An out-of-equilibrium and finite-temperature equation of state (EoS). The core is homogeneous n, p, e matter computed using a relativistic mean-field theory constrained by chiral effective field theory calculations of pure neutron matter at zero temperature (from 0.08 fm−3 to 0.32 fm−3), by properties of isospin-symmetric nuclear matter around nuclear saturation density, and by astrophysical observations of neutron stars [ABHT_2022 ]. To describe nuclear matter over the physically-relevant range of densities for use in, e.g., simulations of neutron star mergers, we attach the HS(IUF) EoS [ HSNP_2010 ][FHPSP_2010 ] in a thermodynamically consistent manner to model inhomogeneous nuclear matter at low densities. See Ref. [ABHT_2023 ] for more details about this EoS.