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 ΛCDM, known as the Hubble tension, has become one of the most pressing problems in cosmology. A large number of amendments to the ΛCDM 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_⋆. We demonstrate here that any model which only reduces r_⋆ 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_mh² run into tension with the observations of baryon acoustic oscillations, while models with larger Ω_mh² develop tension with galaxy weak lensing data.

局部测量的宇宙膨胀率与普朗克在标准 ΛCDM 背景下从宇宙微波背景测量推断的膨胀率之间的不匹配，即哈勃张力，已成为宇宙学中最紧迫的问题之一。为了解决这种张力，已经提出了对 ΛCDM 模型的大量修正。他们中的许多人引入了新的物理学，例如早期暗能量、标准模型中微子扇区的修改、额外辐射、原始磁场或变化的基本常数，目的是减少重组r _{⋆ 时}的声界。我们在这里证明，任何只减少r 的_模型在与其他宇宙学数据集保持一致的同时，永远无法完全解决哈勃张力。我们明确地表明，在物质密度 Ω _m h ²值较低的情况下，实现更高哈勃常数的模型会因重子声学振荡的观察而产生张力，而具有较大 Ω _m h ^{2 的}模型会因星系弱透镜数据而产生张力。