Searching for TeV Gamma-Ray Emission from SGR 1935+2154 during Its 2020 X-Ray and Radio Bursting Phase

被引：7

作者：

Abdalla, H. ^{[1
]}

Aharonian, F. ^{[2
,3
,4
]}

Benkhali, F. Ait ^{[3
]}

Anguner, E. O. ^{[5
]}

Arcaro, C. ^{[6
]}

Armand, C. ^{[7
]}

Armstrong, T. ^{[8
]}

Ashkar, H. ^{[9
]}

Backes, M. ^{[1
,6
]}

Baghmanyan, V ^{[10
]}

Martins, V. Barbosa ^{[11
]}

Barnacka, A. ^{[12
]}

Barnard, M. ^{[6
]}

Becherini, Y. ^{[13
]}

Berge, D. ^{[11
]}

Bernloehr, K. ^{[3
]}

Bi, B. ^{[14
]}

Bottcher, M. ^{[6
]}

Boisson, C. ^{[15
]}

Bolmont, J. ^{[16
]}

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

Breuhaus, M. ^{[3
]}

Brose, R. ^{[2
]}

Brun, F. ^{[9
]}

Brun, P. ^{[9
]}

Bryan, M. ^{[17
]}

Buechele, M. ^{[18
]}

Bulik, T. ^{[19
]}

Bylund, T. ^{[13
]}

Cangemi, F. ^{[20
]}

Caroff, S. ^{[7
]}

Carosi, A. ^{[7
]}

Casanova, S. ^{[3
,10
]}

Chambery, P. ^{[21
]}

Chand, T. ^{[6
]}

Chandra, S. ^{[6
]}

Chen, A. ^{[22
]}

Cotter, G. ^{[8
]}

Curylo, M. ^{[19
]}

Mbarubucyeye, J. Damascene ^{[11
]}

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

Davies, J. ^{[8
]}

Deil, C. ^{[3
]}

Devin, J. ^{[23
]}

Dirson, L. ^{[24
]}

Djannati-Atai, A. ^{[23
]}

Dmytriiev, A. ^{[15
]}

Donath, A. ^{[3
]}

Doroshenko, V ^{[14
]}

Dreyer, L. ^{[6
]}

机构：

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

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

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

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

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

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

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

[11] DESY, D-15738 Zeuthen, Germany

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

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

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

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

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

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

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

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

[20] LPNHE, Hautes Energies, 4 Pl Jussieu, F-75252 Paris, France

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

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

[23] Univ Paris, Astroparticule & Cosmol, CNRS, F-75013 Paris, France

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[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] IDESY, D-15738 Zeuthen, Germany

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

[42] Konan Univ, Dept Phys, Higashinada Ku, 8-9-1 Okamoto, Kobe, Hyogo 6588501, Japan

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

来源：

ASTROPHYSICAL JOURNAL | 2021年 / 919卷 / 02期

基金：

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

关键词：

MAGNETARS; LIMITS; FLARE;

D O I：

10.3847/1538-4357/ac0fe1

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Magnetar hyperflares are the most plausible explanation for fast radio bursts (FRBs)-enigmatic powerful radio pulses with durations of several milliseconds and high brightness temperatures. The first observational evidence for this scenario was obtained in 2020 April when an FRB was detected from the direction of the Galactic magnetar and soft gamma-ray repeater SGR 1935+2154. The FRB was preceded by two gamma-ray outburst alerts by the BAT instrument aboard the Swift satellite, which triggered follow-up observations by the High Energy Stereoscopic System (H.E.S.S.). H.E.S.S. observed SGR 1935+2154 for 2 hr on 2020 April 28. The observations are coincident with X-ray bursts from the magnetar detected by INTEGRAL and Fermi-GBM, thus providing the first very high energy gamma-ray observations of a magnetar in a flaring state. High-quality data acquired during these follow-up observations allow us to perform a search for short-time transients. No significant signal at energies E > 0.6 TeV is found, and upper limits on the persistent and transient emission are derived. We here present the analysis of these observations and discuss the obtained results and prospects of the H.E.S.S. follow-up program for soft gamma-ray repeaters.

引用

页数：9

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