HESS OBSERVATIONS OF THE PROMPT AND AFTERGLOW PHASES OF GRB 060602B

被引:27
作者
Aharonian, F. [1 ,2 ]
Akhperjanian, A. G. [3 ]
De Almeida, U. Barres [4 ]
Bazer-Bachi, A. R. [5 ]
Behera, B. [6 ]
Beilicke, M. [7 ]
Benbow, W. [1 ]
Bernloehr, K. [1 ]
Boisson, C. [9 ]
Borrel, V. [5 ]
Braun, I. [1 ]
Brion, E. [10 ]
Brucker, J. [11 ]
Buehler, R. [1 ]
Bulik, T. [12 ]
Buesching, I. [13 ]
Boutelier, T. [14 ]
Carrigan, S. [1 ]
Chadwick, P. M. [4 ]
Chaves, R. [1 ]
Chounet, L. -M. [15 ]
Clapson, A. C. [1 ]
Coignet, G.
Cornils, R. [7 ]
Costamante, L. [1 ]
Dalton, M. [8 ]
Degrange, B. [15 ]
Dickinson, H. J. [4 ]
Djannati-Atai, A. [16 ]
Domainko, W. [1 ]
Drury, L. O'C. [2 ]
Dubois, F.
Dubus, G. [14 ]
Dyks, J. [12 ]
Egberts, K. [1 ]
Emmanoulopoulos, D. [6 ]
Espigat, P. [16 ]
Farnier, C. [17 ]
Feinstein, F. [17 ]
Fiasson, A. [17 ]
Foerster, A. [1 ]
Fontaine, G. [15 ]
Fuessling, M. [8 ]
Gabici, S. [2 ]
Gallant, Y. A. [17 ]
Giebels, B. [15 ]
Glicenstein, J. F. [10 ]
Glueck, B. [11 ]
Goret, P. [10 ]
Hadjichristidis, C. [4 ]
机构
[1] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany
[2] Dublin Inst Adv Studies, Dublin, Ireland
[3] Yerevan Phys Inst, Yerevan, Armenia
[4] Univ Durham, Dept Phys, Durham DH1 3HP, England
[5] CNRS UPS, Ctr Etud Spatiale Rayonnements, Toulouse, France
[6] Heidelberg Univ, Konigstuhl, Germany
[7] Univ Hamburg, Inst Expt Phys, Hamburg, Germany
[8] Humboldt Univ, Inst Phys, D-1086 Berlin, Germany
[9] Univ Paris Diderot, CNRS, Observ Paris, LUTH, Paris, France
[10] CE Saclay, CEA, DSM, DAPNIA, Gif Sur Yvette, France
[11] Univ Erlangen Nurnberg, Inst Phys, D-8520 Erlangen, Germany
[12] Nicholas Copernicus Astron Ctr, Warsaw, Poland
[13] North West Univ, Unit Space Phys, Potchefstroom, South Africa
[14] Univ Grenoble 1, CNRS, INSU, Lab Astrophys Grenoble, Grenoble, France
[15] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France
[16] CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, Annecy Le Vieux, France
[17] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, Montpellier, France
[18] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England
[19] Univ Tubingen, Inst Astron & Astrophys, D-72074 Tubingen, Germany
[20] Nicholas Copernicus Univ, Torun Ctr Astron, Torun, Poland
[21] Univ Paris 06, Univ Paris 07, CNRS, IN2P3,LPNHE, F-75252 Paris 05, France
[22] Charles Univ Prague, Inst Particle & Nucl Phys, Prague, Czech Republic
[23] Uniwersytet Jagiellonski, Obserwatorium Astron, Krakow, Poland
[24] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia
[25] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, Bochum, Germany
[26] Univ Namibia, Windhoek, Namibia
基金
新加坡国家研究基金会; 英国科学技术设施理事会;
关键词
gamma rays: bursts; gamma rays: observations; GAMMA-RAY BURSTS; VERY-HIGH-ENERGY; TEV EMISSION; MODEL; CONSTRAINTS; COMPONENT; DURATION; SPECTRUM; 970417A; PROTONS;
D O I
10.1088/0004-637X/690/2/1068
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report on the first completely simultaneous observation of a gamma-ray burst (GRB) using an array of Imaging Atmospheric Cherenkov Telescopes, which is sensitive to photons in the very high energy (VHE) gamma-ray range (greater than or similar to 100 GeV). On 2006 June 2, the Swift Burst Alert Telescope (BAT) registered an unusually soft gamma-ray burst (GRB 060602B). The burst position was under observation using the High Energy Stereoscopic System (HESS) at the time the burst occurred. Data were taken before, during, and after the burst. A total of 5 hr of observations were obtained during the night of 2006 June 2-3, and five additional hours were obtained over the next three nights. No VHE gamma-ray signal was found during the period covered by the HESS observations. The 99% confidence level flux upper limit (> 1 TeV) for the prompt phase (9 s) of GRB 060602B is 2.9 x 10(-9) erg cm(-2) s(-1). Due to the very soft BAT spectrum of the burst compared with other Swift GRBs and its proximity to the Galactic center, the burst is likely associated with a Galactic X-ray burster, although the possibility of it being a cosmological GRB cannot be ruled out. We discuss the implications of our flux limits in the context of these two bursting scenarios.
引用
收藏
页码:1068 / 1073
页数:6
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