Assessing the systematic uncertainties by using assumed shapes. Left panel: The cumulative distribution of obliquities for JTs (orange), for synthetic JTs population assuming the shape models of (433) Eros (green) and (3) Juno (red), and of planetesimals obtained in our simulations of the streaming instability (SI) model (blue). We also plot the cumulative distributions for randomly oriented spins (brown), and large (D > 100 km) MBAs (purple, spin states adopted from DAMIT). Right panel: The a′/b′ vs. b′/c′ axis ratios of JTs, of large MBAs (D > 30 km), and of synthetic JT populations assuming the shape models of (433) Eros and (3) Juno. We also indicate the axis ratios for the original shapes of (433) Eros and (3) Juno.