Probing quantum gravity using photons from a flare of the active galactic nucleus Markarian 501 observed by the MAGIC telescope

Albert, J.; Aliu, E.; Anderhub, H.; Antonelli, L. A.; Antoranz, P.; Backes, Michael; Baixeras, C.; Barrio, J. A.; Bartko, H.; Bastieri, D.; Becker, J.; Bednarek, W.; Berger, K.; Bernardini, E.; Bigongiari, C.; Biland, A.; Böck, R.; Bonnoli, G.; Bordas, P.; Bosch‐Ramon, V.; Bretz, T.; Britvitch, I.; Cámara, Miguel; Carmona, E.; Chilingarian, A.; Commichau, S.; Contreras, J. L.; Cortina, J.; Costado, M. T.; Covino, S.; Curtef, V.; Dazzi, F.; Angelis, A. De; Pozo, E. De Cea del; Mendez, C. Delgado; Reyes, R. de los; Lotto, B. De; María, Mónica; Sabata, F. De; Domínguez, A.; Dorner, D.; Doro, M.; Errando, M.; Fagiolini, M.; Ferenc, D.; Fernández, E.; Firpo, R.; Fonseca, M. V.; Font, L.; Galante, N.; López, R. J. García; Garczarczyk, M.; Gaug, M.; Göebel, F.; Hayashida, M.; Herrero, A.; Höhne, D.; Hose, J.; Hsu, C. C.; Huber, Stefan; Jogler, T.; Kranich, D.; Barbera, A. La; Laille, A.; Leonardo, E.; Lindfors, E.; Lombardi, S.; Longo, F.; López, M.; Lorenz, E.; Majumdar, P.; Maneva, G.; Mankuzhiyil, N.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Meucci, M.; Meyer, M.; Miranda, J. M.; Mirzoyan, R.; Moles, M.; Moralejo, A.; Nieto, D.; Nilsson, K.; Ninković, J.; Otte, A. N.; Oya, I.; Panniello, M.; Paoletti, R.; Paredes, J. M.; Pasanen, M.; Pascoli, D.; Pauß, F.; Pegna, R.; Pérez-Torres, M. A.; Peršić, M.; Peruzzo, L.; Piccioli, A.; Prada, Francisco; Prandini, E.; Puchades, N.; Raymers, A.; Rhode, W.; Ribó, M.; Rico, J.; Rissi, M.; Robert, Aymeric; Rügamer, S.; Saggion, A.; Saito, Takayuki; Salvati, M.; Sánchez‐Conde, Miguel A.; Sartori, P.; Satalecka, K.; Scalzotto, V.; Scapin, V.; Schmitt, R.; Schweizer, T.; Shayduk, M.; Shinozaki, K.; Sidro, N.; Sierpowska-Bartosik, A.; Sillanpää, A.; Sobczyńska, D.; Spanier, F.; Stamerra, A.; Stark, L. S.; Takalo, L. O.; Tavecchio, F.; Temnikov, P.; Tescaro, D.; Teshima, M.; Tluczykont, M.; Torres, D. F.; Turini, N.; Vankov, H.; Venturini, A.; Vitale, V.; Wagner, R. M.; Wittek, W.; Zabalza, V.; Zandanel, F.; Zanin, R.; Zapatero, J.; Ellis, John; Mavromatos, Nikolaos; Nanopoulos, Dimitri V.; Sakharov, A.; Sarkisyan, E. K.G.

doi:10.1016/j.physletb.2008.08.053

Cited by 211 publications

(220 citation statements)

References 31 publications

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“…Strong flux variations on different timescales were observed from many AGNs. Variability in the VHE γ-ray regime was measured down to the minute timescale (Albert et al 2008b;Aharonian et al 2007). Many AGN lightcurves were produced by different γ-ray experiments from observations of flaring states, dedicated monitoring programs, or from joint campaigns with other experiments.…”

Section: Introductionmentioning

confidence: 99%

Long-term lightcurves from combined unified very high energyγ-ray data

Tluczykont

Bernardini²,

Satalecka³

et al. 2010

A&A

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Context. Very high-energy (VHE, E > 100 GeV) γ-ray data are a valuable input for multi-wavelength and multi-messenger (e.g. combination with neutrino data) studies. Aims. We aim at the conservation and homogenization of historical, current, and future VHE γ-ray-data on active galactic nuclei (AGN). Methods. We have collected lightcurve data taken by major VHE experiments since 1991 and combined them into long-term lightcurves for several AGN, and now provide our collected datasets for further use. Due to the lack of common data formats in VHE γ-ray astronomy, we have defined relevant datafields to be stored in standard data formats. The time variability of the combined VHE lightcurve data was investigated, and correlation with archival X-ray data collected by RXTE/ASM tested.Results. The combination of data on the prominent blazar Mrk 421 from different experiments yields a lightcurve spanning more than a decade. From this combined dataset we derive an integral baseline flux from Mrk 421 that must be lower than 33% of the Crab Nebula flux above 1 TeV. The analysis of the time variability yields log-normal flux variations in the VHE-data on Mrk 421. Conclusions. Existing VHE data contain valuable information concerning the variability of AGN and can be an important ingredient for multi-wavelength or multi-messenger studies. In the future, upcoming and planned experiments will provide more data from many transient objects, and the interaction of VHE astronomy with classical astronomy will intensify. In this context a unified and exchangeable data format will become increasingly important.

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Section: Introductionmentioning

confidence: 99%

Long-term lightcurves from combined unified very high energyγ-ray data

Tluczykont

Bernardini²,

Satalecka³

et al. 2010

A&A

Self Cite

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“…Specifically ω f is the inflexion point (see figure 5) where the quadratic dependence on energy terminates and the velocity tends to a limiting value. One could give an estimate of this point by comparing with the recent data of the current experiments of MAGIC [17,18], H.E.S.S [19] and FERMI [20] telescopes. In the case of our model, which predicts a quadratic dependence on the energy for the velocity (see eq.…”

Section: Discussionmentioning

confidence: 99%

“…[18] by fitting the recent experimental data of MAGIC [17] assuming a quadratic energy dependence for the photon refractive index. Hence, if we take the lowest bound for M 2 (M 2 = 2.6 × 10 10 GeV ) we conclude that the energy ω f , after which perturbation theory breaks down, should be quite smaller than 2.6×10 10 GeV .…”

Section: Discussionmentioning

confidence: 99%

Lorentz violation effects in asymmetric two brane models: a nonperturbative analysis

Farakos

2009

J. High Energy Phys.

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Lorentz violation effects in asymmetric two brane models: a nonperturbative analysisTo cite this article: K. Farakos JHEP08 (2009)031 View the article online for updates and enhancements. Abstract: We consider the case of bulk photons in a Lorentz violating brane background, with an asymmetric warping between space and time warp factors. A perturbative analysis, in a previous work, gave an energy dependent phase (or group) velocity of light: V ph (ω) = V ph (0) − C G ω 2 (C G > 0), which was derived up to second order of time independent perturbation theory. In this paper, we go beyond the perturbative result and we study the nonperturbative behavior of the phase velocity for larger energies, by solving numerically an eigenvalue problem for the wave function of the zero mode (4D photon). In particular we see that V ph (ω) is in general a monotonically decreasing function which tends asymptotically to a final value V ph (∞). We compare with the results of perturbation theory and we obtain a very good agreement in the range of small energies. We also present a wave function analysis and we see that in the nonperturbative sector of the theory (very high energies), the zero mode and the massive KK modes tend to decouple from matter localized on the TeV brane.

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“…Hence, from the observation of linearly polarized radiation coming from a distant source we obtain upper limits of the operator parameter values. Most birefringence tests are much more sensitive than dispersion tests, so only when no birefringence is present does dispersion provide useful information as is the case for d = 6 limits, obtained from the non observation of any time-offlight/energy correlations in AGN flares (of Mrk 501 by MAGIC [18], of PKS 2155-304 by HESS [19]) nor in GRB090510 by the Fermi-LAT [20]. For d = 3, limits are based on cosmic microwave background (CMB) polarization studies, while for d = 4 and d = 5, birefringence limits are obtained from measurements of the polarization fraction of the soft-γ-ray emission of GRBs (in the 200-325 keV and in the 70-300 keV energy ranges for integral/IBIS and IKAROS, respectively) [17].…”

Section: γ-Ray Polarimetry and Fundamental Sciencementioning

confidence: 99%

γ-Ray polarimetry with conversions to e+e− pairs: Polarization asymmetry and the way to measure it

Gros

Bernard

2017

Astroparticle Physics

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We revisit the measurement of the polarization fraction, P , and the measurement of the polarization angle of partially linearly-polarized gamma rays using their conversion to e + e − pairs in the field of a nucleus. We show that an inappropriate definition of the azimuthal angle, ϕ, used to reference the orientation of the final state degrades the precision of the measurement of P , by comparison to the optimal case where the bisector angle of the electron and of the positron momenta is used. We then focus on the lowest part of the energy spectrum, below ≈ 10 MeV, where a large part of the statistics lie for a cosmic source. We obtain the value of the polarization asymmetry, A, of pair conversion at threshold and we show that in the case where the correct expression is used for ϕ, the measured value of A tends to the limit.

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Probing quantum gravity using photons from a flare of the active galactic nucleus Markarian 501 observed by the MAGIC telescope

Cited by 211 publications

References 31 publications

Long-term lightcurves from combined unified very high energyγ-ray data

Long-term lightcurves from combined unified very high energyγ-ray data

Lorentz violation effects in asymmetric two brane models: a nonperturbative analysis

γ-Ray polarimetry with conversions to e+e− pairs: Polarization asymmetry and the way to measure it

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