HESS upper limit on the very high energy γ-ray emission from the globular cluster 47 Tucanae

被引：25

作者：

Aharonian, F. ^{[1
,2
]}

Akhperjanian, A. G. ^{[3
]}

Anton, G. ^{[4
]}

de Almeida, U. Barres ^{[5
]}

Bazer-Bachi, A. R. ^{[6
]}

Becherini, Y. ^{[7
]}

Behera, B. ^{[8
]}

Bernloehr, K. ^{[1
,9
]}

Boisson, C. ^{[10
]}

Bochow, A. ^{[1
]}

Borrel, V. ^{[6
]}

Braun, I. ^{[1
]}

Brion, E. ^{[11
]}

Brucker, J. ^{[4
]}

Brun, P. ^{[11
]}

Buehler, R. ^{[1
]}

Bulik, T. ^{[12
]}

Buesching, I. ^{[13
]}

Boutelier, T. ^{[14
]}

Chadwick, P. M. ^{[5
]}

Charbonnier, A. ^{[15
]}

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

Cheesebrough, A. ^{[5
]}

Chounet, L. -M. ^{[16
]}

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

Coignet, G. ^{[17
]}

Dalton, M. ^{[9
]}

Daniel, M. K. ^{[5
]}

Davids, I. D. ^{[13
,18
]}

Degrange, B. ^{[16
]}

Deil, C. ^{[1
]}

Dickinson, H. J. ^{[5
]}

Djannati-Atai, A. ^{[7
]}

Domainko, W. ^{[1
]}

Drury, L. O'C. ^{[2
]}

Dubois, F. ^{[17
]}

Dubus, G. ^{[14
]}

Dyks, J. ^{[12
]}

Dyrda, M. ^{[19
]}

Egberts, K. ^{[1
]}

Emmanoulopoulos, D. ^{[8
]}

Espigat, P. ^{[7
]}

Farnier, C. ^{[20
]}

Feinstein, F. ^{[20
]}

Fiasson, A. ^{[20
]}

Foerster, A. ^{[1
]}

Fontaine, G. ^{[16
]}

Fuessling, M. ^{[9
]}

Gabici, S. ^{[2
]}

Gallant, Y. A. ^{[20
]}

机构：

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

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

[3] Yerevan Phys Inst, Yerevan 375036, Armenia

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

[5] Univ Durham, Dept Phys, Durham DH1 3LE, England

[6] CNRS UPS, Ctr Etud Spatiale Rayonnements, F-31029 Toulouse 4, France

[7] Univ Paris 07, CNRS, CEA, Observ Paris,UMR 7164, F-75205 Paris 13, France

[8] Univ Heidelberg, D-69117 Heidelberg, Germany

[9] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany

[10] Univ Paris Diderot, LUTH, Observ Paris, CNRS, F-92190 Meudon, France

[11] CE Saclay, IRFU, DSM, CEA, F-91191 Gif Sur Yvette, France

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

[13] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa

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

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

[16] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France

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

[18] Univ Namibia, Windhoek, Namibia

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

[20] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3,CC 70, F-34095 Montpellier 5, France

[21] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany

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

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

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

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

[26] Univ Jagiellonski, Obserwatorium Astron, PL-30244 Krakow, Poland

[27] Stanford Univ, HEPL & KIPAC, Stanford, CA 94305 USA

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2009年 / 499卷 / 01期

关键词：

Galaxy: globular clusters: individual: 47 Tucanae; stars: pulsars: general; gamma rays: observations; MILLISECOND PULSARS; GLOBULAR-CLUSTER-47; TUCANAE; VELA-X; 47-TUCANAE; RADIATION; DISCOVERY; NEBULA; CATALOG; CORE; CRAB;

D O I：

10.1051/0004-6361/200811564

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Observations of the globular cluster 47 Tucanae (NGC 104), which contains at least 23 ms pulsars, were performed with the HESS telescope system. The observations lead to an upper limit of F(E > 800 GeV) < 6.7 x 10(-13) cm(-2) s(-1) on the integral gamma-ray photon flux from 47 Tucanae. Considering millisecond pulsars as the unique potential source of gamma-rays in the globular cluster, constraints based on emission models are derived: on the magnetic field in the average pulsar nebula and on the conversion efficiency of spin-down power to gamma-ray photons or to relativistic leptons.

引用

页码：273 / 277

页数：5

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