$H_0$之外的麻烦和新的宇宙三角形
The trouble beyond $H_0$ and the new cosmic triangles
摘要：
使用超新星的距离阶梯得出的哈勃常数$H_0$值高于从宇宙微波背景测量和星系巡天中推断出的值，这种差异后来被称为“哈勃张力”。这激发了对标准宇宙学模型扩展的探索，在标准宇宙学模型中，可以从CMB测量和星系巡天中获得更高的$H_0$值。然而，问题不仅限于$H_0$，这样的修改也会影响其他量。特别是，它们对宇宙时间的影响通常被忽视。我们在这里探讨宇宙年龄$t_{\rm U}$的测量，如最近的推断，从年龄最老的球状星团，可能有潜在的解决方案的$H_0$张力的影响。从CMB和星系巡天中推断出的$H_0$值与CMB退耦（或辐射阻力）时的声视界有关，但它也与物质密度和$t_{\rm U}$有关。鉴于这一观察结果，我们展示了独立于模型的测量如何支持或不支持针对哈勃张力提出的新物理解决方案。最后，我们认为，宇宙学测量今天提供的限制，在一个给定的宇宙学模型，代表一个过度约束的系统，提供了一个强大的诊断工具的一致性。我们建议使用三元图，同时可视化的独立约束的关键量相关的$H_0$像$t_{\rm U}$，在辐射阻力的声音地平线，和物质密度参数。我们设想，这种表示将有助于找到一个解决方案的麻烦和超越$H_0$。
英文摘要：
The distance ladder using supernovae yields higher values of the Hubble constant $H_0$ than those inferred from measurements of the cosmic microwave background (CMB) and galaxy surveys, a discrepancy that has come to be known as the `Hubble tension'. This has motivated the exploration of extensions to the standard cosmological model in which higher values of $H_0$ can be obtained from CMB measurements and galaxy surveys. The trouble, however, goes beyond $H_0$; such modifications affect other quantities, too. In particular, their effects on cosmic times are usually neglected. We explore here the implications that measurements of the age $t_{\rm U}$ of the Universe, such as a recent inference from the age of the oldest globular clusters, can have for potential solutions to the $H_0$ tension. The value of $H_0$ inferred from the CMB and galaxy surveys is related to the sound horizon at CMB decoupling (or at radiation drag), but it is also related to the matter density and to $t_{\rm U}$. Given this observation, we show how model-independent measurements may support or disfavor proposed new-physics solutions to the Hubble tension. Finally, we argue that cosmological measurements today provide constraints that, within a given cosmological model, represent an over-constrained system, offering a powerful diagnostic tool of consistency. We propose the use of ternary plots to simultaneously visualize independent constraints on key quantities related to $H_0$ like $t_{\rm U}$, the sound horizon at radiation drag, and the matter density parameter. We envision that this representation will help find a solution to the trouble of and beyond $H_0$.
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