Beyond $\hat{I}›$CDM: Exploring a Dynamical Cosmological Constant Framework Consistent with Late-Time Observations

Abstract

In this work, we investigate a cosmological scenario with a time-dependent cosmological constant $\hat{I}›$(t) within the spatially flat Friedmann-Lemaître-Robertson-Walker (FLRW) framework. Here we study a power-law $\hat{I}›(t)$CDM model characterized by a dynamic cosmological constant expressed as a function of the Hubble parameter and its derivative $\hat{I}›(t)$ $=\hat{I}\pm (\dot{H}+H^2)+\hat{I}»H^2+4\ddot{I}€G\ddot{I}\hat{I}\cdot .$ Using recent observational datasets (DESI BAO, OHD, and PP\&SH0ES), we constrain the model's free parameters $(H_0,\hat{I}\pm ,\hat{I}»,\hat{I}\cdot )$ and analyze their impact on key cosmological quantities. A Markov chain Monte Carlo (MCMC) analysis of the best-fit value of $H_0=71.9\pm 0.23$ km/s/Mpc from PP\&SH0ES analysis only, which substantially alleviates the existing tension between early and late-time determinations of the Hubble constant, reducing it to $\sim 1.5\ddot{I}ƒ$. The reconstructed $Om$ diagnostic exhibits a negative slope, indicating a dynamic dark energy behavior with quintessence-like characteristics ($\ddot{I}‰>-1$). These results suggest that the proposed $\hat{I}›(t)$ model provides a viable alternative to the standard $\hat{I}›$CDM paradigm to explain the late-time acceleration of the universe. Our findings show that this model alleviates the Hubble tension more effectively than the standard $\hat{I}›$CDM . The model also demonstrates compatibility with late-time Hubble parameter observations and offers a compelling framework to address the limitations of $\hat{I}›$CDM.

14 pages, 5 figures, 3 tables, original published research paper