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One of the most prominent features of the $\gamma$-ray sky is the emissionfrom our own Galaxy. The Galactic plane has been observed by Fermi-LAT in GeVand H.E.S.S. in TeV light. Fermi has modeled the Galactic emission as the sumof a complex 'diffuse' emission model with the predominately point sourcecatalogs of 1FHL and 2FGL, while H.E.S.S. has primarily detected extended TeVsources. At GeV energies, Galactic diffuse emission dominates the $\gamma$-rayMilky Way but, as sources have hard spectra, it is likely their emissiondominates at TeV energies. Generally the spatial shape and fraction of sourceemission compared to diffuse emission in the Galactic plane is not well knownand is dependent on the source detection method, threshold and diffuse emissionmodeling methods used.  We present a simple image-analysis based method applied to Fermi-LAT datafrom 10 GeV to 500 GeV, covering a region of +/- 5 degrees in Galactic latitudeand +/- 100 degrees in Galactic longitude, to separate source and diffuseemission. This method involves elongated filter smoothing, combined withsignificance clipping to exclude sources. We test the method against modelsbased on the 1FHL catalog and very simple model Galaxies to evaluate theresponse for an input of known fraction and shape of diffuse and sourceemission.

The $\gamma$-ray Milky Way above 10 GeV: Distinguishing Sources from Diffuse Emission