The Tunka-133 EAS Cherenkov light array: Status of 2011

Berezhnev, S.F.; Besson, D.; Буднев, Н.; Чиавасса, А.; Chvalaev, O.; Gress, O.; Dyachok, A. N.; Epimakhov, S.; Haungs, A.; Karpov, N.; Калмыков, Н. Н.; Konstantinov, E.; Коробченко, А. В.; Коростелева, Е. Е.; Кожин, В. А.; Kuzmichev, L. A.; Лубсандоржиев, Б.; Лубсандоржиев, Н.; Миргазов, Р. Р.; Panasyuk, M. I.; Pankov, L.; Popova, E.; Просин, В. В.; Птускин, В. С.; Semeney, Yu.; Shaibonov, B.; Силаев, А.; Скурихин, А. В.; Snyder, J.; Spiering, C.; Schröder, Frank G.; Stockham, M.; Свешникова, Л.; Wischnewski, R.; Yashin, I. V.; Загородников, А.

doi:10.1016/j.nima.2011.12.091

Cited by 118 publications

(104 citation statements)

References 11 publications

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“…EAS Cherenkov light array Tunka-133 with ∼3 km 2 geometric area operated since 2009 [1]. Five winter seasons of data acquisition (∼10 7 triggers) and high quality of information permitted us to reconstruct primary energy spectrum and mass composition in the energy range 6 · 10 15 −10 18 eV.…”

Section: Introductionmentioning

confidence: 99%

Results from Tunka-133 (5 years observation) and from the Tunka-HiSCORE prototype

Просин

Berezhnev

Буднев

et al. 2016

EPJ Web of Conferences

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Abstract. Data obtained with two detectors located at the Tunka Cosmic Ray facility are presented. The Cherenkov light array for registration of extensive air showers (EAS) Tunka-133 collected data during 5 winter seasons since 2009 to 2014. The differential energy spectrum of all particles and the dependence of the average maximum depth on the energy in the range of 6 · 10 15 −10 18 eV measured for 1540 hours of observation are presented.The preliminary all particle energy spectrum by the data of TunkaHiSCORE prototype array, installed in 2013, is presented. Some additional experiments in the Tunka Valley are briefly described.

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Section: Introductionmentioning

confidence: 99%

Results from Tunka-133 (5 years observation) and from the Tunka-HiSCORE prototype

Просин

Berezhnev

Буднев

et al. 2016

EPJ Web of Conferences

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“…Many imaging and non-imaging techniques of observing air showers are based on the detection of the abundant number of photons produced as Cherenkov radiation of the secondary electrons and positrons in these showers (see, for example, [1][2][3][4][5]). Cherenkov light also constitutes an important contribution [6] to the optical signal recorded by fluorescence telescopes built for the observation of air showers above 10 17 eV [7][8][9][10].…”

Section: Introductionmentioning

confidence: 99%

“…All the shower simulations used for deriving the parametrization were made with 40 observational levels (planes perpendicular to the shower axis) spaced by a constant atmospheric depth interval ∆X = 25 g/cm 2 (see With use of the above tools we have developed an efficient parametrization that can be used at an arbitrarily selected experimental site if the local geomagnetic field vector is known. As an example, the location of the Tunka experiment [3] (51 • 48' N, 103 • 04' E) is considered in the following. In this experiment a surface array of non-imaging photon detectors is used to record the Cherenkov light emitted by extensive air showers of energies between 10 14 eV and 10 18 eV.…”

Section: Introductionmentioning

confidence: 99%

Asymmetry of the angular distribution of Cherenkov photons of extensive air showers induced by the geomagnetic field

Homola

Engel

Wilczyński

2015

Astroparticle Physics

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The angular distribution of Cherenkov light in an air shower is closely linked to that of the shower electrons and positrons. As charged particles in extensive air showers are deflected by the magnetic field of the Earth, a deformation of the angular distribution of the Cherenkov light, that would be approximately symmetric about the shower axis if no magnetic field were present, is expected. In this work we study the variation of the Cherenkov light distribution as a function of the azimuth angle in the plane perpendicular to shower axis. It is found that the asymmetry induced by the geomagnetic field is most significant for early stages of shower evolution and for showers arriving almost perpendicular to the vector of the local geomagnetic field. Furthermore, it is shown that ignoring the azimuthal asymmetry of Cherenkov light might lead to a significant under-or overestimation of the Cherenkov light signal especially at sites where the local geomagnetic field is strong. Based on CORSIKA simulations, the azimuthal distribution of Cherenkov light is parametrized in dependence on the magnetic field component perpendicular to the shower axis and the local air density. This parametrization provides an efficient approximation for estimating the asymmetry of the Cherenkov light distribution for shower simulation and reconstruction in cosmic ray and gamma-ray experiments in which the Cherenkov signal of showers with energies above 10 14 eV is observed.

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“…The following paragraphs summarize the analysis. A more detailed description is available in reference [142], and a short summary of the results is published in reference [143].…”

Section: A Radio Measurements At Tunkamentioning

confidence: 99%

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

Schröder¹

2012

Springer Theses

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Instruments and Methods for the Radio Detection of High Energy Cosmic RaysCosmic rays at energies above 10 15 eV cannot be measured directly due to the low flux. Instead, the properties of the primary cosmic ray particles (arrival direction, energy, mass) have to be reconstructed from measurements of secondary particles forming an air shower. For this, digital radio antenna arrays, like LOPES at the Karlsruhe Institute of Technology (KIT), are a relatively new instrument. The radio emission mainly originates from the deflection of secondary air shower electrons and positrons in the Earth's magnetic field. The radio technique aims at achieving a similar quality in the reconstruction of air shower parameters as the established Cherenkov or fluorescence light detection methods, which in contrast to the radio technique are limited to dark, moonless nights.The present studies aim to advance the air shower radio detection in technological aspects and analysis methods. The developments are mainly applied to LOPES, but also provide a useful set of tools, which will soon be applied on the analysis of first AERA measurements. AERA is a next generation digital radio array at the Pierre Auger Observatory in Argentina. Moreover, this thesis reflects the recent progress in the understanding of the radio emission by air showers. The main results of the studies are:• A new method for time calibration with a reference beacon has been developed.It allows a time resolution of ∼ 1 ns even with large antenna arrays. This is necessary for digital radio interferometry which improves the signal-to-noise ratio and the reconstruction accuracy of the primary particle properties. This method is essential for the measurement of cosmic rays with LOPES, and is going to be applied at AERA.• A per-event comparison of lateral distributions measured with LOPES and REAS3 simulations reflects a significantly improved understanding of the radio emission mechanisms. For the first time a Monte Carlo simulation of the radio emission by air showers can in average reproduce measured data. A detailed investigation of systematic effects was performed to accurately reconstruct LOPES lateral distributions. In particular, a method has been developed to appropriately treat the influence of radio noise on measured lateral distributions.• It is shown that a conical radio wavefront fits LOPES measurements and REAS3 simulations better than a spherical wavefront, which up to now has been assumed for LOPES beamforming analyses. Furthermore, the atmospheric depth of the shower maximum X max can be reconstructed by determining the opening angle of the conical wavefront. However, due to the small lateral extension of LOPES of about 200 m and the high radio background at KIT, the measurement uncertainty (∆X max ≈ 200 g/cm 2 ) is too large for a per-event reconstruction of the primary mass. This will improve at AERA, but could not be examined in detail because of a delay in the construction. • Eine neue Methode zur Zeitkalibration mit einen Rerefenzsender (Beaco...

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The Tunka-133 EAS Cherenkov light array: Status of 2011

Cited by 118 publications

References 11 publications

Results from Tunka-133 (5 years observation) and from the Tunka-HiSCORE prototype

Results from Tunka-133 (5 years observation) and from the Tunka-HiSCORE prototype

Asymmetry of the angular distribution of Cherenkov photons of extensive air showers induced by the geomagnetic field

Instruments and Methods for the Radio Detection of High Energy Cosmic Rays

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