Published in
EDP Sciences, Astronomy & Astrophysics, 2(432), p. L25-L29, 2005
DOI: 10.1051/0004-6361:200500022
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Very high energy gamma rays from the composite SNR G 0.9+0.1
,
Adnane Robert Bazer-Bachi,
Matthias Beilicke,
Wystan Benbow,
D. Berge,
Patrick Berghaus,
Konrad Bernlöhr,
K. Bernl�hr,
Claire Boisson,
O. Bolz,
Christoph Borgmeier,
C. Borgneier,
I. Bruan
and other authors.
Full text: Download
Abstract
Very high energy (> 100 GeV) gamma-ray emission has been detected for the first time from the composite supernova remnant G0.9+0.1 using the H.E.S.S. instrument. The source is detected with a significance of 13 sigma, and a photon flux above 200 GeV of (5.7+/-0.7 stat +/- 1.2 sys) * 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 ∝ E^-Gamma) with photon index Gamma = 2.40 +/- 0.11 stat +/- 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. ; Comment: 5 pages, 4 figures, accepted by A&A letters