The cosmological Mass Varying Neutrino model in the late universe

The cosmological Mass Varying Neutrino (MaVaN) model is considered, where the interaction between a fermionic field and a scalar field with a Ratra-Peebles potential via a Yukawa coupling is investigated. Observational constraints on the flat and non-flat MaVaN models, as well as on the standard $\mathrm{\Lambda }$CDM model, are derived from 32 $H(z)$ measurements using MCMC analysis. Comparison with the $\mathrm{\Lambda }$CDM model using the criteria $\mathrm{\Delta }{\chi }_{\mathrm{m}\mathrm{i}\mathrm{n}}^2$, $AICc$, and $BIC$ shows no statistically significant improvement for MaVaN models. Deviations in the expansion history remain well below $1\sigma$, indicating that the $H(z)$ data alone do not provide sufficient constraining power to distinguish MaVaN models from the $\mathrm{\Lambda }$CDM model. The non-flat MaVaN model reduces the tension between the $H_0$ value inferred from $H(z)$ data and the Planck CMB measurement from $\sim 2\sigma$ in the $\mathrm{\Lambda }$CDM framework to $\sim 1.1\sigma$. The discrepancy with the SH0ES measurement of $H_0$ is also reduced to below $1\sigma$, primarily due to the large uncertainties of the $H(z)$ data.