Constraining the Kaniadakis holography dark energy: A Bayesian statistical approach

This paper investigates a Kaniadakis holographic dark energy (KHDE) model within a flat Friedmann–Lemaitre–Robertson–Walker (FLRW) universe, utilizing the Hubble horizon as infrared (IR) cutoff. Based on Kaniadakis’ relativistic generalized framework, the model provides a dynamical explanation for the late-time acceleration of the universe. We employ a kinematic parametrization to solve the field equations and constrain the model’s free parameters — specifically the Hubble constant [Formula: see text] and the expansion index [Formula: see text] — using Bayesian inference and Markov Chain Monte Carlo (MCMC) simulations. Our analysis incorporates multiple observational datasets, including 57 OHD points, 1048 Pantheon SNIa events, and six BAO measurements. The best-fit value for the Hubble constant [Formula: see text] for OHD and by following OHD + BAO + Pantheon dataset, [Formula: see text]. Evolutionary diagnostics, including the deceleration parameter q, equation of state [Formula: see text], statefinder [Formula: see text], [Formula: see text] diagnostics, and jerk parameter [Formula: see text] indicate that the model transitions from quintessence era ([Formula: see text]) into phantom region ([Formula: see text]), eventually converging to a de-Sitter phase in far future. Furthermore, the violation of the strong energy condition (SEC) and dominant energy conditions (DECs) provides physical validation for the observed cosmic acceleration. An analysis of classical stability confirms that the model remains consistent with the causality condition.