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Search for TeV emission from the region around PSR B1706-44 with the H.E.S.S. experiment

Aharonian, F. / Akhperjanian, A.G. / Aye, K.-M. / Bazer-Bachi, A.R. / Beilicke, M. / Benbow, W. / Berge, D. / Berghaus, P. / Bernlohr, K. / Boisson, C. / Bolz, O. / Borgneier, C. / Bruan, I. / Breitling, F. / Brown, A.M. / Bussons Gordo, J. / Chadwick, P.M. / Chounet, L.-M. / Cornils, R. / Costamante, L. / Degrange, B. / Djannati-Ataï, A. / Drury, L.O'C. / Dubus, G. / Ergin, T. / Espigat, P. / Feinstein, F. / Fleury, P. / Fontaine, G. / Fuchs, Y. / Funk, S. / Gallant, Y. / Giebels, B. / Gillessen, S. / Goret, P. / Hadjichristidis, C. / Hauser, M. / Heinzelmann, G. / Henri, G. / Hermann, G. / Hofmann, W. / Holleran, M. / Horns, D. / De Jager, O.C. / Jung, I. / Khelifi, B. / Komin, Nu. / Konopelko, A. / Latham, I.J. / Le Gallou, R. / Lemière, A. / Lemoine, M. / Leroy, N. / Lohse, T. / Marcowith, A. / Masterson, C. / Mccomb, T.J.L. / De Naurois, M. / Nolan, S.J. / Noutsos, A. / Orford, K.J. / Osborne, J.L. / Ouchrif, M. / Panter, M. / Pelletier, G. / Pita, S. / Puhlhofer, G. / Punch, M. / Raubenheimer, B.C. / Raue, M. / Raux, J. / Rayner, S.M. / Redondo, I. / Reimer, A. / Reimer, O. / Ripken, J. / Rob, L. / Rolland, L. / Rowell, G. / Sahakian, V. / Sauge, L. / Schlenker, S. / Schlickeiser, R. / Schuster, C. / Schwanke, U. / Siewert, M. / Sol, H. / Steenkamp, R. / Stegmann, C. / Tavernet, J.-P. / Terrier, R. / Théoret, C.G. / Tluczykont, M. / Vasileiadis, G. / Venter, C. / Vincent, P. / Visser, B. / Volk, H.J. / Wagner, S.J. - 2015
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.

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