Predominantly electromagnetic air showers of energy 10<sup>14</sup> eV to 10<sup>16</sup> eV

Kamata, K.; Shibata, S.; Saavedra, O.; Domingo, V.; Suga, K.; Murakami, K.; Toyoda, Y.; Pointe, M. La; Gaebler, J.; Escobar, I.

doi:10.1139/p68-177

Cited by 19 publications

(6 citation statements)

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“…There was some evidence in the binned data for excess event numbers toward both outer radio lobes (Clay et al 1984). Some supporting evidence was also noted in two other Southern Hemisphere experiments (Farley and Storey 1954;Kamata et al 1968), though with differing energy thresholds, angular resolutions, and years of operation. It was also acknowledged that, at PeV energies, the signal could not be due to gamma rays from Cen A as the path length for interactions of PeV gamma rays with CMB photons is only 10 kpc (Clay et al 1984).…”

Section: Searches At Pev Energiessupporting

confidence: 62%

Centaurus A at Ultra-High Energies

Clay

Whelan

Edwards

2010

Publ. – Astron. Soc. Aust

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Abstract:We review the importance of Centaurus A in high-energy astrophysics as a nearby object with many of the properties expected of a major source of very high-energy cosmic rays and gamma rays. We examine observational techniques and the results so far obtained in the energy range from 200 GeV to above 100 EeV and attempt to fit those data to expectations of Centaurus A as an astrophysical source from very high to ultra-high energies.

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Section: Searches At Pev Energiessupporting

confidence: 62%

Centaurus A at Ultra-High Energies

Clay

Whelan

Edwards

2010

Publ. – Astron. Soc. Aust

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“…The results of this counting experiment show their most significant peak (~3a) at 14 h sidereal time, close to the direction of Cen A. The experiment at Mt Chacaltaya (Kamata et ale 1968) studied the arrival directions of a subset of all showers (with typical energies of 10 15_101 6 eV) which were apparently deficient in muons (mu-poor showers). This criterion was thought to be characteristic of photon initiated showers.…”

Section: Other Anisotropy Studiesmentioning

confidence: 98%

“…These are the very early counting experiment at Auckland of Farley and' Storey (1954), and a mu-poor experiment at Mt Chacaltaya in the 1960s (Kamata et ale 1968).…”

Section: Other Anisotropy Studiesmentioning

confidence: 99%

Observation of an Excess of Cosmic Ray Showers from the Direction of Centaurus A

Clay¹,

Gerhardy²,

Liebing³

1984

Aust. J. Phys.

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“…The presence of the muon-poor showers was reported by the BASJE [107][108][109] and also by a Polish-French [110,111] collaborations. Subsequently, other detections were also reported by the [112] and the Tien-Shan [113] experiments.…”

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

confidence: 82%

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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Predominantly electromagnetic air showers of energy 10¹⁴ eV to 10¹⁶ eV

Cited by 19 publications

References 1 publication

Centaurus A at Ultra-High Energies

Centaurus A at Ultra-High Energies

Observation of an Excess of Cosmic Ray Showers from the Direction of Centaurus A

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

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Predominantly electromagnetic air showers of energy 1014 eV to 1016 eV

Cited by 19 publications

References 1 publication

Centaurus A at Ultra-High Energies

Centaurus A at Ultra-High Energies

Observation of an Excess of Cosmic Ray Showers from the Direction of Centaurus A

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

Contact Info

Product

Resources

About

Predominantly electromagnetic air showers of energy 10¹⁴ eV to 10¹⁶ eV