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\section*{Discussion and Conclusions}  \label{sec:discussion_and_conclusions}  Our formulation here provides a starting place for relating the population statistics of dust devils as recovered by single-barometer surveys to their physical structures. Understanding these relationships is critical for understanding the atmospheric influence of devils on both planets since it depends so sensitively on both the devils' statistical and physical properties. As noted in \citet{Jackson2015} \cite{Jackson_2015}  and \cite{Lorenz_2014}, in estimating the total flux of dust injected into the martian atmosphere, it is important to consider the population-weighted flux and not the flux from the average dust devil. Of course, knowing the population is critical to calculating that population-weighted flux. Moreover, lab work reported in \citet{Neakrase_2006} suggested an exponential dependence of dust flux on a dust devil's pressure depth, and so even small shifts in the distribution of dust devil pressure depths can result in large shifts in the dust flux. For instance, using the exponential dependence indicated in Figure X of \citet{Neakrase_2006}, we find that the dust flux given by the distribution of $P_{\rm act}$ in Figure \ref{fig:} is XX times more than that given by the $P_{\rm obs}$ distribution. The model for the miss distance effect developed here serves to highlight the many important uncertainties and degeneracies involved in single-barometer dust devil surveys. In particular, these results show that it is difficult to disentangle the geometry of an encounter between a devil and a detector from the devil's structure. The pressure profile observed for a devil will almost always be wider and less deep than the devil's actual profile.