deletions | additions       diff --git a/section_Background_Dust_devils_are__.tex b/section_Background_Dust_devils_are__.tex  index 2c98ede..54ea5c7 100644  --- a/section_Background_Dust_devils_are__.tex  +++ b/section_Background_Dust_devils_are__.tex 
...
\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}. \citep{Thomas_1985}.  A long series of subsequent studies have since identified more dust devils through direct imaging or by identification of their tracks on Mars' dusty surface \citep[cf.][]{Balme_2006}. Meteorological sensors have also provided evidence for Martian dust devils passing near landed craft, either via their pressure signals \citep{Ellehoj_2010} or solar obscuration of photometers \citep{Zorzano_2013}  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.