Electron, muon, and hadron lateral distributions measured in air showers by the KASCADE experiment

Antoni, T.; Apel, W. D.; Badea, F.; Bekk, K.; Bernlöhr, K.; Blümer, H.; Bollmann, E.; Bozdog, H.; Brâncuş, I.M.; Chilingarian, A.; Daumiller, K.; Döll, P.; Engler, J.; Feßler, F.; Gils, H.J.; Glasstetter, R.; Haeusler, R.; Hafemann, W.; Haungs, A.; Heck, D.; Holst, T.; Hörandel, J. R.; Kampert, K.‐H.; Kempa, J.; Klages, H. O.; Knapp, J.; Martello, D.; Mathes, H.J.; Mayer, H.J.; Milke, J.; Mühlenberg, D.; Oehlschläger, J.; Petcu, M.; Rebel, H.; Risse, M.; Roth, M.; Schatz, G.; Schmidt, Fabian; Thouw, T.; Ulrich, H.; Vardanyan, A.; Vulpescu, B.; Weber, J.H.; Wentz, J.; Wiegert, Theresa; Wochele, J.; Zabierowski, J.

doi:10.1016/s0927-6505(00)00125-0

Cited by 100 publications

(55 citation statements)

References 20 publications

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“…Some specific experimental arrangements, as in the Tibet AS experiment [12], which uses burst detectors to sample high energy photons, can be also implemented. On the contrary, an extensive use of the hadron detection to get information on the cosmic ray spectrum was limited up to now by the absence of simple and cheap hadron detectors, being very expensive and quite complicated the use of conventional hadron calorimeters (HCAL) over large areas [13][14] [15]. Emulsion chambers (EC) have been also used to detect high energy hadrons, mainly in stand-alone experiments at high altitude [16] [17][18] [19] .…”

Section: Introductionmentioning

confidence: 99%

Detection of thermal neutrons with the PRISMA-YBJ array in extensive air showers selected by the ARGO-YBJ experiment

Bartoli

Bernardini

et al. 2016

Astroparticle Physics

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We report on a measurement of thermal neutrons, generated by the hadronic component of extensive air showers (EAS), by means of a small array of EN-detectors developed for the PRISMA project (PRImary Spectrum Measurement Array), novel devices based on a compound alloy of ZnS(Ag) and 6 LiF. This array has been operated within the ARGO-YBJ experiment at the high altitude Cosmic Ray Observatory in Yangbajing (Tibet, 4300 m a.s.l.). Due to the tight correlation between the air shower hadrons and thermal neutrons, this technique can be envisaged as a simple way to estimate the number of high energy hadrons in EAS. Coincident events generated by primary cosmic rays of energies greater than 100 TeV have been selected and analyzed. The EN-detectors have been used to record simultaneously thermal neutrons and the air shower electromagnetic component. The density distributions of both components and the total number of thermal neutrons have been measured. The correlation of these data with the measurements carried out by ARGO-YBJ confirms the excellent performance of the EN-detector.2

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Section: Introductionmentioning

confidence: 99%

Detection of thermal neutrons with the PRISMA-YBJ array in extensive air showers selected by the ARGO-YBJ experiment

Bartoli

Bernardini

et al. 2016

Astroparticle Physics

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“…837 [64,65] and the GRAPES-2 [10] are the other recent experiments using either a large area muon detector or an array of muon detectors with the capability to observe the muon-poor showers. However, the GRAPES-3 experiment [61] with its single large area (560 m 2 ) muon detector is attempting to reach a significantly higher level of sensitivity to the γ-initiated showers based on their small muon content, particularly at the sub-PeV energies, lower than those achieved by the CASA-MIA experiment.…”

Section: High Energy Astroparticle Physics At Ooty and The Grapes-3 Ementioning

confidence: 99%

“…Using an array of muon detectors, the muon size is determined for individual showers from an integration over the lateral distribution function as fitted to the observed muon densities, for example in the CASA-MIA [62] and KASCADE [64] experiments. Using a single large area muon detector, such as in the EAS-TOP experiment [74], the muon size has been estimated for individual showers from the lateral distribution function obtained from a fit to the data.…”

Section: High Energy Astroparticle Physics At Ooty and The Grapes-3 Ementioning

confidence: 99%

“…Practical and economic constraints limit the number of detectors deployed in a shower array, thus providing only a sampling of the particle density at a limited number of points. Even in good shower arrays, for example, the CASA-MIA [62], the Tibet AS γ [63] and the KASCADE [64] arrays, the detection area does not exceed about 1 percent of the physical area over which the array is spread out. However, this is an important parameter which contributes significantly to the accuracy of the measurement of shower size (and consequently primary energy) as well as the arrival direction, particularly for γ-ray astronomy.…”

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confidence: 99%

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High Energy Astroparticle Physics at Ooty and the GRAPES-3 Experiment

Gupta¹

2014

Proceedings of the Indian National Science Academy

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The astroparticle studies at Ooty have their roots going way back into the fifties, when studies using cosmic rays were initiated with cloud chambers of progressively larger sizes as the primary detector and measuring device to obtain properties of hadrons at high energies. This study was subsequently strengthened with the installation of a total absorption calorimeter and a modest extensive air shower array to probe the composition of the primary cosmic rays to very high energies. The discovery of pulsars provided a thrust for the exploration of these compact objects as the sources of γ-rays at TeV energies with the aid of atmospheric Cerenkov detectors in the seventies. With the rapid technological advances occurring during the subsequent years in detectors, electronics and computers, physicists world-wide were able to set up very large and remarkably sensitive experiments that were hard to imagine a decade earlier. With the increasing sophistication and complexity the modern experiments require participation of very large teams of scientists. This development has made the formation of collaboration of large number of physicists both experimental and theoretical, engineers, technicians etc., from a number of institutions and universities, a prerequisite for setting up any major experimental facility. The GRAPES-3 experiment is a collaboration of 34 scientists from 13 institutions, including 8 from India and 5 from Japan. The GRAPES-3 experiment contains a dense extensive air shower array operating with ~ 400 scintillator detectors and a 560 m 2 tracking muon detector (Em > 1 GeV), at Ooty in India. 25 % of scintillator detectors are instrumented with two fast photomultiplier tubes (PMTs) for extending the dynamic range to ~ 5x10 3 particles m -2. The scintillators, signal processing electronics and data recording systems were fabricated in-house to cut costs and optimize performance. The muon multiplicity distribution of the EAS is used to probe the composition of primary cosmic rays below the 'knee', with an overlap with direct measurements. Search for multi-TeV γ-rays from point sources is done with the aid of the muon detector. A good angular resolution of 0.7 o at 30 TeV, is measured from shadow of the Moon on the isotropic flux of cosmic rays. Sensitive limit on the diffuse flux of 100 TeV γ-rays is placed by using muon detector to filter out the charged cosmic ray background. The tracking muon detector allows sensitive measurements on the coronal mass ejections and solar flares through Forbush decrease events. We have major expansion plans to enhance the sensitivity of the GRAPES-3 experiment in the areas listed above. PACS

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“…Showers are reconstructed in three stages using different algorithms [120]. First, the shower core position is determined by the center of gravity of the e/γ detector signals.…”

Section: Kascadementioning

confidence: 99%

The HiSPARC cosmic ray experiment : data acquisition and reconstruction of shower direction

Fokkema¹

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Electron, muon, and hadron lateral distributions measured in air showers by the KASCADE experiment

Cited by 100 publications

References 20 publications

Detection of thermal neutrons with the PRISMA-YBJ array in extensive air showers selected by the ARGO-YBJ experiment

Detection of thermal neutrons with the PRISMA-YBJ array in extensive air showers selected by the ARGO-YBJ experiment

High Energy Astroparticle Physics at Ooty and the GRAPES-3 Experiment

The HiSPARC cosmic ray experiment : data acquisition and reconstruction of shower direction

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