studies complementing purely spectral analyses have the potential to help identify multiple particle acceleration regions in one object such as interaction regions with surrounding clouds or the different emissions coming from the SNR and/or the PWN in composite objects.

With an SNR shell and a PWN seen at radio wavelengths, the Galactic SNR G326.3$-$1.8 is a prototype of the so-called composite SNRs [@Mills; @Milne]. Its distance is estimated between 3.1 kpc [@Goss:1972] and 4.1 kpc [@Rosado:1996] as established by the H[i]{} absorption profile and H$\alpha$ velocity measurements respectively. @Temim:2013 estimated this SNR to be 16,500 years old with a shock velocity of 500 km s$^{-1}$, expanding in an ISM density of $n_{0}$ = 0.1 cm$^{-3}$.

![image](SNRradio_norm.pdf)

![image](Countmap_pixelsize_0_05.pdf)

Figure \[fig:MOST\], obtained from radio observations [@MOSTcat:1996], shows a symmetric SNR shell with 0.3° radius and a PWN trailing the putative pulsar and likely crushed by the remnant’s reverse shock. Non-thermal radio emission has been reported with a spectral index of $\alpha$ = 0.34 for the shell and $\alpha$ = 0.18 for the nebula where $S_{\nu}$ $\propto$ $\nu^{-\alpha}$ [@Dickel:2000]. Optical H$\alpha$ filaments were observed in the southwest and northeast parts of the remnant, and appear to spatially correlate with the shell [@Vandenbergh:1979; @Dennefeld:1980] 