AI 中文总结
利用高斯过程，基于哈勃和DESI数据重建狄拉克-玻恩-英费尔德标量场的暗能量模型，得出哈勃常数后验估计值，评估不同标量场势可行性，进行相关分析并讨论模型推广及结果意义。
AI 中文摘要
在本研究中，我们使用高斯过程（GP）从哈勃数据集（32个超新星+26个重子声学振荡）和DESI数据集重建作为狄拉克-玻恩-英费尔德（DBI）标量场的暗能量（DE）。由于GP是一种使用数据重建函数及其导数的非参数且与模型无关的方法，我们对DE状态方程、DE密度参数和势的重建不假设任何特定的宇宙学模型。通过GP重建的膨胀历史的蒙特卡罗实现，我们得出哈勃常数的后验估计值，得到$H_0 = 69.53 \pm 2.68$ km s$^{-1}$ Mpc$^{-1}$。该方法仅依赖数据和GP先验提供了对$H_0$的完全与模型无关的估计，并提供了一个无偏中间值，有助于重新评估普朗克- SH0ES张力。利用标量势作为场$\phi$的函数的重建轮廓及其相关不确定性，我们进行卡方曲线拟合程序以评估四种不同标量场势（如指数势、幂律势、自由场（二次）和希格斯样势）的可行性。这使我们能够确定哪种势最适合重建数据。我们还采用MCMC分析对与每个势相关的模型参数进行定量约束。此外，我们对所有四种势进行$\chi^2$分析并评论它们各自的拟合优度。最后，我们讨论了我们与模型无关框架的可能推广，并概述了我们研究结果的现象学意义。
英文摘要
In this study, we reconstruct the dark energy (DE) as a Dirac-Born-Infeld (DBI) scalar field from the Hubble dataset (32 CC + 26 BAO) and the DESI dataset using the Gaussian process (GP). As the GP is a non-parametric and model-independent way to reconstruct a function and its derivative using the data, our reconstruction of the DE equation of state, the DE density parameter, and the potential does not assume any particular model of cosmology. Using Monte Carlo realizations of the GP-reconstructed expansion history, we derive a posterior estimate of the Hubble constant, obtaining $H_0 = 69.53 \pm 2.68$ km s$^{-1}$ Mpc$^{-1}$. This method offers a fully model-independent estimate of $H_0$, relying only on data and GP priors, and provides an unbiased intermediate value useful for reassessing the Planck-SH0ES tension. Using the reconstructed profiles of the scalar potential as a function of the field $ϕ$, along with their associated uncertainties, we perform a chi-square curve fitting procedure to assess the viability of four different scalar field potentials, such as Exponential, Power-law, Free Field (quadratic), and Higgs-like potential. This allows us to identify which potential best fits the reconstructed data. We also employ MCMC analysis to place quantitative constraints on the model parameters associated with each potential. Furthermore, we do a $χ^2$ analysis for all four potentials and comment on the goodness of the fit for each of them. Finally, we discuss possible generalizations of our model-independent framework and outline the phenomenological implications of our findings.
CommentsJHEAp published version
Journal refJournal of High Energy Astrophysics, 55 (2027) 100730
DOI：10.1016/j.jheap.2026.100730
