Krolewski Alex, Percival Will J, Woodfinden Alex
Perimeter Institute for Theoretical Physics, University of Waterloo, University of Waterloo, Waterloo Centre for Astrophysics, Waterloo, Ontario N2L 3G1, Canada; Department of Physics and Astronomy, Waterloo, Ontario N2L 3G1, Canada; and , 31 Caroline Street North, Waterloo, Ontario NL2 2Y5, Canada.
University of Waterloo, University of Waterloo, Waterloo Centre for Astrophysics, Waterloo, Ontario N2L 3G1, Canada and Department of Physics and Astronomy, Waterloo, Ontario N2L 3G1, Canada.
Phys Rev Lett. 2025 Mar 14;134(10):101002. doi: 10.1103/PhysRevLett.134.101002.
We introduce a new method for measuring the Hubble parameter from low-redshift large-scale observations that is independent of the comoving sound horizon. The method uses the baryon-to-photon ratio determined by the primordial deuterium abundance, together with big bang nucleosynthesis calculations and the present-day cosmic microwave background (CMB) temperature, to determine the physical baryon density Ω_{b}h^{2}. The baryon fraction Ω_{b}/Ω_{m} is measured using the relative amplitude of the baryonic signature in galaxy clustering measured by the Baryon Oscillation Spectroscopic Survey, scaling the physical baryon density to the physical matter density. The physical density Ω_{m}h^{2} is then compared with the geometrical density Ω_{m} from Alcock-Paczynski measurements from baryon acoustic oscillations (BAO) and voids to give H_{0}. Including type Ia supernovae and uncalibrated BAO, we measure H_{0}=67.1_{-5.3}^{+6.3} km s^{-1} Mpc^{-1}. We find similar results when varying analysis choices, such as measuring the baryon signature from the reconstructed correlation function or excluding supernovae or voids. This measurement is currently consistent with both the distance-ladder and CMB H_{0} determinations, but near-future large-scale structure surveys will obtain 3× to 4× tighter constraints.
我们介绍了一种从低红移大规模观测中测量哈勃参数的新方法，该方法独立于共动声视界。该方法利用由原初氘丰度确定的重子与光子比率，结合大爆炸核合成计算和当前的宇宙微波背景（CMB）温度，来确定物理重子密度Ω_bh²。利用重子振荡光谱巡天测量的星系团簇中重子特征的相对振幅来测量重子分数Ω_b/Ω_m，将物理重子密度按比例换算为物理物质密度。然后将物理密度Ω_mh²与通过重子声学振荡（BAO）和空洞的阿尔科克 - 帕钦斯基测量得到的几何密度Ω_m进行比较，从而得出H_0。包括Ia型超新星和未校准的BAO，我们测量得到H_0 = 67.1_{-5.3}^{+6.3} km s⁻¹ Mpc⁻¹。当改变分析选择时，例如从重建的相关函数测量重子特征或排除超新星或空洞，我们得到了类似的结果。目前该测量结果与距离阶梯法和CMB对H_0的测定结果均一致，但在不久的将来，大规模结构巡天将获得紧3倍到4倍的约束。
