The engineering prototype of the wide-field Cherenkov telescope for the Yakutsk array

Иванов, А. А.; Кнуренко, С. П.; Krasilnikov, A. D.; Ksenofontov, I V; Петров, З. Е.; Правдин, М. И.; Timofeev, Lev; Sleptsov, I. E.

doi:10.1088/1742-6596/409/1/012084

Cited by 5 publications

(4 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Information from stations and commands from the center at the station is transmitted over the fiber optic link. A muon component, a charged component, Cherenkov radiation [9,10] and radio emission [11] are measured at the Yakutsk array.…”

Section: The Yakutsk Arraymentioning

confidence: 99%

Radio Emission of Air Showers with Energy E≥1019 eV Registration Results at Frequency 30-35 MHz by the Yakutsk Array Data.

Petrov¹,

Кнуренко²

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

View full text Add to dashboard Cite

Section: The Yakutsk Arraymentioning

confidence: 99%

Radio Emission of Air Showers with Energy E≥1019 eV Registration Results at Frequency 30-35 MHz by the Yakutsk Array Data.

Petrov¹,

Кнуренко²

2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

View full text Add to dashboard Cite

“…The scheme of ray tracing is illustrated in (Fig. 2) , where the spherical aberration of the point source image is seen on the PMT photocathode surface [2] [3].…”

Section: Operation Algorithmmentioning

confidence: 99%

The study of cosmic rays with a wide-angle Cherenkov telescope

Timofeev¹,

Иванов²

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

View full text Add to dashboard Cite

This report presents an observation method of Cherenkov light from extensive air showers (EAS) generated by cosmic rays (CRs) above 10 16 eV and preliminary observations. The interest in Cherenkov light differential detectors of EAS is caused by the possibility to measure the depth of cascade maximum, Xmax, and/or the shower age via angular and temporal distributions of the Cherenkov signal. In particular, it was shown using EAS model simulations that the pulse width measured at the periphery of the shower, r > 300 m, at sea level is pronouncedly connected with Xmax. Cherenkov detector is a wide-angle telescope working in coincidence with scintillation detectors, integral and differential Cherenkov detectors Yakutsk complex EAS. This provides the data on lateral distribution of photon intensity and total flux of Cherenkov light in EAS. The detector is located near (about 2m) with one of the integral Cherenkov detector. This detectors signal was calibrated using plastic optical radiator. So, we have a possibility to normalize an integral signal from telescope to that of the Cherenkov detector. We have completed the field testing of the prototype wide FOV telescope. A number of EAS events are detected in coincidence with the surface detectors of the Yakutsk array. A detection efficiency of the telescope is measured as well as the effective radius of the telescope detecting area. The report details the technical specifications of the telescope, as well as the results of the first experimental observations.

show abstract

“…2. Another goal is to study the transition region between galactic and extragalactic CR components, in which some irregularities in the spectrum and composition can be identified [1]. A crucial role played by the Cherenkov telescope array in this program should be to observe the light emitted by the extensive air showers for measuring the angular and temporal signal structures associated with the cascade curve in showers with energies above E = 10 15 eV [2].…”

Section: Introductionmentioning

confidence: 99%

Cherenkov telescope prototype

Timofeev

Иванов

2017

EPJ Web Conf.

View full text Add to dashboard Cite

Abstract. This report presents a prototype Cherenkov telescope, the observation method of Cherenkov light from extensive air showers (EAS) generated by cosmic rays (CRs) above 10 16 eV and preliminary observations. The interest in Cherenkov light differential detectors of EAS is caused by the possibility to measure the depth of the cascade maximum, X max , and/or the shower age via angular and temporal distributions of the Cherenkov signal. In particular, it was shown, using EAS model simulations, that the pulse width measured at the periphery of the shower, r > 300 m, at sea level is pronouncedly connected with X max . The Cherenkov detector is a wide-angle telescope working in coincidence with scintillation detectors, integral and differential Cherenkov detectors at the Yakutsk complex EAS.

show abstract

The engineering prototype of the wide-field Cherenkov telescope for the Yakutsk array

Cited by 5 publications

References 1 publication

Radio Emission of Air Showers with Energy E≥1019 eV Registration Results at Frequency 30-35 MHz by the Yakutsk Array Data.

Radio Emission of Air Showers with Energy E≥1019 eV Registration Results at Frequency 30-35 MHz by the Yakutsk Array Data.

The study of cosmic rays with a wide-angle Cherenkov telescope

Cherenkov telescope prototype

Contact Info

Product

Resources

About