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arXiv 1811.04083astro-ph.COhep-ph
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早期的暗能量可以解决哈勃的张力

Early Dark Energy Can Resolve The Hubble Tension

Vivian Poulin, Tristan L. Smith, Tanvi Karwal, Marc Kamionkowski

备注：
v1: 4p+appendix, 3 figures. v2: small changes, notably estimates of bayesian evidence. matches the version published in PRL
发表信息：
Phys. Rev. Lett. 122, 221301 (2019)
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摘要：

早期的暗能量（EDE）在早期表现得像宇宙学常数（红移$z\gtrsim3000$），然后像辐射一样稀释，或者在后期更快地稀释，可以解决哈勃张力。在这些模型中，在去耦的声音地平线减少，从而导致更大的值的哈勃参数$H_0$推断从宇宙微波背景（CMB）。我们考虑两个物理模型，这种EDE，一个涉及振荡的标量场和另一个慢滚动场。我们进行了详细的计算在这些模型中的扰动的演变。一个马尔可夫链蒙特卡罗搜索的参数空间的EDE参数，结合标准的宇宙学参数，确定区域中，从{ \it普朗克} CMB数据推断的$H_0$同意与SH 0 ES本地测量。在这些宇宙学中，目前的重子声学振荡和超新星数据描述成功的\LCDM，而适合{ \it普朗克}数据略有改善。未来的CMB和大型结构调查将进一步探讨这种情况。

英文摘要：

Early dark energy (EDE) that behaves like a cosmological constant at early times (redshifts $z\gtrsim3000$) and then dilutes away like radiation or faster at later times can solve the Hubble tension. In these models, the sound horizon at decoupling is reduced resulting in a larger value of the Hubble parameter $H_0$ inferred from the cosmic microwave background (CMB). We consider two physical models for this EDE, one involving an oscillating scalar field and another a slowly-rolling field. We perform a detailed calculation of the evolution of perturbations in these models. A Markov Chain Monte Carlo search of the parameter space for the EDE parameters, in conjunction with the standard cosmological parameters, identifies regions in which $H_0$ inferred from {\it Planck} CMB data agrees with the SH0ES local measurement. In these cosmologies, current baryon acoustic oscillation and supernova data are described as successfully as in \LCDM, while the fit to {\it Planck} data is slightly improved. Future CMB and large-scale-structure surveys will further probe this scenario.

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