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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 with the MAGIC telescopes for a total of 31 hours. We detect very high energy $gamma$-ray emission from an extended source located 0.34degr away from the center of the radio SNR. The new source, named mgc 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 $1.9pm0.5$,TeV. The detected $gamma$-ray emission can be interpreted as the results of proton-proton interaction between the supernova and the CO-rich surrounding.
We report the discovery of TeV gamma-ray emission from the Type Ia supernova remnant (SNR) G120.1+1.4, known as Tychos supernova remnant. Observations performed in the period 2008-2010 with the VERITAS ground-based gamma-ray observatory reveal weak e
We report the discovery of an unidentified, extended source of very-high-energy (VHE) gamma-ray emission, VER J2019+407, within the radio shell of the supernova remnant SNR G78.2+2.1, using 21.4 hours of data taken by the VERITAS gamma-ray observator
The pulsar wind nebula (PWN) 3C 58 is one of the historical very-high-energy (VHE; E>100 GeV) gamma-ray source candidates. It is energized by one of the highest spin-down power pulsars known (5% of Crab pulsar) and it has been compared to the Crab Ne
The pulsar wind nebula (PWN) 3C 58 has been proposed as a good candidate for detection at VHE (VHE; E>100 GeV) for many years. It is powered by one of the highest spin-down power pulsars known (5% of Crab pulsar) and it has been compared to the Crab
We report on the first detection of GeV high-energy gamma-ray emission from a young supernova remnant with the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope. These observations reveal a source with no discernible spatial extension d