KASCADE measurements of energy spectra for elemental groups of cosmic rays: Results and open problems

Antoni, T.; Apel, W. D.; Badea, Anthony; Bekk, K.; Bercuci, A.; Blümer, J.; Bozdog, H.; Brâncuş, I.M.; Chilingarian, A.; Daumiller, K.; Döll, P.; Engel, R.; Engler, J.; Feßler, F.; Gils, H.J.; Glasstetter, R.; Haungs, A.; Heck, D.; Hörandel, J. R.; Kampert, K.‐H.; Klages, H. O.; Maier, G.; Mathes, H.J.; Mayer, H.J.; Milke, J.; Müller, M. A.; Obenland, R.; Oehlschläger, J.; Ostapchenko, S.; Petcu, M.; Rebel, H.; Risse, A.; Risse, M.; Roth, M.; Schatz, G.; Schieler, H.; Scholz, J.; Thouw, T.; Ulrich, H.; Buren, J. van; Vardanyan, A.; Weindl, A.; Wochele, J.; Zabierowski, J.

doi:10.1016/j.astropartphys.2005.04.001

Cited by 532 publications

(393 citation statements)

References 37 publications

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“…Our results also agree with the KASKADE results [11] on the proton flux at 1000 TeV. However, the results from the Tibet AS/γ experiment are in serious disagreement, both with the GRAPES-3 as well as with the JACEE and the SOKOL results for the He nuclei, probably showing the inadequacy of the shower size spectrum determined with an air shower array alone, to provide the spectral information on the He and other heavier nuclear groups.…”

Section: S K Guptasupporting

confidence: 79%

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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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Section: S K Guptasupporting

confidence: 79%

“…factors of >10 7 m 2 h are achieved [6][7][8][9][10][11]. However, with the exception of the Tibet-ASg and ARGO-YBJ experiments [8,9], the energy thresholds for most of the EAS arrays are significantly higher than the highest energy cosmic rays observed in the direct measurements.…”

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confidence: 94%

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

Gupta¹

2014

Proceedings of the Indian National Science Academy

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“…These considerations suggested the development of a simple and cheap thermal neutron detector, to be deployed over a large area, as 'hadron counter' in EAS experiments at mountain level. This idea led to the development of the EN-detector, made of a mixture of the well-known inorganic scintillator ZnS(Ag) with 6 LiF, capable of recording both thermal neutrons and charged particles [27] [28]. The study of neutrons in EAS was started in the 1930s [29] and experiments in the late Forties succeeded in demonstrating the production of neutrons in the nuclear interaction of cosmic rays [30][31] [32].…”

Section: Introductionmentioning

confidence: 99%

“…In modern experiments a multiparametric approach, based on the simultaneous detection of some of the EAS observables and their correlation, is carried out to infer the features of the cosmic ray spectrum. In addition to the electromagnetic component, muons (as in the KASCADE [6], CASA-MIA [7], EAS-TOP [8] and ICE-TOP [9] experiments) or Cherenkov light (as in DICE [10] and ARGO/WFCTA [2] [11]) are the most common EAS observables used for this purpose. Some specific experimental arrangements, as in the Tibet AS experiment [12], which uses burst detectors to sample high energy photons, can be also implemented.…”

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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“…At the time of writing of this proceeding, none of the available hadronic generator models is able to comprehensively describe the high energy cosmic ray experimental observations at the ultra high energy range [12,13]. Tuning to accelerator data should lead to convergence of the model predictions.…”

Section: Introductionmentioning

confidence: 99%

\(\langle X_{\text{max}} \rangle \) Uncertainty from Extrapolation of Cosmic Ray Air Shower Parameters

Abbasi

Thomson

2018

Proceedings of 2016 International Conference on Ultra-High Energy Cosmic Rays (UHECR2016)

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In this work we investigate the uncertainties in the prediction of the average shower maximum, < X max >, by the currently used high energy cosmic ray shower simulation models. Recent measurements at the LHC have provided constrains on some of the parameters in these models. However, uncertainties in the prediction of < X max > remain due to extrapolation from accelerator data up to center of mass of 250 TeV. The extrapolation in the elasticity, multiplicity, and p-p cross section from the LHC energy range to 3 × 10 19 eV in a cosmic ray's lab frame is investigated in this proceeding. Our calculation of the uncertainty in < X max > is approximately equal to the difference among the modern models being used in the field.

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KASCADE measurements of energy spectra for elemental groups of cosmic rays: Results and open problems

Cited by 532 publications

References 37 publications

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

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

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

\(\langle X_{\text{max}} \rangle \) Uncertainty from Extrapolation of Cosmic Ray Air Shower Parameters

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