A lower bound on intergalactic magnetic fields from time variability of 1ES 0229+200 from MAGIC and Fermi/LAT observations

被引：29

作者：

Acciari, V. A. ^{[1
,2
]}

Agudo, I. ^{[19
]}

Aniello, T. ^{[3
]}

Ansoldi, S. ^{[4
,5
,53
]}

Antonelli, L. A. ^{[3
]}

Arbet Engels, A. ^{[6
]}

Artero, M. ^{[7
]}

Asano, K. ^{[8
]}

Baack, D. ^{[9
]}

Babic, A. ^{[10
]}

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

Barres de Almeida, U. ^{[13
]}

Barrio, J. A. ^{[11
,12
]}

Batkovic, I. ^{[14
,15
]}

Becerra Gonzalez, J. ^{[1
,2
]}

Bednarek, W. ^{[16
]}

Bernardini, E. ^{[14
,15
]}

Bernardos, M. ^{[14
,15
]}

Berti, A. ^{[6
]}

Besenrieder, J. ^{[6
]}

Bhattacharyya, W. ^{[17
]}

Bigongiari, C. ^{[3
]}

Biland, A. ^{[18
]}

Blanch, O. ^{[7
]}

Boekenkamp, H. ^{[9
]}

Bonnoli, G. ^{[19
]}

Bosnjak, Z. ^{[10
]}

Burelli, I. ^{[4
,5
]}

Busetto, G. ^{[14
,15
]}

Carosi, R. ^{[20
,21
]}

Ceribella, G.

Cerruti, M. ^{[22
]}

Chai, Y. ^{[6
]}

Chilingarian, A. ^{[23
]}

Cikota, S. ^{[10
]}

Colombo, E. ^{[1
,2
]}

Contreras, J. L. ^{[11
,12
]}

Cortina, J. ^{[24
]}

Covino, S. ^{[3
]}

D'Amico, G. ^{[25
]}

D'Elia, V. ^{[3
]}

Da Vela, P. ^{[20
,21
,54
]}

Dazzi ^{[3
]}

De Angelis ^{[14
,15
]}

De Lotto, B. ^{[4
,5
]}

Del Popolo, A. ^{[26
,27
]}

Delfino, M. ^{[7
,55
]}

Delgado, J. ^{[7
,55
]}

Delgado Mendez, C. ^{[24
]}

Depaoli, D. ^{[28
,29
]}

机构：

[1] Univ La Laguna, Inst Astrofis Canarias, San Cristobal la Laguna 38200, Tenerife, Spain

[2] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38200, Tenerife, Spain

[3] Natl Inst Astrophys INAF, I-00136 Rome, Italy

[4] Univ Udine, I-33100 Udine, Italy

[5] INFN Trieste, I-33100 Udine, Italy

[6] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

[7] Barcelona Inst Sci & Technol, IFAE, Barcelona 08193, Spain

[8] Univ Tokyo, Japanese MAGIC Grp, Inst Cosm Ray Res ICRR, Kashiwa, Chiba 2778582, Japan

[9] Tech Univ Dortmund, D-44221 Dortmund, Germany

[10] Univ Zagreb, Croatian MAGIC Grp, Fac Elect Engn & Comp FER, Zagreb 10000, Croatia

[11] Univ Complutense Madrid, IPARCOS Inst, Madrid 28040, Spain

[12] Univ Complutense Madrid, EMFTEL Dept, Madrid 28040, Spain

[13] Ctr Brasileiro Pesquisas Fis, BR-22290180 Rio De Janeiro, RJ, Brazil

[14] Univ Padua, I-35131 Padua, Italy

[15] Ist Nazl Fis Nucl, I-35131 Padua, Italy

[16] Univ Lodz, Fac Phys & Appl Informat, Dept Astrophys, PL-90236 Lodz, Poland

[17] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany

[18] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland

[19] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, Granada 18008, Spain

[20] Univ Pisa, I-56126 Pisa, Italy

[21] INFN Pisa, I-56126 Pisa, Italy

[22] Univ Barcelona, ICCUB, IEEC UB, Barcelona 08028, Spain

[23] A Alikhanyan Natl Sci Lab, Armenian MAGIC Grp, Yerevan 0036, Armenia

[24] Ctr Invest Energet Medioambient & Tecnol, Madrid 28040, Spain

[25] Univ Bergen, Dept Phys & Technol, Bergen, Norway

[26] Ist Nazl Fis Nucl, Sez Catania, INFN MAGIC Grp, I-95123 Catania, Italy

[27] Univ Catania, Dipartimento Fis & Astron, I-95123 Catania, Italy

[28] Ist Nazl Fis Nucl, Sez Torino, INFN MAGIC Grp, I-10125 Turin, Italy

[29] Univ Turin, I-10125 Turin, Italy

[30] Ist Nazl Fis Nucl, Sez Bari, INFN MAGIC Grp, I-70125 Bari, Italy

[31] Univ Politecn Bari, Dipartimento Interateneo Fis, I-70125 Bari, Italy

[32] Univ Rijeka, Croatian MAGIC Grp, Dept Phys, Rijeka 51000, Croatia

[33] Univ Wurzburg, D-97074 Wurzburg, Germany

[34] Univ Turku, Finnish MAGIC Grp, Finnish Ctr Astron ESO, Turku 20014, Finland

[35] Univ Autonoma Barcelona, Dept Fis, Bellaterra 08193, Spain

[36] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain

[37] Hiroshima Univ, Grad Sch Adv Sci & Engn, Japanese MAGIC Grp, Phys Program, Hiroshima 7398526, Japan

[38] NAS RA, ICRANet Armenia, Armenian MAGIC Grp, Yerevan 0019, Armenia

[39] Univ Split, Fac Elect Engn Mech Engn & Naval Architecture FES, Croatian MAGIC Grp, Split 21000, Croatia

[40] Josip Juraj Strossmayer Univ Osijek, Croatian MAGIC Grp, Dept Phys, Osijek 31000, Croatia

[41] Kyoto Univ, Japanese MAGIC Grp, Dept Phys, Kyoto 6068502, Japan

[42] Tokai Univ, Japanese MAGIC Grp, Dept Phys, Hiratsuka, Kanagawa 2591292, Japan

[43] Univ Siena, I-53100 Siena, Italy

[44] INFN Pisa, I-53100 Siena, Italy

[45] HBNI, Saha Inst Nucl Phys, 1 AF Bidhannagar,Sect 1, Kolkata 700064, India

[46] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, Sofia 1784, Bulgaria

[47] Yamagata Univ, Japanese MAGIC Grp, Dept Phys, Yamagata 9908560, Japan

[48] Univ Oulu, Finnish MAGIC Grp, Astron Res Unit, Oulu 90014, Finland

[49] Rudjer Boskovic Inst, Croatian MAGIC Grp, Zagreb 10000, Croatia

[50] Ist Nazl Fis Nucl, Sez Perugia, INFN MAGIC Grp, I-06123 Perugia, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 670卷

基金：

芬兰科学院;

关键词：

intergalactic medium; galaxies: active; gamma rays: galaxies; early Universe; LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; PLASMA INSTABILITIES; ELECTROSTATIC INSTABILITY; ELECTROMAGNETIC CASCADES; BACKGROUND-RADIATION; TEV BLAZARS; EVOLUTION; SEARCH; CONSTRAINTS;

D O I：

10.1051/0004-6361/202244126

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Extended and delayed emission around distant TeV sources induced by the effects of propagation of gamma ray s through the intergalactic medium can be used for the measurement of the intergalactic magnetic field (IGMF). Aims. We search for delayed GeV emission from the hard-spectrum TeV gamma-ray emitting blazar 1ES 0229+200, with the goal of detecting or constraining the IGMF-dependent secondary flux generated during the propagation of TeV gamma rays through the intergalactic medium.Methods. We analysed the most recent MAGIC observations over a 5 year time span, and complemented them with historic data of the H.E.S.S. and VERITAS telescopes, along with a 12-year-long exposure of the Fermi/LAT telescope. We used them to trace source evolution in the GeV-TeV band over a decade and a half. We used Monte Carlo simulations to predict the delayed secondary gamma-ray flux, modulated by the source variability, as revealed by TeV-band observations. We then compared these predictions for various assumed IGMF strengths to all available measurements of the gamma-ray flux evolution. Results. We find that the source flux in the energy range above 200 GeV experiences variations around its average on the 14-year time span of observations. No evidence for the flux variability is found in the 1 - 100 GeV energy range accessible to Fermi/LAT. The non-detection of variability due to delayed emission from electromagnetic cascade developing in the intergalactic medium imposes a lower bound of B>1.8 x 10(-17) G for the long-correlation-length IGMF and B>10(-14) G for an IGMF of cosmological origin. Though weaker than the one previously derived from the analysis of Fermi/LAT data, this bound is more robust, being based on a conservative intrinsic source spectrum estimate and accounting for the details of source variability in the TeV energy band. We discuss implications of this bound for cosmological magnetic fields that might explain the baryon asymmetry of the Universe.

引用

页数：8

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