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The Gamma Cygni supernova remnant (G78.2+2.1) is a middle-aged SNR ($\sim$ 7000 years old) situated in the Cygnus region. The high-energy observations by VERITAS and Fermi-LAT re vealed a complex, energy-dependent morphology of the SNR in the GeV-TeV band, different from that observed in X-rays. G78.2+2.1 also hosts the pulsar PSR J2021+4026, which is the only variable gamma-ray pulsar known to date. Using recent observations of the Gamma Cygni region with the MAGIC telescopes together with data from the Fermi-LAT, we present the structure of the emission from the northern and southern shell in the GeV to TeV energy range. We discuss the implication of the result of this morphological analysis in the context of our current understanding of supernova remnant models and view possible counterparts of the emission in a multi-wavelength context.

$\gamma$ -Cygni: the GeV to TeV morphology of an unique Sedov-phase SNR with MAGIC and $Fermi$-LAT