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

Vereš, P.; Bhat, P. N.; Briggs, M. S.; Cleveland, W. H.; Hamburg, R.; Hui, C. M.; Mailyan, B.; Preece, R. D.; Roberts, O. J.; Kienlin, A. von; Wilson-Hodge, C.; Kocevski, D.; Arimoto, M.; Tak, D.; Asano, Katsuaki; Axelsson, M.; Barbiellini, G.; Bissaldi, E.; Dirirsa, F.; Gill, Ramandeep; Granot, Jonathan; McEnery, J. E.; Omodei, N.; 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. T.; Capalbi, M.; D’Aí, A.; Pasquale, M. De; Gropp, J. D.; Klingler, N. J.; Osborne, J. P.; Perri, M.; Starling, R. L. C.; 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.; Castellón, A.; Segura, N. Castro; Castro-Tirado, A. J.; Cherukuri, S. V.; Cockeram, A. M.; D’Avanzo, P.; Dato, A. Di; Diretse, R.; Fender, R. P.; Fernández-García, E.; Fynbo, J. P. U.; Fruchter, A. S.; Greiner, J.; Gromadzki, M.; Heintz, K. E.; Heywood, Ian; Horst, A. J. van der; Hu, Y.-D.; Inserra, C.; Izzo, L.; Jaiswal, V.; Jakobsson, P.; Japelj, J.; Kankare, E.; Канн, Д. А.; Kouveliotou, C.; Klose, S.; Levan, A. J.; Li, X. Y.; Lotti, Simone; Maguire, K.; Malesani, D.; Manulis, I.; Marongiu, M.; Martín, S.; Melandri, A.; Michałowski, M. J.; Miller-Jones, J. C. A.; Misra, Kuntal; Moin, A.; Mooley, K. P.; Nasri, Salah; Nicholl, M.; Noschese, Alfonso; Novara, G.; Pandey, S. B.; Peretti, Enrico; Pulgar, C. J. Pérez del; Pérez-Torres, M. Á.; Perley, D.; Piro, L.; Ragosta, Fabio; Resmi, L.; Ricci, R.; Rossi, A.; Sánchez-Ramírez, R.; Selsing, J.; Schulze, S.; Smartt, S. J.; Smith, I. A.; Соколов, В. В.; Stevens, J.; Tanvir, N. R.; Thöne, C. C.; Tiengo, A.; Tremou, Evangelia; Troja, E.; Postigo, A. de Ugarte; Valeev, A. F.; Vergani, S. D.; Wieringa, M.; Woudt, P. A.; Xu, D.; Yaron, O.; Young, D. R.

doi:10.1038/s41586-019-1754-6

Cited by 173 publications

(54 citation statements)

References 71 publications

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“…Finally, note that the afterglow model of Ref. [102] paper assumes a uniform (non-decaying) microturbulence with B = 8 × 10 −5 but, interestingly, our above values B+ = 0.01 and B ∝ xω p /c −0.4 lead to B− = 6 × 10 −5 in the emission region.…”

Section: Fate Of Downstream Turbulencementioning

confidence: 63%

“…The red line presents the synchrotron spectrum, which typically extends up to the GeV range at this early timescale, as discussed above, while the magenta line shows the inverse Compton spectrum. These parameters have not been chosen at random, but lie very close to those quoted for the modelling of the recent GRB190114C which has been detected up to sub-TeV energies by the MAGIC telescope [102], and indeed it is possible to check that the above spectral energy distribution reproduces qualitatively well that observed at early times. Importantly, all of the input microphysical parameters (i.e., e , B , s and γ e,max ), are based on, or derived from, the physical model described in previous sections.…”

Section: Fate Of Downstream Turbulencementioning

confidence: 73%

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Physics and Phenomenology of Weakly Magnetized, Relativistic Astrophysical Shock Waves

et al. 2020

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Weakly magnetized, relativistic collisionless shock waves are not only the natural offsprings of relativistic jets in high-energy astrophysical sources, they are also associated with some of the most outstanding displays of energy dissipation through particle acceleration and radiation. Perhaps their most peculiar and exciting feature is that the magnetized turbulence that sustains the acceleration process, and (possibly) the secondary radiation itself, is self-excited by the accelerated particles themselves, so that the phenomenology of these shock waves hinges strongly on the microphysics of the shock. In this review, we draw a status report of this microphysics, benchmarking analytical arguments with particle-in-cell simulations, and extract consequences of direct interest to the phenomenology, regarding in particular the so-called microphysical parameters used in phenomenological studies.

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Section: Fate Of Downstream Turbulencementioning

confidence: 63%

Section: Fate Of Downstream Turbulencementioning

confidence: 73%

Physics and Phenomenology of Weakly Magnetized, Relativistic Astrophysical Shock Waves

et al. 2020

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“…GRB 190114C (δ = −26°.94, ΔT = 3.8 × 10 3 s): This was the first GRB detected by an imaging air Cherenkov telescope to be announced in real time, with emissions in the 0.2-1.0 TeV band, detected by MAGIC (Acciari et al 2019a). Although the high-energy peak in the broadband spectral energy distribution was later shown to be consistent with a synchrotron self-Compton interpretation (Acciari et al 2019b), GRBs have long been thought of as potential sources of astrophysical neutrinos (Waxman & Bahcall 1997). While no coincident events were observed, the southern declination of this GRB places it in a location in the sky where the event selection places stringent cuts to reduce the atmospheric muon background; see Figure 4.…”

Section: Implications Of Specific Analysesmentioning

confidence: 85%

Follow-up of Astrophysical Transients in Real Time with the IceCube Neutrino Observatory

Abbasi¹,

Ackermann²,

Adams³

et al. 2021

ApJ

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In multi-messenger astronomy, rapid investigation of interesting transients is imperative. As an observatory with a 4π steradian field of view, and ∼99% uptime, the IceCube Neutrino Observatory is a unique facility to follow up transients, as well as to provide valuable insights for other observatories and inform their observational decisions. Since 2016, IceCube has been using low-latency data to rapidly respond to interesting astrophysical events reported by the multi-messenger observational community. Here, we describe the pipeline used to perform these followup analyses, and provide a summary of the 58 analyses performed as of July 2020. We find no significant signal in the first 58 analyses performed. The pipeline has helped inform various electromagnetic observation strategies, and has constrained neutrino emission from potential hadronic cosmic accelerators.

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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 Invarianmentioning

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

Proceedings of 40th International Conference on High Energy Physics — PoS(ICHEP2020)

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

Cited by 173 publications

References 71 publications

Physics and Phenomenology of Weakly Magnetized, Relativistic Astrophysical Shock Waves

Physics and Phenomenology of Weakly Magnetized, Relativistic Astrophysical Shock Waves

Follow-up of Astrophysical Transients in Real Time with the IceCube Neutrino Observatory

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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