This table contains the EoS by Schneider, Roberts, and Ott (SRO) [ SRO_17,SMP_2019] computed using the NRAPR Skyrme parametrization [ SPLE_2005 ]. The nuclear interaction is an effective non-relativistic Skyrme type model without momentum dependence generalized from the seminal work of Lattimer and Swesty [ LSNP_1991 ]. The model includes nucleons, which are treated as non-relativistic particles; alpha-particles, modeled as hard spheres of volume v_alpha = 24 fm^{-3} forming an ideal Boltzmann gas; and photos, electrons, and positrons, all treated as thermally equilibrated non-interacting relativistic gases. At low densities and temperatures nucleons may cluster into heavy nuclei computed within the nuclear statistical equilibrium (NSE). At high densities and temperatures heavy nuclei or the pasta phases dissolve in favor of homogeneous nuclear matter. The configuration of matter and the balance between the different phases is given by the thermodynamically most favorable state, that is, the one that minimizes the Helmholtz free energy of the system and, thus, guarantees thermodynamic consistency of the EoS. Unlike Ref. [ LSNP_1991 ], transitions from inhomogeneous to bulk nuclear matter are first order and simply chosen from the phase which minimizes the Helmholtz free energy. Further details can be found in Refs. [ SRO_17, LSNP_1991 ,SMP_2019]. A link to additional information which includes our open-source SROEOS code and many pre-computed tables for different Skyrme parametrizations found in the literature are found in the webpage SROEOS .