Bounds on Lorentz Invariance Violation from MAGIC Observation of GRB 190114C

Acciari, V. A.; Ansoldi, S.; Antonelli, L. A.; Engels, A. Arbet; Baack, Dominik; Babić, Ana; Banerjee, B.; Almeida, U. Barres de; Barrio, J. A.; González, J. Becerra; Bednarek, W.; Bellizzi, Lorenzo; Bernardini, E.; Berti, Alessio; Besenrieder, Jürgen; Bhattacharyya, W.; Bigongiari, C.; Biland, A.; Blanch, O.; Bonnoli, Giacomo; Bošnjak, Željka; Busetto, G.; Carosi, R.; Ceribella, Giovanni; Cerruti, M.; Chai, Yating; Chilingarian, A.; Cikota, Stefan; Colak, S. M.; Colin, U.; 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; 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; Ferrara, G.; Foffano, Luca; Fonseca, M. V.; Font, L.; Fruck, C.; Fukami, Satoshi; López, R. J. García; Garczarczyk, M.; Gasparyan, Sargis; Gaug, M.; Giglietto, N.; Giordano, F.; Gliwny, Paweł; Godinović, N.; Green, D.; Hadasch, D.; Hahn, Alexander; Herrera, Javier; Hoang, J.; Hrupec, Dario; Hütten, Moritz; Inada, Tomohiro; Inoue, Susumu; Ishio, Kazuma; Iwamura, Y.; Jouvin, L.; Kajiwara, Y.; Karjalainen, Marie; Kerszberg, Daniel; Kobayashi, Yukiho; Kubo, H.; Kushida, J.; Lamastra, Alessandra; Lelas, D.; Leone, F.; Lindfors, E.; Lombardi, S.; Longo, F.; López, M.; López-Coto, R.; López-Oramas, Alicia; Loporchio, Serena; Fraga, Bernardo 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.; Mender, Simone; Mićanović, Saša; Miceli, Davide; Miener, Tjark; Minev, M.; Miranda, Jose Miguel; Mirzoyan, R.; Molina, Edgar; Moralejo, A.; Morcuende, Daniel; Moreno, V.; Moretti, E.; Munar-Adrover, P.; Neustroev, V.; Nigro, Cosimo; Nilsson, K.; Ninci, D.; Nishijima, K.; Noda, K.; Nogués, L.; Nozaki, S.; Ohtani, Y.; Oka, Tomohiko; Otero-Santos, Jorge; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Pavletić, Lovro; Peñil, Pablo; Perennes, C.; Peresano, M.; Peršić, M.; Moroni, P. G. Prada; Prandini, E.; Puljak, I.; Rhode, W.; Ribó, M.; Rico, J.; Righi, Chiara; Rugliancich, A.; Saha, L.; Sahakyan, N.; Saito, Takayuki; Sakurai, S.; Satalecka, K.; Schleicher, Bernd; Schmidt, K.; Schweizer, T.; Sitarek, J.; Šnidarić, Iva; Sobczyńska, D.; Spolon, Alessia; Stamerra, A.; Strom, D.; Strzys, M.; Suda, Y.; Surić, T.; Takahashi, M.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Teshima, M.; Torres-Albà, N.; Tosti, Luca; Scherpenberg, Juliane van; Vanzo, G.; Acosta, Mónica Vázquez; Ventura, Sofia; Verguilov, V.; Vigorito, C.; Vitale, V.; Vovk, Ievgen; Will, Martin; Zarić, Darko; Nava, Lara

doi:10.1103/physrevlett.125.021301

Cited by 69 publications

(38 citation statements)

References 35 publications

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“…The Lorentz invariance is violated as z > 1 but it assumes that there is a foliated diffeomorphism invariance with respect to the spatial sector (although the Lorentz invariance has been verified experimentally at sufficiently large scales, it is possible to have a Lorentz invariance violation at high energies (Please see [2] for details). This possibility also has been partially confirmed in some recent experiments, see [3,4] for examples.). By adding higher order spatial derivative terms into the Lagrangian, it can reconcile the UV divergence and make the theory renormalizable by power-counting [5].…”

Section: Introductionsupporting

confidence: 53%

Extended Hořava Gravity with Physical Ground-State Wavefunction

Shu

2021

Symmetry

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We propose a new extended theory of Hořava gravity based on the following three conditions: (i) power-counting renormalizable, (ii) healthy IR behavior and (iii) a stable vacuum state in a quantized version of the theory. Compared with other extended theories, we stress that any realistic theory of gravity must have physical ground states when quantization is performed. To fulfill the three conditions, we softly break the detailed balance but keep its basic structure unchanged. It turns out that the new model constructed in this way can avoid the strong coupling problem and remains power-counting renormalizable, moreover, it has a stable vacuum state by an appropriate choice of parameters.

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Section: Introductionsupporting

confidence: 53%

Extended Hořava Gravity with Physical Ground-State Wavefunction

Shu

2021

Symmetry

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“…where Λ eff is the effective deformation scale for pair-production, defined as a function of the high-energy scale Λ and the parameters β 1 , β 2 , γ 1 , and γ 2 . Comparison with Equation (18) shows the difference with the modification of the threshold in the LIV case by the large factor (m 2 e )/ε 2 . The alteration of the kinematics of SR is then substantially different in the LIV and the RDK cases.…”

Section: Threshold Of Pair Productionmentioning

confidence: 96%

“…Modified dispersion relations in a LIV scenario are constrained by the time of flight of photons coming from gamma-ray bursts (GRBs) [16][17][18], active galactic nuclei [19], or pulsars [20]. In the framework of the standard model extension [21], a linear (proportional to 1/Λ) variation of the speed of light also implies a birefringence effect, that may be tested in optical polarization measurements [22].…”

Section: Introductionmentioning

confidence: 99%

Bounds on Relativistic Deformed Kinematics from the Physics of the Universe Transparency

et al. 2020

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We analyze the kinematics of electron-positron production in a photon-photon interaction when one has a modification of the special relativistic kinematics as a power expansion in the inverse of a new high-energy scale. We derive the equation for the threshold energy of this reaction to first order in this expansion, including the effects due to a modification of the energy-momentum conservation equation. In contrast with the Lorentz invariance violation case, a scale of the order of a few TeV is found to be compatible with the observations of very high-energy cosmic gamma rays in the case of a modification compatible with the relativity principle.

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“…Although GRB afterglows have frequently been observed to span the radio to GeV bands, they had eluded detection in TeV gamma rays for a long time, despite numerous searches over many decades. A detection in the TeV band was finally achieved for GRB 190114C with the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) telescopes, starting from ∼60 seconds after the burst in the energy range 0.2-1 TeV and beyond, which provided the first strong evidence for inverse Compton emission from the afterglow (Mirzoyan et al 2019;MAGIC Collaboration et al 2019a,b), as well as new constraints on Lorentz invariance violation (Acciari et al 2020). The detection of gamma rays with energies above 0.1 TeV with the High Energy Stereoscopic System (H.E.S.S.)…”

Section: Introductionmentioning

confidence: 99%

MAGIC Observations of the Nearby Short Gamma-Ray Burst GRB 160821B ^*

Acciari

Ansoldi

Antonelli

et al. 2021

ApJ

Self Cite

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The coincident detection of GW170817 in gravitational waves and electromagnetic radiation spanning the radio to MeV gamma-ray bands provided the first direct evidence that short gamma-ray bursts (GRBs) can originate from binary neutron star (BNS) mergers. On the other hand, the properties of short GRBs in high-energy gamma rays are still poorly constrained, with only ∼20 events detected in the GeV band, and none in the TeV band. GRB 160821B is one of the nearest short GRBs known at z = 0.162. Recent analyses of the multiwavelength observational data of its afterglow emission revealed an optical-infrared kilonova component, characteristic of heavy-element nucleosynthesis in a BNS merger. Aiming to better clarify the nature of short GRBs, this burst was automatically followed up with the MAGIC telescopes, starting from 24 seconds after the burst trigger. Evidence of a gammaray signal is found above ∼0.5 TeV at a significance of ∼ 3 σ during observations that lasted until 4 hours after the burst. Assuming that the observed excess events correspond to gamma-ray emission from GRB 160821B, in conjunction with data at other wavelengths, we investigate its origin in the framework of GRB afterglow models. The simplest interpretation with one-zone models of synchrotronself-Compton emission from the external forward shock has difficulty accounting for the putative TeV flux. Alternative scenarios are discussed where the TeV emission can be relatively enhanced. The role of future GeV-TeV observations of short GRBs in advancing our understanding of BNS mergers and related topics is briefly addressed.

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Bounds on Lorentz Invariance Violation from MAGIC Observation of GRB 190114C

Cited by 69 publications

References 35 publications

Extended Hořava Gravity with Physical Ground-State Wavefunction

Extended Hořava Gravity with Physical Ground-State Wavefunction

Bounds on Relativistic Deformed Kinematics from the Physics of the Universe Transparency

MAGIC Observations of the Nearby Short Gamma-Ray Burst GRB 160821B ^*

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Bounds on Lorentz Invariance Violation from MAGIC Observation of GRB 190114C

Cited by 69 publications

References 35 publications

Extended Hořava Gravity with Physical Ground-State Wavefunction

Extended Hořava Gravity with Physical Ground-State Wavefunction

Bounds on Relativistic Deformed Kinematics from the Physics of the Universe Transparency

MAGIC Observations of the Nearby Short Gamma-Ray Burst GRB 160821B *

Contact Info

Product

Resources

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MAGIC Observations of the Nearby Short Gamma-Ray Burst GRB 160821B ^*