Characterisation of the electromagnetic component in ultra-high energy inclined air showers

Valiño, I.; Álvarez-Muñiz, J.; Roth, M.; Vázquez, R. A.; Zas, E.

doi:10.1016/j.astropartphys.2009.09.008

Cited by 15 publications

(18 citation statements)

References 26 publications

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“…For a shower with zenith angle 60 • it is found for the difference in atmospheric depth between the late and early part of the shower 2∆X = 370 g cm −2 at a distance of 1000 m from the core [7]. From equations (33) and (36) it follows for the difference between the late (β = π/2) and early (β = −π/2) part:…”

Section: Cone Modelmentioning

confidence: 97%

The center of lateral iso-density contours for inclined cosmic air showers

Montanus

2015

Exp Astron

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The horizontal lateral density of a cosmic air shower with a nonzero zenith angle is asymmetric. The asymmetry consist of a stretching of the iso-density contours to ellipses and to a shift of the center of the elliptic contours with respect to the core of the shower. The shift is caused by atmospheric attenuation. The modeling of the attenuation results in an equation for the shift as a function of zenith angle and the size of the iso-density contours. A more accurate equation is obtained by investigating the shift in lateral densities of simulated showers. It is shown how the shift can be incorporated in an elliptic lateral density function. A linear approximation for the shift allows for an analytical solution for the shifted elliptic density. Its predictions for the polar variations of the density are compared with data of simulated showers.

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Section: Cone Modelmentioning

confidence: 97%

The center of lateral iso-density contours for inclined cosmic air showers

Montanus

2015

Exp Astron

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“…The simulation is done with the Auger Off line software framework [39]. A residual electromagnetic signal component, mainly due to muon decays in flight, is taken into account according to model predictions [40].…”

Section: A Einv From Inclined Showersmentioning

confidence: 99%

“…Valdés Galicia, 10 I. Valiño,12,13 L. Valore, 22,15 36 Z. Zong, 28 and F. Zuccarello 39,40 (The Pierre Auger Collaboration) , *…”

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confidence: 99%

Data-driven estimation of the invisible energy of cosmic ray showers with the Pierre Auger Observatory

Aab¹,

Abreu²,

Aglietta³

et al. 2019

Phys. Rev. D

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4The determination of the primary energy of extensive air showers using the fluorescence detection technique requires an estimation of the energy carried away by particles that do not deposit all their energy in the atmosphere. This estimation is typically made using Monte Carlo simulations and thus depends on the assumed primary particle mass and on model predictions for neutrino and muon production. In this work we present a new method to obtain the invisible energy from events detected by the Pierre Auger Observatory. The method uses measurements of the muon number at ground level, and it allows us to reduce significantly the systematic uncertainties related to the mass composition and the high energy hadronic interaction models, and consequently to improve the estimation of the energy scale of the Observatory.

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“…It is mainly due to the showering of the electrons from muon decay in flight, although high-energy muons very close to the core also contribute through pair production and bremsstrahlung. More details can be found in [15]. In the reconstruction procedure (see section 4) the signals measured with the SD are compared to the reference muon distribution, and for this purpose it is necessary to extract the signal induced by muons from the total signal at each detector.…”

Section: Electromagnetic Componentmentioning

confidence: 99%

Reconstruction of inclined air showers detected with the Pierre Auger Observatory

Aab¹,

Abreu²,

Aglietta³

et al. 2014

J. Cosmol. Astropart. Phys.

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Abstract. We describe the method devised to reconstruct inclined cosmic-ray air showers with zenith angles greater than 60 • detected with the surface array of the Pierre Auger Observatory. The measured signals at the ground level are fitted to muon density distributions predicted with atmospheric cascade models to obtain the relative shower size as an overall normalization parameter. The method is evaluated using simulated showers to test its performance. The energy of the cosmic rays is calibrated using a sub-sample of events reconstructed with both the fluorescence and surface array techniques. The reconstruction method described here provides the basis of complementary analyses including an independent measurement of the energy spectrum of ultra-high energy cosmic rays using very inclined events collected by the Pierre Auger Observatory.

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Characterisation of the electromagnetic component in ultra-high energy inclined air showers

Cited by 15 publications

References 26 publications

The center of lateral iso-density contours for inclined cosmic air showers

The center of lateral iso-density contours for inclined cosmic air showers

Data-driven estimation of the invisible energy of cosmic ray showers with the Pierre Auger Observatory

Reconstruction of inclined air showers detected with the Pierre Auger Observatory

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