An extreme particle accelerator in the Galactic plane: HESS J1826-130

被引:16
作者
Abdalla, H. [1 ]
Adam, R. [2 ]
Aharonian, F. [3 ,4 ,5 ]
Benkhali, F. Ait [4 ]
Anguner, E. O. [6 ]
Arcaro, C. [1 ]
Armand, C. [7 ]
Armstrong, T. [8 ]
Ashkar, H. [9 ]
Backes, M. [1 ,10 ]
Baghmanyan, V. [11 ]
Martins, V. Barbosa [12 ]
Barnacka, A. [13 ]
Barnard, M. [1 ]
Becherini, Y. [14 ]
Berge, D. [12 ]
Bernlohr, K. [4 ]
Bi, B. [15 ]
Bottcher, M. [1 ]
Boisson, C. [16 ]
Bolmont, J. [17 ]
de Lavergne, M. de Bony [7 ]
Bordas, P. [40 ]
Breuhaus, M. [4 ]
Brun, F. [9 ]
Brun, P. [9 ]
Bryan, M. [18 ]
Buchele, M. [19 ]
Bulik, T. [20 ]
Bylund, T. [14 ]
Caroff, S. [17 ]
Carosi, A. [7 ]
Casanova, S. [4 ,11 ]
Chand, T. [1 ]
Chandra, S. [1 ]
Chen, A. [21 ]
Cotter, G. [8 ]
Curylo, M. [20 ]
Mbarubucyeye, J. Damascene [12 ]
Davids, I. D. [10 ]
Davies, J. [8 ]
Deil, C. [4 ]
Devin, J. [22 ]
deWilt, P. [23 ]
Dirson, L. [24 ]
Djannati-Atai, A. [25 ]
Dmytriiev, A. [16 ]
Donath, A. [4 ]
Doroshenko, V. [15 ]
Duffy, C. [26 ]
机构
[1] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa
[2] CNRS, Inst Polytech Paris, Lab Leprince Ringuet, Ecole Polytech, F-91128 Palaiseau, France
[3] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland
[4] Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany
[5] RAU, High Energy Astrophys Lab, 123 Hovsep Emin St, Yerevan 0051, Armenia
[6] Aix Marseille Univ, CPPM, CNRS, IN2P3, Marseille, France
[7] Univ Savoie Mont Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France
[8] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England
[9] Univ Paris Saclay, IRFU, CEA, F-91191 Gif Sur Yvette, France
[10] Univ Namibia, Dept Phys, Private Bag 13301, Windhoek 10005, Namibia
[11] Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland
[12] DESY, D-15738 Zeuthen, Germany
[13] Uniwersytet Jagiellonski, Obserwatorium Astronom, Ul Orla 171, PL-30244 Krakow, Poland
[14] Linnaeus Univ, Dept Phys & Elect Engn, S-35195 Vaxjo, Sweden
[15] Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany
[16] Univ Paris, Univ PSL, Observ Paris, Lab Universe & Theories,CNRS, F-92190 Meudon, France
[17] Univ Paris Diderot, Sorbonne Univ, Lab Phys Nucl & Hautes Energies, CNRS,IN2P3,LPNHE,Sorbonne Paris Cite, 4 Pl Jussieu, F-75252 Paris, France
[18] Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands
[19] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany
[20] Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland
[21] Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa
[22] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France
[23] Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia
[24] Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany
[25] Univ Paris, CNRS, Astroparticule & Cosmol, F-75013 Paris, France
[26] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England
[27] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland
[28] Univ Potsdam, Inst Physik & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany
[29] Univ Montpellier, Lab Universe & Particules Montpellier, IN2P3, CNRS,CC 72, Pl Eugene Bataillon, F-34095 Montpellier 5, France
[30] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany
[31] Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany
[32] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria
[33] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan
[34] Nicolaus Copernicus Univ, Inst Astron, Fac Phys Astron & Informat, Grudziadzka 5, PL-87100 Torun, Poland
[35] Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa
[36] Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan
[37] Yerevan Phys Inst, 2 Alikhanian Bros St, Yerevan 375036, Armenia
[38] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Inst Adv Study UTIAS, 5-1-5 Kashiwa No Ha, Kashiwa, Chiba 2778583, Japan
[39] Univ Zurich, Phys Inst, Winterthurerstr 190, CH-8057 Zurich, Switzerland
[40] Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICC UB, Marti Franques 1, Barcelona 08028, Spain
基金
新加坡国家研究基金会; 澳大利亚研究理事会; 日本学术振兴会; 英国科学技术设施理事会; 奥地利科学基金会;
关键词
ISM: supernova remnants; ISM: clouds; gamma rays: general; gamma rays: ISM; PULSAR WIND NEBULA; X-RAY; CATALOG; GALAXY;
D O I
10.1051/0004-6361/202038851
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The unidentified very-high-energy (VHE; E > 0.1 TeV) gamma -ray source, HESS J1826-130, was discovered with the High Energy Stereoscopic System (HESS) in the Galactic plane. The analysis of 215 h of HESS data has revealed a steady gamma -ray flux from HESS J1826-130, which appears extended with a half-width of 0.21 degrees +/- 0.02 (stat)degrees stat degrees +/- 0.05 (sys)degrees sys degrees . The source spectrum is best fit with either a power-law function with a spectral index Gamma = 1.78 +/- 0.10(stat) +/- 0.20(sys) and an exponential cut-off at 15.2 (+5.5)(-3.2) -3.2+5.5 TeV, or a broken power-law with Gamma (1) = 1.96 +/- 0.06(stat) +/- 0.20(sys), Gamma (2) = 3.59 +/- 0.69(stat) +/- 0.20(sys) for energies below and above E-br = 11.2 +/- 2.7 TeV, respectively. The VHE flux from HESS J1826-130 is contaminated by the extended emission of the bright, nearby pulsar wind nebula, HESS J1825-137, particularly at the low end of the energy spectrum. Leptonic scenarios for the origin of HESS J1826-130 VHE emission related to PSR J1826-1256 are confronted by our spectral and morphological analysis. In a hadronic framework, taking into account the properties of dense gas regions surrounding HESS J1826-130, the source spectrum would imply an astrophysical object capable of accelerating the parent particle population up to greater than or similar to 200 TeV. Our results are also discussed in a multiwavelength context, accounting for both the presence of nearby supernova remnants, molecular clouds, and counterparts detected in radio, X-rays, and TeV energies.
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页数:8
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