Measurement of the EBL spectral energy distribution using the VHE γ-ray spectra of HESS blazars

被引：49

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
]}

Anguner, E. O. ^{[21
]}

Arakawa, M. ^{[44
]}

Arrieta, M. ^{[15
]}

Aubert, P. ^{[24
]}

Backes, M. ^{[8
]}

Balzer, A. ^{[9
]}

Barnard, M. ^{[1
]}

Becherini, Y. ^{[10
]}

Tjus, J. Becker ^{[11
]}

Berge, D. ^{[9
,12
]}

Bernhard, S. ^{[13
]}

Bernloehr, K. ^{[3
]}

Blackwell, R. ^{[14
]}

Bottcher, M. ^{[1
]}

Boisson, C. ^{[15
]}

Bolmont, J. ^{[16
]}

Bonnefoy, S. ^{[38
]}

Bordas, P. ^{[3
]}

Bregeon, J. ^{[17
]}

Brun, F. ^{[26
]}

Brun, P. ^{[18
]}

Bryan, M. ^{[9
]}

Buechele, M. ^{[37
]}

Bulik, T. ^{[19
]}

Capasso, M. ^{[29
]}

Carr, J. ^{[20
]}

Casanova, S. ^{[3
,21
]}

Cerruti, M. ^{[16
]}

Chakraborty, N. ^{[3
]}

Chaves, R. C. G. ^{[17
,22
]}

Chen, A. ^{[23
]}

Chevalier, J. ^{[24
]}

Coffaro, M. ^{[29
]}

Colafrancesco, S. ^{[23
]}

Cologna, G. ^{[25
]}

Condon, B. ^{[26
]}

Conrad, J. ^{[27
,28
]}

Cui, Y. ^{[29
]}

Davids, I. D. ^{[1
,8
]}

Decock, J. ^{[18
]}

Degrange, B. ^{[30
,31
]}

Deil, C. ^{[3
]}

Devin, J. ^{[17
]}

de Wilt, P. ^{[14
]}

机构：

[1] Northwest Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa

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

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

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

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

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

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

[18] CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France

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

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

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

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

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

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

[25] Univ Bordeaux, Ctr Etudes Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France

[26] Stockholm Univ, Albanova Univ Ctr, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden

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

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

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

[30] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France

[31] IPAG, CNRS, F-38000 Grenoble, France

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

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

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

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

[36] DESY, D-15738 Zeuthen, Germany

[37] Uniwersytet Jagiellonski, Obserwatorium Astronomiczne, Ul Orla 171, PL-30244 Krakow, Poland

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

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

[40] ITA Univ Heidelberg, D-69120 Heidelberg, Germany

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

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

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2017年 / 606卷

基金：

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

关键词：

gamma rays: galaxies; BL Lacertae objects: general; cosmic background radiation; infrared: diffuse background; EXTRAGALACTIC BACKGROUND LIGHT; RADIATION; LIMITS; OBJECTS; EVOLUTION; REDSHIFT; PHOTONS; IMPRINT; MKN-421; NUCLEI;

D O I：

10.1051/0004-6361/201731200

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Very high-energy gamma rays (VHE, E greater than or similar to 100 GeV) propagating over cosmological distances can interact with the low-energy photons of the extragalactic background light (EBL) and produce electron-positron pairs. The transparency of the Universe to VHE gamma rays is then directly related to the spectral energy distribution (SED) of the EBL. The observation of features in the VHE energy spectra of extragalactic sources allows the EBL to be measured, which otherwise is very difficult. An EBL model-independent measurement of the EBL SED with the H.E.S.S. array of Cherenkov telescopes is presented. It was obtained by extracting the EBL absorption signal from the reanalysis of high-quality spectra of blazars. From H.E.S.S. data alone the EBL signature is detected at a significance of 9.5 sigma, and the intensity of the EBL obtained in different spectral bands is presented together with the associated gamma-ray horizon.

引用

页数：11

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