Left: Cumulative distribution of wind luminosity ﹩\dot{E}﹩ in material above a given value of Γ_∞ ≃ σ (Equation (A2)), for the most rapidly spinning, highly magnetized model (B3P1). The Poynting (﹩{\dot{E}}_{{\rm{EM}}}﹩, blue), thermal (﹩{\dot{E}}_{{\rm{therm}}}﹩, red), and kinetic (﹩{\dot{E}}_{{\rm{K}}}﹩, green) luminosities of the wind are measured at a spherical shell of radius r ≃ 236 km, between t ≃ 155−166 ms after magnetic-field initialization. Right: Total isotropic-equivalent energy carried by the outflow over a duration Δt = 2 s, in material with asymptotic Lorentz factor Γ_∞ > 10 (Γ_∞ > 30) shown with blue (red) points, versus total isotropic-equivalent kinetic energy of the outflow E_K(Δt = 2 s), as measured from cumulative distributions shown in the left panel. Most of the energy in fluid with Γ_∞ ≲ 10 resides in sub- or moderately relativistic wind components that would likely couple to the surrounding supernova or kilonova ejecta. Black points show inferred isotropic-equivalent energies of gamma-ray emission E_γ,iso and associated kilonovae E_K from short GRBs compiled by J. C. Rastinejad et al. (2025), rescaled to a common duration of 2 s and assuming a jet half-opening angle θ_j,col ≃ 8° to match those found from the strongly magnetized, rapidly spinning wind models.