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arXiv 2201.11623astro-ph.COgr-qchep-th
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用晚期暗能量同时解决$H_0$和$σ_8$张力

Simultaneously solving the $H_0$ and $σ_8$ tensions with late dark energy

Lavinia Heisenberg, Hector Villarrubia-Rojo, Jann Zosso

备注：
4 pages, 2 figures, submission to PRL
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摘要：

在一个模型独立的方法，我们推导出通用的条件，任何后期修改的$Λ$ CDM扩展历史必须满足，以始终解决$H_0$和$σ_8$紧张局势。我们的结果是完全分析的，该方法仅仅是基于假设，从$Λ$ CDM的后期偏差仍然很小。对于在膨胀历史和引力耦合常数中编码了偏差的暗能量流体的具体情况，我们给出了其状态方程的必要条件。解决$H_0$和$σ_8$张力要求$w(z)$必须跨越体模分界，如果$G_\text{eff}=G$。另一方面，对于$G_\text{eff}=G+δG(z)$和$w(z)\leq -1$，要求$\displaystyle \frac{δG(z)}{G}<α(z)\frac{δH(z)}{H(z)}<0$在某些红移$z$。

英文摘要：

In a model independent approach, we derive generic conditions that any late time modification of the $Λ$CDM expansion history must satisfy in order to consistently solve both the $H_0$ and the $σ_8$ tensions. Our results are fully analytical and the method is merely based on the assumption that the late-time deviations from $Λ$CDM remain small. For the concrete case of a dark energy fluid with deviations encoded in the expansion history and the gravitational coupling constant, we present necessary conditions on its equation of state. Solving both the $H_0$ and $σ_8$ tensions requires that $w(z)$ must cross the phantom divide if $G_\text{eff}=G$. On the other hand, for $G_\text{eff}=G+δG(z)$ and $w(z)\leq -1$, it is required that $\displaystyle \frac{δG(z)}{G}<α(z)\frac{δH(z)}{H(z)}<0$ at some redshift $z$.

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