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AHARONIAN, F; AKHPERJANIAN, A. G; BOLZ, O; BRAUN, I; BREITLING, F; BROWN, A. M; BUSSONS GORDO, J; CHADWICK, P. M; CHOUNET, L.-M; CORNILS, R; COSTAMANTE, L; DEGRANGE, B; AYE, K.-M; DJANNATI-ATAÏ, A; DRURY, L. Oc; DUBUS, G; EMMANOULOPOULOS, D; ESPIGAT, P; FEINSTEIN, F; FLEURY, P; FONTAINE, G; FUCHS, Y; FUNK, S; BAZER-BACHI, A. R; GALLANT, Y. A; GIEBELS, B; GILLESSEN, S; GLICENSTEIN, J. F; GORET, P; HADJICHRISTIDIS, C; HAUSER, M; HEINZELMANN, G; HENRI, G; HERMANN, G; BEILICKE, M; HINTON, J. A; HOFMANN, W; HOLLERAN, M; HARNS, D; DE JAGER, O. C; JOHNSTON, S; KHELIFI, B; KIRK, J. G; KOMIN, Nu; KONOPELKO, A; BENBOW, W; LATHAM, I. J; LE GALLOU, R; LEMIERE, A; LEMOINE-GOUMARD, M; LEROY, N; MARTINEAU-HUYNH, O; LOHSE, T; MARCOWITH, A; MASTERSON, C; MCCOMB, T. J. L; BERGE, D; BERGHAUS, P; BERNLÖHR, K; BOISSON, C
Astronomy & astrophysics, 10/2005, Volume: 442, Issue: 1Journal Article
We report the discovery of very-high-energy (VHE) g-ray emission of the binary system PSR B 1259-63/SS 2883 of a radio pulsar orbiting a massive, luminous Be star in a highly eccentric orbit. The observations around the 2004 periastron passage of the pulsar were performed with the four 13 m Cherenkov telescopes of the HESS experiment, recently installed in Namibia and in full operation since December 2003. Between February and June 2004, a g-ray signal from the binary system was detected with a total significance above 13s. The flux was found to vary significantly on timescales of days which makes PSR B 1259-63 the first variable galactic source of VHE g-rays observed so far. Strong emission signals were observed in pre- and post-periastron phases with a flux minimum around periastron, followed by a gradual flux decrease in the months after. The measured time-averaged energy spectrum above a mean threshold energy of 380 GeV can be fitted by a simple power law F0(E/1 TeV)G with a photon index G = 2.7 c 0.2stat c 0.2sys and flux normalisation F0 = (1.3 c 0.1stat c 0.3sys) x 10-12 TeV-1 cm-2 s-1. This detection of VHE g-rays provides unambiguous evidence for particle acceleration to multi-TeV energies in the binary system. In combination with coeval observations of the X-ray synchrotron emission by the RXTE and INTEGRAL instruments, and assuming the VHE g-ray emission to be produced by the inverse Compton mechanism, the magnetic field strength can be directly estimated to be of the order of 1 G.
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