Model-independent reconstruction of late-time cosmic acceleration in Finsler–Randers cosmology

We investigate a Finsler–Randers cosmological model that introduces anisotropic geometric corrections to the expansion dynamics through a model–independent parametrization of the deceleration parameter q ( z ). The cosmic expansion history is reconstructed using observational data from Cosmic Chronometers (CC), DESI baryon acoustic oscillations (BAO), and DES Y5 Type Ia supernovae. The combined analysis constrains the model parameters to H 0 = 68.16 ± 0.83 km s − 1 Mpc − 1 , η = 1.202 ± 0.017 , and ζ = 1.550 ± 0.032 . The reconstructed expansion history yields present-day values q 0 = − 0.62 ± 0.14 and ω 0 = − 0.746 ± 0.092 , confirming a late-time accelerated phase consistent with observations. Higher-order cosmological diagnostics, including the jerk and snap parameters, together with the statefinder and Om diagnostics, indicate a dynamical dark energy behavior arising from geometric anisotropic corrections. Information criterion analysis shows that the model provides a statistically viable description of the late-time expansion when compared with the ΛCDM scenario. These results suggest that anisotropic geometric effects within the Finsler–Randers framework can reproduce the observed cosmic acceleration without introducing a cosmological constant.