Observational constraints on Tsallis holographic dark energy with Ricci horizon cutoff

TL;DR

This study constrains Tsallis holographic dark energy models with Ricci cutoff using observational data, analyzing their behavior over cosmic history and comparing stability and age estimates with standard cosmology.

Contribution

It introduces observational constraints on both interacting and noninteracting THDE models with Ricci cutoff, including stability analysis and universe age estimation.

Findings

Models are consistent with observational data.

Dark energy can be in phantom state currently, quintessence in early times.

Models transition from matter to dark energy dominance and show stability in past epochs.

Abstract

In this research, we are interested in constraining the nonlinear interacting and noninteracting Tsallis holographic dark energy (THDE) with Ricci horizon cutoff by employing three observational datasets. To this aim, the THDE with Ricci horizon considering the noninteraction and nonlinear interaction terms will be fitted by the SNe Ia, SNe Ia+H(z), and SNe Ia+H(z)+GRB samples to investigate the Hubble ($H(z)$), dark energy equation of state ($\omega_{DE}$), effective equation of state ($\omega_{eff}$), and deceleration ($q$) parameters. Investigating the $H(z)$ parameter illustrates that our models are in good consistent with respect to observation. Also, it can reveal the turning point for both noninteracting and nonlinear interacting THDE with Ricci cutoff in the late time era. Next, the analysis of the $\omega_{DE}$ for our models displays that the dark energy can experience the phantom state at the current time. However, it lies in the quintessence regime in the early era and approaches the cosmological constant in the late-time epoch. Similar results will be for the $\omega_{eff}$ parameter with this difference that the $\omega_{eff}$ will experience the quintessence region at the current redshift. Next to the mentioned parameters, the study of the $q$ parameter indicates that the models satisfy an acceptable transition phase from the matter to the dark energy-dominated era. After that, the classical stability ($v_{s}^{2}$) will be analyzed for our models. The $v_{s}^{2}$ shows that the noninteracting and nonlinear interacting THDE with Ricci cutoff will be stable in the past era, unstable in the present, and progressive epochs. Then, we will employ the $Jerk$ ($J$) and $OM$ parameters to distinguish between our models and the $\Lambda CDM$ model. Finally, we will calculate the age of the Universe for the THDE and nonlinear interacting THDE with Ricci as the IR cutoff.