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We have analysed the Fermi LAT data on the SNR G73.9+0.9. We have confirmed aprevious detection of high-energy gamma-rays from this source at a highsignificance of $\simeq 12\sigma$. The observed spectrum shows a significantcurvature, peaking in $E F_E$ at $\sim$1 GeV. We have also calculated the fluxupper limits in the mm-wavelength and X-ray ranges from Planck and XMM-Newton,respectively. We have inspected the intensity of the CO (1$\rightarrow $0)emission line and found a large peak at a velocity range corresponding to thepreviously estimated source distance of $\sim$4 kpc, which may indicate anassociation between a molecular cloud and the SNR. The gamma-ray emissionappears due to interaction of accelerated particles within the SNR with thematter of the cloud. The most likely radiative process responsible for thegamma-ray emission is decay of neutral pions produced in ion-ion collisions.While a dominant leptonic origin of this emission can be ruled out, therelativistic electron population related to the observed radio flux willnecessarily lead to a certain level of bremsstrahlung gamma-ray emission. Basedon this broad-band modelling, we have developed a method to estimate themagnetic field, yielding $B\geq 80\,\mu$G at our best estimate of the molecularcloud density (or less at a lower density). G73.9+0.9 appears similar, thoughsomewhat weaker, to other SNRs interacting with a local dense medium detectedby the LAT.

The high-energy gamma-ray detection of G73.9+0.9, a supernova remnant interacting with a molecular cloud