γCygni SNR morphology viewed in the electromagnetic spectrum

The investigation of very high energy gamma-ray sources touches on the problem of the cosmic ray origin and the role of the Galaxy in their generation. The SHALON observations have yielded the results on $$$ \gamma $$$Cygni SNR Galactic supernova remnant. The observation results are presented with spectral energy distribution and emission map by SHALON in comparison with other experiment data obtained by ROSAT in x-ray energy range, radio-data by CGPS, and also observations of GeV–TeV gamma-rays by Fermi LAT. The overall $$$ \gamma $$$Cygni SNR characteristics detected in radio, x-rays, and GeV–TeV gamma-rays can be a result of the shocks at the interaction of the supernova ejecta and the surrounding medium. The collected experimental data help to make clear the origin of TeV $$$ \gamma $$$-ray emission in the $$$ \gamma $$$Cygni SNR. The density of target material in the SNR surroundings is enough to produce the observable TeV gamma-ray flux via the shock acceleration of hadrons in the detected regions. The detection of gamma-ray emission at 0.8–60 TeV from the North-West and South-East shells of $$$ \gamma $$$Cygni SNR by SHALON would favor the hadronic origin of the gamma-rays in this supernova remnant.