This table corresponds to the zero temperature unified equation of state (EoS) for cold non-accreting neutron stars in beta equilibrium based on the Brussels-Montreal energy- density functional BSk24 [GCP_2013]. Details on the EoS model can be found in Ref. [PCP_2018] and the routines to construct an analytical fit of the EoS are also available on the Ioffe website. The tidal deformability associated to this EoS model was calculated in Ref. [ PCS_2019]. The outer crust was calculated using the Hartree-Fock-Bogoliubov atomic mass table HFB-24 available on the BRUSLIB data base [ XGJCA_2013], except when experimental values were available, for which we used the 2016 Atomic Mass Evaluation [ WGKH_2016], supplemented by the measurements of copper isotopes from Ref. [ W_2017]. The inner crust was computed using the 4th-order Extended Thomas-Fermi (ETF) method with proton shell and pairing corrections added perturbatively via the Strutinsky integral (SI); the nucleon distributions were parametrized using damped Fermi profiles and the Coulomb energy was calculated within the Wigner-Seitz (WS) approximation. Although the EoS was originally calculated ignoring nuclear pastas, their presence in neutron-star crust was later discussed in Refs. [ PCP_2020, PC_2022] and was shown to be marginal in the Extended Thomas-Fermi plus Strutinski Integral framework [ PC_2022]. The core was assumed to be made up by an admixture of neutrons and protons neutralised by electrons and possibly by muons. ^1S_0 neutron and proton pairing gaps in neutron-star cores were calculated in Ref. [ AC_2021].