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\section{Introduction}  \subsection{Motivation}  There is a need in the community to find ways of reliably and automatically seperating sources from background emission. This may be for the purpose of better understanding sources for which background contributions are removed, for instance in the development of galactic diffuse models [fermi], \cite{Fermidiffuse},  construction of source catalogs [1fhl, hgps] \cite{1fhl, hgps}  or for the improvement of background subtraction methods for source or region morphology studies. Alternatively, applications also exist for cases where sources must be removed instead of background, for instance galacitc diffuse emission studies (egberts) \cite{Egberts}  or in the analysis of extended galactic or extragalactic sources [example reference]. reference?].  While at lower energies, many methods are be successfully devised to separate source and background emission [example reference], reference??],  the challenge lies in finding successful methods for the high-energy GeV and TeV regime where available datasets are increasingly limited by the number of cosmic rays observed. \subsection{Galactic Emission}  At GeV and TeV energies, galactic emission may be split into three components; sources, truly galactic diffuse emission and the flux contributed by sources as yet to be resolved. While definitions in the literature vary, particularly with regard to unresolved and truly diffuse emission contributions, this study adopts the following convention (as illustrated in Figure 1).