Constraining very-high-energy and optical emission from FRB 121102 with the MAGIC telescopes

被引：23

作者：

Acciari, V. A. ^{[2
,3
]}

Ansoldi, S. ^{[4
,5
,6
,7
,8
]}

Antonelli, L. A. ^{[9
]}

Engels, A. Arbet ^{[10
]}

Arcaro, C. ^{[11
,12
]}

Baack, D. ^{[13
]}

Babic, A. ^{[14
,15
,16
,17
,18
]}

Banerjee, B. ^{[19
]}

Bangale, P. ^{[20
]}

Barres de Almeida, U. ^{[1
,20
]}

Barrio, J. A. ^{[21
]}

Becerra Gonzalez, J. ^{[2
,3
]}

Bednarek, W. ^{[22
]}

Bernardini, E. ^{[11
,12
,23
,24
]}

Berti, A. ^{[7
,8
,25
]}

Besenrieder, J. ^{[20
]}

Bhattacharyya, W. ^{[23
]}

Bigongiari, C. ^{[9
]}

Biland, A. ^{[10
]}

Blanch, O. ^{[26
]}

Bonnoli, G. ^{[27
,28
]}

Carosi, R. ^{[29
,30
]}

Ceribella, G. ^{[20
]}

Chatterjee, A. ^{[19
]}

Colak, S. M. ^{[26
]}

Colin, P. ^{[20
]}

Colombo, E. ^{[2
,3
]}

Contreras, J. L. ^{[21
]}

Cortina, J. ^{[26
]}

Covino, S. ^{[9
]}

Cumani, P. ^{[26
]}

D'Elia, V ^{[9
]}

Da Vela, P. ^{[27
,28
]}

Dazzi, F. ^{[9
]}

De Angelis, A. ^{[11
,12
]}

De Lotto, B. ^{[7
,8
]}

Delfino, M. ^{[26
,31
]}

Delgado, J. ^{[26
,31
]}

Di Pierro, F. ^{[11
,12
]}

Dominguez, A. ^{[21
]}

Prester, D. Dominis ^{[14
,15
,16
,17
,18
]}

Dorner, D. ^{[32
]}

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

Einecke, S. ^{[13
]}

Elsaesser, D. ^{[13
]}

Ramazani, V. Fallah ^{[33
,34
,35
]}

Fattorini, A. ^{[13
]}

Fernandez-Barral, A. ^{[11
,12
]}

Ferrara, G. ^{[9
]}

Fidalgo, D. ^{[21
]}

机构：

[1] URCA, CBPF, BR-22290180 Rio De Janeiro, RJ, Brazil

[2] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain

[3] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

[4] Univ Tokyo, Japanese MAGIC Consortium ICRR, Chiba 2778582, Japan

[5] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan

[6] RIKEN, Wako, Saitama 3510198, Japan

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

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

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

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

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

[12] INFN, I-35131 Padua, Italy

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

[14] Univ Rijeka, Croatian MAGIC Consortium, Rijeka 51000, Croatia

[15] Univ Split, FESB, Split 21000, Croatia

[16] Univ Zagreb, FER, Zagreb 10000, Croatia

[17] Univ Osijek, Osijek 31000, Croatia

[18] Rudjer Boskovic Inst, Zagreb 10000, Croatia

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

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

[21] Univ Complutense, Unidad Particular & Cosmol UPARCOS, E-28040 Madrid, Spain

[22] Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland

[23] DESY, D-15738 Zeuthen, Germany

[24] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany

[25] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

[26] BIST, IFAE, E-08193 Barcelona, Spain

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

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

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

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

[31] Port Informacio Cient PIC Bellaterra, E-08193 Barcelona, Spain

[32] Univ Wurburg, D-97074 Wurzburg, Germany

[33] Univ Turku, Finnish MAGIC Consortium Tuorla Observ, Vaisalantie 20, FI-21500 Piikkio, Finland

[34] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Piikkio, Finland

[35] Univ Oulu, Astron Div, FIN-90014 Oulu, Finland

[36] Univ Autonoma Barcelona, Dept Fis, E-08193 Barcelona, Spain

[37] Univ Autonoma Barcelona, CERES IEEC, E-08193 Barcelona, Spain

[38] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BG-1784 Sofia, Bulgaria

[39] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain

[40] Univ Bologna, INAF Trieste, Bologna, Italy

[41] Univ Bologna, Dept Phys & Astron, Bologna, Italy

[42] Joint Inst VLBI ERIC, Postbus 2, NL-7990 AA Dwingeloo, Netherlands

[43] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

[44] Netherlands Fdn Res Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands

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

[46] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan

[47] Penn State Univ, Dept Phys, University Pk, PA 16802 USA

[48] Arecibo Observ, Natl Astron & Ionosphere Ctr, Arecibo, PR 00612 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2018年 / 481卷 / 02期

关键词：

radiation mechanisms: non-thermal; methods: data analysis; methods: observational; gamma-rays: general; FAST RADIO-BURST; REIONIZATION HISTORY; MAJOR UPGRADE; CRAB-NEBULA; HOST GALAXY; ENVIRONMENT; PULSES; MODEL; AFTERGLOWS; DISPERSION;

D O I：

10.1093/mnras/sty2422

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Fast radio bursts (FRBs) are bright flashes observed typically at GHz frequencies with millisecond duration, whose origin is likely extragalactic. Their nature remains mysterious, motivating searches for counterparts at other wavelengths. FRB 121102 is so far the only source known to repeatedly emit FRBs and is associated with a host galaxy at redshift z similar or equal to 0.193. We conducted simultaneous observations of FRB 121102 with the Arecibo and MAGIC telescopes during several epochs in 2016-2017. This allowed searches for millisecond time-scale burst emission in very-high-energy (VHE) gamma-rays as well as the optical band. While a total of five FRBs were detected during these observations, no VHE emission was detected, neither of a persistent nature nor burst-like associated with the FRBs. The average integral flux upper limits above 100 GeV at 95 percent confidence level are 6.6 x 10(-12) photons cm(-2) s(-1) (corresponding to luminosity L-VHE < 10 (45) erg s(-1)) over the entire observation period, and 1.2 x 10(-7) photons cm(-2) s(-1 )(L-VHE < 10 (49) erg s( -1)) over the total duration of the five FRBs. We constrain the optical U-band flux to be below 8.6 mJy at 5 sigma level for 1-ms intervals around the FRB arrival times. A bright burst with U-band flux 29 mJy and duration similar to 12 ms was detected 4.3 s before the arrival of one FRB. However, the probability of spuriously detecting such a signal within the sampled time space is 1.5 percent (2.2, post-trial), i.e. consistent with the expected background. We discuss the implications of the obtained upper limits for constraining FRB models.

引用

页码：2479 / 2486

页数：8

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