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The Tunka Radio Extension (Tunka-Rex): Radio Measurements of Cosmic Rays in Siberia (PISA 2015)

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Title: The Tunka Radio Extension (Tunka-Rex): Radio Measurements of Cosmic Rays in Siberia (PISA 2015)
Authors: Schröder, F. G., Bezyazeekov, P., Budnev, N. M., Gress, O. A., Haungs, A., Hiller, R., Huege, T., Kazarina, Y., Kleifges, M., Konstantinov, E. N., Korosteleva, E. E., Kostunin, D., Krömer, O., Kuzmichev, L. A., Lubsandorzhiev, N., Mirgazov, R. R., Monkhoev, R., Pakhorukov, A., Pankov, L., Prosin, V. V., Rubtsov, G. I., Wischnewski, R., Zagorodnikov, A.
Source: Nucl. Instr. Meth. A 824 (2016) 652
Publication Year: 2015
Collection: Astrophysics
Subject Terms: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
More Details: The Tunka observatory is located close to Lake Baikal in Siberia, Russia. Its main detector, Tunka-133, is an array of photomultipliers measuring Cherenkov light of air showers initiated by cosmic rays in the energy range of approximately $10^{16}-10^{18}\,$eV. In the last years, several extensions have been built at the Tunka site, e.g., a scintillator array named Tunka-Grande, a sophisticated air-Cherenkov-detector prototype named HiSCORE, and the radio extension Tunka-Rex. Tunka-Rex started operation in October 2012 and currently features 44 antennas distributed over an area of about $3\,$km$^2$, which measure the radio emission of the same air showers detected by Tunka-133 and Tunka-Grande. Tunka-Rex is a technological demonstrator that the radio technique can provide an economic extension of existing air-shower arrays. The main scientific goal is the cross-calibration with the air-Cherenkov measurements. By this cross-calibration, the precision for the reconstruction of the energy and mass of the primary cosmic-ray particles can be determined. Finally, Tunka-Rex can be used for cosmic-ray physics at energies close to $1\,$EeV, where the standard Tunka-133 analysis is limited by statistics. In contrast to the air-Cherenkov measurements, radio measurements are not limited to dark, clear nights and can provide an order of magnitude larger exposure.
Comment: Accepted for publication in Nuclear Instruments and Methods A, within Proceedings of the 13th Pisa Meeting on Advanced Detectors 2015
Document Type: Working Paper
DOI: 10.1016/j.nima.2015.08.075
Access URL: http://arxiv.org/abs/1509.01495
Accession Number: edsarx.1509.01495
Database: arXiv
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  Data: The Tunka Radio Extension (Tunka-Rex): Radio Measurements of Cosmic Rays in Siberia (PISA 2015)
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  Data: Nucl. Instr. Meth. A 824 (2016) 652
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  Data: The Tunka observatory is located close to Lake Baikal in Siberia, Russia. Its main detector, Tunka-133, is an array of photomultipliers measuring Cherenkov light of air showers initiated by cosmic rays in the energy range of approximately $10^{16}-10^{18}\,$eV. In the last years, several extensions have been built at the Tunka site, e.g., a scintillator array named Tunka-Grande, a sophisticated air-Cherenkov-detector prototype named HiSCORE, and the radio extension Tunka-Rex. Tunka-Rex started operation in October 2012 and currently features 44 antennas distributed over an area of about $3\,$km$^2$, which measure the radio emission of the same air showers detected by Tunka-133 and Tunka-Grande. Tunka-Rex is a technological demonstrator that the radio technique can provide an economic extension of existing air-shower arrays. The main scientific goal is the cross-calibration with the air-Cherenkov measurements. By this cross-calibration, the precision for the reconstruction of the energy and mass of the primary cosmic-ray particles can be determined. Finally, Tunka-Rex can be used for cosmic-ray physics at energies close to $1\,$EeV, where the standard Tunka-133 analysis is limited by statistics. In contrast to the air-Cherenkov measurements, radio measurements are not limited to dark, clear nights and can provide an order of magnitude larger exposure.<br />Comment: Accepted for publication in Nuclear Instruments and Methods A, within Proceedings of the 13th Pisa Meeting on Advanced Detectors 2015
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