216 research outputs found
Direct measurement of the muonic content of extensive air showers between and eV at the Pierre Auger Observatory
The hybrid design of the Pierre Auger Observatory allows for the measurement of the properties of extensive air showers initiated by ultra-high energy cosmic rays with unprecedented precision. By using an array of prototype underground muon detectors, we have performed the first direct measurement, by the Auger Collaboration, of the muon content of air showers between 2×10 and 2×10 eV. We have studied the energy evolution of the attenuation-corrected muon density, and compared it to predictions from air shower simulations. The observed densities are found to be larger than those predicted by models. We quantify this discrepancy by combining the measurements from the muon detector with those from the Auger fluorescence detector at 10eV and 10eV. We find that, for the models to explain the data, an increase in the muon density of 38% ±4%(12%) ± (21%)¦(18%) for EPOS-LHC, and of 50%(53%) ±4%(13%) ± (23%)¦(20%) for QGSJetII-04, is respectively needed
Design, upgrade and characterization of the silicon photomultiplier front-end for the AMIGA detector at the Pierre Auger Observatory
AMIGA (Auger Muons and Infill for the Ground Array) is an upgrade of the
Pierre Auger Observatory to complement the study of ultra-high-energy cosmic
rays (UHECR) by measuring the muon content of extensive air showers (EAS). It
consists of an array of 61 water Cherenkov detectors on a denser spacing in
combination with underground scintillation detectors used for muon density
measurement. Each detector is composed of three scintillation modules, with 10
m detection area per module, buried at 2.3 m depth, resulting in a total
detection area of 30 m. Silicon photomultiplier sensors (SiPM) measure the
amount of scintillation light generated by charged particles traversing the
modules. In this paper, the design of the front-end electronics to process the
signals of those SiPMs and test results from the laboratory and from the Pierre
Auger Observatory are described. Compared to our previous prototype, the new
electronics shows a higher performance, higher efficiency and lower power
consumption, and it has a new acquisition system with increased dynamic range
that allows measurements closer to the shower core. The new acquisition system
is based on the measurement of the total charge signal that the muonic
component of the cosmic ray shower generates in the detector.Comment: 40 pages, 33 figure
Searches for Ultra-High-Energy Photons at the Pierre Auger Observatory
The Pierre Auger Observatory, being the largest air-shower experiment in the
world, offers an unprecedented exposure to neutral particles at the highest
energies. Since the start of data taking more than 18 years ago, various
searches for ultra-high-energy (UHE, ) photons have
been performed: either for a diffuse flux of UHE photons, for point sources of
UHE photons or for UHE photons associated with transient events like
gravitational wave events. In the present paper, we summarize these searches
and review the current results obtained using the wealth of data collected by
the Pierre Auger Observatory.Comment: Review article accepted for publication in Universe (special issue on
ultra-high energy photons
Extraction of the Muon Signals Recorded with the Surface Detector of the Pierre Auger Observatory Using Recurrent Neural Networks
The Pierre Auger Observatory, at present the largest cosmic-ray observatory
ever built, is instrumented with a ground array of 1600 water-Cherenkov
detectors, known as the Surface Detector (SD). The SD samples the secondary
particle content (mostly photons, electrons, positrons and muons) of extensive
air showers initiated by cosmic rays with energies ranging from eV up
to more than eV. Measuring the independent contribution of the muon
component to the total registered signal is crucial to enhance the capability
of the Observatory to estimate the mass of the cosmic rays on an event-by-event
basis. However, with the current design of the SD, it is difficult to
straightforwardly separate the contributions of muons to the SD time traces
from those of photons, electrons and positrons. In this paper, we present a
method aimed at extracting the muon component of the time traces registered
with each individual detector of the SD using Recurrent Neural Networks. We
derive the performances of the method by training the neural network on
simulations, in which the muon and the electromagnetic components of the traces
are known. We conclude this work showing the performance of this method on
experimental data of the Pierre Auger Observatory. We find that our predictions
agree with the parameterizations obtained by the AGASA collaboration to
describe the lateral distributions of the electromagnetic and muonic components
of extensive air showers.Comment: 23 pages, 15 figures. Version accepted for publication in JINS
Measurement of the cosmic-ray energy spectrum above 2.5 x 10(18) eV using the Pierre Auger Observatory
We report a measurement of the energy spectrum of cosmic rays for energies above 2.5×10 eV based on 215,030 events recorded with zenith angles below 60°. A key feature of the work is that the estimates of the energies are independent of assumptions about the unknown hadronic physics or of the primary mass composition. The measurement is the most precise made hitherto with the accumulated exposure being so large that the measurements of the flux are dominated by systematic uncertainties except at energies above 5×10 eV. The principal conclusions are
(1) The flattening of the spectrum near 5×10 eV, the so-called “ankle,” is confirmed.
(2) The steepening of the spectrum at around 5×10 eV is confirmed.
(3) A new feature has been identified in the spectrum: in the region above the ankle the spectral index γ of the particle flux (∝E) changes from 2.51±0.03 (stat)±0.05 (syst) to 3.05±0.05 (stat)±0.10 (syst) before changing sharply to 5.1±0.3 (stat)±0.1 (syst) above 5×10 eV.
(4) No evidence for any dependence of the spectrum on declination has been found other than a mild excess from the Southern Hemisphere that is consistent with the anisotropy observed above 8×10 eV
Features of the energy spectrum of cosmic rays above 2.5×1018 eV using the pierre auger observatory
We report a measurement of the energy spectrum of cosmic rays above 2.5×10 eV based on 215 030 events. New results are presented: at about 1.3×10 eV, the spectral index changes from 2.51±0.03(stat)±0.05(syst) to 3.05±0.05(stat)±0.10(syst), evolving to 5.1±0.3(stat)±0.1(syst) beyond 5×10 eV, while no significant dependence of spectral features on the declination is seen in the accessible range. These features of the spectrum can be reproduced in models with energy-dependent mass composition. The energy density in cosmic rays above 5×10 eV is [5.66±0.03(stat)±1.40(syst)]×10 erg Mpc
Deep-Learning based Reconstruction of the Shower Maximum using the Water-Cherenkov Detectors of the Pierre Auger Observatory
The atmospheric depth of the air shower maximum is an
observable commonly used for the determination of the nuclear mass composition
of ultra-high energy cosmic rays. Direct measurements of are
performed using observations of the longitudinal shower development with
fluorescence telescopes. At the same time, several methods have been proposed
for an indirect estimation of from the characteristics of
the shower particles registered with surface detector arrays. In this paper, we
present a deep neural network (DNN) for the estimation of .
The reconstruction relies on the signals induced by shower particles in the
ground based water-Cherenkov detectors of the Pierre Auger Observatory. The
network architecture features recurrent long short-term memory layers to
process the temporal structure of signals and hexagonal convolutions to exploit
the symmetry of the surface detector array. We evaluate the performance of the
network using air showers simulated with three different hadronic interaction
models. Thereafter, we account for long-term detector effects and calibrate the
reconstructed using fluorescence measurements. Finally, we
show that the event-by-event resolution in the reconstruction of the shower
maximum improves with increasing shower energy and reaches less than
at energies above .Comment: Published version, 29 pages, 12 figure
Status and performance of the underground muon detector of the Pierre Auger Observatory
The Auger Muons and Infill for the Ground Array (AMIGA) is an enhancement of the Pierre Auger Observatory, whose purpose is to lower the energy threshold of the observatory down to 1016.5 eV, and to measure the muonic content of air showers directly. These measurements will significantly contribute to the determination of primary particle masses in the range between the second knee and the ankle, to the study of hadronic interaction models with air showers, and, in turn, to the understanding of the muon puzzle. The underground muon detector of AMIGA is concomitant to two triangular grids of water-Cherenkov stations with spacings of 433 and 750 m; each grid position is equipped with a 30 m2 plastic scintillator buried at 2.3 m depth. After the engineering array completion in early 2018 and general improvements to the design, the production phase commenced. In this work, we report on the status of the underground muon detector, the progress of its deployment, and the performance achieved after two years of operation. The detector construction is foreseen to finish by mid-2022
A Catalog of the Highest-energy Cosmic Rays Recorded during Phase I of Operation of the Pierre Auger Observatory
A catalog containing details of the highest-energy cosmic rays recorded through the detection of extensive air-showers at the Pierre Auger Observatory is presented with the aim of opening the data to detailed examination. Descriptions of the 100 showers created by the highest-energy particles recorded between 1 January 2004 and 31 December 2020 are given for cosmic rays that have energies in the range 78 EeV to 166 EeV. Details are also given of a further nine very-energetic events that have been used in the calibration procedure adopted to determine the energy of each primary. A sky plot of the arrival directions of the most energetic particles is shown. No interpretations of the data are offered
Measurement of the fluctuations in the number of muons in extensive air showers with the Pierre Auger Observatory
We present the first measurement of the fluctuations in the number of muons
in extensive air showers produced by ultra-high energy cosmic rays. We find
that the measured fluctuations are in good agreement with predictions from air
shower simulations. This observation provides new insights into the origin of
the previously reported deficit of muons in air shower simulations and
constrains models of hadronic interactions at ultra-high energies. Our
measurement is compatible with the muon deficit originating from small
deviations in the predictions from hadronic interaction models of particle
production that accumulate as the showers develop.Comment: Accepted for publication in PR
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