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

We present a detailed and pedagogical analysis of recent cosmological data, including CMB, BAO, SnIa and the recent local measurement of H-0. We thus obtain constraints on the parameters of these standard dark energy parameterizations, including Lambda CDM, 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) = w(0) + w(a) z/1+z). The fitted parameters include the dark matter density Omega(0m), the SnIa absolute magnitude M, the Hubble constant H-0 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.

Automated summary

This study provides a detailed analysis of recent cosmological data, including CMB, BAO, and SnIa, to constrain dark energy parameterizations. The results show inconsistencies with locally determined values and reveal late phantom behavior in the dark energy equation-of-state parameter.