A deep spectromorphological study of the γ-ray emission surrounding the young massive stellar cluster Westerlund 1

被引：24

作者：

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

Ashkar, H. ^{[3
]}

Backes, M. ^{[4
,5
]}

Martins, V. Barbosa ^{[6
]}

Becherini, Y. ^{[7
,8
]}

Berge, D. ^{[6
,9
]}

Bi, B. ^{[10
]}

Bottcher, M. ^{[5
]}

de Lavergne, M. de Bony ^{[11
]}

Bradascio, F. ^{[12
]}

Brose, R. ^{[1
]}

Brun, F. ^{[12
]}

Bulik, T. ^{[13
]}

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

Cangemi, F. ^{[14
]}

Caroff, S. ^{[14
]}

Casanova, S. ^{[15
]}

Cerruti, M. ^{[7
]}

Chand, T. ^{[5
]}

Chandra, S. ^{[5
]}

Chen, A. ^{[16
]}

Chibueze, O. ^{[5
]}

Cristofari, P. ^{[17
]}

Mbarubucyeye, J. Damascene ^{[6
]}

Djannati-Atai, A. ^{[7
]}

Ernenwein, J-P ^{[18
]}

Feijen, K. ^{[19
]}

de Clairfontaine, G. Fichet ^{[17
]}

Fontaine, G. ^{[3
]}

Funk, S. ^{[20
]}

Gabici, S. ^{[7
]}

Gallant, Y. A. ^{[21
]}

Ghafourizadeh, S. ^{[22
]}

Giavitto, G. ^{[6
]}

Giunti, L. ^{[7
,12
]}

Glawion, D. ^{[20
]}

Glicenstein, J. F. ^{[12
]}

Goswami, P. ^{[5
]}

Grondin, M-H ^{[23
]}

Haerer, L. K. ^{[2
]}

Haupt, M. ^{[6
]}

Hinton, J. A. ^{[2
]}

Horbe, M. ^{[24
]}

Hofmann, W. ^{[2
]}

Holch, T. L. ^{[6
]}

Holler, M. ^{[25
]}

Horns, D. ^{[26
]}

Jamrozy, M. ^{[27
]}

Joshi, V ^{[20
]}

Jung-Richardt, I ^{[20
]}

机构：

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

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

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

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

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

[6] DESY, D-15738 Zeuthen, Germany

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[28] Nicolaus Copernicus Univ, Fac Phys, Inst Astron 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 Amsterdam, Anton Pannekoek Inst Astron, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

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

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

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

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

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

[37] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia

[38] Armagh Observ & Planetarium, Armagh BT61 7HT, North Ireland

[39] Western Sydney Univ, Locked Bag 1797, Penrith, NSW 2751, Australia

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 666卷

基金：

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

关键词：

acceleration of particles; radiation mechanisms; non-thermal; shock waves; stars; massive; gamma rays; general; galaxies; star clusters; individual; Westerlund; 1; PARTICLE-ACCELERATION; MOLECULAR CLOUDS; CYGNUS REGION; COSMIC-RAYS; MILKY-WAY; STAR; DIFFUSE; PULSAR; FERMI; WINDS;

D O I：

10.1051/0004-6361/202244323

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Young massive stellar clusters are extreme environments and potentially provide the means for efficient particle acceleration. Indeed, they are increasingly considered as being responsible for a significant fraction of cosmic rays (CRs) that are accelerated within the Milky Way. Westerlund 1, the most massive known young stellar cluster in our Galaxy, is a prime candidate for studying this hypothesis. While the very-high-energy gamma-ray source HESS J1646-458 has been detected in the vicinity of Westerlund 1 in the past, its association could not be firmly identified. Aims. We aim to identify the physical processes responsible for the gamma-ray emission around Westerlund 1 and thus to understand the role of massive stellar clusters in the acceleration of Galactic CRs better. Methods. Using 164 h of data recorded with the High Energy Stereoscopic System (H.E.S.S.), we carried out a deep spectromorphological study of the gamma-ray emission of HESS J1646-458. We furthermore employed H I and CO observations of the region to infer the presence of gas that could serve as target material for interactions of accelerated CRs. Results. We detected large-scale (similar to 2 degrees diameter) gamma-ray emission with a complex morphology, exhibiting a shell-like structure and showing no significant variation with gamma-ray energy. The combined energy spectrum of the emission extends to several tens of TeV, and it is uniform across the entire source region. We did not find a clear correlation of the gamma-ray emission with gas clouds as identified through H I and CO observations. Conclusions. We conclude that, of the known objects within the region, only Westerlund 1 can explain the majority of the gamma-ray emission. Several CR acceleration sites and mechanisms are conceivable and discussed in detail. While it seems clear that Westerlund 1 acts as a powerful particle accelerator, no firm conclusions on the contribution of massive stellar clusters to the flux of Galactic CRs in general can be drawn at this point.

引用

页数：18

共 111 条

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共 111 条

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Bulik, T. ;

Bylund, T. ;

Caroff, S. ;

Carosi, A. ;

Casanova, S. ;

Cerruti, M. ;

Chand, T. ;

Chandra, S. ;

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