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We present numerical simulations of giant planet migration in our solarsystem and examine how the speed of planetary migration affects inclinations inthe resulting population of small bodies (test particles) scattered outward andsubsequently captured into Neptune's 3:2 mean motion resonance (the Plutinos)as well as the hot classical Kuiper belt population. We do not find aconsistent relationship between the degree of test particle inclinationexcitation and e-folding planet migration timescales in the range 5-50 Myr. Ourresults present a counter-example to Nesvorny 2015's finding that the Plutinoand hot classical inclinations showed a marked increase with increasinge-folding timescales for Neptune's migration. We argue that these differingresults are likely due to differing secular architectures of the giant planetsduring and after migration. Small changes in the planets' initial conditionsand differences in the numerical implementation of planet migration can resultin different amplitudes of the planets' inclination secular modes, and this canlead to different final inclination distributions for test particles in thesimulations. We conclude that the observed large inclination dispersion ofKuiper belt objects does not require Neptune's migration to be slow; planetarymigration with e-folding timescales of 5, 10, 30, and 50 Myr can all yieldinclination dispersions similar to the observed Plutino and hot classicalpopulations, with no correlation between the degree of inclination excitationand migration speed.

Not a simple relationship between Neptune's migration speed and Kuiper belt inclination excitation