Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and HESS Blazar Observations

被引：12

作者：

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

Aschersleben, J. ^{[3
]}

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

Martins, V. Barbosa ^{[6
]}

Batzofin, R. ^{[7
]}

Becherini, Y. ^{[8
,9
]}

Berge, D. ^{[10
]}

Bi, B. ^{[11
]}

Bouyahiaoui, M. ^{[2
]}

Breuhaus, M. ^{[2
]}

Brose, R. ^{[1
]}

Brun, F. ^{[12
]}

Bruno, B. ^{[13
]}

Bulik, T. ^{[14
]}

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

Bylund, T. ^{[9
]}

Caroff, S. ^{[15
]}

Casanova, S. ^{[16
]}

Celic, J. ^{[13
]}

Cerruti, M. ^{[8
]}

Chand, T. ^{[5
]}

Chandra, S. ^{[5
]}

Chen, A. ^{[17
]}

Chibueze, J. ^{[5
]}

Chibueze, O. ^{[5
]}

Cotter, G. ^{[18
]}

de Bony, M. ^{[15
]}

Egberts, K. ^{[7
]}

Ernenwein, J. -P. ^{[19
]}

de Clairfontaine, G. Fichet ^{[20
]}

Filipovic, M. ^{[21
]}

Fontaine, G. ^{[22
]}

Fuessling, M. ^{[23
]}

Funk, S. ^{[13
]}

Gabici, S. ^{[8
]}

Ghafourizadeh, S. ^{[23
]}

Giavitto, G. ^{[6
]}

Glawion, D. ^{[13
]}

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

Goswami, P. ^{[5
]}

Grondin, M. -H. ^{[24
]}

Haerer, L. ^{[2
]}

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

Holler, M. ^{[25
]}

Horns, D. ^{[26
]}

Jamrozy, M. ^{[27
]}

Jankowsky, F. ^{[23
]}

Joshi, V. ^{[13
]}

Jung-Richardt, I. ^{[13
]}

Kasai, E. ^{[4
]}

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

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

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

[6] DESY, D-15738 Zeuthen, Germany

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

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

[9] Linnaeus Univ, Dept Phys & Elect Engn, SE-35195 Vaxjo, Sweden

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

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

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

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

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

[15] Univ Savoie Mont Blanc, Labo Annecy Phys Particules IN2P3, CNRS, F-74000 Annecy, France

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

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

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

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

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

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

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

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

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

[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, Inst Astron, Fac Phys Astron & Informat, Grudziadzka 5, PL-87100 Torun, Poland

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

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

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

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

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

[37] Univ Southern Denmark, CP3 Origins, Campusvej 55, DK-5230 Odense M, Denmark

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2023年 / 950卷 / 02期

基金：

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

关键词：

GAMMA-RAY EMISSION; EXTRAGALACTIC BACKGROUND LIGHT; SEARCH; TELESCOPE; EVOLUTION; DISCOVERY; RADIATION; REDSHIFT; SCALE; ARRAY;

D O I：

10.3847/2041-8213/acd777

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Magnetic fields in galaxies and galaxy clusters are believed to be the result of the amplification of intergalactic seed fields during the formation of large-scale structures in the universe. However, the origin, strength, and morphology of this intergalactic magnetic field (IGMF) remain unknown. Lower limits on (or indirect detection of) the IGMF can be obtained from observations of high-energy gamma rays from distant blazars. Gamma rays interact with the extragalactic background light to produce electron-positron pairs, which can subsequently initiate electromagnetic cascades. The gamma-ray signature of the cascade depends on the IGMF since it deflects the pairs. Here we report on a new search for this cascade emission using a combined data set from the Fermi Large Area Telescope and the High Energy Stereoscopic System. Using state-of-the-art Monte Carlo predictions for the cascade signal, our results place a lower limit on the IGMF of B > 7.1 x 10(-16) G for a coherence length of 1 Mpc even when blazar duty cycles as short as 10 yr are assumed. This improves on previous lower limits by a factor of 2. For longer duty cycles of 10(4) (10(7)) yr, IGMF strengths below 1.8 x 10(-14) G (3.9 x 10(-14) G) are excluded, which rules out specific models for IGMF generation in the early universe.

引用

页数：16

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