/ Astrophysics


The TUS space fluorescence detector for study of UHECR and other phenomena of variable fluorescence light in the atmosphere


Abrashkin, V. (Automatic Systems, Samara) ; Alexandrov, V. (Moscow State U.) ; Arakcheev, Y. (Automatic Systems, Samara) ; Bitkin, E. (ISTOK, Moscow) ; Cordero, A. (Puebla U., Mexico) ; Eremin, S. (ISTOK, Moscow) ; Finger, M. (Dubna, JINR) ; Garipov, G. (SINP, Moscow) ; Grebenyuk, V. (Ewha Women's U., Seoul) ; Kalmykov, N. (SINP, Moscow) ; Khrenov, B. (SINP, Moscow) ; Koval, V. (Automatic Systems, Samara) ; Martinez, O. (Puebla U., Mexico) ; Matyushkin, A. (ISTOK, Moscow) ; Moreno, E. (Puebla U., Mexico) ; Naumov, D. (Dubna, JINR) ; Olshevsky, A. (Dubna, JINR) ; Panasyuk, M. (SINP, Moscow) ; Park, I. (Ewha Women's U., Seoul) ; Robledo, C. (Puebla U., Mexico) ; Rubinstein, I. (SINP, Moscow) ; Sharakin, S. (SINP, Moscow) ; Silaev, A. (SINP, Moscow) ; Tkatchev, L. (Dubna, JINR) ; Tulupov, V. (SINP, Moscow) ; Tyukaev, R. (Energia RSC, Korolyov) ; Sabirov, B. (Dubna, JINR) ; Salazar, H. (Puebla U., Mexico) ; Saprykin, O. (Energia RSC, Korolyov) ; Syromyatnikov, V. (Energia RSC, Korolyov) ; Urmantsev, F. (ISTOK, Moscow) ; Villasenor, L. (IFM-UMSNH, Michoacan) ; Yashin, I. (SINP, Moscow) ; Zaikin, N. (Dubna, JINR) ; Zepeda, A. (CINVESTAV, IPN)

Published in: Adv.Space Res.
Year: 2006
Vol.: 37
Page No: 1876-1883
Pages: 8
Year: 2006 published

Abstract: The Tracking Ultraviolet Set Up (TUS) instrument has been designed to observe from space the fluorescence light in the atmosphere when Extensive Air Shower (EAS) or other phenomena such as meteors or dust grains traverse it. The TUS design concepts will allow us to construct the next generation of fluorescence detectors with increasing light collection power and higher resolution. The KLYPVE instrument with collection power 5 times larger of the TUS will be the next space detector. Light collection is obtained with the help of segmented “low frequency Fresnel type” mirrors. Photo receiver retina in the focal consists of modules of PM tubes. For stable performance in conditions of variable light noise and variable temperature the tube type with a multi-alcali cathode was chosen. Voltage supplies for PMT in one module were designed for keeping the performance of photo receiver retina uniform when the tube gain change. From every tube the signal amplitude is recorded in time bins of 400 ns. The digital data are kept and analyzed in the module FPGA connected to the central FPGA controlling all data. The RAM memory is large, capable to record events with different duration of the light signal (up to several seconds). The preliminary event data are analyzed in the triggering system of the central FPGA. The trigger criteria have several options for events of different origin (different pixel signal duration). The trigger integration time is controlled from the space mission center. The performances of the detector were simulated and zenith angle dependent trigger efficiencies were calculated. The TUS detector will be efficient in recording “horizontal” EAS (zenith angles more than 60°), developed to their maximum above the cloud cover. The EAS Cherenkov light, back scattered from the cloud cover, will be recorded and will improve data on the EAS direction and position of maximum. For better accuracy in physical parameters of the events and for the experimental check of this accuracy the performance of two TUS detectors at the space platform was recommended. The accommodation of 2 TUS detectors at space platform of the “RESURS O” type was tried and approved. The TUS prototypes are being tested in the Mexican mountains. The photo receiver of two PM tubes with the TUS electronics on-board of the MSU Tatiana satellite is measuring the atmosphere light background.

Keyword(s): Cosmic rays ; Extreme energy ; Atmosphere ; Fluorescence ; Space Platform ; Mirror-concentrator

Total numbers of views: 291
Numbers of unique views: 172
DOI: 10.1016/j.asr.2005.05.095
 Record created 2016-11-09, last modified 2016-11-09



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