A constrained cosmological model in $f(R,L_m)$ gravity

TL;DR

This paper explores a specific $f(R,L_m)$ gravity model to explain the universe's accelerated expansion, fitting observational data and showing consistency with standard cosmological models.

Contribution

It introduces a new $f(R,L_m)$ gravity model with constrained parameters that explains late-time cosmic acceleration and aligns with observational data.

Findings

The model predicts a transition from deceleration to acceleration.

Energy density and EoS parameters indicate a quintessence dark energy behavior.

The model is consistent with $\, ext{Lambda CDM}$ and observational data.

Abstract

In this article, we study the expanding nature of universe in the contest of $f(R,L_m)$ gravity theory, here $ R $ represents the Ricci scalar and $ L_m $ is the matter Lagrangian density. With a specific form of $ f(R,L_m) $, we obtain the field equations for flat FLRW metric. We parametrize the deceleration parameter in terms of the Hubble parameter and from here we find four free parameters, which are constraints and estimated by using $H(z)$, $Pantheon$, and their joint data sets. Further, we investigate the evolution of the deceleration parameter which depicts a transition from the deceleration to acceleration phases of the universe. The evolution behaviour of energy density, pressure, and EoS parameters shows that the present model is an accelerated quintessence dark energy model. To compare our model with the $ \Lambda $CDM model we use some of the diagnostic techniques. Thus, we find that our model in $ f(R,L_m) $ gravity supports the recent standard observational studies and delineates the late-time cosmic acceleration.