TY - JOUR
T1 - Upper limits on the very high energy emission from GRBs observed by MAGIC
AU - Acciari, V. A.
AU - Ansoldi, S.
AU - Antonelli, L. A.
AU - Arbet Engels, A.
AU - Artero, M.
AU - Asano, K.
AU - Baack, D.
AU - Babić, A.
AU - Baquero, A.
AU - Barres de Almeida, U.
AU - Barrio, J. A.
AU - Batković, I.
AU - Becerra González, J.
AU - Bednarek, W.
AU - Bellizzi, L.
AU - Bernardini, E.
AU - Bernardos, M.
AU - Berti, Alessio
AU - Besenrieder, J.
AU - Bhattacharyya, W.
AU - Bigongiari, C.
AU - Biland, A.
AU - Blanch, O.
AU - Bökenkamp, H.
AU - Bonnoli, G.
AU - Bošnjak, Željka
AU - Busetto, G.
AU - Carosi, R.
AU - Ceribella, G.
AU - Cerruti, M.
AU - Chai, Y.
AU - Chilingarian, A.
AU - Cikota, S.
AU - Colak, S. M.
AU - Colombo, E.
AU - Contreras, J. L.
AU - Cortina, J.
AU - Covino, S.
AU - D'Amico, G.
AU - D'Elia, V.
AU - Da Vela, P.
AU - Dazzi, F.
AU - De Angelis, A.
AU - De Lotto, B.
AU - Delfino, M.
AU - Delgado, J.
AU - Font, L.
AU - Gaug, M.
AU - Maggio, C.
AU - Moreno, V.
AU - Nigro, C.
AU - Ubach, S.
N1 - Publisher Copyright:
© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0)
PY - 2022/3/18
Y1 - 2022/3/18
N2 - 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.
AB - 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.
UR - http://www.scopus.com/inward/record.url?scp=85145007916&partnerID=8YFLogxK
M3 - Article
AN - SCOPUS:85145007916
SN - 1824-8039
VL - 395
JO - Proceedings of Science
JF - Proceedings of Science
ER -