2024/03/28 by Alex Krolewski, Will J. Percival, Krolewski, Alex +3 · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Cosmology and Gravitation Theories #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena
paper · pdf · doi:10.48550/arxiv.2403.19227
openalex publication_date 2024/03/28 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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 (BBN) calculations and the present-day CMB temperature to determine the physical baryon density Ωb h2. The baryon fraction Ωb/Ωm 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 Ωmh2 is then compared with the geometrical density Ωm from Alcock-Paczynski measurements from Baryon Acoustic Oscillations (BAO) and voids, to give H0. Including type Ia supernovae and uncalibrated BAO, we measure H0 = 67.1+6.3-5.3 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 H0 determinations, but near-future large-scale structure surveys will obtain 3--4× tighter constraints.