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

Abstract

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 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 $w(z)=w_0+w_a\frac{z}{1+z}$). 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.

arXiv comment69 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

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