发表机构
Sharif University of Technology; Research Center for High Energy Physics, Department of Physics, Sharif University of Technology（谢里夫理工大学; 谢里夫理工大学物理系高能物理研究中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
基于 DESI 数据，本文提出非局部引力的局域极限通过引力磁化率 S(z) 自然解释暗能量状态方程在 z≈0.4 处的幻影穿越，并给出对应关系与数据拟合，发现 S(z) 存在特征性低红移凹陷。
AI 中文摘要
暗能量光谱仪（DESI）的第二次数据发布基于超过一千四百万个星系和类星体，其数据偏好于一个状态方程为动力学形式的暗能量组分。在这种行为的二参数最简描述中，即 Chevallier-Polarski-Linder (CPL) 参数化，数据支持 $w_0>-1$、$w_a<0$ 的象限，这意味着状态方程在红移 $z\simeq0.4$ 处穿越幻影分界线 $w=-1$。我们表明，非局部引力的局域极限——一种由标量函数引力磁化率 $S(x)$ 支配的广义相对论的遥平行推广——为此提供了一个自然的解释。在该模型中，宇宙学常数是不被允许的；暗能量必然是动力学的。观测者所见的幻影穿越是由 $S(z)$ 的时间演化所产生的有效现象。我们建立了一个对应关系：对于每一个具有状态方程 $w(z)$ 的广义相对论暗能量模型，都存在一个对应的修正 TEGR 宇宙学，其中 $w=-1$ 且具有适当的磁化率 $S(z)$，两者在背景膨胀层面上是不可区分的。我们构造了能够重现 DESI 数据所青睐的 CPL 行为的磁化率函数，并使用玻尔兹曼求解器代码将模型与 CMB、BAO 和 SNe 的联合数据进行了对比。恢复出的磁化率在 $z\simeq0.4$ 处呈现出一个特征性的低红移凹陷，其深度为 $\beta = -0.025 \pm 0.007$，并且其导数在等于幻影穿越时代的红移处改变符号。
英文摘要
The second data release of the Dark Energy Spectroscopic Instrument (DESI), based on more than fourteen million galaxies and quasars, prefers a dark energy component whose equation of state is dynamical. In the simplest two-parameter description of this behavior, the Chevallier--Polarski--Linder (CPL) parametrization, the data favor the quadrant $w_0>-1$, $w_a<0$, which implies that the equation of state crosses the phantom divide $w=-1$ at a redshift $z\simeq0.4$. We show that the local limit of nonlocal gravity, a teleparallel extension of general relativity governed by a scalar function called gravitational susceptibility $S(x)$, offers a natural explanation. In this model a cosmological constant is not allowed; dark energy is necessarily dynamical. The phantom crossing seen by an observer is an effective phenomenon generated by the time evolution of $S(z)$. We establish a correspondence: to every general-relativistic dark energy model with equation of state $w(z)$, there corresponds a modified TEGR cosmology with $w=-1$ and a suitable susceptibility $S(z)$ that are indistinguishable at the level of the background expansion. We construct the susceptibility functions that reproduce the CPL behavior favored by DESI data, and we confront the model with the combined CMB,BAO, and SNe data using Boltzmann solver codes. The recovered susceptibility displays a characteristic low-redshift dip with depth $β= -0.025 \pm 0.007$ at $z\simeq 0.4 $, and its derivative changes sign at a redshift equal to the phantom-crossing epoch.
Comments13 pages, 4 figures, 2 tables. Updated references and minor improvements
