Late-time acceleration in f(Q) gravity: Analysis and constraints in an anisotropic background

This paper is devoted to investigate the anisotropic locally rotationally symmetric (LRS) Bianchi type-I space–time in the context of the recently proposed f(Q) gravity in which Q is the non-metricity scalar. For this purpose, we consider a linear form of fQ gravity model, specifically, fQ=αQ+β, where α and β are free parameters and then we analyze the exact solutions of LRS Bianchi type-I space–time. The modified Friedmann equations are solved by presuming an expansion scalar θt is proportional to the shear scalar σt which leads to the relation between the metric potentials as A=Bn where n is an arbitrary constant. Then we constrain our model parameters with the observational Hubble datasets of 57 data points. Moreover, we discuss the physical behavior of cosmological parameters such as energy density, pressure, EoS parameter, and deceleration parameter. The behavior of the deceleration parameter predicts a transition from deceleration to accelerated phases in an expanding Universe. Finally, the EoS parameter indicates that the anisotropic fluid behaves like the standard ΛCDM model. •The anisotropic locally rotationally symmetric (LRS) Bianchi type-I space–time has been investigated in f(Q) symmetric teleparallel gravity, where Q is the non-metricity scalar.•The linear form of f(Q) gravity model has been considered, specifically, f(Q)=αQ+β, where α and β are free model parameters.•Model parameters were constrained by using the observational Hubble datasets of 57 data points.•We found that the anisotropic fluid behaves like the standard ΛCDM model.