Discovery of very-high-energy γ-ray emission from the vicinity of PSR J1913+1011 with HESS

被引：28

作者：

Aharonian, F.

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

de Almeida, U. Barres

Bazer-Bachi, A. R. ^{[3
]}

Behera, B. ^{[15
]}

Beilicke, M. ^{[4
]}

Benbow, W. ^{[1
]}

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

Boisson, C. ^{[6
]}

Bolz, O. ^{[1
]}

Borrel, V. ^{[3
]}

Braun, I. ^{[1
]}

Brion, E. ^{[7
]}

Brown, A. M. ^{[8
]}

Buehler, R. ^{[1
]}

Bulik, T. ^{[26
]}

Buesching, I. ^{[9
]}

Boutelier, T. ^{[18
]}

Carrigan, S. ^{[1
]}

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

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

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

Coignet, G. ^{[11
]}

Cornils, R. ^{[4
]}

Costamante, L. ^{[1
,30
]}

Dalton, M. ^{[5
]}

Degrange, B. ^{[10
]}

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

Djannati-Atai, A. ^{[12
,13
]}

Domainko, W. ^{[1
]}

Drury, L. O'C. ^{[14
]}

Dubois, F. ^{[11
]}

Dubus, G. ^{[18
]}

Dyks, J. ^{[26
]}

Egberts, K. ^{[1
]}

Emmanoulopoulos, D. ^{[15
]}

Espigat, P. ^{[12
,13
]}

Farnier, C. ^{[16
]}

Feinstein, F. ^{[16
]}

Fiasson, A. ^{[16
]}

Foerster, A. ^{[1
]}

Fontaine, G. ^{[10
]}

Funk, Seb. ^{[5
]}

Fuessling, M. ^{[5
]}

Gallant, Y. A. ^{[16
]}

Giebels, B. ^{[10
]}

Glicenstein, J. F. ^{[7
]}

Glueck, B. ^{[16
,17
]}

Goret, P. ^{[7
]}

Hadjichristidis, C. ^{[8
]}

机构：

[1] Max Planck Inst Kernphys, D-69117 Heidelberg, Germany

[2] Yerevan Phys Inst, Yerevan, Armenia

[3] CNRS UPS, Ctr Etud Spatiale Rayonnements, Toulouse, France

[4] Univ Hamburg, Inst Expt Phys, Hamburg, Germany

[5] Humboldt Univ, Inst Phys, D-1086 Berlin, Germany

[6] Univ Paris 07, LUTH, Observ Paris, CNRS, Meudon, France

[7] CE Saclay, DAPNIA DSM CEA, Gif Sur Yvette, France

[8] Univ Durham, Dept Phys, Durham DH1 3HP, England

[9] NW Univ, Unit Space Phys, Potchefstroom, South Africa

[10] CNRS IN2P3, Lab Leprince Ringuet, Ecole Polytech, Palaiseau, France

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

[12] Univ Paris 07, CNRS, APC, Paris, France

[13] Univ Paris 07, UMR 7164, CNRS, CEA,Observ Paris, F-75221 Paris 05, France

[14] Dublin Inst Adv Studies, Dublin, Ireland

[15] Univ Heidelberg, Landessternwarte Konigstuhl, Konigstuhl, Germany

[16] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS IN2P3, Montpellier, France

[17] Univ Erlangen Nurnberg, Inst Phys, D-8520 Erlangen, Germany

[18] Univ Grenoble 1, Astrophys Lab, INSU CNRS, Grenoble, France

[19] Univ Tubingen, Inst Astron & Astrophys, D-72074 Tubingen, Germany

[20] Univ Paris 06, LPNHE, CNRS IN2P3, Paris, France

[21] Univ Paris 07, LPNHE, CNRS IN2P3, Paris, France

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

[23] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl 4, D-4630 Bochum, Germany

[24] Univ Namibia, Windhoek, Namibia

[25] Univ Jagiellonski, Astron Observ, Krakow, Poland

[26] Nicolaus Copernicus Astron Ctr, Warsaw, Poland

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

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

[29] Nicholas Copernicus Univ, Torun Ctr Astron, Torun, Poland

[30] CNRS & MPG, European Associated Lab Gamma Ray Astron, F-75700 Paris, France

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

来源：

ASTRONOMY & ASTROPHYSICS | 2008年 / 484卷 / 02期

基金：

英国科学技术设施理事会;

关键词：

ISM : supernova remnants; gamma rays : observations;

D O I：

10.1051/0004-6361:20078715

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The HESS experiment, an array of four Imaging Atmospheric Cherenkov Telescopes with high sensitivity and large field-of-view, has been used to search for emitters of very-high-energy (VHE, > 100 GeV) gamma-rays along the Galactic plane, covering the region 30 degrees < l < 60 degrees, 280 degrees < l < 330 degrees, and -3 degrees < b < 3 degrees. In this continuation of the HESS Galactic Plane Scan, a new extended VHE gamma-ray source was discovered at alpha(2000)= 19(h)12(m)49(s), delta(2000)=+ 10 degrees 09' 06 ''( HESS J1912+101). Its integral flux between 1-10 TeV is similar to 10% of the Crab Nebula flux in the same energy range. The measured energy spectrum can be described by a power law dN/dE similar to E(-Gamma) with a photon index Gamma = 2.7 +/- 0.2(stat) +/- 0.3sys. HESS J1912+101 is plausibly associated with the high spin-down luminosity pulsar PSR J1913+1011. We also discuss associations with an as yet unconfirmed SNR candidate proposed from low frequency radio observation and/or with molecular clouds found in (13)CO data.

引用

页码：435 / 440

页数：6

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