Characterising the VHE diffuse emission in the central 200 parsecs of our Galaxy with HESS

被引:68
作者
Abdalla, H. [1 ]
Abramowski, A. [2 ]
Aharonian, F. [3 ,4 ,5 ]
Benkhali, F. Ait [3 ]
Akhperjanian, A. G. [5 ,6 ]
Andersson, T. [10 ]
Anguener, E. O. [22 ]
Arakawa, M. [43 ]
Arrieta, M. [16 ]
Aubert, P. [24 ]
Backes, M. [8 ]
Balzer, A. [9 ]
Barnard, M. [1 ]
Becherini, Y. [10 ]
Tjus, J. Becker [11 ]
Berge, D. [14 ]
Bernhard, S. [14 ]
Bernloehr, K. [15 ]
Blackwell, R. [15 ]
Boettcher, M. [1 ]
Boisson, C. [16 ]
Bolmont, J. [17 ]
Bonnefoy, S. [37 ]
Bordas, P. [3 ]
Bregeon, J. [18 ]
Brun, F. [26 ]
Brun, P. [19 ]
Bryan, M. [9 ]
Buechele, M. [36 ]
Bulik, T. [20 ]
Capasso, M. [28 ]
Carr, J. [21 ]
Casanova, S. [3 ,22 ]
Cerruti, M. [17 ]
Chakraborty, N. [3 ]
Chaves, R. C. G. [18 ]
Chen, A. [23 ]
Chevalier, J. [24 ]
Coffaro, M. [28 ]
Colafrancesco, S. [23 ]
Cologna, G. [25 ]
Condon, B. [26 ]
Conrad, J. [27 ]
Cui, Y. [28 ]
Davids, I. D. [1 ,8 ]
Decock, J. [19 ]
Degrange, B. [29 ]
Deil, C. [3 ]
Devin, J. [18 ]
deWilt, P. [15 ]
机构
[1] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa
[2] Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany
[3] Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany
[4] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland
[5] Natl Acad Sci Republ Armenia, Marshall Baghramian Ave 24, Yerevan 0019, Armenia
[6] Yerevan Phys Inst, 2 Alikhanian Bros St, Yerevan 375036, Armenia
[7] Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany
[8] Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia
[9] Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands
[10] Linnaeus Univ, Dept Phys & Elect Engn, S-35195 Vaxjo, Sweden
[11] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany
[12] Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands
[13] Univ Amsterdam, Inst High Energy Phys, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands
[14] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria
[15] Univ Adelaide, Sch Phys Sci, Adelaide, SA 5005, Australia
[16] Univ Paris Diderot, PSL Res Univ, CNRS, Observ Paris,LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France
[17] UPMC Univ Paris 06, Univ Paris Diderot, Sorbonne Univ, CNRS,Sorbonne Paris Cite,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France
[18] Univ Montpellier, CNRS, IN2P3, Lab Univers & Particules Montpellier, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France
[19] CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France
[20] Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland
[21] Aix Marseille Univ, CNRS, IN2P3, CPPM UMR 7346, F-13288 Marseille, France
[22] PAN, Inst Fizyki Jadrowej, Ul Radzikowskiego 152, PL-31342 Krakow, Poland
[23] Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa
[24] Univ Savoie Mt t Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France
[25] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany
[26] Univ Bordeaux, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France
[27] Stockholm Univ, Albanova Univ Ctr, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden
[28] Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany
[29] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France
[30] Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France
[31] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France
[32] CNRS, IPAG, F-38000 Grenoble, France
[33] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England
[34] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland
[35] Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany
[36] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany
[37] DESY, D-15738 Zeuthen, Germany
[38] Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland
[39] Nicolaus Copernicus Univ, Fac Phys Astron & Informat, Ctr Astron, Grudziadzka 5, PL-87100 Torun, Poland
[40] Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa
[41] Heidelberg Univ, ITA, DFG, D-69120 Heidelberg, Germany
[42] Univ Amsterdam, Inst High Energy Phys, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands
[43] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan
[44] Japan Aerosp Explorat Agcy JAXA, ISAS, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan
[45] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia
基金
英国科学技术设施理事会; 新加坡国家研究基金会; 奥地利科学基金会; 澳大利亚研究理事会;
关键词
gamma rays: general; gamma rays: ISM; Galaxy: center; cosmic rays; GALACTIC-CENTER REGION; ENERGY GAMMA-RAYS; WIND; QUINTUPLET; GAS; ARC; SAGITTARIUS; ASTRONOMY; BUBBLES; NEBULA;
D O I
10.1051/0004-6361/201730824
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The diffuse very high-energy (VHE; > 100 GeV) gamma-ray emission observed in the central 200 pc of the Milky Way by H.E.S.S. was found to follow dense matter distribution in the central molecular zone (CMZ) up to a longitudinal distance of about 130 pc to the Galactic centre (GC), where the flux rapidly decreases. This was initially interpreted as the result of a burst-like injection of energetic particles 104 yr ago, but a recent more sensitive H.E.S.S. analysis revealed that the cosmic-ray (CR) density profile drops with the distance to the centre, making data compatible with a steady cosmic PeVatron at the GC. In this paper, we extend this analysis to obtain, for the first time, a detailed characterisation of the correlation with matter and to search for additional features and individual gamma-ray sources in the inner 200 pc. Taking advantage of 250 h of H.E.S.S. data and improved analysis techniques, we perform a detailed morphology study of the diffuse VHE emission observed from the GC ridge and reconstruct its total spectrum. To test the various contributions to the total gamma-ray emission, we used an iterative 2D maximum-likelihood approach that allows us to build a phenomenological model of the emission by summing a number of different spatial components. We show that the emission correlated with dense matter covers the full CMZ and that its flux is about half the total diffuse emission flux. We also detect some emission at higher latitude that is likely produced by hadronic collisions of CRs in less dense regions of the GC interstellar medium. We detect an additional emission component centred on the GC and extending over about 15 pc that is consistent with the existence of a strong CR density gradient and confirms the presence of a CR accelerator at the very centre of our Galaxy. We show that the spectrum of full ridge diffuse emission is compatible with that previously derived from the central regions, suggesting that a single population of particles fills the entire CMZ. Finally, we report the discovery of a VHE gamma-ray source near the GC radio arc and argue that it is produced by the pulsar wind nebula candidate G0.13-0.11.
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页数:13
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