Left: Kolmogorov-Smirnov distance d between observed and modeled distribution of η grouping data by bins of heliocentric distance (r_h < 25 AU, 25 < r_h < 41 AU, and r_h > 41 AU). In all models, a uniform distribution of the polar axes over the sphere and the “random roughness” case are assumed. Right: histograms showing the distribution of best fit Γ₀, when accounting for uncertainties in the measured η.