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We add an ensemble of nuclei to the equation of state for homogeneousnucleonic matter to generate a new set of models suitable for astrophysicalsimulations of core-collapse supernovae and neutron star mergers. We implementempirical constraints from (i) nuclear mass measurements, (ii) proton-protonscattering phase shifts, and (iii) neutron star observations. Our model is alsoguided by microscopic many-body theory calculations based on realistic nuclearforces, including the zero-temperature neutron matter equation of state fromquantum Monte Carlo simulations and thermal contributions to the free energyfrom finite-temperature many-body perturbation theory. We ensure that theparameters of our model can be varied while preserving thermodynamicconsistency and the connection to experimental or observational data, thusproviding a probability distribution of the astrophysical hot and dense matterequation of state. We compare our results with those obtained from otheravailable equations of state. While our probability distributions indeedrepresent a large number of possible equations of state, we cannot yet claim tohave fully explored all of the uncertainties, especially with regard to thestructure of nuclei in the hot and dense medium.

Hot and Dense Matter Equation of State Probability Distributions for Astrophysical Simulations