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Abstract
The Tunka Radio Extension (Tunka-Rex) is an antenna array consisting of 63 antennas at the location of the TAIGA facility (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy) in Eastern Siberia, nearby Lake Baikal. Tunka-Rex is triggered by the air-Cherenkov array Tunka-133 during clear and moonless winter nights and by the scintillator array Tunka-Grande during the remaining time. Tunka-Rex measures the radio emission from the same air-showers as Tunka-133 and Tunka-Grande, but with a higher threshold of about 100 PeV. During the first stages of its operation, Tunka-Rex has proven, that sparse radio arrays can measure air-showers with an energy resolution of better than 15\% and the depth of the shower maximum with a resolution of better than 40 g/cm\textsuperscript{2}. To improve and interpret our measurements as well as to study systematic uncertainties due to interaction models, we perform radio simulations with CORSIKA and CoREAS. In this overview we present the setup of Tunka-Rex, discuss the achieved results and the prospects of mass-composition studies with radio arrays.
Highlights
The study of cosmic rays of ultra-high energies sheds light on the most powerful processes in the Universe
The calibration of the Tunka-Rex antenna was performed in the following way: the directivity of the short aperiodic loaded loop antennas (SALLA) antenna was simulated with the NEC2 code [15], and normalized to an amplitude calibration made with the commercial reference source VSQ1000+DPA4000 by Schaffner Electrotest GmbH ( Teseq)
Since Xmax is very sensitive to the shape of the lateral distribution function (LDF), we apply additional quality cuts to select high-quality events: the event must contain at least one antenna further than 200 m from the shower axis, and the resulting fit uncertainty of Xmax must be less than 50 g/cm2
Summary
The study of cosmic rays of ultra-high energies sheds light on the most powerful processes in the Universe. At energies of about EeV, a transition from galactic to extragalactic cosmic ray sources is expected [1]. To distinguish between galactic and extragalactic sources, the precise determination of fluxes of different primary nuclei is required. Modern optical detectors nonimaging air-Cherenkov arrays and fluorescence telescopes reach energy resolutions of about 10% and a resolution for the depth of the shower maximum (Xmax) of about 20 g/cm. As a novel technique, which allows for measurements of air-showers produced by primary cosmic rays with energies above 100 PeV. A broad description of radio emission from air-showers, the technique of its detection and of historical and modern experiments is given in Ref. A broad description of radio emission from air-showers, the technique of its detection and of historical and modern experiments is given in Ref. [4]
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