Observation of inverse Compton emission from a long $γ$-ray burst

Acciari, V. A.; Ansoldi, S.; Antonelli, L. A.; Engels, A. Arbet; Baack, D.; Babić, A.; Banerjee, B.; de Almeida, U. Barres; Barrio, J. A.; González, J. Becerra; Bednarek, W.; Bellizzi, L.; Bernardini, E.; Berti, A.; Besenrieder, J.; Bhattacharyya, W.; Bigongiari, C.; Biland, A.; Blanch, O.; Bonnoli, G.; Bošnjak, Ž.; Busetto, G.; Carosi, R.; Ceribella, G.; Chai, Y.; Chilingaryan, A.; Cikota, S.; Colak, S. M.; Colin, U.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; D'Elia, V.; Da Vela, P.; Dazzi, F.; De Angelis, A.; De Lotto, B.; Delfino, M.; Delgado, J.; Depaoli, D.; Di Pierro, F.; Di Venere, L.; Espiñeira, E. Do Souto; Prester, D. Dominis; Donini, A.; Dorner, D.; Doro, M.; Elsaesser, D.; Ramazani, V. Fallah; Fattorini, A.; Ferrara, G.; Fidalgo, D.; Foffano, L.; Fonseca, M. V.; Font, L.; Fruck, C.; Fukami, S.; López, R. J. García; Garczarczyk, M.; Gasparyan, S.; Gaug, M.; Giglietto, N.; Giordano, F.; Godinović, N.; Green, D.; Guberman, D.; Hadasch, D.; Hahn, A.; Herrera, J.; Hoang, J.; Hrupec, D.; Hütten, M.; Inada, T.; Inoue, S.; Ishio, K.; Iwamura, Y.; Jouvin, L.; Kerszberg, D.; Kubo, H.; Kushida, J.; Lamastra, A.; Lelas, D.; Leone, F.; Lindfors, E.; Lombardi, S.; Longo, F.; López, M.; López-Coto, R.; López-Oramas, A.; Loporchio, S.; Fraga, B. Machado de Oliveira; Maggio, C.; Majumdar, P.; Makariev, M.; Mallamaci, M.; Maneva, G.; Manganaro, M.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martínez, M.; Mazin, D.; Mićanović, S.; Miceli, D.; Minev, M.; Miranda, J. M.; Mirzoyan, R.; Molina, E.; Moralejo, A.; Morcuende, D.; Moreno, V.; Moretti, E.; Munar-Adrover, P.; Neustroev, V.; Nigro, C.; Nilsson, K.; Ninci, D.; Nishijima, K.; Noda, K.; Nogués, L.; Nozaki, S.; Paiano, S.; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Peñil, P.; Peresano, M.; Persic, M.; Moroni, P. G. Prada; Prandini, E.; Puljak, I.; Rhode, W.; Ribó, M.; Rico, J.; Righi, C.; Rugliancich, A.; Saha, L.; Sahakyan, N.; Saito, T.; Sakurai, S.; Satalecka, K.; Schmidt, K.; Schweizer, T.; Sitarek, J.; Šnidarić, I.; Sobczynska, D.; Somero, A.; Stamerra, A.; Strom, D.; Strzys, M.; Suda, Y.; Surić, T.; Takahashi, M.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Teshima, M.; Torres-Albà, N.; Tosti, L.; Vagelli, V.; van Scherpenberg, J.; Vanzo, G.; Acosta, M. Vazquez; Vigorito, C. F.; Vitale, V.; Vovk, I.; Will, M.; Zarić, D.; Nava, L.; Veres, P.; Bhat, P. N.; Briggs, M. S.; Cleveland, W. H.; Hamburg, R.; Hui, C. M.; Mailyan, B.; Preece, R. D.; Roberts, O.; von Kienlin, A.; Wilson-Hodge, C. A.; Kocevski, D.; Arimoto, M.; Tak, D.; Asano, K.; Axelsson, M.; Barbiellini, G.; Bissaldi, E.; Dirirsa, F. Fana; Gill, R.; Granot, J.; McEnery, J.; Razzaque, S.; Piron, F.; Racusin, J. L.; Thompson, D. J.; Campana, S.; Bernardini, M. G.; Kuin, N. P. M.; Siegel, M. H.; Cenko, S. Bradley; O'Brien, P.; Capalbi, M.; D'Aì, A.; De Pasquale, M.; Gropp, J.; Klingler, N.; Osborne, J. P.; Perri, M.; Starling, R.; Tagliaferri, G.; Tohuvavohu, A.; Ursi, A.; Tavani, M.; Cardillo, M.; Casentini, C.; Piano, G.; Evangelista, Y.; Verrecchia, F.; Pittori, C.; Lucarelli, F.; Bulgarelli, A.; Parmiggiani, N.; Anderson, G. E.; Anderson, J. P.; Bernardi, G.; Bolmer, J.; Caballero-García, M. D.; Carrasco, I. M.; Castellón, A.; Segura, N. Castro; Castro-Tirado, A. J.; Cherukuri, S. V.; Cockeram, A. M.; D'Avanzo, P.; Di Dato, A.; Diretse, R.; Fender, R. P.; Fernández-García, E.; Fynbo, J. P. U.; Fruchter, A. S.; Greiner, J.; Gromadzki, M.; Heintz, K. E.; Heywood, I.; van der Horst, A. J.; Hu, Y. -D.; Inserra, C.; Izzo, L.; Jaiswal, V.; Jakobsson, P.; Japelj, J.; Kankare, E.; Kann, D. A.; Kouveliotou, C.; Klose, S.; Levan, A. J.; Li, X. Y.; Lotti, S.; Maguire, K.; Malesani, D. B.; Manulis, I.; Marongiu, M.; Martin, S.; Melandri, A.; Michałowski, M.; Miller-Jones, J. C. A.; Misra, K.; Moin, A.; Mooley, K. P.; Nasri, S.; Nicholl, M.; Noschese, A.; Novara, G.; Pandey, S. B.; Peretti, E.; del Pulgar, C. J. Pérez; Pérez-Torres, M. A.; Perley, D. A.; Piro, L.; Ragosta, F.; Resmi, L.; Ricci, R.; Rossi, A.; Sánchez-Ramírez, R.; Selsing, J.; Schulze, S.; Smartt, S. J.; Smith, I. A.; Sokolov, V. V.; Stevens, J.; Tanvir, N. R.; Thóne, C. C.; Tiengo, A.; Tremou, E.; Troja, E.; Postigo, A. de Ugarte; Vergani, S. D.; Wieringa, M.; Woudt, P. A.; Xu, D.; Yaron, O.; Young, D. R.

doi:10.48550/arxiv.2006.07251

Cited by 4 publications

(9 citation statements)

References 47 publications

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“…Gamma-ray bursts (GRBs) are intense and short pulses of gamma rays lasting from a fraction of a second to several hundred seconds. They are followed by an afterglow -lower-energy, long-lasting emission in the X-ray, optical and radio [711], up to gamma rays [712][713][714]. They are transients events occurring at an average rate of a few per day throughout the universe [715], whose radiation, for a period of seconds, completely flood with their radiation an otherwise almost dark gamma-ray sky [716].…”

Section: Gamma-ray Burstsmentioning

confidence: 99%

“…The field of GRB observations has recently seen significant breakthroughs with the detection of emission with imaging atmospheric Cherenkov telescopes (IACTs), namely from GRB 180720B [731] and GRB 190829A [732] by the High Energy Stereoscopic System (H.E.S.S. ), and GRB 190114C [733,734] and GRB 201216C [735] by the Major Atmospheric Gamma Imaging Cherenkov (MAGIC).…”

Section: Gamma-ray Burstsmentioning

confidence: 99%

“…In 2017 another important multi-messenger observation was performed, when a GW generated by a BNS inspiral was associated with a GRB [1178], later reclassified as a kilonova. The detection of AGNs in the VHE gamma-ray band [731,733,734], roused the expectations in the astrophysical community of a nearby connection between multi-wavelength observations and GWs [1202]. Gathering simultaneous data from all the available messengers would improve sensibly our knowledge of astrophysical objects and emission mechanisms.…”

Section: Multiwavelength and Multimessenger Astronomymentioning

confidence: 99%

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Quantum gravity phenomenology at the dawn of the multi-messenger era -- A review

Addazi,

Alvarez-Muniz,

Batista

et al. 2021

Preprint

Self Cite

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The exploration of the universe has recently entered a new era thanks to the multi-messenger paradigm, characterized by a continuous increase in the quantity and quality of experimental data that is obtained by the detection of the various cosmic messengers (photons, neutrinos, cosmic rays and gravitational waves) from numerous origins. They give us information about their sources in the universe and the properties of the intergalactic medium. Moreover, multi-messenger astronomy opens up the possibility to search for phenomenological signatures of quantum gravity. On the one hand, the most energetic events allow us to test our physical theories at energy regimes which are not directly accessible in accelerators; on the other hand, tiny effects in the propagation of very high energy particles could be amplified by cosmological distances. After decades of merely theoretical investigations, the possibility of obtaining phenomenological indications of Planck-scale effects is a revolutionary step in the quest for a quantum theory of gravity, but it requires cooperation between different communities of physicists (both theoretical and experimental). This review, prepared within the COST Action CA18108 "Quantum gravity phenomenology in the multi-messenger approach", is aimed at promoting this cooperation by giving a state-of-the art account of the interdisciplinary expertise that is needed in the effective search of quantum gravity footprints in the production, propagation and detection of cosmic messengers.

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Section: Gamma-ray Burstsmentioning

confidence: 99%

Section: Gamma-ray Burstsmentioning

confidence: 99%

Section: Multiwavelength and Multimessenger Astronomymentioning

confidence: 99%

See 1 more Smart Citation

Quantum gravity phenomenology at the dawn of the multi-messenger era -- A review

Addazi,

Alvarez-Muniz,

Batista

et al. 2021

Preprint

Self Cite

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show abstract

“…Hence solely a realistic, physically motivated intrinsic spectrum will provide a sensible cascade flux. With this in mind, we inferred the VHE spectral shape at energies higher than 1 TeV from the SSC model fitted to the multiwavelength SED by the MAGIC Collaboration [25]. We estimated the best-fit parameters of the time-averaged log-parabola shape in the energy range 0.2-1 TeV:…”

Section: Simulation Of Pair-echo Emissionmentioning

confidence: 99%

Intergalactic magnetic field studies by means of $γ$-ray emission from GRB 190114C

Vela¹,

Martí-Devesa²,

Saturni³

et al. 2023

Preprint

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The presence of delayed GeV emission after a strong transient, such as a GRB (Gamma-Ray Burst), in the VHE (Very-High Energy, E > 100 GeV) band can be the signature of a non-zero magnetic field in the intergalactic medium. We used a synchrotron self-Compton multiwavelength model to infer an analytical description of the intrinsic VHE spectrum (corrected for absorption by the Extragalactic Background Light, EBL) of GRB 190114C to predict the lightcurves and SEDs of the delayed emission with Monte Carlo simulations for different IGMF (Intergalactic Magnetic Field) configurations (strengths B = 8 × 10 −21 G, 10 −20 G, 3 × 10 −20 G and correlation length λ > 1 Mpc), and compared them with the Fermi-LAT (Fermi Large Area Telescope) limits computed for several exposure times. We found that Fermi LAT is not sensitive enough to constrain any IGMF strengths using GRB 190114C.

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“…It would be crucial to test the frequency/energy dependence of the delay experimentally. That requires the exact measurement time of observation of GRB and spectral resolutions and therefore, the planned broad energy range measurements are utmost crucial [16].…”

Section: Resolution Between Dispersion In Plasma and Lorentz Invarian...mentioning

confidence: 99%

Can the gamma-ray bursts travelling through the interstellar space be explained without invoking the drastic assumption of Lorentz invariance violation?

Чайчиан¹,

Brevik²,

Oksanen³

2021

Preprint

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Experimental observations indicate that gamma-ray bursts (GRB) and highenergy neutrino bursts may travel at different speeds with a typical delay measured at the order of hours or days. We discuss two potential interpretations for the GRB delay: dispersion of light in interstellar medium and violation of Lorentz invariance due to quantum gravitational fluctuations. Among a few other media, we consider dispersion of light in an axion plasma, obtaining the axion plasma frequency and the dispersion relation from quantum field theory for the first time. We find that the density of axions inferred from observations is far too low to produce the observed GRB delay. However, a more precise estimation of the spatial distribution of axions is required for a conclusive result. Other known media are also unable to account for the GRB delay, although there remains uncertainties in the observations of the delays. The interpretation in terms of Lorentz invariance violation and modified dispersion relation suffers from its own problems: since the modification of the dispersion relation should not be dependent on particle type, delays between photons and neutrinos are hard to explain. Thus neither interpretation is sufficient to explain the observations. We conclude that a crucial difference between the two interpretations is the frequency dependence of the propagation speed of radiation: in dispersive plasma the group speed increases with higher frequency, while Lorentz invariance violation implies lower speed at higher frequency. Future experiments shall resolve which one of the two frequency dependencies of GRB is actually the case.

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Observation of inverse Compton emission from a long $γ$-ray burst

Abstract: Long-duration gamma-ray bursts (GRBs) originate from ultra-relativistic jets launched from

Cited by 4 publications

References 47 publications

Quantum gravity phenomenology at the dawn of the multi-messenger era -- A review

Quantum gravity phenomenology at the dawn of the multi-messenger era -- A review

Intergalactic magnetic field studies by means of $γ$-ray emission from GRB 190114C

Can the gamma-ray bursts travelling through the interstellar space be explained without invoking the drastic assumption of Lorentz invariance violation?

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