Observation of inverse Compton emission from a long γ-ray burst

被引：190

作者：

Acciari, V. A. ^{[98
,99
]}

Ansoldi, S. ^{[97
,102
]}

Antonelli, L. A. ^{[103
]}

Engels, A. Arbet ^{[104
]}

Baack, D. ^{[105
]}

Babic, A. ^{[106
]}

Banerjee, B. ^{[107
]}

de Almeida, U. Barres ^{[108
]}

Barrio, J. A. ^{[109
,110
]}

Gonzalez, J. Becerra ^{[98
,99
]}

Bednarek, W. ^{[111
]}

Bellizzi, L. ^{[109
,110
]}

Bernardini, E. ^{[114
,115
,116
]}

Berti, A. ^{[117
]}

Besenrieder, J. ^{[118
]}

Bhattacharyya, W. ^{[114
]}

Bigongiari, C. ^{[103
]}

Biland, A. ^{[104
]}

Blanch, O. ^{[119
]}

Bonnoli, G. ^{[109
,110
]}

Bosnjak, Z. ^{[106
]}

Busetto, G. ^{[115
,116
]}

Carosi, R. ^{[120
,121
]}

Ceribella, G. ^{[118
]}

Chai, Y. ^{[118
]}

Chilingaryan, A. ^{[122
]}

Cikota, S. ^{[106
]}

Colak, S. M. ^{[119
]}

Colin, U. ^{[118
]}

Colombo, E. ^{[1
]}

Contreras, J. L. ^{[109
,110
]}

Cortina, J. ^{[123
]}

Covino, S. ^{[103
]}

D'Elia, V. ^{[103
]}

Da Vela, P. ^{[120
,121
]}

Dazzi, F. ^{[103
]}

De Angelis, A. ^{[115
,116
]}

De Lotto, B. ^{[97
]}

Delfino, M. ^{[119
,124
]}

Delgado, J. ^{[119
,124
]}

Depaoli, D. ^{[117
]}

Di Pierro, F. ^{[117
]}

Di Venere, L. ^{[117
]}

Espineira, E. Do Souto ^{[125
]}

Prester, D. Dominis

Donini, A. ^{[97
]}

Dorner, D. ^{[126
]}

Doro, M. ^{[115
,116
]}

Elsaesser, D. ^{[105
]}

Ramazani, V. Fallah ^{[127
]}

机构：

[1] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA

[2] Univ Alabama, Space Sci Dept, Huntsville, AL 35899 USA

[3] Univ Space Res Assoc, Sci & Technol Inst, Huntsville, AL USA

[4] NASA, Astrophys Branch, ST12, Marshall Space Flight Ctr, Huntsville, AL USA

[5] Max Planck Inst Extraterr Phys, Garching, Germany

[6] Kanazawa Univ, Inst Sci & Engn, Fac Math & Phys, Kanazawa, Ishikawa 9201192, Japan

[7] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[8] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD USA

[9] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba, Japan

[10] Stockholm Univ, Dept Phys, Stockholm, Sweden

[11] KTH Royal Inst Technol, Dept Phys, Stockholm, Sweden

[12] Ist Nazl Fis Nucl, Trieste, Italy

[13] Univ Politecn Bari, Dipartimento Fis M Merlin, Bari, Italy

[14] Ist Nazl Fis Nucl, Sez Bari, Bari, Italy

[15] Univ Johannesburg, Dept Phys, Auckland Pk, South Africa

[16] Open Univ Israel, Dept Nat Sci, Raanana, Israel

[17] Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA USA

[18] Stanford Univ, LAC Natl Accelerator Lab, Stanford, CA 94305 USA

[19] Univ Montpellier, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France

[20] INAF, Astron Observ Brera, Merate, Italy

[21] Univ Coll London, Mullard Space Sci Lab, Dorking, Surrey, England

[22] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

[23] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA

[24] Univ Leicester, Dept Phys & Astron, Leicester, Leics, England

[25] INAF, Ist Astrofis Spaziale & Fis Cosm Palermo, Palermo, Italy

[26] Istanbul Univ, Dept Astron & Space Sci, Istanbul, Turkey

[27] INAF, Osservatorio Astron Roma, Rome, Italy

[28] ASI, SSDC, Rome, Italy

[29] INAF IAPS, Rome, Italy

[30] Univ Tor Vergata, Rome, Italy

[31] Gran Sasso Sci Inst, Laquila, Italy

[32] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA, Australia

[33] European Southern Observ, Santiago, Chile

[34] INAF Ist Radioastron, Bologna, Italy

[35] Rhodes Univ, Dept Phys & Elect, Grahamstown, South Africa

[36] South African Radio Astron Observ, Cape Town, South Africa

[37] Astron Inst Acad Sci, Prague, Czech Republic

[38] Univ Malaga, Fac Ciencias, Dept Fis Aplicada, Malaga, Spain

[39] Univ Malaga, Fac Ciencias, Dept Algebra Geometria & Topol, Malaga, Spain

[40] Univ Southampton, Phys & Astron Dept, Southampton, Hants, England

[41] Univ Malaga, Dept Ingn Sistemas & Automat ETS Ingenieros Ind, Unidad Asociada CSIC, Malaga, Spain

[42] CSIC, IAA, Granada, Spain

[43] Indian Inst Space Sci & Technol, Trivandrum, Kerala, India

[44] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool, Merseyside, England

[45] Osservatorio Astron S Di Giacomo Astrocampania, Agerola, Italy

[46] INAF Astron Observ Naples, Naples, Italy

[47] Univ Cape Town, Dept Astron, Interuniv Inst Data Intens Astron, Rondebosch, South Africa

[48] Univ Oxford, Dept Phys, Keble Rd, Oxford, England

[49] Cosm Dawn Ctr DAWN, Copenhagen, Denmark

[50] Univ Copenhagen, Niels Bohr Inst, Copenhagen, Denmark

来源：

NATURE | 2019年 / 575卷 / 7783期

基金：

英国科学技术设施理事会; 瑞典研究理事会; 澳大利亚研究理事会; 欧盟地平线“2020”; 美国国家航空航天局; 芬兰科学院;

关键词：

EXTRAGALACTIC BACKGROUND LIGHT; HIGH-ENERGY EMISSION; MAGIC TELESCOPES; SYNCHROTRON; PERFORMANCE; AFTERGLOW; GRB; CALIBRATION; EVOLUTION; CURVES;

D O I：

10.1038/s41586-019-1754-6

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Long-duration gamma-ray bursts (GRBs) originate from ultra-relativistic jets launched from the collapsing cores of dying massive stars. They are characterized by an initial phase of bright and highly variable radiation in the kiloelectron volt-to-mega electronvoltband, which is probably produced within the jet and lasts from milliseconds to minutes, known as the prompt emission(1,2). Subsequently, the interaction of the jet with the surrounding medium generates shock waves that are responsible for the afterglow emission, which lasts from days to months and occurs over a broad energy range from the radio to the gigaelectronvolt bands(1-6). The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock(7-9). Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C(10,11). Here we report multifrequency observations of GRB 190114C, and study the evolution in time of the GRB emission across 17 orders of magnitude in energy, from 5 x 10(-6) to 10(12) electronvolts. We find that the broadband spectral energy distribution is double-peaked, with the teraelectronvolt emission constituting a distinct spectral component with power comparable to the synchrotron component. This component is associated with the afterglow and is satisfactorily explained by inverse Compton up-scattering of synchrotron photons by high-energy electrons. We find that the conditions required to account for the observed teraelectronvolt component are typical for GRBs, supporting the possibility that inverse Compton emission is commonly produced in GRBs.

引用

页码：459 / +

页数：23

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