Spin obliquities and pole ecliptic latitudes within various populations. Left panel: cumulative distribution of obliquities for JTs (orange) and of planetesimals obtained in our simulations of the streaming instability (SI) model (blue). The thick orange line corresponds to the nominal spin state solutions, while the thin orange lines represent the spin states based on the bootstrapped photometric datasets. The spins in SI are predominantly prograde with ≃75% having obliquity ε < 90°. We also plot the cumulative distributions for randomly oriented spins (red), and large MBAs (green, spin states adopted from DAMIT). Right panel: same but now for the ecliptic latitude of the rotational pole instead of the spin obliquity.