Detection of very-high-energy γ-ray emission from the colliding wind binary η Car with HESS

被引：14

作者：

Abdalla, H. ^{[1
]}

Adam, R. ^{[26
]}

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

Benkhali, F. Ait ^{[3
]}

Anguner, E. O. ^{[19
]}

Arakawa, M. ^{[37
]}

Arcaro, C. ^{[1
]}

Armand, C. ^{[22
]}

Armstrong, T. ^{[41
]}

Ashkar, H. ^{[17
]}

Backes, M. ^{[1
,8
]}

Martins, V. Barbosa ^{[33
]}

Barnard, M. ^{[1
]}

Becherini, Y. ^{[10
]}

Berge, D. ^{[33
]}

Bernloehr, K. ^{[3
]}

Blackwell, R. ^{[13
]}

Bottcher, M. ^{[1
]}

Boisson, C. ^{[14
]}

Bolmont, J. ^{[15
]}

Bonnefoy, S. ^{[33
]}

Bregeon, J. ^{[16
]}

Breuhaus, M. ^{[3
]}

Brun, F. ^{[17
]}

Brun, P. ^{[17
]}

Bryan, M. ^{[9
]}

Buchele, M. ^{[32
]}

Bulik, T. ^{[18
]}

Bylund, T. ^{[10
]}

Caroff, S. ^{[15
]}

Carosi, A. ^{[22
]}

Casanova, S. ^{[3
,20
]}

Cerruti, M. ^{[15
,42
]}

Chand, T. ^{[1
]}

Chandra, S. ^{[1
]}

Chen, A. ^{[21
]}

Colafrancesco, S. ^{[21
]}

Cotter, G. ^{[41
]}

Curylo, M. ^{[18
]}

Davids, I. D. ^{[8
]}

Davies, J. ^{[41
]}

Deil, C. ^{[3
]}

Devin, J. ^{[24
]}

dewilt, P. ^{[13
]}

Dirson, L. ^{[2
]}

Djannati-Atai, A. ^{[27
]}

Dmytriiev, A. ^{[1
,14
]}

Donath, A. ^{[3
]}

Doroshenko, V. ^{[25
]}

Dyks, J. ^{[30
]}

机构：

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

[2] Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany

[3] Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany

[4] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland

[5] RAU, High Energy Astrophys Lab, 123 Hovsep Emin St, Yerevan 0051, Armenia

[6] Yerevan Phys Inst, 2 Alikhanian Bros St, Yerevan 375036, Armenia

[7] Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany

[8] Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia

[9] Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[10] Linnaeus Univ, Dept Phys & Elect Engn, S-35195 Vaxjo, Sweden

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

[12] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[13] Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia

[14] Univ Paris Diderot, PSL Res Univ, Observ Paris, LUTH,CNRS, 5 Pl Jules Janssen, F-92190 Meudon, France

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

[16] Univ Montpellier, Lab Univers & Particules Montpellier, CNRS, IN2P3, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France

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

[18] Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland

[19] Aix Marseille Univ, CNRS, IN2P3, CPPM, Marseille, France

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

[21] Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa

[22] Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS,LAPP, F-74000 Annecy, France

[23] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany

[24] Univ Bordeaux, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France

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

[26] Ecole Polytech, CNRS, Lab Leprince Ringuet, Inst Polytech Paris, F-91128 Palaiseau, France

[27] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, AstroParticule & Cosmol,APC,CNRS,IN2P3,CEA Irfu, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France

[28] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

[29] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England

[30] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland

[31] Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany

[32] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany

[33] DESY, D-15738 Zeuthen, Germany

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

[35] Nicolaus Copernicus Univ, Fac Phys Astron & Informat, Ctr Astron, Grudziadzka 5, PL-87100 Torun, Poland

[36] Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa

[37] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan

[38] Univ Tokyo, Inst Adv Study UTIAS, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwa No Ha, Kashiwa, Chiba 2778583, Japan

[39] Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan

[40] RIKEN, 2-1 Hirosawa, Wako, Saitama 3510198, Japan

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

[42] Univ Barcelona, Inst Ciencies Cosmos ICC UB, Marti Franques 1, E-08028 Barcelona, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 635卷

基金：

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

关键词：

astroparticle physics; radiation mechanisms: non-thermal; binaries: general; stars: individual: eta Car; stars: Wolf-Rayet; cosmic rays; CARINAE; ACCELERATION; NEBULA;

D O I：

10.1051/0004-6361/201936761

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. Colliding wind binary systems have long been suspected to be high-energy (HE; 100 MeV < E < 100 GeV) gamma-ray emitters. eta Car is the most prominent member of this object class and is confirmed to emit phase-locked HE gamma rays from hundreds of MeV to 100 GeV energies. This work aims to search for and characterise the very-high-energy (VHE; E >100 GeV) gamma-ray emission from eta Car around the last periastron passage in 2014 with the ground-based High Energy Stereoscopic System (H.E.S.S.).Methods. The region around eta Car was observed with H.E.S.S. between orbital phase p = 0.78-1.10, with a closer sampling at p approximate to 0.95 and p approximate to 1.10 (assuming a period of 2023 days). Optimised hardware settings as well as adjustments to the data reduction, reconstruction, and signal selection were needed to suppress and take into account the strong, extended, and inhomogeneous night sky background (NSB) in the eta Car field of view. Tailored run-wise Monte-Carlo simulations (RWS) were required to accurately treat the additional noise from NSB photons in the instrument response functions.Results. H.E.S.S. detected VHE gamma-ray emission from the direction of eta Car shortly before and after the minimum in the X-ray light-curve close to periastron. Using the point spread function provided by RWS, the reconstructed signal is point-like and the spectrum is best described by a power law. The overall flux and spectral index in VHE gamma rays agree within statistical and systematic errors before and after periastron. The gamma-ray spectrum extends up to at least 400 GeV. This implies a maximum magnetic field in a leptonic scenario in the emission region of 0.5 Gauss. No indication for phase-locked flux variations is detected in the H.E.S.S. data.

引用

页数：8

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