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\section*{Background}  Dust devils are small-scale (few to many tens of meters) low-pressure vortices rendered visible by lofted dust. They usually occur in arid climates on the Earth and ubiquitously on Mars, where they likely dominate the supply of atmospheric dust and influence climate. Martian dust devils have been studied with orbiting and landed spacecraft and were first identified on Mars using images from the Viking Orbiter \citep{THOMAS_1985}. A long series of subsequentimaging  studies have since identified more dust devils and measured important propre through direct imaging or by identification of the tracks on Mars' dusty surface  while planetary analog studies of terrestrial dust devils involve in-person monitoring of field sites and surveys with in-situ barometers \citet[e.g.][]{Jackson_2015} and, recently, using photovoltaic sensors. In \citet{JacksonLorenz2015} and \citet{LorenzJackson2015}, we used time-series from individual barometers and photometers to reveal seasonal, annual, and spatial dust devil variability and the influence of sample size on the derived population statistics.