0.11 & 2.43 $\pm$ 0.23 & 0.33 $\pm$ 0.11 & 2.31 $\pm$ 0.23\

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$\Gamma$ & 2.07 $\pm$ 0.04 & 1.74 $\pm$ 0.15 & 2.16 $\pm$ 0.06 & 1.79 $\pm$ 0.12 & 2.17 $\pm$ 0.06\

![image](SED_Disk_with_TS_values_final-crop.pdf) ![image](SED_SNRmask_PWN_with_bars-crop.pdf)

For all components, the $\gamma$-ray emission is described by a power law and the free spectral parameters are those of the components, the nearest point source, and those of the Galactic and isotropic diffuse emissions. The results from our maximum likelihood fit are given in Table \[tab:LL\] with the numbers of free parameters associated to the models (spectral and/or spatial).\
First, the TS values obtained using the one-component models (disk, radio SNR or SNR mask) alone are clearly higher than that obtained using only the radio PWN, indicating that the fit prefers a model more extended than the radio PWN. For comparison, Figure \[fig:TSmap\_PWN\] (right) depicts the residual TS map when only the SNR mask is included to the model, showing a residual emission coincident with the position of the PWN. In terms of test statistic, when adding a second component, the model with one component becomes the null hypothesis to test the significance of the second component. In Table \[tab:LL\], we compare 