Very-high-energy gamma-ray emission from GRB 201216C detected by MAGIC

Fukami, Satoshi; Berti, Alessio; Loporchio, Serena; Suda, Y.; Nava, Lara; Noda, K.; Bošnjak, Željka; Asano, Katsuaki; Longo, F.; Acciari, V. A.; Ansoldi, S.; Antonelli, L. A.; Engels, A. Arbet; Artero, Manuel; Baack, Dominik; Babić, Ana; Baquero, Andrés; Almeida, U. Barres de; Barrio, J. A.; Batković, Ivana; González, J. Becerra; Bednarek, W.; Bellizzi, Lorenzo; Bernardini, E.; Bernardos, Maria-Isabel; Besenrieder, Jürgen; Bhattacharyya, W.; Bigongiari, C.; Biland, A.; Blanch, O.; Bökenkamp, Hendrik; Bonnoli, Giacomo; Busetto, G.; Carosi, R.; Ceribella, Giovanni; Cerruti, M.; Chai, Yating; Chilingarian, A.; Cikota, Stefan; Colak, S. M.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; D’Amico, Giacomo; D’Elia, V.; Vela, P. Da; Dazzi, F.; Angelis, A. De; Lotto, B. De; Delfino, Manuel; Delgado, Jordi; Mendez, C. Delgado; Depaoli, Davide; Pierro, F. Di; Venere, L. Di; Espiñeira, E. Do Souto; Prester, D. Dominis; Donini, Alice; Dorner, D.; Doro, M.; Elsäesser, D.; Ramazani, Vandad Fallah; Fattorini, Alicia; Fonseca, M. V.; Font, L.; Fruck, C.; Fukazawa, Yasushi; López, R. J. García; Garczarczyk, M.; Gasparyan, Sargis; Gaug, M.; Giglietto, N.; Giordano, F.; Gliwny, Paweł; Godinović, N.; Green, David; Green, Jarred Gershon; Hadasch, D.; Hahn, Alexander; Heckmann, Lea; Herrera, Javier; Hoang, J.; Hrupec, Dario; Hütten, Moritz; Inada, Tomohiro; Ishio, Kazuma; Iwamura, Y.; Martínez, Irene Jiménez; Jormanainen, Jenni; Jouvin, L.; Karjalainen, Marie; Kerszberg, Daniel; Kobayashi, Yukiho; Kubo, H.; Kushida, J.; Lamastra, Alessandra; Lelas, D.; Leone, F.; Lindfors, E.; Linhoff, Lena; Lombardi, S.; López-Coto, R.; López-Moya, Marcos; López-Oramas, Alicia; Fraga, Bernardo Machado de Oliveira; Maggio, C.; Majumdar, P.; Makariev, M.; Mallamaci, M.; Maneva, G.; Manganaro, Marina; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Menchiari, Stefano; Mender, Simone; Mićanović, Saša; Miceli, Davide; Miener, Tjark; Miranda, Jose Miguel; Mirzoyan, R.; Molina, Edgar; Moralejo, A.; Morcuende, Daniel; Moreno, V.; Moretti, E.; Nakamori, Takeshi; Neustroev, V.; Nigro, Cosimo; Nilsson, K.; Nishijima, K.; Nozaki, Seiya; Ohtani, Yoshiki; Oka, Tomohiko; Otero-Santos, Jorge; Paiano, S.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Pavletić, Lovro; Peñil, Pablo; Peršić, M.; Pihet, Marine; Moroni, Pier Giorgio Prada; Prandini, E.; Priyadarshi, Chaitanya; Puljak, I.; Rhode, W.; Ribó, M.; Rico, J.; Righi, Chiara; Rugliancich, A.; Sahakyan, N.; Saito, Takayuki; Sakurai, Shunsuke; Satalecka, K.; Saturni, Francesco Gabriele; Schleicher, Bernd; Schmidt, Kevin; Schweizer, T.; Sitarek, J.; Šnidarić, Iva; Sobczyńska, Dorota; Spolon, Alessia; Stamerra, A.; Strišković, Jelena; Strom, D.; Strzys, M.; Surić, T.; Takahashi, Mitsunari; Takeishi, Ryuji; Tavecchio, F.; Temnikov, P.; Terzić, T.; Teshima, M.; Tosti, Luca; Truzzi, Stefano; Tutone, Antonio; Ubach, Santiago; Scherpenberg, Juliane van; Vanzo, G.; Acosta, Mónica Vázquez; Ventura, Sofia; Verguilov, V.; Vigorito, C.; Vitale, V.; Vovk, Ievgen; Will, Martin; Wunderlich, Carolin; Yamamoto, Tokonatsu; Zarić, Darko

doi:10.22323/1.395.0788

Cited by 16 publications

(13 citation statements)

References 6 publications

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“…MAGIC observed the GRB for about 2.2 h, starting 56 s after the BAT trigger. An excess of counts, dominated by events at ∼100 GeV in the first 20 min of observations was detected with a significance of about 6σ [56]. GRB 201216C has a prompt energy and an afterglow X-ray luminosity very similar to those observed from GRB 180720B and GRB 190114C (Figure 7, bottom panel).…”

Section: Grb 201216cmentioning

confidence: 69%

Gamma-ray Bursts at the Highest Energies

Nava

2021

Universe

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Emission from Gamma-ray bursts is thought to be powered mainly by synchrotron radiation from energetic electrons. The same electrons might scatter these synchrotron seed photons to higher (>10 GeV) energies, building a distinct spectral component (synchrotron self-Compton, SSC). This process is expected to take place, but its relevance (e.g., the ratio between the SSC and synchrotron emitted power) is difficult to predict on the basis of current knowledge of physical conditions at GRB emission sites. Very high-energy radiation in GRBs can be produced also by other mechanisms, such as synchrotron itself (if PeV electrons are produced at the source), inverse Compton on external seed photons, and hadronic processes. Recently, after years of efforts, very high-energy radiation has been finally detected from at least four confirmed long GRBs by the Cherenkov telescopes H.E.S.S. and MAGIC. In all four cases, the emission has been recorded during the afterglow phase, well after the end of the prompt emission. In this work, I give an overview, accessible also to non-experts of the field, of the recent detections, theoretical implications, and future challenges, with a special focus on why very high-energy observations are relevant for our understanding of Gamma-ray bursts and which long-standing questions can be finally answered with the help of these observations.

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Section: Grb 201216cmentioning

confidence: 69%

Gamma-ray Bursts at the Highest Energies

Nava

2021

Universe

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“…The zenith angle of the observation ranged from 37 to 68 deg, in good weather on a moonless night, which made possible the analysis of the data with an energy threshold below 100 GeV (changing w.r.t the zenith angle). MAGIC detected the gamma rays with a significance of 5.9 sigma from the first 20 min of the observation [60,61]. The light curve obtained from the first 20 min (with an energy threshold of 70 GeV) was monotonically decaying, and the spectrum from the first 20 min is consistent with a power-law extended from 50 GeV to 200 GeV [61].…”

Section: Grb 201216cmentioning

confidence: 99%

“…MAGIC detected the gamma rays with a significance of 5.9 sigma from the first 20 min of the observation [60,61]. The light curve obtained from the first 20 min (with an energy threshold of 70 GeV) was monotonically decaying, and the spectrum from the first 20 min is consistent with a power-law extended from 50 GeV to 200 GeV [61].…”

Section: Grb 201216cmentioning

confidence: 99%

Gamma-Ray Bursts at TeV Energies: Observational Status

Noda

Parsons

2022

Galaxies

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Gamma-ray bursts (GRBs) are some of the most energetic events in the Universe and are potential sites of cosmic ray acceleration up to the highest energies. GRBs have therefore been a target of interest for very high energy gamma-ray observatories for many years, leading to the recent discovery of a number of bursts with photons reaching energies above 100 GeV. We summarize the GRB observational campaigns of the current generation of very high energy gamma-ray observatories as well as describing the observations and properties of the GRBs discovered so far. We compare the properties of the very high energy bursts to the total GRB distribution and make predictions for the next generation of very high energy gamma-ray observations.

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“…MAGIC started the observation of the burst about one minute after the onset, with a detection reaching 6 above ∼ 100 GeV. From preliminary analyses of the MAGIC data, the photon flux monotonically decays in time, and the spectrum (both intrinsic and observed) can be described by a power law [6]. Work is ongoing on the MAGIC collaboration side to model the MWL emission, despite the lack of simultaneous data e.g.…”

Section: Grb 201216cmentioning

confidence: 99%

Very high energy observations of gamma-ray bursts with Cherenkov telescopes

Berti¹

2022

Proceedings of the European Physical Society Conference on High Energy Physics — PoS(EPS-HEP2021)

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Gamma-ray bursts (GRBs) are transient events releasing a large amount of energy in a short amount of time as electromagnetic radiation. In the past decades, both observational and theoretical efforts were made to understand their inner workings, both in the prompt and afterglow phase. The origin of the GeV emission detected by Fermi-LAT in several GRBs is one of the aspects of GRB physics which is currently not well understood. Observations at very high energies (VHE, E>100 GeV) by Cherenkov telescopes, given their better sensitivity, can provide crucial information to understand the mechanisms behind such high energy components. After almost 15 years of efforts, the MAGIC and H.E.S.S. collaborations finally detected their first bursts, GRB190114C and GRB180720B respectively, opening a new era in the study of GRBs. Such detections proved the presence of a new additional emission component up to TeV energies in the GRB afterglow phase, which can be explained by the synchrotron self-Compton process. Other two GRBs were also detected, GRB190829A by H.E.S.S. and GRB201216C by MAGIC, bringing more information but also revealing a complex picture to explain the origin of the VHE emission. In this context, observations by future facilities as the Cherenkov Telescope Array (CTA) observatory will play a crucial role to increase our understanding of the VHE emission in GRBs. In this contribution I will present the outstanding results accomplished in the last years by Cherenkov telescopes in the observation of GRBs and provide an overview of what can be achieved with future instruments.

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Very-high-energy gamma-ray emission from GRB 201216C detected by MAGIC

Cited by 16 publications

References 6 publications

Gamma-ray Bursts at the Highest Energies

Gamma-ray Bursts at the Highest Energies

Gamma-Ray Bursts at TeV Energies: Observational Status

Very high energy observations of gamma-ray bursts with Cherenkov telescopes

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