Discovery of extended VHE gamma-ray emission from the asymmetric pulsar wind nebula in MSH 15-52 with H.E.S.S.
- Aharonian, F.
- Akhperjanian, A.
- Aye, K.
- Bazer-Bachi, A.
- Beilicke, M.
- Benbow, W.
- Berge, D.
- Berghaus, P.
- Bernlöhr, K.
- Bolz, O.
- Boisson, C.
- Glicenstein, J.
- Breitling, F.
- Brown, A.
- Bussons Gordo, J.
- Chadwick, P.
- Braun, I.
- Chounet, L.
- Cornils, R.
- Costamante, L.
- Degrange, B.
- Djannati-Atai, A.
- Drury, L.
- Emmanoulopoulos, D.
- Espigat, P.
- Feinstein, F.
- Fleury, P.
- Fontaine, G.
- Funk, S.
- Gallant, Y.
- Giebels, B.
- Gillessen, S.
- Goret, P.
- Dubus, G.
- Hadjichristidis, C.
- Hauser, M.
- Heinzelmann, G.
- Henri, G.
- Hermann, G.
- Hinton, J.
- Hofmann, W.
- Holleran, M.
- Horns, D.
- de Jager, O.
- Khélifi, B.
- Komin, N.
- Konopelko, A.
- Latham, I.
- Le Gallou, R.
- Lemoine-Goumard, M.
- Lemière, A.
- Leroy, N.
- Lohse, T.
- Marcowith, A.
- Masterson, C.
- McComb, T.
- de Naurois, M.
- Nolan, S.
- Noutsos, A.
- Orford, K.
- Osborne, J.
- Ouchrif, M.
- Panter, M.
- Pelletier, G.
- Pita, S.
- Fuchs, Y.
- Pühlhofer, G.
- Punch, M.
- Raubenheimer, B.
- Raue, M.
- Raux, J.
- Rayner, S.
- Redondo, I.
- Reimer, A.
- Reimer, O.
- Ripken, J.
- Terrier, R.
- Rob, L.
- Rolland, L.
- Rowell, G.
- Sahakian, V.
- Saugé, L.
- Schlenker, S.
- Schlickeiser, R.
- Schuster, C.
- Schwanke, U.
- Siewert, M.
- Sol, H.
- Steenkamp, R.
- Stegmann, C.
- Tavernet, J.
- Théoret, C.
- Tluczykont, M.
- Venter, C.
- Vasileiadis, G.
- Vincent, P.
- Völk, H.
- Wagner, S.
- Martineau-Huynh, O.
DOIAbstract
The Supernova Remnant MSH 15-52 has been observed in very high energy (VHE) gamma-rays using the HESS 4-telescope array located in Namibia. A gamma-ray signal is detected at the 25 sigma level during an exposure of 22.1 h live time. The image reveals an elliptically shaped emission region around the pulsar PSR B1509-58, with semi-major axis ~6' in the NW-SE direction and semi-minor axis ~2'. This morphology coincides with the diffuse pulsar wind nebula as observed at X-ray energies by ROSAT. The overall energy spectrum from 280 GeV up to 40 TeV can be fitted by a power law with photon index Γ = 2.27 ± 0.03stat ± 0.20syst. The detected emission can be plausibly explained by inverse Compton scattering of accelerated relativistic electrons wi...
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