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Astronomy and Astrophysics 432 (2005) L25-L29
Very high energy gamma rays from the composite SNR G0.9+0.1
F. Aharonian, A.G. Akhperjanian, K.-M. Aye, A.R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, P. Berghaus1, 2, K. Bernlohr, C. Boisson, O. Bolz, C. Borgneier, I. Bruan, F. Breitling, A.M. Brown, J. Bussons Gordo3, P.M. Chadwick, L.-M. Chounet4, R. Cornils, L. Costamante, B. Degrange4, A. Djannati-Ataï1, 2, L.O'C. Drury, G. Dubus, T. Ergin, P. Espigat1, 2, F. Feinstein3, P. Fleury4, G. Fontaine4, S. Funk, Y. Gallant3, B. Giebels4, S. Gillessen, P. Goret, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, W. Hofmann, M. Holleran, D. Horns, O.C. de Jager, I. Jung, B. Khelifi, Nu. Komin, A. Konopelko, I.J. Latham, R. Le Gallou, A. Lemière1, 2, M. Lemoine4, N. Leroy4, T. Lohse, A. Marcowith, C. Masterson, T.J.L. Mccomb, M. De Naurois5, S.J. Nolan, A. Noutsos, K.J. Orford, J.L. Osborne, M. Ouchrif5, M. Panter, G. Pelletier, S. Pita1, 2, M. Pohl, G. Puhlhofer, M. Punch1, 2, B.C. Raubenheimer, M. Raue, J. Raux, S.M. Rayner, I. Redondo, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland, G. Rowell, V. Sahakian, L. Sauge, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, R. Steenkamp, C. Stegmann, J.-P. Tavernet5, R. Terrier1, 2, C.G. Théoret1, 2, M. Tluczykont4, G. Vasileiadis3, C. Venter, P. Vincent5, B. Visser, H.J. Volk, S.J. Wagner
For the HESS collaboration(s)

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 \propto 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.
1:  PCC - Physique Corpusculaire et Cosmologie - Collège de France
2:  APC - UMR 7164 - AstroParticule et Cosmologie
3:  LPTA - Laboratoire de Physique Théorique et Astroparticules
4:  LLR - Laboratoire Leprince-Ringuet
5:  LPNHE - Laboratoire de Physique Nucléaire et de Hautes Énergies
Physics/Astrophysics/Cosmology and Extra-Galactic Astrophysics

Sciences of the Universe/Astrophysics
ISM: supernova remnants – ISM: individual objects: G 0.9+0.1 – gamma-rays: observations
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