Understanding dust mobilization on Mars is essential for understanding and predicting the background atmospheric dust distribution, the onset and evolution of dust storms (the largest of which can cover the entire planet in a veil of dust for weeks on end, e.g., Guzewich et al., 2019), and the effects of lifted dust on Martian atmospheric dynamics. Due to Mars' low atmospheric density, which absorbs and scatters relatively little solar or thermal radiation, the presence of dust in the atmosphere has a major impact on its radiative balance, which in turn strongly affects thermal gradients and winds (Kahre et al., 2017;Wolff et al., 2017). The global distribution of atmospheric dust depends on atmospheric transport, interactions with ice particles (microphysics), fallout rate, and dust mobilization from the surface. The last process is least understood and in greatest need of investigation (Newman, Bertrand, et al., 2022). Dust lifting has been observed in both straight-line winds and vortices (dust-devils), which may be roughly equally important both outside dust storms (Newman, Hueso, et al., 2022) and during the onset of regional storms (Lemmon et al., 2022).