Evidence of 100 TeV γ-ray emission from HESS J1702-420: A new PeVatron candidate

被引：20

作者：

Abdalla, H. ^{[1
]}

Aharonian, F. ^{[3
,4
,5
]}

Benkhali, F. Ait ^{[4
]}

Anguner, E. O. ^{[6
]}

Arcaro, C. ^{[10
]}

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. ^{[10
]}

Becherini, Y. ^{[14
]}

Berge, D. ^{[12
]}

Bernloehr, K. ^{[4
]}

Bi, B. ^{[15
]}

Bottcher, M. ^{[10
]}

Boisson, C. ^{[16
]}

Bolmont, J. ^{[17
]}

de Lavergne, M. de Bony ^{[7
]}

Breuhaus, M. ^{[4
]}

Brun, F. ^{[9
]}

Brun, P. ^{[9
]}

Bryan, M. ^{[18
]}

Buechele, M. ^{[19
]}

Bulik, T. ^{[20
]}

Bylund, T. ^{[14
]}

Caroff, S. ^{[7
]}

Carosi, A. ^{[7
]}

Casanova, S. ^{[4
,11
]}

Chand, T. ^{[10
]}

Chandra, S. ^{[10
]}

Chen, A. ^{[21
]}

Cotter, G. ^{[8
]}

Mbarubucyeye, J. Damascene ^{[12
]}

Davids, I. D. ^{[1
]}

Davies, J. ^{[8
]}

Deil, C. ^{[4
]}

Devin, J. ^{[25
]}

Dirson, L. ^{[24
]}

Djannati-Atai, A. ^{[25
]}

Dmytriiev, A. ^{[16
]}

Donath, A. ^{[4
]}

Doroshenko, V ^{[15
]}

Dreyer, L. ^{[10
]}

Duffy, C. ^{[26
]}

Dyks, J. ^{[27
]}

Egberts, K. ^{[28
]}

Eichhorn, F. ^{[19
]}

机构：

[1] Univ Namibia, Dept Phys, Private Bag 13301, Windhoek 10005, Namibia

[2] Ecole Polytech, Lab Leprince Ringuet, CNRS, Inst Polytech Paris, 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 Grenoble Alpes, Univ Savoie Mt Blanc, Lab Annecy Phys Particules, LAPP,CNRS, F-74000 Annecy, France

[8] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

[9] Univ Paris Saclay, CEA, IRFU, F-91191 Gif Sur Yvette, France

[10] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa

[11] Inst Fizyki Jadrowej PAN, Ul Radzikowskiego 152, PL-31342 Krakow, Poland

[12] DESY, D-15738 Zeuthen, Germany

[13] Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland

[14] Linnaeus Univ, Dept Phys & Elect Engn, SE-35195 Vaxjo, Sweden

[15] Inst Astron & Astrophys, Univ Tubingen, Sand 1, D-72076 Tubingen, Germany

[16] Univ Paris, Univ PSL, Observ Paris, Lab Univers & Theories,CNRS, F-92190 Meudon, France

[17] Univ Paris Diderot, Sorbonne Univ, Lab Phys Nucl & Hautes Energies, LPNHE,CNRS IN2P3,Sorbonne Paris Cite, 4 Pl Jussieu, F-75252 Paris, France

[18] Univ Amsterdam, Anton Pannekoek Inst Astron, 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, CNRS IN2P3, Ctr Etud Nucl Bordeaux Gradignan, 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 Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany

[29] Univ Montpellier, Lab Univers & Particules Montpellier, CNRS IN2P3, 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, Fac Phys Astron & Informat, Inst Astron, 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, Univ Tokyo Inst Adv Study UTIAS, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwa No Ha, Kashiwa, Chiba 2778583, Japan

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 653卷

基金：

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

关键词：

gamma rays; general; radiation mechanisms; non-thermal; cosmic rays; methods; data analysis; PULSAR WIND NEBULA; PARTICLE-ACCELERATION; LIKELIHOOD ANALYSIS; AREA TELESCOPE; COSMIC-RAYS; X-RAY; GALAXY; ASSOCIATIONS; SPECTRA; CATALOG;

D O I：

10.1051/0004-6361/202140962

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. The identification of PeVatrons, hadronic particle accelerators reaching the knee of the cosmic ray spectrum (few x 10(15) eV), is crucial to understand the origin of cosmic rays in the Galaxy. We provide an update on the unidentified source HESS J1702-420, a promising PeVatron candidate. Methods. We present new observations of HESS J1702-420 made with the High Energy Stereoscopic System (H.E.S.S.), and processed using improved analysis techniques. The analysis configuration was optimized to enhance the collection area at the highest energies. We applied a threedimensional likelihood analysis to model the source region and adjust non thermal radiative spectral models to the gamma-ray data. We also analyzed archival Fermi Large Area Telescope data to constrain the source spectrum at gamma-ray energies >10 GeV. Results. We report the detection of gamma-rays up to 100 TeV from a specific region of HESS J1702-420, which is well described by a new source component called HESS J1702-420A that was separated from the bulk of TeV emission at a 5:4 sigma confidence level. The power law gamma-ray spectrum of HESS J1702-420A extends with an index of Gamma = 1:53 +/- 0:19(stat) +/- 0:20(sys) and without curvature up to the energy band 64 113 TeV, in which it was detected by H.E.S.S. at a 4:0 sigma confidence level. This makes HESS J1702-420A a compelling candidate site for the presence of extremely high energy cosmic rays. With a flux above 2 TeV of (2:08 +/- 0:49(stat) +/- 0:62(sys)) x 10(-13) cm(-2) s(-1) and a radius of (0:06 +/- 0:02(stat) +/- 0:03(sys))degrees, HESS J1702-420A is outshone - below a few tens of TeV - by the companion HESS J1702-420B. The latter has a steep spectral index of = 2:62 +/- 0:10(stat) +/- 0:20(sys) and an elongated shape, and it accounts for most of the low-energy HESS J1702-420 flux. Simple hadronic and leptonic emission models can be well adjusted to the spectra of both components. Remarkably, in a hadronic scenario, the cut-o ff energy of the particle distribution powering HESS J1702-420A is found to be higher than 0:5 PeV at a 95% confidence level. Conclusions. For the first time, H.E.S.S. resolved two components with significantly di fferent morphologies and spectral indices, both detected at >5 sigma confidence level, whose combined emissions result in the source HESS J1702-420. We detected HESS J1702-420A at a 4:0 sigma confidence level in the energy band 64 113 TeV, which brings evidence for the source emission up to 100 TeV. In a hadronic emission scenario, the hard gamma-ray spectrum of HESS J1702-420A implies that the source likely harbors PeV protons, thus becoming one of the most solid PeVatron candidates detected so far in H.E.S.S. data. However, a leptonic origin of the observed TeV emission cannot be ruled out either.

引用

页数：21

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