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

被引：0

作者：

Aharonian, F. ^{[1
]}

Akhperjanian, A.G. ^{[2
]}

Bazer-Bachi, A.R. ^{[3
]}

Beilicke, M. ^{[4
]}

Benbow, W. ^{[1
]}

Berge, D. ^{[1
]}

Bernlöhr, K. ^{[1
,5
]}

Boisson, C. ^{[6
]}

Bolz, O. ^{[1
]}

Borrel, V. ^{[3
]}

Braun, I. ^{[1
]}

Brown, A.M. ^{[7
]}

Bühler, R. ^{[1
]}

Büsching, I. ^{[8
]}

Carrigan, S. ^{[1
]}

Chadwick, P.M. ^{[7
]}

Chounet, L.-M. ^{[9
]}

Cornils, R. ^{[4
]}

Costamante, L. ^{[1
,20
]}

Degrange, B. ^{[9
]}

Dickinson, H.J. ^{[7
]}

Djannati-Ataï, A. ^{[10
]}

O'C Drury, L. ^{[11
]}

Dubus, G. ^{[9
]}

Egberts, K. ^{[1
]}

Emmanoulopoulos, D. ^{[12
]}

Espigat, P. ^{[10
]}

Feinstein, F. ^{[13
]}

Ferrero, E. ^{[12
]}

Fiasson, A. ^{[13
]}

Fontaine, G. ^{[9
]}

Funk, S. ^{[5
]}

Funk, S. ^{[1
]}

Füßling, M. ^{[5
]}

Gallant, Y.A. ^{[13
]}

Giebels, B. ^{[9
]}

Glicenstein, J.F. ^{[14
]}

Goret, P. ^{[14
]}

Hadjichristidis, C. ^{[7
]}

Hauser, D. ^{[1
]}

Hauser, M. ^{[12
]}

Heinzelmann, G. ^{[4
]}

Henri, G. ^{[15
]}

Hermann, G. ^{[1
]}

Hinton, J.A. ^{[1
,12
]}

Hoffmann, A. ^{[16
]}

Hofmann, W. ^{[1
]}

Holleran, M. ^{[8
]}

Horns, D. ^{[16
]}

Jacholkowska, A. ^{[13
]}

机构：

[1] Max-Planck-Institut für Kernphysik, PO Box 103980, 69029 Heidelberg, Germany

[2] Yerevan Physics Institute, 2 Alikhanian Brothers St., 375036 Yerevan, Armenia

[3] Centre d'Étude Spatiale des Rayonnements, CNRS/UPS, 9 Av. du Colonel Roche, 31029 Toulouse Cedex 4, France

[4] Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, 22761 Hamburg, Germany

[5] Institut für Physik, Humboldt-Universität zu Berlin, Newtonstr. 15, 12489 Berlin, Germany

[6] LUTH, UMR 8102 du CNRS, Section de Meudon, 92195 Meudon Cedex, France

[7] University of Durham, Department of Physics, South Road, Durham DH1 3LE, United Kingdom

[8] Unit for Space Physics, North-West University, Potchefstroom 2520, South Africa

[9] Laboratoire Leprince-Ringuet, IN2P3/CNRS, École Polytechnique, 91128 Palaiseau, France

[10] APC, UMR 7164 (CNRS, Université Paris VII, CEA, Observatoire de Paris), 11 place Marcelin Berthelot, 75231 Paris Cedex 05, France

[11] Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Ireland

[12] Landessternwarte, Universität Heidelberg, Königstuhl, 69117 Heidelberg, Germany

[13] Laboratoire de Physique Théorique et Astroparticules, IN2P3/CNRS, Université Montpellier II, CC 70, Place Eugène Bataillon, 34095 Montpellier Cedex 5, France

[14] DAPNIA/DSM/CEA, CE Saclay, 91191 Gif-sur-Yvette Cedex, France

[15] Laboratoire d'Astrophysique de Grenoble, INSU/CNRS, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, France

[16] Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany

[17] Laboratoire de Physique Nucléaire et de Hautes Énergies, IN2P3/CNRS, Universités Paris VI and VII, 4 place Jussieu, 75252 Paris Cedex 5, France

[18] Institute of Particle and Nuclear Physics, Charles University, V Holesovickach 2, 180 00 Prague 8, Czech Republic

[19] Institut für Theoretische Physik, Lehrstuhl IV: Weltraum und Astrophysik, Ruhr-Universität Bochum, 44780 Bochum, Germany

[20] European Associated Laboratory for Gamma-Ray Astronomy

来源：

Astronomy and Astrophysics | 2006年 / 456卷 / 01期

关键词：

Aims. Search for Very High Energy γ-ray emission in the Kookaburra complex through observations with the HESS array. Methods. Stereoscopic imaging of Cherenkov light emission of the γ-ray showers in the atmosphere is used for the reconstruction and selection of the events to search for γ-ray signals. Their spectrum is derived by a forward-folding maximum likelihood fit. Results. Two extended γ-ray sources with an angular (68%) radius of 3.3-3.4′ are discovered at high (>13σ) statistical significance: HESS J1420-607 and HESS J1418-609. They exhibit a flux above 1 TeV of (2.97 ±0.188stat ±0.60sys) × 1012 and (2.17 ±0.17stat ±0.43sys) × 1012 cm-2 s-1; respectively; and similar hard photon indices ∼2.2. Multi-wavelength comparisons show spatial coincidence with the wings of the Kookaburra. Two pulsar wind nebulae 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 γ-ray emission and establish their connection with the two X-ray pulsar wind nebulae 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 γ-rays discovered by HESS is inverse Compton emission of accelerated electrons on the Cosmic Microwave Background near the two candidate pulsar wind nebulæ; K3/PSR J1420-6048 and the Rabbit. Two scenarios which could lead to the observed large (∼10 pc) offset-nebula type morphologies are briefly discussed. © ESO 2006;

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页码：245 / 251

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