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The equations of state (EoSs) governing neutron star (NS) matter obtained forboth non-relativistic and relativistic mean-field models are systematicallyconfronted with a diverse set of terrestrial data and astrophysicalobservations within the Bayesian framework. The terrestrial data, spans frombulk properties of finite nuclei to the heavy-ion collisions, constrain thesymmetric nuclear matter EoS and the symmetry energy up to twice the saturationdensity ($\rho_0$= 0.16 fm$^{-3}$). The astrophysical observations encompassthe NS radius, the tidal deformability, and the lower bound on maximum mass.Three distinct posterior distributions of EoSs are generated by graduallyupdating the priors with different constraints: (i) only the maximum NS mass,(ii) incorporating additional terrestrial data, (iii) combining both theterrestrial data and astrophysical observations. These distributions are thencompared using the Kullback-Liebler divergence which highlights the significantconstraints imposed on the EoSs by the currently available lower bound of NSmaximum mass and terrestrial data. The remaining astrophysical observationsmarginally refine the EoS within the density range $\sim$ 2-3$\rho_0$. It isobserved that the non-relativistic mean field model yields stiffer EoS for thesymmetric nuclear matter while softer density dependent symmetry energycompared to the relativistic one when all the data/observations are considered.

Implications of comprehensive nuclear and astrophysics data on the equations of state of neutron star matter