Teraelectronvolt emission from the $γ$-ray burst GRB 190114C

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, A.; 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'Amico, G.; 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.; Fernández-Barral, A.; Ferrara, G.; Fidalgo, D.; Foffano, L.; Fonseca, M. V.; Font, L.; Fruck, C.; Fukami, S.; Gallozzi, 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.; Masuda, S.; 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.; Nöthe, M.; Nozaki, S.; Paiano, S.; Palacio, J.; 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.; Tsujimoto, S.; Vagelli, V.; van Scherpenberg, J.; Vanzo, G.; Acosta, M. Vazquez; Vigorito, C. F.; Vitale, V.; Vovk, I.; Will, M.; Zarić, D.; Nava, L.

doi:10.48550/arxiv.2006.07249

Cited by 2 publications

(3 citation statements)

References 43 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Recently multi-frequency observations of the ultrabright GRB 190114C at redshift z = 0.425 (Selsing et al 2019;Castro-Tirado, et al 2019) and its afterglow emission across 17 orders of magnitude in energy, from 5 × 10 −6 to 10 12 eV, found that its broad band spectral energy density, was double-peaked. Its high energy hump which was observed with the HAWC telescope (Acciari et al 2019c) peaked around TeV (after correcting for absorption by extragalactic background light, while the Fermi and Swift observations of GRB 190114C (Ajello et al 2020) indicated a broad SED hump which peaked around 5.2 keV. The observed peaks ratio, (1+z)E p2 /E p1 ≈ 2.74 × 10 8 , is consistent with that observed in blazars (eq.…”

Section: Double Hump Afterglow Of Grbs ?supporting

confidence: 82%

“…The SSC model of high energy emission had considerable success in fitting the observed broad band SED of many blazars. The SSC models have been used also to explain the recent discoveries of TeV gamma ray emission from the gamma ray burst (GRB) 190114C (Ajello et al 2020) Acciari et al 2019c) and from the terminal lobes of the bipolar jet of the Galactic microquasar SS 433 (Abeysekara et al 2018;Xing et al 2019). These successful fits, however, involved many adjustable parameters and free choices.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Universal Peaks Ratio In The Spectral Energy Density Of Double Hump Blazars, Gamma Ray Bursts, And Microquasars

Dado,

Dar

2020

Preprint

View full text Add to dashboard Cite

The peak frequencies of the two broad humps evident in the spectral energy density of blazars are time dependent and vary a lot between different blazars. However, their ratio in most blazars, appears to be almost universal and equal to m e c 2 /2(1+z)ǫ p to a good approximation, where m e is the electron mass, ǫ p is the peak energy of the cosmic microwave background radiation, and z is the redshift of the blazar. We discuss a possible origin of such a universal ratio in blazars, gamma ray bursts (GRBs), and perhaps also in microquasars. We also point out a possible connection between the knee in the energy spectrum of cosmic ray electrons and the maximal peak energies of the two broad humps in the spectral energy density of high-energy peaked blazars and GRBs.

show abstract

Section: Double Hump Afterglow Of Grbs ?supporting

confidence: 82%

Section: Introductionmentioning

confidence: 99%

Universal Peaks Ratio In The Spectral Energy Density Of Double Hump Blazars, Gamma Ray Bursts, And Microquasars

Dado,

Dar

2020

Preprint

View full text Add to dashboard Cite

show abstract

“…Gamma-ray detectors have hitherto utilized three types of sources for LIV studies: Gamma-Ray Bursts (GRBs), Pulsars, and Active Galactic Nuclei (AGNs) flares. Some of the most stringent constraints, outlined in Table 1, have been acquired from observations performed with the FermiLarge Area Telescope (LAT) [24], the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes [25][26][27][28], the High Energy Stereoscopic System (H.E.S.S.) telescopes [29,30], or, very recently, from the Large High Altitude Air Shower Observatory (LHAASO) [31].…”

Section: Introductionmentioning

confidence: 99%

Constraints on Lorentz invariance violation from the extraordinary Mrk 421 flare of 2014 using a novel analysis method

Abe,

Abhir,

Abhishek

et al. 2024

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

The Lorentz Invariance Violation (LIV), a proposed consequence of certain quantum gravity (QG) scenarios, could instigate an energy-dependent group velocity for ultra-relativistic particles. This energy dependence, although suppressed by the massive QG energy scale E_QG, expected to be on the level of the Planck energy 1.22 × 1019 GeV, is potentially detectable in astrophysical observations. In this scenario, the cosmological distances traversed by photons act as an amplifier for this effect. By leveraging the observation of a remarkable flare from the blazar Mrk 421, recorded at energies above 100 GeV by the MAGIC telescopes on the night of April 25 to 26, 2014, we look for time delays scaling linearly and quadratically with the photon energies. Using for the first time in LIV studies a binned-likelihood approach we set constraints on the QG energy scale. For the linear scenario, we set 95% lower limits E_QG>2.7×1017 GeV for the subluminal case and E_QG> 3.6 ×1017 GeV for the superluminal case. For the quadratic scenario, the 95% lower limits for the subluminal and superluminal cases are E_QG>2.6 ×1010 GeV and E_QG>2.5×1010 GeV, respectively.

show abstract

Teraelectronvolt emission from the $γ$-ray burst GRB 190114C

Cited by 2 publications

References 43 publications

Universal Peaks Ratio In The Spectral Energy Density Of Double Hump Blazars, Gamma Ray Bursts, And Microquasars

Universal Peaks Ratio In The Spectral Energy Density Of Double Hump Blazars, Gamma Ray Bursts, And Microquasars

Constraints on Lorentz invariance violation from the extraordinary Mrk 421 flare of 2014 using a novel analysis method

Contact Info

Product

Resources

About