one-component modeling. Since the PSF below 1 GeV is not small enough to resolve the SNR, the following morphological analysis uses data between 1 and 300 GeV.

Electrons and positrons, accelerated in the PWN, that radiate by synchrotron emission are expected to also radiate in the GeV band by IC scattering on photon fields. Since this SNR is relatively young, particles are well-confined inside the PWN. [@Temim:2013] estimate the magnetic field to be $B_{\rm{PWN}}$ $\approx$ 34 $\mu$G when the SNR has already begun significantly compressing the PWN at an age of 19,000 years. The emission seen in the radio band should track the older accelerated electrons and we expect that the extension of the $\gamma$-ray emission should not be larger than the radio emission. We thus model the $\gamma$-ray emission from the PWN using its radio template (see Figure \[fig:Templates\], left panel), knowing that the magnetic field spatial distribution inside the PWN should only moderately impact our model given the small size of the PWN compared to the $\textit{Fermi}$-LAT PSF.

![\[fig:TS\_and\_TSext\]Test statistic of the source (black bars) and of extension (colored bars) for the best-fit Gaussian in individual energy bands.](TS_TSext_bis-crop.pdf)

![image](T4.png)

![image](TSmap_PWN_only2.png){width="50.00000%"} ![image](TSmap_SNRmask_only_1_300GeV.png){width="50.00000%"}

Since the best-fit position of the $\gamma$-ray 