Influence of the scattered Cherenkov light on the width of shower images as measured in the EAS fluorescence experiments

Giller, M.; Wieczorek, G.

doi:10.1016/j.astropartphys.2009.01.003

Cited by 12 publications

(18 citation statements)

References 17 publications

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“…The average ζ opt of the events used in this analysis is 1.3 • , reaching up to 4 • for showers detected close to the telescope. The amount of light outside of ζ opt due to the finite width of the shower image [58,59] and the point spread function of the optical system [60,61] is corrected for in later stages of the reconstruction and multiplyscattered light within ζ opt is also accounted for [62][63][64].…”

Section: Event Reconstructionmentioning

confidence: 99%

Depth of maximum of air-shower profiles at the Pierre Auger Observatory. I. Measurements at energies above1017.8 eV

Aab¹,

Abreu²,

Aglietta³

et al. 2014

Phys. Rev. D

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363

316

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We report a study of the distributions of the depth of maximum, Xmax, of extensive air-shower profiles with energies above 10 17.8 eV as observed with the fluorescence telescopes of the Pierre Auger Observatory. The analysis method for selecting a data sample with minimal sampling bias is described in detail as well as the experimental cross-checks and systematic uncertainties. Furthermore, we discuss the detector acceptance and the resolution of the Xmax measurement and provide parameterizations thereof as a function of energy. The energy dependence of the mean and standard 4 deviation of the Xmax-distributions are compared to air-shower simulations for different nuclear primaries and interpreted in terms of the mean and variance of the logarithmic mass distribution at the top of the atmosphere.

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Section: Event Reconstructionmentioning

confidence: 99%

Depth of maximum of air-shower profiles at the Pierre Auger Observatory. I. Measurements at energies above1017.8 eV

Aab¹,

Abreu²,

Aglietta³

et al. 2014

Phys. Rev. D

Self Cite

363

316

View full text Add to dashboard Cite

show abstract

“…Parametrizations of this distribution as a function of shower age and height can be found e.g. in [15] and [19]. These parametrizations are very good approximations of the true angular distribution if the local geomagnetic field component perpendicular to the shower axis is small or if one considers distributions averaged over the azimuthal angle relative to the shower axis.…”

Section: Universality Of Electron and Cherenkov Photon Distributionsmentioning

confidence: 99%

“…Based on such approximations several parametrizations of the angular distribution of Cherenkov light have been derived, see [7,11,15,19]. In these studies, the angular distribution of Cherenkov photons is considered as approximately symmetric about the shower axis and the influence of the local magnetic field has been neglected.…”

Section: Introductionmentioning

confidence: 99%

Asymmetry of the angular distribution of Cherenkov photons of extensive air showers induced by the geomagnetic field

Homola

Engel

Wilczyński

2015

Astroparticle Physics

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The angular distribution of Cherenkov light in an air shower is closely linked to that of the shower electrons and positrons. As charged particles in extensive air showers are deflected by the magnetic field of the Earth, a deformation of the angular distribution of the Cherenkov light, that would be approximately symmetric about the shower axis if no magnetic field were present, is expected. In this work we study the variation of the Cherenkov light distribution as a function of the azimuth angle in the plane perpendicular to shower axis. It is found that the asymmetry induced by the geomagnetic field is most significant for early stages of shower evolution and for showers arriving almost perpendicular to the vector of the local geomagnetic field. Furthermore, it is shown that ignoring the azimuthal asymmetry of Cherenkov light might lead to a significant under-or overestimation of the Cherenkov light signal especially at sites where the local geomagnetic field is strong. Based on CORSIKA simulations, the azimuthal distribution of Cherenkov light is parametrized in dependence on the magnetic field component perpendicular to the shower axis and the local air density. This parametrization provides an efficient approximation for estimating the asymmetry of the Cherenkov light distribution for shower simulation and reconstruction in cosmic ray and gamma-ray experiments in which the Cherenkov signal of showers with energies above 10 14 eV is observed.

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“…In this paper, the angular distribution of Cherenkov photons is simulated using the most updated simulation software and a new parametrization based on shower physics is proposed. The parametrization presented here improves the precision in the description of the angular distribution of Cherenkov light in comparison to models found in previous publications [8,24,26]. Beside the needed update of the parametrizations concerning the new shower models made available after the previous works, this paper aims at the improvement of the precision requested by the new generation of experiments [7,19] and at the refinement demanded by the new uses of Cherenkov light as the main signal source in FD analyses [15,16].…”

Section: Introductionmentioning

confidence: 82%

“…Experiments have measured the angular distribution of Cherenkov photons [25] in regime (b). Since the pioneering work [21], the angular distribution was simulated for regime (a) [8] and (b) [24,26].…”

Section: Introductionmentioning

confidence: 99%

Parametrization of the angular distribution of Cherenkov light in air showers

Arbeletche

Souza

2021

Eur. Phys. J. C

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The Cherenkov light produced in air showers largely contributes to the signal observed in ground-based gamma-ray and cosmic-ray observatories. Yet, no description of this phenomenon is available covering both regions of small and large angles to the shower axis. To fill this gap, a parametrization of the angular distribution of Cherenkov photons is performed in terms of a physically-motivated parametric function. Model parameters are constrained using simulated gamma-ray and proton showers with energies in the TeV to EeV region. As a result, a new parametrization is obtained that improves the precision of previous works. Results presented here can be used in the reconstruction of showers with imaging Cherenkov telescopes as well as in the reconstruction of shower profiles with fluorescence detectors.

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Influence of the scattered Cherenkov light on the width of shower images as measured in the EAS fluorescence experiments

Cited by 12 publications

References 17 publications

Depth of maximum of air-shower profiles at the Pierre Auger Observatory. I. Measurements at energies above1017.8 eV

Depth of maximum of air-shower profiles at the Pierre Auger Observatory. I. Measurements at energies above1017.8 eV

Asymmetry of the angular distribution of Cherenkov photons of extensive air showers induced by the geomagnetic field

Parametrization of the angular distribution of Cherenkov light in air showers

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