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

被引：17

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

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 644卷

基金：

澳大利亚研究理事会; 奥地利科学基金会; 日本学术振兴会; 新加坡国家研究基金会; 英国科学技术设施理事会;

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.

引用

页数：8

共 42 条

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