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This work reports on the detection of $\gamma$-ray emission coincident withthe supernova remnant (SNR) SNR G5.7-0.1 using data collected by the Large AreaTelescope aboard the Fermi Gamma-ray Space Telescope. The SNR is believed to beinteracting with molecular clouds, based on 1720 MHz hydroxyl (OH) maseremission observations in its direction. This interaction is expected to providetargets for the production of $\gamma$-ray emission from $\pi^0$-decay. A$\gamma$-ray source was observed in the direction of SNR G5.7-0.1, positionednearby the bright $\gamma$-ray source SNR W28. We model the emission from radioto $\gamma$-ray energies using a one-zone model. Following consideration ofboth $\pi^0$-decay and leptonically dominated emission scenarios for theMeV-TeV source, we conclude that a considerable component of the $\gamma$-rayemission must originate from the $\pi^0$-decay channel. Finally, constraintswere placed on the reported ambiguity of the SNR distance through X-ray columndensity measurements made using XMM-Newton observations. We conclude SNRG5.7-0.1 is a significant $\gamma$-ray source positioned at a distance of $\sim3$ kpc with luminosity in the 0.1--100 GeV range of $L_{\gamma} \approx 7.4\times 10^{34}$ erg/s.

FERMI-LAT Observations of Supernova Remnant G5.7-0.1, Believed to be Interacting with Molecular Clouds