Discovery of the two "wings" of the Kookaburra complex in VHE γ-rays with HESS

被引：75
作者：
Aharonian, F.
Akhperjanian, A. G.
Bazer-Bachi, A. R.
Beilicke, M.
Benbow, W.
Berge, D.
Bernloehr, K.
Boisson, C.
Bolz, O.
Borrel, V.
Braun, I.
Brown, A. M.
Buehler, R.
Buesching, I.
Carrigan, S.
Chadwick, P. M.
Chounet, L. -M.
Cornils, R.
Costamante, L.
Degrange, B.
Dickinson, H. J.
Djannati-Atai, A.
Drury, L. O'C.
Dubus, G.
Egberts, K.
Emmanoulopoulos, D.
Espigat, P.
Feinstein, F.
Ferrero, E.
Fiasson, A.
Fontaine, G.
Funk, S.
Funk, S.
Fuessling, M.
Gallant, Y. A.
Giebels, B.
Glicenstein, J. F.
Goret, P.
Hadjichristidis, C.
Hauser, D.
Hauser, M.
Heinzelmann, G.
Henri, G.
Hermann, G.
Hinton, J. A.
Hoffmann, A.
Hofmann, W.
Holleran, M.
Horns, D.
Jacholkowska, A.
机构：
[1] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany
[2] Yerevan Phys Inst, Yerevan 375036, Armenia
[3] CNRS, Ctr Etud Spatiale Rayonnements, UPS, F-31029 Toulouse 4, France
[4] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany
[5] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany
[6] Observ Paris, CNRS, UMR 8102, LUTH,Sect Meudon, F-92195 Meudon, France
[7] Univ Durham, Dept Phys, Durham DH1 3LE, England
[8] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa
[9] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France
[10] Univ Paris 07, CEA, Observ Paris, CNRS,UMR 7164,APC, F-75231 Paris 05, France
[11] Dublin Inst Adv Studies, Dublin 2, Ireland
[12] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany
[13] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticulaires, F-34095 Montpellier 5, France
[14] CEA Saclay, CEA, DSM, DAPNIA, F-91191 Gif Sur Yvette, France
[15] Univ Grenoble 1, CNRS, INSU, Lab Astrophys Grenoble, F-38041 Grenoble 9, France
[16] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany
[17] Univ Paris 06, CNRS, Lab Phys Nucl & Hautes Energies, IN2P3, F-75252 Paris 5, France
[18] Univ Paris 07, CNRS, Lab Phys Nucl & Hautes Energies, IN2P3, F-75252 Paris 5, France
[19] Charles Univ Prague, Inst Nucl & Particle Phys, CR-18000 Prague 8, Czech Republic
[20] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany
[21] Univ Namibia, Windhoel, Namibia
[22] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany
来源：
ASTRONOMY & ASTROPHYSICS | 2006年 / 456卷 / 01期
关键词：
ISM : general; gamma rays : observations; radiation mechanisms : non-thermal;
D O I：
10.1051/0004-6361:20065511
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Aims. Search for Very High Energy gamma-ray emission in the Kookaburra complex through observations with the HESS array. Methods. Stereoscopic imaging of Cherenkov light emission of the gamma-ray showers in the atmosphere is used for the reconstruction and selection of the events to search for gamma-ray signals. Their spectrum is derived by a forward-folding maximum likelihood fit. Results. Two extended gamma-ray sources with an angular (68%) radius of 3.3-3.4' are discovered at high (> 13 sigma) statistical significance: HESS J1420-607 and HESS J1418-609. They exhibit a flux above 1 TeV of (2.97 +/- 0.18(stat) +/- 0.60(sys)) x 10(-12) and (2.17 +/- 0.17d(stat) +/- 0.43(sys)) x 10(-12) cm(-2) s(-1), respectively, and similar hard photon indices similar to 2.2. Multi-wavelength comparisons show spatial coincidence with the wings of the Kookaburra. Two pulsar wind nebul ae candidates, K3/PSR J1420-6048 and the Rabbit, lie on the edge of the HESS sources. Conclusions. The two new sources confirm the non-thermal nature of at least parts of the two radio wings which overlap with the gamma-ray emission and establish their connection with the two X-ray pulsar wind nebul ae candidates. Given the large point spread function of EGRET, the unidentified source(s) 3EG J1420-6038/GeV J1417-6100 could possibly be related to either or both HESS sources. The most likely explanation for the Very High Energy gamma-rays discovered by HESS is inverse Compton emission of accelerated electrons on the CosmicMicrowave Background near the two candidate pulsar wind nebul ae, K3/PSR J1420-6048 and the Rabbit. Two scenarios which could lead to the observed large (similar to 10 pc) offset-nebula type morphologies are briefly discussed.
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页码：245 / 251
页数：7
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