First detection of VHE γ-rays from SN 1006 by HESS

被引：135

作者：

Acero, F. ^{[15
]}

Aharonian, F. ^{[1
,13
]}

Akhperjanian, A. G.

Anton, G. ^{[16
]}

de Almeida, U. Barres ^{[8
]}

Bazer-Bachi, A. R.

Becherini, Y. ^{[12
]}

Behera, B. ^{[14
]}

Beilicke, M.

Bernloehr, K. ^{[1
]}

Bochow, A. ^{[1
]}

Boisson, C. ^{[6
]}

Bolmont, J. ^{[19
]}

Borrel, V. ^{[3
]}

Brucker, J. ^{[16
]}

Brun, F. ^{[19
]}

Brun, P. ^{[7
]}

Buehler, R. ^{[1
]}

Bulik, T. ^{[29
]}

Buesching, I. ^{[9
]}

Boutelier, T. ^{[17
]}

Chadwick, P. M. ^{[8
]}

Charbonnier, A. ^{[1
,19
]}

Chaves, R. C. G. ^{[1
]}

Cheesebrough, A. ^{[8
]}

Conrad, J. ^{[31
]}

Chounet, L. -M. ^{[10
]}

Clapson, A. C.

Coignet, G. ^{[11
]}

Dalton, M. ^{[5
]}

Daniel, M. K. ^{[8
]}

Davids, I. D. ^{[9
,22
]}

Degrange, B. ^{[10
]}

Deil, C. ^{[1
]}

Dickinson, H. J. ^{[8
]}

Djannati-Atai, A. ^{[12
]}

Domainko, W. ^{[1
]}

Drury, L. O'C. ^{[13
]}

Dubois, F. ^{[11
]}

Dubus, G. ^{[17
]}

Dyks, J. ^{[24
]}

Dyrda, M. ^{[28
]}

Egberts, K. ^{[1
,30
]}

Eger, P. ^{[16
]}

Espigat, P. ^{[12
]}

Fallon, L. ^{[13
]}

Farnier, C. ^{[15
]}

Fegan, S. ^{[10
]}

Feinstein, F. ^{[15
]}

Fiasson, A. ^{[11
]}

机构：

[1] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany

[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] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92190 Meudon, 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, Lab Leprince Ringuet, CNRS, IN2P3, 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, Astroparticule & Cosmol APC, UMR 7164, F-75205 Paris 13, France

[13] Dublin Inst Adv Studies, Dublin 2, Ireland

[14] Heidelberg Univ, Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany

[15] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, F-34095 Montpellier 5, France

[16] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany

[17] Univ Grenoble 1, CNRS, INSU, Lab Astrophys Grenoble, F-38041 Grenoble 9, France

[18] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany

[19] Univ Paris 06, CNRS, IN2P3, LPNHE,Univ Denis Diderot Paris 7, F-75252 Paris 5, France

[20] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, Prague 18000 8, Czech Republic

[21] Ruhr Univ Bochum, Lehrstuhl Weltraum & Astrophy 4, Inst Theoret Phys, D-44780 Bochum, Germany

[22] Univ Namibia, Windhoek, Namibia

[23] Univ Jagiellonski, Astron Observ, PL-30244 Krakow, Poland

[24] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland

[25] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England

[26] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia

[27] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland

[28] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland

[29] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland

[30] Univ Innsbruck, Inst Astro & Teilchenphy, A-6020 Innsbruck, Austria

[31] Univ Stockholm, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden

[32] Royal Inst Technol KTH, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden

[33] Univ Bordeaux 1, CEN Bordeaux Gradignan, CNRS, IN2P3,UMR 5797, F-33175 Gradignan, France

[34] Univ Utrecht, Astron Inst Utrecht, NL-3508 TA Utrecht, Netherlands

来源：

ASTRONOMY & ASTROPHYSICS | 2010年 / 516卷

基金：

英国科学技术设施理事会; 新加坡国家研究基金会;

关键词：

gamma rays: stars; supernovae: individual: SN 1006 (G327.6+14.6); AZIMUTHAL VARIATIONS; SUPERNOVA-REMNANTS; ACCELERATION; SHOCK; SN-1006; INJECTION; EMISSION; SYSTEM; TELESCOPE; PARTICLES;

D O I：

10.1051/0004-6361/200913916

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. Recent theoretical predictions of the lowest very high energy (VHE) luminosity of SN 1006 are only a factor 5 below the previously published HESS upper limit, thus motivating further in-depth observations of this source. Methods. Deep observations at VHE energies (above 100 GeV) were carried out with the high energy stereoscopic system (HESS) of Cherenkov Telescopes from 2003 to 2008. More than 100 h of data have been collected and subjected to an improved analysis procedure. Results. Observations resulted in the detection of VHE gamma-rays from SN 1006. The measured gamma-ray spectrum is compatible with a power-law, the flux is of the order of 1% of that detected from the Crab Nebula, and is thus consistent with the previously established HESS upper limit. The source exhibits a bipolar morphology, which is strongly correlated with non-thermal X-rays. Conclusions. Because the thickness of the VHE-shell is compatible with emission from a thin rim, particle acceleration in shock waves is likely to be the origin of the gamma-ray signal. The measured flux level can be accounted for by inverse Compton emission, but a mixed scenario that includes leptonic and hadronic components and takes into account the ambient matter density inferred from observations also leads to a satisfactory description of the multi-wavelength spectrum.

引用

页数：7

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