Bonn 2010 – wissenschaftliches Programm
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T: Fachverband Teilchenphysik
T 93: Gammaastronomie II
T 93.5: Vortrag
Dienstag, 16. März 2010, 17:50–18:05, HG XVII
Detection of VHE gamma-ray emission from the vicinity of PSR B1706-44 with H.E.S.S. — •Ryan C. G. Chaves1, Emma de Oña Wilhelmi1, Régis Terrier2, Christian Stegmann3, Bruno Khélifi4, and Okkie C. de Jager5 — 1Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany — 2APC, CNRS, Univ. Paris 7 Denis Diderot, 10, rue Alice Domon et Leonie Duquet, F-75205 Paris Cedex 13, France — 3Universität Erlangen-Nürnberg, Physikalisches Institut, Erwin-Rommel-Str. 1, D 91058 Erlangen, Germany — 4LLR, Ecole Polytechnique, CNRS/IN2P3, F-91128 Palaiseau, France — 5Unit for Space Physics, North-West Univ., Potchefstroom 2520, South Africa
The gamma-ray pulsar PSR B1706-44 and the adjacent supernova remnant (SNR) candidate G343.1-2.3 were observed by H.E.S.S. during a dedicated observational campaign in 2007. A new source of very-high-energy (VHE; E > 100 GeV) gamma-ray emission, HESS J1708-443, was discovered with its centroid at RA(J2000.0) = 17h8m10s and Dec(J2000.0) = -44d21’ (± 3’ statistical error on each axis). The VHE gamma-ray source is significantly more extended than the H.E.S.S. point-spread function and has an intrinsic Gaussian width of 0.29 deg ± 0.04 deg. Its energy spectrum can be described by a power law with a photon index = 2.0 ± 0.1 (stat) ± 0.2 (syst). The integral flux measured between 1 and 10 TeV is ∼17% of the Crab Nebula flux in the same energy range. The possible associations with the energetic PSR B1706-44, also recently detected in the GeV domain with Fermi/LAT and AGILE, and SNR G343.1-2.3 are discussed.