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Very high energy gamma rays from the composite SNR G0.9+0.1

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2005-03-01
Aharonian, F
Akhperjanian, AG
Aye, KM
Bazer-Bachi, AR
Beilicke, M
Benbow, W
Berge, D
Berghaus, P
Bernlohr, K
Boisson, C
Bolz, O
Borgmeier, C
Braun, I
Breitling, F
Brown, AM
Gordo, JB
Chadwick, PM
Chounet, LM
Cornils, R
Costamante, L
Degrange, B
Djannati-Atai, A
Drury, LO
Dubus, G
Ergin, Tülün
Espigat, P
Feinstein, F
Fleury, P
Fontaine, G
Funk, S
Gallant, YA
Giebels, B
Gillessen, S
Goret, P
Hadjichristidis, C
Hauser, M
Heinzelmann, G
Henri, G
Hermann, G
Hinton, JA
Hofmann, W
Holleran, M
Horns, D
de Jager, OC
Jung, I
Khelifi, B
Komin, N
Konopelko, A
Latham, IJ
Le Gallou, R
Lemiere, A
Lemoine, M
Leroy, N
Lohse, T
Marcowith, A
Masterson, C
McComb, TJL
de Naurois, M
Nolan, SJ
Noutsos, A
Orford, KJ
Osborne, JL
Ouchrif, M
Panter, M
Pelletier, G
Pita, S
Puhlhofer, G
Punch, M
Raubenheimer, BC
Raue, M
Raux, J
Rayner, SM
Redondo, I
Reimer, A
Reimer, O
Ripken, J
Rob, L
Rolland, L
Rowell, G
Sahakian, V
Sauge, L
Schlenker, S
Schlickeiser, R
Schuster, C
Schwanke, U
Siewert, M
Sol, H
Steenkamp, R
Stegmann, C
Tavernet, JP
Terrier, R
Theoret, CG
Tluczykont, M
Vasileiadis, G
Venter, C
Vincent, P
Visser, B
Volk, HJ
Wagner, SJ
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 HESS instrument. The source is detected with a significance of approximate to 13sigma, and a photon flux above 200 GeV of ( 5.7 +/- 0.7(stat) +/- 1.2(sys)) x 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 proportional to 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.