Search for γ-Ray Line Signals from Dark Matter Annihilations in the Inner Galactic Halo from 10 Years of Observations with HESS

被引：116

作者：

Abdallah, H. ^{[1
]}

Abramowski, A. ^{[2
]}

Aharonian, F. ^{[3
,4
,5
]}

Benkhali, F. Ait ^{[3
]}

Anguner, E. O. ^{[6
]}

Arakawa, M. ^{[7
]}

Arrieta, M. ^{[8
]}

Aubert, P. ^{[9
]}

Backes, M. ^{[10
]}

Balzer, A. ^{[11
,12
]}

Barnard, M. ^{[1
]}

Becherini, Y. ^{[13
]}

Tjus, J. Becker ^{[14
]}

Berge, D. ^{[11
,12
]}

Bernhard, S. ^{[15
]}

Bernloehr, K. ^{[3
]}

Blackwell, R. ^{[16
]}

Bottcher, M. ^{[1
]}

Boisson, C. ^{[8
]}

Bolmont, J. ^{[17
]}

Bonnefoy, S. ^{[18
]}

Bordas, P. ^{[3
]}

Bregeon, J. ^{[19
]}

Brun, F. ^{[20
]}

Brun, P. ^{[21
]}

Bryan, M. ^{[11
,12
]}

Buechele, M. ^{[22
]}

Bulik, T. ^{[23
]}

Capasso, M. ^{[24
]}

Caroff, S. ^{[25
]}

Carosi, A. ^{[9
]}

Carr, J. ^{[26
]}

Casanova, S. ^{[3
,6
]}

Cerruti, M. ^{[17
]}

Chakraborty, N. ^{[3
]}

Chaves, R. C. G. ^{[19
]}

Chen, A. ^{[27
]}

Chevalier, J. ^{[9
]}

Colafrancesco, S. ^{[27
]}

Condon, B. ^{[20
]}

Conrad, J. ^{[28
]}

Davids, I. D. ^{[10
]}

Decock, J. ^{[21
]}

Deil, C. ^{[3
]}

Devin, J. ^{[19
]}

Dewilt, P. ^{[16
]}

Dirson, L. ^{[2
]}

Djannati-Atai, A. ^{[29
]}

Domainko, W. ^{[3
]}

Donath, A. ^{[3
]}

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

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

[8] Univ Paris Diderot, PSL Res Univ, CNRS, LUTH,Observ Paris, 5 Pl Jules Janssen, F-92190 Meudon, France

[9] Univ Savoie Mont Blanc, Lab Annecy le Vieux Phys Particules, CNRS, IN2P3, F-74941 Annecy Le Vieux, France

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

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

[12] Univ Amsterdam, Inst High Energy Phys, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

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

[14] Ruhr Univ Bochum, Lehrstuhl Weltraum & Astrophys 4, Inst Theoret Phys, D-44780 Bochum, Germany

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

[16] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia

[17] Sorbonne Univ, UPMC Univ Paris 06, Univ Paris Diderot, Sorbonne Paris Cite,CNRS,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France

[18] DESY, D-15738 Zeuthen, Germany

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

[20] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France

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

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

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

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

[25] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France

[26] Aix Marseille Univ, CNRS, IN2P3, CPPM UMR 7346, F-13288 Marseille, France

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

[28] Stockholm Univ, Albanova Univ Ctr, Oskar Klein Ctr, Dept Phys, SE-10691 Stockholm, Sweden

[29] Univ Paris Diderot, APC, CNRS IN2P3, Sorbonne Paris Cite,CEA Irfu,Observ Paris, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France

[30] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England

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

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

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

[34] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

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

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

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

[38] Japan Aeropspace Explorat Agcy JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2298510, Japan

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

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

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

[42] Univ Sao Paulo, Inst Fis Sao Carlos, Ave Trabalhador Sao Carlense 400, BR-13566590 Sao Carlos, SP, Brazil

来源：

PHYSICAL REVIEW LETTERS | 2018年 / 120卷 / 20期

基金：

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; 日本学术振兴会; 英国科学技术设施理事会;

关键词：

CANDIDATES; MILKY;

D O I：

10.1103/PhysRevLett.120.201101

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

Spectral lines are among the most powerful signatures for dark matter (DM) annihilation searches in very-high-energy gamma rays. The central region of the Milky Way halo is one of the most promising targets given its large amount of DM and proximity to Earth. We report on a search for a monoenergetic spectral line from self-annihilations of DM particles in the energy range from 300 GeV to 70 TeV using a two-dimensional maximum likelihood method taking advantage of both the spectral and spatial features of the signal versus background. The analysis makes use of Galactic center observations accumulated over ten years (2004-2014) with the H.E.S.S. array of ground-based Cherenkov telescopes. No significant gamma-ray excess above the background is found. We derive upper limits on the annihilation cross section (sigma v) for monoenergetic DM lines at the level of 4 x 10(-28) cm(3) s(-1) at 1 TeV, assuming an Einasto DM profile for the Milky Way halo. For a DM mass of 1 TeV, they improve over the previous ones by a factor of 6. The present constraints are the strongest obtained so far for DM particles in the mass range 300 GeV-70 TeV. Ground-based gamma-ray observations have reached sufficient sensitivity to explore relevant velocity-averaged cross sections for DM annihilation into two gamma-ray photons at the level expected from the thermal relic density for TeV DM particles.

引用

页数：7

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