LAUSR

The Hubble constant (H0) is a key parameter in cosmology, yet its precise value remains contentious due to discrepancies between early- and late-universe measurement methods, a problem known as the “Hubble tension.” In this study, we revisit the Cepheid-based distance ladder calibration, focusing on two potential sources of bias in the period-luminosity relation (PLR): (1) the assumed prior for the residual parallax offset of the Milky Way (MW) Cepheids and (2) systematic differences between Cepheid periods in anchor galaxies versus supernova host galaxies. To address the latter, we adopt two different strategies alongside a renewed MW Cepheid calibration. The first strategy involves resampling anchor and host Cepheids from a common distribution of periods. This approach provides a conservative estimate of H0 = (72.18 ± 1.76) km/s/Mpc, including the renewed MW analysis. The increased uncertainty reflects the reduced sample size—about 700 Cepheids per resampling compared to 3200 in the original dataset. This method reduces the Hubble tension from 5.4 σ (as reported by the SH0ES collaboration with H0 = (73.17 ± 0.86) km/s/Mpc) to 2.4 σ. The second strategy allows the PLR slope to vary with the period, yielding H0 = (72.35 ± 0.91) km/s/Mpc, including the renewed MW analysis, and the tension reduced to 4.4 σ. A statistical comparison of the model with the single-linear PLR shows a significant preference for the broken PLR (p-value <0.001). Both strategies consistently indicate a downward shift of approximately −1 km/s/Mpc in H0. Our findings underscore the importance of careful consideration of Cepheid population characteristics for precise H0 calibrations.