Density versus core radius. The central density is plotted within the fit core radius for each dwarf, estimated as (σ_c/r_c)². Since the values of σ_c are not available for the galaxy dataset, we used σ_los instead. A clear separation between UFD’s and classical dSph’s is apparent with both populations following parallel trends. The slope d log ρ_c/d log r_c = −4 corresponds to the time-independent soliton solution of the Schrödinger–Poisson equation, where more massive solitons produce narrower cores. The blue lines represent the predicted relation for the UFD’s and dSph’s, whereas the green lines correspond to the input boson masses of the simulation and can be compared with the star symbols (simulated halos) and halo ID number. In the case of halos, 12₂ and 13₂ represent halos 12 and 13 in a scenario where they do not experience tidal forces. Note how the dSph galaxies and the non-tidally affected extrapolated UFDs follow their theoretical trend lines. We also mark Leo K ($r_c=0.{034}_{-0.019}^{+0.002}$ Kpc) and Leo M ($r_c=0.{081}_{-0.01}^{+0.01}$ Kpc) galaxies and color-code them by luminosity; this plot provides a prediction of their predicted velocity dispersions, which are as yet unmeasured. Crater II is marked with a white point.