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dc.contributor.authorAharonian, F.-
dc.contributor.authorAkhperjanian, A. G.-
dc.contributor.authorAye, K. M.-
dc.contributor.authorBazer-Bachi, A. R.-
dc.contributor.authorBeilicke, M.-
dc.contributor.authorBenbow, W.-
dc.contributor.authorBerge, D.-
dc.contributor.authorBerghaus, P.-
dc.contributor.authorBernlohr, K.-
dc.contributor.authorBoisson, C.-
dc.contributor.authorBolz, O.-
dc.contributor.authorSchlenker, S.-
dc.contributor.authorSchlickeiser, R.-
dc.contributor.authorSchuster, C.-
dc.contributor.authorSchwanke, U.-
dc.contributor.authorSiewert, M.-
dc.contributor.authorSkjaeraasen, O.-
dc.contributor.authorSol, H.-
dc.contributor.authorSteenkamp, R.-
dc.contributor.authorStegmann, C.-
dc.contributor.authorTavernet, J. P.-
dc.contributor.authorTerrier, R.-
dc.contributor.authorTheoret, C. G.-
dc.contributor.authorTluczykont, M.-
dc.contributor.authorVasileiadis, G.-
dc.contributor.authorVenter, C.-
dc.contributor.authorVincent, P.-
dc.contributor.authorVolk, H. J.-
dc.contributor.authorWagner, S. J.-
dc.contributor.authorBraun, I.-
dc.contributor.authorBreitling, F.-
dc.contributor.authorBrown, A. M.-
dc.contributor.authorGordo, J. B.-
dc.contributor.authorChadwick, P. M.-
dc.contributor.authorChounet, L. M.-
dc.contributor.authorCornils, R.-
dc.contributor.authorCostamante, L.-
dc.contributor.authorDegrange, B.-
dc.contributor.authorDjannati-Atai, A.-
dc.contributor.authorDrury, L. O.-
dc.contributor.authorDubus, G.-
dc.contributor.authorEmmanoulopoulos, D.-
dc.contributor.authorEspigat, P.-
dc.contributor.authorFeinstein, F.-
dc.contributor.authorFleury, P.-
dc.contributor.authorFontaine, G.-
dc.contributor.authorFuchs, Y.-
dc.contributor.authorFunk, S.-
dc.contributor.authorGallant, Y. A.-
dc.contributor.authorGiebels, B.-
dc.contributor.authorGillessen, S.-
dc.contributor.authorGlicenstein, J. F.-
dc.contributor.authorGoret, P.-
dc.contributor.authorHadjichristidis, C.-
dc.contributor.authorHauser, M.-
dc.contributor.authorHeinzelmann, G.-
dc.contributor.authorHenri, G.-
dc.contributor.authorHermann, G.-
dc.contributor.authorHinton, J. A.-
dc.contributor.authorHofmann, W.-
dc.contributor.authorHolleran, M.-
dc.contributor.authorHorns, D.-
dc.contributor.authorde Jager O. C.-
dc.contributor.authorJohnston, S.-
dc.contributor.authorKhelifi, B.-
dc.contributor.authorKirk, J. G.-
dc.contributor.authorKomin, N.-
dc.contributor.authorKonopelko, A.-
dc.contributor.authorLatham, IJ.-
dc.contributor.authorLe Gallou R.-
dc.contributor.authorLemiere, A.-
dc.contributor.authorLemoine-Goumard, M.-
dc.contributor.authorLeroy, N.-
dc.contributor.authorMartineau-Huynh, O.-
dc.contributor.authorLohse, T.-
dc.contributor.authorMarcowith, A.-
dc.contributor.authorMasterson, C.-
dc.contributor.authorMcComb, T. J. L.-
dc.contributor.authorde Naurois M.-
dc.contributor.authorNolan, S. J.-
dc.contributor.authorNoutsos, A.-
dc.contributor.authorOrford, K. J.-
dc.contributor.authorOsborne, J. L.-
dc.contributor.authorOuchrif, M.-
dc.contributor.authorPanter, M.-
dc.contributor.authorPelletier, G.-
dc.contributor.authorPita, S.-
dc.contributor.authorPuhlhofer, G.-
dc.contributor.authorPunch, M.-
dc.contributor.authorRaubenheimer, B. C.-
dc.contributor.authorRaue, M.-
dc.contributor.authorRaux, J.-
dc.contributor.authorRayner, S. M.-
dc.contributor.authorRedondo, I.-
dc.contributor.authorReimer, A.-
dc.contributor.authorReimer, O.-
dc.contributor.authorRipken, J.-
dc.contributor.authorRob, L.-
dc.contributor.authorRolland, L.-
dc.contributor.authorRowell, G.-
dc.contributor.authorSahakian, V.-
dc.contributor.authorSauge, L.-
dc.identifier.citationAstronomy & Astrophysics, 2005, 442 (1), pp. 1-10-
dc.description.abstractWe report the discovery of very-high-energy (VHE) $\gamma$-ray emission of the binary system PSR B1259-63 / 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 $\gamma$-ray signal from the binary system was detected with a total significance above $13\sigma$. The flux was found to vary significantly on timescales of days which makes PSR B1259-63 the first variable galactic source of VHE $\gamma$-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 $F_0(E/1\,\rm TeV)^{-\Gamma}$ with a photon index $\Gamma = 2.7\pm0.2_\mathrm{stat}\pm0.2_\mathrm{sys}$ and flux normalisation $F_0 = (1.3 \pm 0.1_\mathrm{stat} \pm 0.3_\mathrm{sys}) \times 10^{-12}\,\rm TeV^{-1}\,\rm cm^{-2}\,\rm s^{-1}$. This detection of VHE $\gamma$-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 $\gamma$-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.-
dc.publisherEDP Sciences for European Southern Observatory (ESO)-
dc.rightsCopyright © 2005 ESO. Reproduced with permission from Astronomy & Astrophysics, © ESO.-
dc.sourceWeb of Science (Lite)-
dc.subjectgamma-rays : observations-
dc.subjectstars : pulsars : individual : PSR B1259-63-
dc.titleDiscovery of the binary pulsar PSRB1259-63 in very-high-energy gamma rays around periastron with HESS-
dc.typeJournal Article-
dc.description.versionPublisher Version-
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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