Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/11141
Title: Very high energy gamma rays from the composite SNR G0.9+0.1
Authors: Aharonian, F.
Akhperjanian, A. G.
Aye, K. M.
Bazer-Bachi, A. R.
Beilicke, M.
Benbow, W.
Berge, D.
Berghaus, P.
Bernlohr, K.
Boisson, C.
Bolz, O.
Borgmeier, C.
Braun, I.
Breitling, F.
Brown, A. M.
Gordo, J. B.
Chadwick, P. M.
Chounet, L. M.
Cornils, R.
Costamante, L.
Degrange, B.
Djannati-Atai, A.
Drury, LO.
Dubus, G.
Ergin, T.
Espigat, P.
Feinstein, F.
Fleury, P.
Fontaine, G.
Funk, S.
Gallant, Y. A.
Giebels, B.
Gillessen, S.
Goret, P.
Hadjichristidis, C.
Hauser, M.
Heinzelmann, G.
Henri, G.
Hermann, G.
Hinton, J. A.
Hofmann, W.
Holleran, M.
Horns, D.
de Jager O. C.
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, T. J. L.
de Naurois M.
Nolan, S. J.
Noutsos, A.
Orford, K. J.
Osborne, J. L.
Ouchrif, M.
Panter, M.
Pelletier, G.
Pita, S.
Puhlhofer, G.
Punch, M.
Raubenheimer, B. C.
Raue, M.
Raux, J.
Rayner, S. M.
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, J. P.
Terrier, R.
Theoret, C. G.
Tluczykont, M.
Vasileiadis, G.
Venter, C.
Vincent, P.
Visser, B.
Volk, H. J.
Wagner, S. J.
First Published: Mar-2005
Publisher: EDP Sciences for European Southern Observatory (ESO)
Citation: Astronomy & Astrophysics, 2005, 432 (2), pp. L25-L29
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 $\approx$$13\sigma$, and a photon flux above 200 GeV of ( $5.7\pm0.7_{\rm stat}\pm1.2_{\rm sys})\times10^{-12}$ 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 ( ${\rm d}N/{\rm d}E \propto E^{-\Gamma}$) with photon index $\Gamma = 2.40\pm0.11_{\rm stat}\pm0.20_{\rm sys}$. 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.
DOI Link: 10.1051/0004-6361:200500022
ISSN: 0004-6361
Links: http://hdl.handle.net/2381/11141
http://www.aanda.org/articles/aa/abs/2005/11/aagl153/aagl153.html
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: Copyright © 2005 ESO. Reproduced with permission from Astronomy & Astrophysics, © ESO.
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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