标题： 关于“宇宙校准张力”在$H_0$之外的含义以及早期和晚期新物理之间的协同作用 显示英文标题

标题： On the implications of the `cosmic calibration tension' beyond $H_0$ and the synergy between early- and late-time new physics

摘要： “宇宙校准张力”是基于重子声学振荡（BAO）构建的宇宙学距离阶梯与通过普朗克/$\Lambda$冷暗物质声音视差（$r_s$）校准的距离阶梯之间的$> 5\sigma$差异，以及通过 S$H_0$ES 绝对星等校准的 Ia 型超新星（SN1a）之间的差异，假设距离对偶关系（DDR）成立。 在本研究中，我们强调这种张力超出哈勃常数$H_0$值的影响，以及对超越$\Lambda$冷暗物质物理的意义。 最重要的是，它意味着更大的物理物质密度 $\omega_m\equiv \Omega_m h^2$，因为从晚期数据中，物质密度的分数 $\Omega_m$ 和 $h\equiv H_0/100$ km/s/Mpc 都被很好地约束了。 因此，再结合时期的新物理必须能够降低 $r_s$，同时要么减少 $\Omega_m$的值，要么增加 $\omega_m$的值。 假设一个$\Lambda$类 CDM 的原始功率谱，这必然会导致聚类幅度$\sigma_8$的增加。 晚期膨胀历史中对$\Lambda$CDM 的偏离无法解决校准器矛盾，但可以帮助缓解物质密度和$\sigma_8$所需的偏移量：从这个意义上说，早期和晚期新物理的结合可能有助于缓解矛盾。 更准确地说，修改再结合前膨胀历史的模型可以在不需要额外修改的情况下容纳$\omega_m$的增加。 只有影响再结合的模型需要在晚期引入额外的偏离才能成功。 因此，“宇宙校准矛盾”要么指向对再结合前膨胀历史的针对性修改，要么指向影响多个宇宙时期的更广泛变化。 显示英文摘要

摘要： The `cosmic calibration tension' is a $> 5\sigma$ discrepancy between the cosmological distance ladder built from baryonic acoustic oscillations (BAO) calibrated by the Planck/$\Lambda$CDM sound horizon ($r_s$) and Type Ia supernovae (SN1a) calibrated instead with the S$H_0$ES absolute magnitude, assuming the distance-duality relationship (DDR) holds. In this work, we emphasize the consequences of this tension beyond the value of the Hubble constant $H_0$, and the implications for physics beyond $\Lambda$CDM. Of utmost importance, it implies a larger physical matter density $\omega_m\equiv \Omega_m h^2$, as both the fractional matter density $\Omega_m$ and $h\equiv H_0/100$ km/s/Mpc are well constrained from late-time data. New physics in the pre-recombination era must thus be able to decrease $r_s$ while either reducing the value of $\Omega_m$, or increasing the value of $\omega_m$. Assuming a $\Lambda$CDM-like primordial power spectrum, this necessarily results in an increase in the clustering amplitude $\sigma_8$. Deviations from $\Lambda$CDM in the late-time expansion history cannot resolve the calibrator tension but can help relax the required shifts to the matter density and $\sigma_8$: it is in that sense that a combination of early and late-time new physics may help alleviate the tension. More precisely, models that modify the pre-recombination expansion history can accommodate the increase in $\omega_m$ without the need for additional modifications. It is those models which only affect recombination that require additional deviations at late-times to be successful. Hence, the `cosmic calibration tension' points either to a targeted modification of the pre-recombination expansion history, or to a broader change affecting multiple cosmic epochs.