Author(s): Aharonian F., Akhperjanian A.G., Aye K.-M., Bazer-Bachi A.R., Berghaus P., Bussons Gordo J., Chounet L.-M., Degrange B., Djannati-Ataï A., Espigat P., Feinstein F., Fleury P., Fontaine G., Gallant Y., Giebels B., Lemière A., Leroy N., Marcowith A., De Naurois M., Ouchrif M., Pita S., Punch M., Raux J., Rolland L., Tavernet J.-P., Terrier R., Théoret C.G., Tluczykont M., Vasileiadis G., Vincent P.
(Article) Published:
Astronomy & Astrophysics, vol. 432 p.L9-L12 (2005)
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Ref HAL: in2p3-00023668_v1
Ref Arxiv: astro-ph/0501512
DOI: 10.1051/0004-6361:200500008
Ref. & Cit.: NASA ADS
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Abstract:
The region around PSR B1706-44 has been observed with the H.E.S.S. imaging atmospheric Cherenkov telescopes in 2003. No evidence for gamma-ray emission in the TeV range was found at the pulsar position or at the radio arc which corresponds to the supernova remnant G 343.1-2.3. The 99% confidence level flux upper limit at the pulsar position is Ful(E > 350GeV) = 1.4e-12 /cm^2/s assuming a power law with photon index of 2.5 and Ful(E > 500GeV) = 1.3e-12 /cm^2/s without an assumption on the spectral shape. The reported upper limits correspond to 8% of the flux from an earlier detection by the CANGAROO experiment.