Probing the Magnetic Field in the GW170817 Outflow Using HESS Observations

被引：14

作者：

Abdalla, H. ^{[1
]}

Adam, R. ^{[2
]}

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

Benkhali, F. Ait ^{[3
]}

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

Arakawa, M. ^{[7
]}

Arcaro, C. ^{[1
]}

Armand, C. ^{[8
]}

Armstrong, T. ^{[9
]}

Ashkar, H. ^{[10
]}

Backes, M. ^{[1
,11
]}

Baghmanyan, V ^{[12
]}

Barbosa-Martins, V ^{[13
]}

Barnacka, A. ^{[14
]}

Barnard, M. ^{[1
]}

Becherini, Y. ^{[15
]}

Berge, D. ^{[13
]}

Bernloehr, K. ^{[3
]}

Blackwell, R. ^{[16
]}

Bottcher, M. ^{[1
]}

Boisson, C. ^{[17
]}

Bolmont, J. ^{[18
]}

Bonnefoy, S. ^{[13
]}

Bregeon, J. ^{[19
]}

Breuhaus, M. ^{[3
]}

Brun, F. ^{[10
]}

Brun, P. ^{[10
]}

Bryan, M. ^{[20
]}

Buechele, M. ^{[21
]}

Bulik, T. ^{[22
]}

Bylund, T. ^{[15
]}

Caroff, S. ^{[18
]}

Carosi, A. ^{[8
]}

Casanova, S. ^{[3
,12
]}

Cerruti, M. ^{[18
,41
]}

Chand, T. ^{[1
]}

Chandra, S. ^{[1
]}

Chen, A. ^{[23
]}

Cotter, G. ^{[9
]}

Curylo, M. ^{[22
]}

Davids, I. D. ^{[11
]}

Davies, J. ^{[9
]}

Deil, C. ^{[3
]}

Devin, J. ^{[24
]}

deWilt, P. ^{[16
]}

Dirson, L. ^{[25
]}

Djannati-Ata, A. ^{[26
]}

Dmytriiev, A. ^{[17
]}

Donath, A. ^{[3
]}

Doroshenko, V ^{[27
]}

机构：

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

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

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

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

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

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

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

[11] Univ Namibia, Dept Phys, Private Bag 13301, Windhoek 12010, Namibia

[12] Inst Fizyki Jadrowej Pan, Ul Radzikowskiego 152, PL-31342 Krakow, Poland

[13] DESY, D-15738 Zeuthen, Germany

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

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

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

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

[18] Sorbonne Univ, Univ Paris Diderot, Lab Phys Nucl & Hautes Energies, Sorbonne Paris Cite,CNRS IN2P3,LPNHE, 5 Pl Jules Janssen, F-75252 Paris, France

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2020年 / 894卷 / 02期

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：

Gamma-ray transient sources; Stellar mergers; Gamma-ray bursts; Gamma-ray astronomy; Ejecta;

D O I：

10.3847/2041-8213/ab8b59

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The detection of the first electromagnetic counterpart to the binary neutron star (BNS) merger remnant GW170817 established the connection between short gamma-ray bursts and BNS mergers. It also confirmed the forging of heavy elements in the ejecta (a so-called kilonova) via the r-process nucleosynthesis. The appearance of nonthermal radio and X-ray emission, as well as the brightening, which lasted more than 100 days, were somewhat unexpected. Current theoretical models attempt to explain this temporal behavior as either originating from a relativistic off-axis jet or a kilonova-like outflow. In either scenario, there is some ambiguity regarding how much energy is transported in the nonthermal electrons versus the magnetic field of the emission region. Combining the Very Large Array (radio) and Chandra (X-ray) measurements with observations in the GeV-TeV domain can help break this ambiguity, almost independently of the assumed origin of the emission. Here we report for the first time on deep H.E.S.S. observations of GW170817/GRB 170817A between 124 and 272 days after the BNS merger with the full H.E.S.S. array of telescopes, as well as on an updated analysis of the prompt (<5 days) observations with the upgraded H.E.S.S. phase-I telescopes. We discuss implications of the H.E.S.S. measurement for the magnetic field in the context of different source scenarios.

引用

页数：5

共 33 条

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