Very high energy ( > 100 GeV ) gamma-ray emission has been detected for the first time from the composite supernova remnant G 0.9+0.1 using the H.E.S.S . instrument .
The source is detected with a significance of \approx 13 \sigma , and a photon flux above 200 GeV of ( 5.7 \pm 0.7 _ { stat } \pm 1.2 _ { sys } ) \times 10 ^ { -12 } cm ^ { -2 } s ^ { -1 } , making it one of the weakest sources ever detected at TeV energies .
The photon spectrum is compatible with a power law ( dN / dE \propto E ^ { - \Gamma } ) with photon index \Gamma = 2.40 \pm 0.11 _ { stat } \pm 0.20 _ { sys } .
The gamma-ray emission appears to originate in the plerionic core of the remnant , rather than the shell , and can be plausibly explained as inverse Compton scattering of relativistic electrons .

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