Resolving the Crab pulsar wind nebula at teraelectronvolt energies

被引：27

作者：

Abdalla, H. ^{[1
]}

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

Ait Benkhali, F. ^{[2
]}

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

Arakawa, M. ^{[6
]}

Arcaro, C. ^{[1
]}

Armand, C. ^{[7
]}

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

Barnard, M. ^{[1
]}

Becherini, Y. ^{[9
]}

Becker Tjus, J. ^{[10
]}

Berge, D. ^{[11
]}

Bernloehr, K. ^{[2
]}

Blackwell, R. ^{[12
]}

Bottcher, M. ^{[1
]}

Boisson, C. ^{[13
]}

Bolmont, J. ^{[14
]}

Bonnefoy, S. ^{[11
]}

Bordas, P. ^{[2
]}

Bregeon, J. ^{[15
]}

Brun, F. ^{[16
]}

Brun, P. ^{[16
]}

Bryan, M. ^{[17
]}

Buechele, M. ^{[18
]}

Bulik, T. ^{[19
]}

Bylund, T. ^{[9
]}

Capasso, M. ^{[20
]}

Caroff, S. ^{[21
]}

Carosi, A. ^{[7
]}

Casanova, S. ^{[2
,22
]}

Cerruti, M. ^{[14
,23
]}

Chakraborty, N. ^{[2
]}

Chand, T. ^{[1
]}

Chandra, S. ^{[1
]}

Chaves, R. C. G. ^{[15
]}

Chen, A. ^{[24
]}

Colafrancesco, S. ^{[24
]}

Condon, B. ^{[25
]}

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

Deil, C. ^{[2
]}

Devin, J. ^{[15
]}

DeWilt, P. ^{[12
]}

Dirson, L. ^{[26
]}

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

Dmytriiev, A. ^{[13
]}

Donath, A. ^{[2
]}

Doroshenko, V. ^{[20
]}

Drury, L. O'C ^{[3
]}

Dyks, J. ^{[28
]}

Egberts, K. ^{[29
]}

机构：

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

[2] Max Planck Inst Kernphys, Heidelberg, Germany

[3] Dublin Inst Adv Studies, Dublin, Ireland

[4] Natl Acad Sci Republ Armenia, Yerevan, Armenia

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

[6] Rikkyo Univ, Dept Phys, Toshima Ku, Tokyo, Japan

[7] Univ Savoie Mt Blanc, Univ Grenoble Alpes, Lab Annecy Phys Particules, CNRS, Annecy, France

[8] Univ Namibia, Dept Phys, Windhoek, Namibia

[9] Linnaeus Univ, Dept Phys & Elect Engn, Vaxjo, Sweden

[10] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl 4 Weltraum & Astrophys, Bochum, Germany

[11] DESY, Zeuthen, Germany

[12] Univ Adelaide, Sch Phys Sci, Adelaide, SA, Australia

[13] Univ Paris Diderot, PSL Res Univ, Observ Paris, LUTH,CNRS, Meudon, France

[14] Univ Paris Diderot, Sorbonne Univ, Sorbonne Paris Cite, CNRS,IN2P3,LPNHE, Paris, France

[15] Univ Montpellier, CNRS, IN2P3, Lab Univers & Particules Montpellier, CC 72, Montpellier, France

[16] Univ Paris Saclay, CEA, IRFU, Gif Sur Yvette, France

[17] Univ Amsterdam, Anton Pannekoek Inst Astron, GRAPPA, Amsterdam, Netherlands

[18] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erlangen, Germany

[19] Univ Warsaw, Astron Observ, Warsaw, Poland

[20] Univ Tubingen, Inst Astron & Astrophys, Tubingen, Germany

[21] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, Palaiseau, France

[22] Inst Fizyki Jadrowej PAN, Krakow, Poland

[23] Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICC UB, Barcelona, Spain

[24] Univ Witwatersrand, Sch Phys, Johannesburg, South Africa

[25] Univ Bordeaux, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, Gradignan, France

[26] Univ Hamburg, Inst Expt Phys, Hamburg, Germany

[27] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, APC,CNRS,IN2P3,CEA,Irfu, Paris, France

[28] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Warsaw, Poland

[29] Univ Potsdam, Inst Phys & Astron, Potsdam, Germany

[30] Heidelberg Univ, Landessternwarte, Heidelberg, Germany

[31] Univ Grenoble Alpes, CNRS, IPAG, Grenoble, France

[32] Humboldt Univ, Inst Phys, Berlin, Germany

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

[34] Uniwersytet Jagiellonski, Obserwatorium Astron, Krakow, Poland

[35] Nicolaus Copernicus Univ, Ctr Astron, Fac Phys Astron & Informat, Torun, Poland

[36] Univ Tokyo, Inst Adv Study UTIAS, Kavli Inst Phys & Math Universe Kavli IPMU, Kashiwa, Chiba, Japan

[37] Univ Free State, Dept Phys, Bloemfontein, South Africa

[38] Univ Zurich, Phys Inst, Zurich, Switzerland

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

[40] RIKEN, Wako, Saitama, Japan

[41] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo, Japan

[42] Yerevan Phys Inst, Yerevan, Armenia

[43] Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, Stockholm, Sweden

来源：

NATURE ASTRONOMY | 2020年 / 4卷 / 02期

基金：

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; 奥地利科学基金会;

关键词：

RELATIVISTIC MHD SIMULATIONS; TELESCOPE OBSERVATIONS; GAMMA-RAYS; EMISSION; SYNCHROTRON; ORIGIN; TORUS; TEV;

D O I：

10.1038/s41550-019-0910-0

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

An angular extension at gamma-ray energies of 52 arcseconds is detected for the Crab nebula, revealing the emission region of the highest-energy gamma rays; simulations of the electromagnetic emission provide a non-trivial test of our understanding of particle acceleration in the Crab nebula. The Crab nebula is one of the most-studied cosmic particle accelerators, shining brightly across the entire electromagnetic spectrum up to very-high-energy gamma rays(1,2). It is known from observations in the radio to gamma-ray part of the spectrum that the nebula is powered by a pulsar, which converts most of its rotational energy losses into a highly relativistic outflow. This outflow powers a pulsar wind nebula, a region of up to ten light-years across, filled with relativistic electrons and positrons. These particles emit synchrotron photons in the ambient magnetic field and produce very-high-energy gamma rays by Compton up-scattering of ambient low-energy photons. Although the synchrotron morphology of the nebula is well established, it has not been known from which region the very-high-energy gamma rays are emitted(3-8). Here we report that the Crab nebula has an angular extension at gamma-ray energies of 52 arcseconds (assuming a Gaussian source width), much larger than at X-ray energies. This result closes a gap in the multi-wavelength coverage of the nebula, revealing the emission region of the highest-energy gamma rays. These gamma rays enable us to probe a previously inaccessible electron and positron energy range. We find that simulations of the electromagnetic emission reproduce our measurement, providing a non-trivial test of our understanding of particle acceleration in the Crab nebula.

引用

页码：167 / 173

页数：7

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