Very high energy gamma-ray observations of the galaxy clusters Abell 496 and Abell 85 with HESS

被引：41

作者：

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

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

Anton, G. ^{[16
]}

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

Bazer-Bachi, A. R.

Becherini, Y. ^{[12
,29
]}

Behera, B. ^{[14
]}

Bernloehr, K. ^{[1
,5
]}

Boisson, C.

Bochow, A. ^{[1
]}

Borrel, V.

Braun, I. ^{[1
]}

Brion, E. ^{[7
]}

Brucker, J. ^{[16
]}

Brun, P. ^{[7
]}

Buehler, R. ^{[1
]}

Bulik, T. ^{[24
]}

Buesching, I. ^{[9
]}

Boutelier, T. ^{[17
]}

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

Charbonnier, A. ^{[19
]}

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

Cheesebrough, A. ^{[8
]}

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

Clapson, A. C. ^{[1
]}

Coignet, G. ^{[11
]}

Dalton, M. ^{[5
]}

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

Degrange, B. ^{[10
]}

Deil, C. ^{[1
]}

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

Djannati-Atai, A. ^{[12
,29
]}

Domainko, W. ^{[1
]}

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

Dubois, F. ^{[11
]}

Dubus, G. ^{[17
]}

Dyks, J. ^{[24
]}

Dyrda, M. ^{[28
]}

Egberts, K. ^{[1
]}

Emmanoulopoulos, D. ^{[14
]}

Espigat, P. ^{[12
,29
]}

Farnier, C. ^{[15
]}

Feinstein, F. ^{[15
]}

Fiasson, A. ^{[15
]}

Foerster, A. ^{[1
]}

Fontaine, G. ^{[10
]}

Fuessling, M. ^{[5
]}

Gabici, S. ^{[13
]}

Gallant, Y. A. ^{[15
]}

Gerard, L. ^{[12
,29
]}

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, LUTH, Observ Paris, F-92190 Meudon, France

[7] CE Saclay, DSM, IRFU, CEA, 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, Lab Leprince Ringuet, CNRS, IN2P3, F-91128 Palaiseau, France

[11] CNRS, Lab Annecy Le Vieux Phys Particules, IN2P3, F-74941 Annecy Le Vieux, France

[12] Univ Paris 07, CNRS, F-75205 Paris 13, France

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

[14] Heidelberg Univ, 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 07, Univ Paris 06, LPNHE, CNRS,IN2P3, F-75252 Paris 5, France

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

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

[22] Univ Namibia, Windhoek, Namibia

[23] Uniwersytet Jagiellonski, Obserwatorium Astron, 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 Paris 07, CNRS, UMR 7164, CEA,Observ Paris, F-75205 Paris 13, France

来源：

ASTRONOMY & ASTROPHYSICS | 2009年 / 495卷 / 01期

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：

galaxies: clusters: individual: Abell 496; galaxies: clusters: individual: Abell 85; gamma rays: observations; LARGE-SCALE STRUCTURE; X-RAY; INTRACLUSTER MEDIUM; SUPERNOVA-REMNANTS; MAGNETIC-FIELDS; CRAB-NEBULA; EMISSION; PROTONS; RADIATION; HALO;

D O I：

10.1051/0004-6361:200811372

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. The nearby galaxy clusters Abell 496 and Abell 85 are studied in the very high-energy (VHE, E > 100 GeV) band to investigate VHE cosmic rays (CRs) in this class of objects which are the largest gravitationally bound systems in the Universe. Methods. HESS, an array of four imaging atmospheric cherenkov telescopes (IACT), was used to observe the targets in the range of VHE gamma rays. Results. No significant gamma-ray signal is found at the respective position of the two clusters with several different source size assumptions for each target. In particular, emission regions corresponding to the high-density core, to the extension of the entire X-ray emission in these clusters, and to the very extended region where the accretion shock is expected are investigated. Upper limits are derived for the gamma-ray flux at energies E > 570 GeV for Abell 496 and E > 460 GeV for Abell 85. Conclusions. From the non-detection in VHE gamma rays, upper limits on the total energy of hadronic CRs in the clusters are calculated. If the cosmic-ray energy density follows the large-scale gas density profile, the limit on the fraction of energy in these non-thermal particles with respect to the total thermal energy of the intra-cluster medium (ICM) is 51% for Abell 496 and only 8% for Abell 85 due to its higher mass and higher gas density. These upper limits are compared with theoretical estimates. They predict about similar to 10% of the thermal energy of the ICM in non-thermal particles. The observations presented here can constrain these predictions especially for the case of the Abell 85 cluster.

引用

页码：27 / 35

页数：9

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