Spectral energy distribution of the γ-ray emission measured with the LAT for the Cygnus Loop. The filled histograms show the TS values in each energy bin. Vertical barsshow 1σ statistical errors. Where the detection is not significant (TS < 4), we show upper limits at the 95% confidence level. Upperpanel: SED extracted using the UV template. The PLSuperExpCutoff4 best-fit spectrum for the global γ-ray data (Table 3) is plotted as the dashed black line, and its upper and lower 1σ bounds asthe solid black lines. Lower panel: red (green) points are LAT flux points using the X-ray (UV) maps as spatial templates together. The lines are the best-fit LogParabola models (Table 4).