefers flat $Λ$CDM ($\ln B=-2.66\pm0.24$), and allowing curvature costs $\ln B=-1.39\pm0.25$. The data cannot yet measure $R_k$: the GO and Ricci cutoffs fit equally well ($\ln B=+0.28\pm0.26$). With Union3 supernovae the model is on a par with $Λ$CDM ($\ln B=+0.53$). A fraction 0.91 of the posterior reaches the finite-time fold.
Comments48 pages, 14 figures, 7 tables
