2020/10/08 by Karsten Jedamzik, Levon Pogosian, Gong-Bo Zhao · 1 voice · 1 citation
Physics and Astronomy · #astro-ph.CO #hep-ph
paper · pdf · doi:10.1038/s42005-021-00628-x
7 pages (including appendices), 3 figures; v2: improved clarity and organization of the presentation, added appendices with expanded description of the methods, improved the figures and added references, matches the version accepted for publication in Communications Physics
arxiv published 2020/10/08 · arxiv created 2021/05/17 · arxiv updated 2021/06/11
The mismatch between the locally measured expansion rate of the universe and the one inferred from the cosmic microwave background measurements by Planck in the context of the standard ΛCDM, known as the Hubble tension, has become one of the most pressing problems in cosmology. A large number of amendments to the ΛCDM model have been proposed in order to solve this tension. Many of them introduce new physics, such as early dark energy, modifications of the standard model neutrino sector, extra radiation, primordial magnetic fields or varying fundamental constants, with the aim of reducing the sound horizon at recombination r⋆. We demonstrate here that any model which only reduces r⋆ can never fully resolve the Hubble tension while remaining consistent with other cosmological datasets. We show explicitly that models which achieve a higher Hubble constant with lower values of matter density Ωm h2 run into tension with the observations of baryon acoustic oscillations, while models with larger Ωmh2 develop tension with galaxy weak lensing data.