论文标题
在没有声音范围的情况下确定哈勃常数：CMB镜头的测量
Determining the Hubble Constant without the Sound Horizon Scale: Measurements from CMB Lensing
论文作者
论文摘要
如果假定假定flank $λ$ CDM宇宙学模型，则目前从宇宙距离梯子中对哈勃常数（$ h_0 $）的测量值与来自CMB和其他高红移数据集的值相关。这种张力的少数有希望的理论分辨率之一是调用新物理学，以改变早期宇宙中的声音范围。这可以使$ H_0 $上的CMB和BAO限制与本地测量更好地达成一致性。在本文中，我们讨论了如何通过CMB制作Hubble常数的测量，而无需使用Sound Horizon量表$ R_S $的信息。特别是，我们展示了CMB镜头功率谱的测量结果如何与$ H_0 $的有趣约束一起在$ H_0 $上加上$ H_0 $的限制，并结合了超级新闻或Galaxy弱透镜的测量，这限制了物质密度参数。限制是由CMB镜头功率谱对物质辐射平等（投影）的敏感性产生的；该量表可能对新物理学的依赖性与声音范围不同。通过对具有保守外部先验的普朗克和万神殿超新星的当前CMB镜头数据的分析，我们得出了$ r_s $独立的约束$ H_0 = 73.5 = 73.5 \ pm 5.3 $ km/s/s/mpc。对未来CMB调查的预测表明，CMB镜头的改进限制超出$σ（H_0）= 3 $ km/s/mpc的误差将很困难，尽管对银河功率谱应用类似的方法可能允许进一步改进。
Measurements of the Hubble constant, $H_0$, from the cosmic distance ladder are currently in tension with the value inferred from Planck observations of the CMB and other high redshift datasets if a flat $Λ$CDM cosmological model is assumed. One of the few promising theoretical resolutions of this tension is to invoke new physics that changes the sound horizon scale in the early universe; this can bring CMB and BAO constraints on $H_0$ into better agreement with local measurements. In this paper, we discuss how a measurement of the Hubble constant can be made from the CMB without using information from the sound horizon scale, $r_s$. In particular, we show how measurements of the CMB lensing power spectrum can be used to place interesting constraints on $H_0$ when combined with measurements of either supernovae or galaxy weak lensing, which constrain the matter density parameter. The constraints arise from the sensitivity of the CMB lensing power spectrum to the horizon scale at matter-radiation equality (in projection); this scale could have a different dependence on new physics than the sound horizon. From an analysis of current CMB lensing data from Planck and Pantheon supernovae with conservative external priors, we derive an $r_s$-independent constraint of $H_0 = 73.5\pm 5.3$ km/s/Mpc. Forecasts for future CMB surveys indicate that improving constraints beyond an error of $σ(H_0) = 3$ km/s/Mpc will be difficult with CMB lensing, although applying similar methods to the galaxy power spectrum may allow for further improvements.
