Upper limits on the very high energy emission from GRBs observed by MAGIC

被引：0

作者：

Longo, Francesco ^{[1
,2
,3
]}

Berti, Alessio ^{[4
]}

Bosnjak, Zeljka ^{[5
]}

Donini, Alice ^{[2
,6
,7
]}

Fukami, Satoshi ^{[8
]}

Green, Jarred Gershon ^{[9
]}

Miceli, Davide ^{[2
,6
,10
]}

Moretti, Elena ^{[7
]}

Nava, Lara ^{[2
,3
,11
]}

Noda, Koji

机构：

[1] Univ Trieste, Dept Phys, Via Valerio 2, Trieste, Italy

[2] Ist Nazl Fis Nucl, Sez Trieste, Via Valerio 2, Trieste, Italy

[3] Inst Fundamental Phys Universe IFPU, Via Beirut 12, Trieste, Italy

[4] Max Planck Inst Phys & Astrophys, Fohringer Ring 6, Munich, Germany

[5] Univ Zagreb, Fac Elect Engn & Comp FER, Zagreb, Croatia

[6] Univ Udine, Dipartimento Sci Matemat Informat & Fis, Via Sci 206, Udine, Italy

[7] Barcelona Inst Sci & Technol, Inst Fis Altes Energies, Bellaterra, Barcelona, Spain

[8] Univ Tokyo, Inst Cosm Ray Res, Kashiwanoha 5-1-5, Kashiwa, Chiba, Japan

[9] Osserv Astron Roma, INAF, Via Frascati 33, Monte Porzio Catone, Italy

[10] CNRS, IN2P3, LAPP, 9 Chemin Bellevue,BP 110, Annecy, France

[11] Osserv Astron Brera, INAF, Via Bianchi 46, Merate, LC, Italy

来源：

37TH INTERNATIONAL COSMIC RAY CONFERENCE, ICRC2021 | 2022年

基金：

芬兰科学院;

关键词：

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The MAGIC collaboration has developed a dedicated observational strategy to repoint rapidly towards gamma-ray bursts (GRBs). In this contribution we present the information extracted from the large sample of the GRBs observed by MAGIC from 2013 to 2019. None of these GRBs were significantly detected, and this study aims to shed light on the reasons behind those non-detections. The same strategy had led to the successful detection of two GRBs at Very High Energies (VHE, E > 100 GeV). We describe the details of the MAGIC GRB observational procedure and the general properties of each observed GRB. The lack of detection can be attributed either to unfavourable conditions or GRB intrinsic properties, such as the magnetic field's energy density, the bulk Lorentz factor, or the emitting region's size. For the presented sample of GRBs, we show the methods used to obtain flux upper limits in the VHE range, and propose physical implications of the non-detection of VHE emission. These results constitute an essential reference point to study the broadband emission of GRBs, and for the Cherenkov telescope community to organize future follow-ups of GRBs at VHE energies.

引用

页数：8

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