SNR G24.7+0.6 is a 9.5 kyrs radio and \gamma -ray supernova remnant evolving in a dense medium .
In the GeV regime , SNR G24.7+0.6 ( 3FHL J1834.1–0706e/FGES J1834.1–0706 ) shows a hard spectral index ( \Gamma \sim 2 ) up to 200 GeV , which makes it a good candidate to be observed with Cherenkov telescopes such as MAGIC .
We observed the field of view of SNR G24.7+0.6 with the MAGIC telescopes for a total of 31 hours .
We detect very high energy \gamma -ray emission from an extended source located 0.34 \degr away from the center of the radio SNR .
The new source , named MAGIC J1835–069 is detected up to 5 TeV , and its spectrum is well-represented by a power-law function with spectral index of 2.74 \pm 0.08 .
The complexity of the region makes the identification of the origin of the very-high energy emission difficult , however the spectral agreement with the LAT source and overlapping position at less than 1.5 \sigma point to a common origin .
We analysed 8 years of Fermi -LAT data to extend the spectrum of the source down to 60 MeV . Fermi -LAT and MAGIC spectra overlap within errors and the global broad band spectrum is described by a power-law with exponential cutoff at 1.9 \pm 0.5 TeV .
The detected \gamma -ray emission can be interpreted as the results of proton-proton interaction between the supernova and the CO-rich surrounding .