our best models found in the previous section: the disk alone and the radio PWN with either the SNR mask or the disk. Here the $\gamma$-ray emissions are still described with power laws since other spectral representations did not improve the fit. We do not take into account the energy dispersion (this induces a bias $\sim$ $-$ 5% on flux[^4]). Using `gtlike`, we perform a maximum likelihood fit leaving the same spectral parameters free as before. Table \[tab:Fit\] reports the results obtained from the fit.

When we use the disk alone to describe the $\gamma$-ray emission, the photon index is found to be close to 2. Using differentiated models for the PWN and the SNR, the fit leads to a spectral separation between the two components: a softer spectrum for the remnant ($\Gamma \approx 2.16$ using the disk and $\Gamma \approx 2.17$ using the SNR mask) and a harder spectrum for the nebula ($\Gamma \approx 1.74$ and $\Gamma \approx 1.79$). The choice of the model for the remnant (either the disk or the SNR mask) has a very slight impact on the spectral study.

To compute the spectral energy distribution (SED), we divide the whole energy range (300 MeV – 