deletions | additions       diff --git a/section_Background_Dust_devils_are__.tex b/section_Background_Dust_devils_are__.tex  index 953b92e..f3ffc75 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 may 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 subsequent dust devil studies have followed, either 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 obscuration of the Sun by On  the Earth,  dust column \citep{Zorzano_2013} or their pressure signals \citep{Ellehoj_2010}. devils may help degrade air quality in arid climates \citep{Gillette_1990} and may pose an aviation hazard  Studies The dust-lifting capacity  ofterrestrial  dust devils frequently involve in-person monitoring seems to depend sensitively on their structures, in particular on the pressure wells at their centers \citep{Neakrase_2006}, so the dust supply from dust devils on both planets may be dominated by the seldom observed larger devils. Thus, it is particularly important to study the underlying distribution  of field sites, dust devil properties. Thus, elucidating the origin, evolution,  and population statistics of  dust devils are visually surveyed \citep{Pathare_2010} or directly sampled \citep{Balme_2003}. As noted in \citet{Lorenz_2009}, in-person visual surveys are likely to be biased toward detection is critical for understanding important terrestrial and Martian atmospheric properties and for in-situ exploration  of larger, more easily seen devils. Such surveys would Mars -- dust devils might pose a hazard for human exploration \citep{Balme_2006} but have  also fail to recover dustless vortices \citep{Lorenz_2015}. apparently lengthened the operational lifetime of Martian rovers (http://mars.jpl.nasa.gov/mer/mission/status_opportunityAll.html#sol3603).  Recently, terrestrial surveys similar to Martian dust devil surveys have been conducted using in-situ single barometers \citep{Lorenz_2012, Lorenz_2014, Jackson_2015} and photovoltaic sensors \citep{Lorenz_2015}. These sensor-based terrestrial surveys have the advantage of being directly analogous to Martian surveys and are highly cost-effective compared to the in-person surveys.  In these single-barometer surveys, a sensor is deployed in-situ record a pressure time A long  seriesat a sampling rate $\lesssim 1$ s. As a low-pressure convective vortex, the nearby passage  of a subsequent  dust devil will register as pressure dip discernible against a background ambient (but not necessarily constant) pressure. Figure \ref{fig:conditioning_detection_b_inset} from \citet{Jackson_2015} shows a time-series with a typical dust devil signal. However, as with visual surveys, single-sensor barometer surveys suffer from biases as well, primarily from the ``miss distance'' effect: a fixed barometric sensor is more likely to studies have followed, either through direct imaging or by identification of their tracks on Mars' dusty surface \citep[cf.][]{Balme_2006}. Meteorological sensors  have a more distant than closer encounter with a also provided evidence for Martian  dust devil. Since the pressure perturbation associated with a devil falls off with distance, the deepest point in the observed pressure profile will almost always be less than the actual pressure well at the devil's center. The observed shape devils passing near landed craft, either via obscuration  of the profile will be distorted as well. These biases are intrinsic to the detection methods, and additional biases can influence the inferred statistical properties. For instance, noise in Sun by  thepressure time series from a barometer may make more difficult detection of a  dust devils with smaller column \citep{Zorzano_2013} or their  pressure perturbations, depending on the exact detection scheme. signals \citep{Ellehoj_2010}.  The dust-lifting capacity Studies  of terrestrial  dust devils seems to depend sensitively on their structures, in particular on the pressure wells at their centers \citep{Neakrase_2006}, so the dust supply from frequently involve in-person monitoring of field sites, and  dust devils on both planets may are visually surveyed \citep{Pathare_2010} or directly sampled \citep{Balme_2003}. As noted in \citet{Lorenz_2009}, in-person visual surveys are likely to  be dominated by the seldom observed larger biased toward detection of larger, more easily seen  devils. Thus, it is particularly important Such surveys would also fail  to study the underlying distribution of recover dustless vortices \citep{Lorenz_2015}. Recently, terrestrial surveys similar to Martian  dust devil properties. Thus, elucidating the origin, evolution, surveys have been conducted using in-situ single barometers \citep{Lorenz_2012, Lorenz_2014, Jackson_2015}  and population statistics of dust devils is critical for understanding important photovoltaic sensors \citep{Lorenz_2015}. These sensor-based  terrestrial and Martian atmospheric properties and for in-situ exploration of Mars -- dust devils might pose a hazard for human exploration but surveys  havealso apparently lengthened  the operational lifetime advantage  of being directly analogous to Martian surveys and are highly cost-effective compared to  the Spirit rover. in-person surveys.  On both Mars and In this kind of single-barometer survey, a sensor is deployed in-situ record a pressure time series at a sampling rate $\lesssim 1$ s. As a low-pressure convective vortex,  the Earth, nearby passage of a  dust devils contribute to the atmospheric aerosol content, sometimes increasing the devil will register as pressure dip discernible against a background ambient (but not necessarily constant) pressure. Figure \ref{fig:conditioning_detection_b_inset} from \citet{Jackson_2015} shows a time-series with a typical  dust content over devil signal. However, as with visual surveys, single-sensor barometer surveys suffer from biases as well, primarily from  the U.S. Southwest by ``miss distance'' effect: a fixed barometric sensor is  more likely to have a more distant  than an order of magnitude, they primary source for atmospheric dust, which plays closer encounter with  a role in the radiative balance of the Martian atmosphere and, therefore, on dust devil. Since  the planet's meteorology [Basu et al., 2004]. Dust devils also seem to have lengthened pressure perturbation associated with a devil falls off with distance,  the operating lifetime of Martian rovers by frequently cleaning their solar panels (http://mars.jpl.nasa.gov/mer/mission/status_opportunityAll.html#sol3603). Since deepest point in  the dust supply from dust devils on both planets may observed pressure profile will almost always  be dominated by less than  the seldom observed larger devils, it is particularly important to study actual pressure well at  the underlying distribution devil's center. The observed shape  ofdust devils, rather than focusing on  the typical devil. Thus, elucidating profile will be distorted as well. These biases are intrinsic to  the origin, evolution, and population statistics of dust devils is critical for understanding important terrestrial and Martian atmospheric properties detection methods,  and for additional biases can influence the inferred statistical properties. For instance, noise  insitu exploration of Mars.  %While  the pressure dips associated with dust devils have been recorded on Earth [e.g., Wyett, 1954; Lambeth, 1966; Sinclair, 1973], they are actually time series from a barometer may make  more systematically documented in studies difficult detection  of a  dust devils with smaller pressure perturbations, depending  onMars (e.g., by Mars Pathfinder: Murphy and Nelli, 2002; and by  the Phoenix mission: Ellehoj et al., 2010), where landers have recorded meteorological parameters over long periods with a high enough cadence to detect small vortical structures. Most terrestrial meteorological records have cadence too low (canonically, 15 min) to record dust devils, for which a sampling rate of ∼1 Hz or better is typically required. exact detection scheme.  The plan of this paper is as follow: In Section \ref{sec:miss_distance_effect}, we discuss the influence of the miss distance effect on the observed parameters for dust devil profiles and on their distributions. In    
...