Very-high-energy γ-Ray Emission from Young Massive Star Clusters in the Large Magellanic Cloud

被引：0

作者：

Aharonian, F. ^{[1
,2
,3
]}

Benkhali, F. Ait ^{[4
]}

Aschersleben, J. ^{[5
]}

Ashkar, H. ^{[6
]}

Backes, M. ^{[7
,8
]}

Martins, V. Barbosa ^{[9
]}

Batzofin, R. ^{[10
]}

Becherini, Y. ^{[11
,12
]}

Berge, D. ^{[9
,13
]}

Bernloehr, K. ^{[2
]}

Boettcher, M. ^{[8
]}

Bolmont, J. ^{[14
]}

de Lavergne, M. de Bony ^{[15
]}

Borowska, J. ^{[13
]}

Brose, R. ^{[1
]}

Brown, A. ^{[16
]}

Brun, F. ^{[15
]}

Bruno, B. ^{[17
]}

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

Casanova, S. ^{[18
]}

Celic, J. ^{[17
]}

Cerruti, M. ^{[11
]}

Chand, T. ^{[8
]}

Chandra, S. ^{[8
]}

Chen, A. ^{[19
]}

Chibueze, J. ^{[8
]}

Chibueze, O. ^{[8
]}

Cotter, G. ^{[16
]}

Cristofari, P. ^{[20
]}

Devin, J. ^{[21
]}

Djannati-Atai, A. ^{[11
]}

Djuvsland, J. ^{[2
]}

Dmytriiev, A. ^{[8
]}

Egberts, K. ^{[10
]}

Einecke, S. ^{[22
]}

Feijen, K. ^{[11
]}

Filipovic, M. ^{[23
]}

Fontaine, G. ^{[6
]}

Funk, S. ^{[17
]}

Gabici, S. ^{[11
]}

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

Glicenstein, J. F. ^{[15
]}

Glombitza, J. ^{[17
]}

Grolleron, G. ^{[14
]}

Haerer, L. ^{[2
]}

Hess, B. ^{[21
]}

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

Hofmann, W. ^{[2
]}

Holch, T. L. ^{[9
]}

Horns, D. ^{[25
]}

机构：

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

[2] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany

[3] Yerevan State Univ, 1 Alek Manukyan St, Yerevan 0025, Armenia

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

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

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

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

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

[9] Deutsch Elektronen Synchrotron DESY, Platanenallee 6, D-15738 Zeuthen, Germany

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

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

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

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

[14] Sorbonne Univ, Lab Phys Nucl & Hautes Energies, CNRS IN2P3, LPNHE, 4 Pl Jussieu, F-75005 Paris, France

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

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

[17] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Nikolaus Fiebiger Str 2, D-91058 Erlangen, Germany

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

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

[20] Univ Paris Cite, Univ PSL, CNRS, Lab Univers & Theories,Observ Paris, 5 Pl Jules Janssen, F-92190 Meudon, France

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

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

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

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

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

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

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

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

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

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

[31] Univ Innsbruck, Inst Astro & Teilchenphys, Technikerstr 25, A-6020 Innsbruck, Austria

[32] Yerevan Phys Inst, 2 Alikhanian Bros St, Yerevan 0036, Armenia

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

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

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2024年 / 970卷 / 01期

基金：

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

关键词：

30 DORADUS C; PARTICLE-ACCELERATION; SUPERNOVA REMNANT; ASSOCIATION LH90; !text type='PYTHON']PYTHON[!/text] PACKAGE; ATOMIC CLOUDS; CHANDRA ACIS; R136; ASTROPY; CORE;

D O I：

10.3847/2041-8213/ad5e67

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Tarantula Nebula in the Large Magellanic Cloud is known for its high star formation activity. At its center lies the young massive star cluster R136, providing a significant amount of the energy that makes the nebula shine so brightly at many wavelengths. Recently, young massive star clusters have been suggested to also efficiently produce very high-energy cosmic rays, potentially beyond PeV energies. Here, we report the detection of very-high-energy gamma-ray emission from the direction of R136 with the High Energy Stereoscopic System, achieved through a multicomponent, likelihood-based modeling of the data. This supports the hypothesis that R136 is indeed a very powerful cosmic-ray accelerator. Moreover, from the same analysis, we provide an updated measurement of the gamma-ray emission from 30 Dor C, the only superbubble detected at TeV energies presently. The gamma-ray luminosity above 0.5 TeV of both sources is (2-3) x 10(35) erg s(-1). This exceeds by more than a factor of 2 the luminosity of HESS J1646-458, which is associated with the most massive young star cluster in the Milky Way, Westerlund 1. Furthermore, the gamma-ray emission from each source is extended with a significance of >3 sigma and a Gaussian width of about 30 pc. For 30 Dor C, a connection between the gamma-ray emission and the nonthermal X-ray emission appears likely. Different interpretations of the gamma-ray signal from R136 are discussed.

引用

页数：15

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