论文标题
为什么仅仅减少宇宙声音范围无法完全解决哈勃张力
Why reducing the cosmic sound horizon alone can not fully resolve the Hubble tension
论文作者
论文摘要
在标准的$λ$ CDM（称为哈勃张力）的背景下，普朗克从宇宙微波背景测量中推断出的本地测量的宇宙膨胀率与从宇宙微波背景测量中的不匹配已成为宇宙学中最紧迫的问题之一。为了解决这种张力，已经提出了$λ$ CDM模型的大量修订。他们中的许多人介绍了新的物理，例如早期的暗能量，标准模型中微子部门的修改，额外的辐射，原始磁场或不同的基本常数，目的是减少重组$ r _ {\ star} $时的声音范围。我们在这里证明，任何仅降低$ r _ {\ star} $的模型永远无法完全解决哈勃张力，同时与其他宇宙数据集保持一致。我们明确地表明，具有较低物质密度$ω_mh^2 $较低值的模型，并具有baryon声学振荡的观察结果，而具有较大$ω_mh^2 $的型号则与Galaxy弱透镜数据产生张力。
The mismatch between the locally measured expansion rate of the universe and the one inferred from the cosmic microwave background measurements by Planck in the context of the standard $Λ$CDM, known as the Hubble tension, has become one of the most pressing problems in cosmology. A large number of amendments to the $Λ$CDM model have been proposed in order to solve this tension. Many of them introduce new physics, such as early dark energy, modifications of the standard model neutrino sector, extra radiation, primordial magnetic fields or varying fundamental constants, with the aim of reducing the sound horizon at recombination $r_{\star}$. We demonstrate here that any model which only reduces $r_{\star}$ can never fully resolve the Hubble tension while remaining consistent with other cosmological datasets. We show explicitly that models which achieve a higher Hubble constant with lower values of matter density $Ω_m h^2$ run into tension with the observations of baryon acoustic oscillations, while models with larger $Ω_mh^2$ develop tension with galaxy weak lensing data.
