Eccentricity and inclination dispersions estimated from the radial and vertical density distributions, respectively. Points with black outlines use the upper limits on ⟨e_rms⟩ presented in Han et al. (2026), while points with red outlines have ⟨e_rms⟩ estimated using Eq. (14). Disks may be dynamically dominated by catastrophic collisions when ⟨e_rms⟩/⟨i_rms⟩ ≲ 1, rather than self-stirred or planet-stirred scenarios that result in a larger ratio of ⟨e_rms⟩/⟨i_rms⟩. We note that the y-axis shows upper limits of ⟨e_rms⟩, so we only find upper limits on ⟨e_rms⟩/⟨i_rms⟩.