The equation of state of dense nuclear matter is explored using the KIDS (Korea-IBS-Daegu-Sungkyunkwan) density functional. The equation-of-state parameters, which are coefficients of the energy density expanded in powers of $(\rho - \rho_0)/3\rho_0$ where $\rho$ is the nuclear matter density and $\rho_0$ is its density at saturation, are constrained by using both nuclear data and the mass-radius relation of a neutron star, as determined from modern astronomy data. We find that a combination of both types of data can significantly reduce the uncertainties in the equation-of-state parameters that are determined experimentally. We verify that the newly constrained parameters reproduce with high accuracy the basic properties of spherical magic nuclei. Neutron drip lines, on the other hand, show a non-negligible dependence in the uncertainty of the nuclear symmetry energy.

Keywords: Nuclear matter, Density functional theory, Neutron star