Please use this identifier to cite or link to this item: https://hdl.handle.net/2440/37439
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Type: Journal article
Title: Very high energy gamma rays from the composite SNR G 0.9+0.1
Author: Aharonian, F.
Akhperjanian, A.
Aye, K.
Bazer-Bachi, A.
Beilicke, M.
Benbow, W.
Berge, D.
Berghaus, P.
Bernlohr, K.
Boisson, C.
Bolz, O.
Borgmeier, C.
Braun, I.
Breitling, F.
Brown, A.
Bussons Gordo, J.
Chadwick, P.
Chounet, L.
Cornils, R.
Costamante, L.
et al.
Citation: Astronomy and Astrophysics: a European journal, 2005; 432(2):L25-L29
Publisher: E D P Sciences
Issue Date: 2005
ISSN: 0004-6361
1432-0746
Statement of
Responsibility: 
F. Aharonian...G. Rowell...et al.
Abstract: 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 HESS instrument. The source is detected with a significance of ≈13σ, 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 Γ) with photon index Γ = 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. © ESO 2005.
Rights: © The European Southern Observatory 2005
DOI: 10.1051/0004-6361:200500022
Published version: http://dx.doi.org/10.1051/0004-6361:200500022
Appears in Collections:Aurora harvest
Chemistry and Physics publications

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