HESS J1809-193: A halo of escaped electrons around a pulsar wind nebula?

被引：9

作者：

Aharonian, F. ^{[1
,2
]}

Ait Benkhali, F. ^{[3
]}

Aschersleben, J. ^{[4
]}

Ashkar, H. ^{[5
]}

Backes, M. ^{[6
,7
]}

Barbosa Martins, V. ^{[8
]}

Batzofin, R. ^{[9
]}

Becherini, Y. ^{[10
,11
]}

Berge, D. ^{[8
,12
]}

Boettcher, M. ^{[7
]}

Boisson, C. ^{[13
]}

Bolmont, J. ^{[14
]}

Borowska, J. ^{[12
]}

Bouyahiaoui, M. ^{[2
]}

Bradascio, F. ^{[15
]}

Breuhaus, M. ^{[2
]}

Brose, R. ^{[1
]}

Brun, F. ^{[15
]}

Bruno, B. ^{[16
]}

Bulik, T. ^{[17
]}

Burger-Scheidlin, C. ^{[1
]}

Bylund, T. ^{[11
]}

Caroff, S. ^{[18
]}

Casanova, S. ^{[19
]}

Celic, J. ^{[16
]}

Cerruti, M. ^{[10
]}

Chambery, P. ^{[20
]}

Chand, T. ^{[7
]}

Chen, A. ^{[9
]}

Chibueze, J. ^{[7
]}

Chibueze, O. ^{[7
]}

Damascene Mbarubucyeye, J. ^{[8
]}

Djannati-Atai, A. ^{[10
]}

Dmytriiev, A. ^{[7
]}

Einecke, S. ^{[21
]}

Ernenwein, J. -p. ^{[22
]}

Feijen, K. ^{[21
]}

Filipovic, M. ^{[23
]}

Fontaine, G. ^{[5
]}

Fuessling, M. ^{[8
]}

Funk, S. ^{[16
]}

Gabici, S. ^{[10
]}

Gallant, Y. A. ^{[24
]}

Ghafourizadeh, S. ^{[3
]}

Giavitto, G. ^{[8
]}

Giunti, L. ^{[10
,15
]}

Glawion, D. ^{[16
]}

Goswami, P. ^{[7
]}

Grolleron, G. ^{[14
]}

Grondin, M. -h. ^{[20
]}

机构：

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

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

[3] Heidelberg Univ, Landessternwarte, Konigstuhl, D-69117 Heidelberg, Germany

[4] Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands

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

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

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

[8] DESY, D-15738 Zeuthen, Germany

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

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

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

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

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

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

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

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

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

[18] Univ Savoie Mont Blanc, CNRS, Lab Annecy Phys Particules IN2P3, F-74000 Annecy, France

[19] Inst Fizyki Jdrowej PAN, ul Radzikowskiego 152, PL-31342 Krakow, Poland

[20] Univ Bordeaux, CNRS, UMR 5797, LP2I Bordeaux, F-33170 Gradignan, France

[21] Univ Adelaide, Sch Phys Sci, Adelaide 5005, Australia

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

[23] Western Sydney Univ, Sch Sci, NSW 2751, Penrith, NSW 1797, Australia

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

[25] Leopold Franzens Univ Innsbruck, Inst Astround Teilchenphys, A-6020 Innsbruck, Austria

[26] Univ Hamburg, Inst Experimentalphys, Luruper Chaussee 149, D-22761 Hamburg, Germany

[27] Uniwersytet Jagiellonski, Obserwatorium Astron, ul Orla 171, PL-30244 Krakow, Poland

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

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

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

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

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

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

[34] Univ Tokyo, Inst Adv Study UTIAS, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwa Ha, Kashiwa, Chiba 2778583, Japan

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 672卷

基金：

爱尔兰科学基金会; 奥地利科学基金会; 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; 新加坡国家研究基金会;

关键词：

acceleration of particles; radiation mechanisms; non-thermal; pulsars; individual; PSR J1809-1917; gamma rays; general; GAMMA-RAY EMISSION; X-RAY; SUPERNOVA-REMNANTS; CRAB-NEBULA; DISCOVERY; ORIGIN; TELESCOPE; EVOLUTION; J1702-420; ASTROPY;

D O I：

10.1051/0004-6361/202245459

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. HESS J1809-193 is an unassociated very-high-energy gamma-ray source located on the Galactic plane. While it has been connected to the nebula of the energetic pulsar PSR J1809-1917, supernova remnants and molecular clouds present in the vicinity also constitute possible associations. Recently, the detection of gamma-ray emission up to energies of similar to 100 TeV with the HAWC observatory has led to renewed interest in HESS J1809-193.Aims. We aim to understand the origin of the gamma-ray emission of HESS J1809-193.Methods. We analysed 93.2 h of data taken on HESS J1809-193 above 0.27 TeV with the High Energy Stereoscopic System (H.E.S.S.), using a multi-component, three-dimensional likelihood analysis. In addition, we provide a new analysis of 12.5 yr of Fermi-LAT data above 1 GeV within the region of HESS J1809-193. The obtained results are interpreted in a time-dependent modelling framework.Results. For the first time, we were able to resolve the emission detected with H.E.S.S. into two components: an extended component (modelled as an elongated Gaussian with a 1-sigma semi-major and semi-minor axis of similar to 0.62 degrees and similar to 0.35 degrees, respectively) that exhibits a spectral cutoff at similar to 13 TeV, and a compact component (modelled as a symmetric Gaussian with a 1-sigma radius of similar to 0.1 degrees) that is located close to PSR J1809-1917 and shows no clear spectral cutoff. The Fermi-LAT analysis also revealed extended gamma-ray emission, on scales similar to that of the extended H.E.S.S. component.Conclusions. Our modelling indicates that based on its spectrum and spatial extent, the extended H.E.S.S. component is likely caused by inverse Compton emission from old electrons that form a halo around the pulsar wind nebula. The compact component could be connected to either the pulsar wind nebula or the supernova remnant and molecular clouds. Due to its comparatively steep spectrum, modelling the Fermi-LAT emission together with the H.E.S.S. components is not straightforward.

引用

页数：23

共 85 条

[41] The evolution and structure of pulsar wind nebulae [J].