The Hubble Tension, the M Crisis of Late Time H(z) Deformation Models and the Reconstruction of Quintessence Lagrangians

2021/08/13 by A. Theodoropoulos, Anastasios Theodoropoulos, Leandros Perivolaropoulos
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics #Baryon acoustic oscillations #Cosmic microwave background #Cosmology #Cosmology and Gravitation Theories #Dark energy #Dark fluid #Deceleration parameter #Equation of state #Galaxies: Formation, Evolution, Phenomena #Hubble's law #Mathematical physics #Omega #Physics #Quantum mechanics #Quintessence #astro-ph.CO

paper · pdf · doi:10.3390/universe7080300

69 pages,4 tables,33 figures. Based on the BSc thesis of AT. Published in Universe 7 (2021) 8, 300. The numerical analysis files that were used for the production of the figures may be downloaded from: https://github.com/TasosTheodoropoulos/M_crisis

openalex publication_date 2021/08/13 · arxiv created 2021/09/13 · arxiv updated 2021/09/15 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05

Abstract

We present a detailed and pedagogical analysis of recent cosmological data, including CMB, BAO, SnIa and the recent local measurement of H0. We thus obtain constraints on the parameters of these standard dark energy parameterizations, including ΛCDM, and H(z) deformation models such as wCDM (constant equation of state w of dark energy), and the CPL model (corresponding to the evolving dark energy equation-of-state parameter w(z)=w0+waz1+z). The fitted parameters include the dark matter density Ω0m, the SnIa absolute magnitude M, the Hubble constant H0 and the dark energy parameters (e.g., w for wCDM). All models considered lead to a best-fit value of M that is inconsistent with the locally determined value obtained by Cepheid calibrators (M tension). We then use the best-fit dark energy parameters to reconstruct the quintessence Lagrangian that would be able to reproduce these best-fit parameterizations. Due to the derived late phantom behavior of the best-fit dark energy equation-of-state parameter w(z), the reconstructed quintessence models have a negative kinetic term and are therefore plagued with instabilities.

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