HESS upper limits on very high energy gamma-ray emission from the microquasar GRS 1915+105

被引:11
作者
Acero, F. [1 ]
Aharonian, F. [13 ,31 ]
Akhperjanian, A. G. [2 ]
Anton, G. [15 ]
de Almeida, U. Barres [8 ]
Bazer-Bachi, A. R. [3 ]
Becherini, Y. [12 ]
Behera, B. [14 ]
Bernloehr, K. [5 ,31 ]
Bochow, A. [31 ]
Boisson, C. [6 ]
Bolmont, J. [18 ]
Borrel, V. [3 ]
Brucker, J. [15 ]
Brun, F. [18 ]
Brun, P. [7 ]
Bulik, T. [27 ]
Buesching, I. [9 ]
Boutelier, T. [16 ]
Chadwick, P. M. [8 ]
Charbonnier, A. [18 ]
Chaves, R. C. G. [31 ]
Cheesebrough, A. [8 ]
Conrad, J. [29 ]
Chounet, L. -M. [10 ]
Clapson, A. C. [31 ]
Coignet, G. [11 ]
Dalton, M. [5 ]
Daniel, M. K. [8 ]
Davids, I. D. [9 ,20 ]
Degrange, B. [10 ]
Deil, C. [31 ]
Dickinson, H. J. [8 ]
Djannati-Atai, A. [12 ]
Domainko, W. [31 ]
Drury, L. O'C. [13 ]
Dubois, F. [11 ]
Dubus, G. [16 ]
Dyks, J. [22 ]
Dyrda, M. [26 ]
Egberts, K. [28 ,31 ]
Eger, P. [15 ]
Espigat, P. [12 ]
Fallon, L. [13 ]
Farnier, C. [1 ]
Fegan, S. [10 ]
Feinstein, F. [1 ]
Fiasson, A. [11 ]
Foerster, A. [31 ]
Fontaine, G. [10 ]
机构
[1] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor & Astroparticules, F-34095 Montpellier 5, France
[2] Yerevan Phys Inst, Yerevan 375036, Armenia
[3] UPS, CNRS, Ctr Etud Spatiale Rayonnements, 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] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92190 Meudon, France
[7] CE Saclay, CEA, IRFU, DSM, F-91191 Gif Sur Yvette, France
[8] Univ Durham, Dept Phys, Durham DH1 3LE, England
[9] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa
[10] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France
[11] Univ Savoie, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France
[12] Univ Paris 07, CNRS, UMR 7164, CEA,Observ Paris, F-75205 Paris 13, France
[13] Dublin Inst Adv Studies, Dublin 2, Ireland
[14] Univ Heidelberg, D-69117 Heidelberg, Germany
[15] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany
[16] Univ Grenoble 1, INSU, CNRS, Astrophys Lab, F-38041 Grenoble 9, France
[17] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany
[18] Univ Paris 07, Univ Paris 06, CNRS, LPNHE,IN2P3, F-75252 Paris 5, France
[19] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany
[20] Univ Namibia, Windhoek, Namibia
[21] Uniwersytet Jagiellonski, Obserwatorium Astron, PL-30244 Krakow, Poland
[22] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland
[23] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England
[24] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia
[25] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland
[26] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland
[27] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland
[28] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria
[29] Stockholm Univ, Albanova Univ Ctr, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden
[30] Royal Inst Technol, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden
[31] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany
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
X-rays: binaries; X-rays: individuals: GRS 1915+105; gamma rays: observations; SUPERLUMINAL SOURCE; UNIFIED MODEL; GRS-1915+105; JETS; VARIABILITY; EJECTIONS; DISCOVERY; LS-5039; RADIO; MASS;
D O I
10.1051/0004-6361/200913389
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. High energy particles reside in the relativistic jets of microquasars, making them possible sources of very high energy radiation (VHE, > 100 GeV). Detecting this emission would provide a new handle on jet physics. Aims. Observations of the microquasar GRS 1915+105 with the HESS telescope array were undertaken in 2004-2008 to search for VHE emission. Methods. Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the energy and direction of the incident gamma rays. Results. There is no evidence for a VHE gamma-ray signal either from the direction of the microquasar or its vicinity. An upper limit of 6.1 x 10(-13) ph cm(-2) s(-1) (99.9% confidence level) is set on the photon flux above 410 GeV, equivalent to a VHE luminosity of similar to 10(34) erg s(-1) at 11 kpc. Conclusions. The VHE to X-ray luminosity ratio in GRS 1915+105 is at least four orders of magnitude lower than the ratio observed in gamma-ray binaries. The VHE radiative efficiency of the compact jet is less than 0.01% based on its estimated total power of 10(38) erg s(-1). Particle acceleration in GRS 1915+105 is not efficient at high energies and/or the magnetic field is too strong. It is also possible that VHE gamma-rays are produced by GRS 1915+105, but the emission is highly time-dependent.
引用
收藏
页码:1135 / 1140
页数:6
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