A method of observing Cherenkov light at the Yakutsk EAS array

Lev Timofeev,Anatoly Ivanov,B Pattison

doi:10.1051/epjconf/201614514002

Abstract

A proposed new method for measuring the cherenkov light from extensive air showers (EAS) of cosmic rays (CR), which allows to determine not only the primary particle energy and angle of arrival, but also the parameters of the shower in the atmosphere – the maximum depth and “age”. For measurements it is proposed to use Cherenkov light produced by EAS in a ground network of wide-angle telescopes which are separated from each other by a distance 100–300 m depending on the total number of telescopes operating in coincidence, acting autonomously, or includes a detector of the charged components, radio waves, etc. as part of the EAS. Results of such an array should be developed. The energy measurement and CR angle of the arrival data on the depth of the maximum and the associated mass of the primary particle generating by EAS. This is particularly important in the study of galactic cosmic ray for E > 1014 eV, where currently there are no direct measurements of the maximum depth of the EAS.

Highlights

Investigation of Cherenkov light induced by cosmic rays (CRs) in the atmosphere began in the middle of the previous century in the UK and USSR
It was realized that the angular and temporal structure of the Cherenkov light emitted by extensive air shower (EAS) can be used to infer the longitudinal development parameters of the shower [4,5,6,7]. the angular distribution of Cherenkov photons from EAS was calculated by V.I
As part of the modernization program we developed two new integral Cherenkov telescopes, equipping them with the latest electronics we achieved a significant improvement in the time resolution, and combined them into the Cherenkov light registration system with adjustable zenith angle, to get information about the longitudinal shower development see Fig. 10

Summary

Introduction

Investigation of Cherenkov light induced by cosmic rays (CRs) in the atmosphere began in the middle of the previous century in the UK and USSR. It was realized that the angular and temporal structure of the Cherenkov light emitted by extensive air shower (EAS) can be used to infer the longitudinal development parameters of the shower [4,5,6,7]. The angular distribution of Cherenkov photons from EAS was calculated by V.I. Zatsepin [4] assuming it was determined mainly by that of the electrons in the shower. Fomin and Khristiansen proposed [5] to use the pulse shape of the Cherenkov signal, namely the pulse width, to indicate the shower maximum position, Xmax , in the atmosphere. A variety of detectors are used for instance, at the Tunka experiment forming an array of Cherenkov detectors functioning currently near Lake Baikal [10]

Data acquisition system

Pulse duration as a function of the distance to the shower core

Conclusions