distinct spectral signatures, while the different emissions seem to be mixed when we use a single component model. The TS values in each energy bin highlight the different contributions of the two components: at low energy (E $<$ 10 GeV), the emission is dominated by the SNR while the contribution of the PWN becomes important above 10 GeV, bringing out the spatial and spectral distinctions between these two nested objects.

Results and discussion
======================

For this entire section we assume the distance to the SNR is 4.1 kpc [@Temim:2013].

SNR spectrum
------------

To understand the observed $\gamma$-ray spectrum of the SNR, we perform multi-wavelength modeling using the one-zone models provided by the `naima` package [@naima]. From [@Dickel:2000] we take the five radio flux measurements of the shell. As there is no associated synchrotron emission in the X-ray domain, we use the *ROSAT* thermal flux reported by [@Kassim:1993] as an upper limit. We also use the TeV upper limit derived from H.E.S.S. with 14 hours of observational live time and assuming a photon index of 2.3 [@HESS:SNRpop:2018].

Assuming the Sedov phase, we derive the kinetic energy released by the supernova: $$\hspace{0.5cm}
\frac{E_{\rm{SN}}}{10^{51} \hspace{0.1cm} \rm{erg}} = R_{12.5}^5 \times \Big(\frac{n_{0}}{ \textrm{cm}^{-3}}\Big) \times t_{4}^{-2} 