Present status and prospects of the Tunka Radio Extension. (arXiv:1812.03070v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kostunin_D/0/1/0/all/0/1">D. Kostunin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bezyazeekov_P/0/1/0/all/0/1">P. A. Bezyazeekov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Budnev_N/0/1/0/all/0/1">N. M. Budnev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chernykh_D/0/1/0/all/0/1">D. Chernykh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fedorov_O/0/1/0/all/0/1">O. Fedorov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gress_O/0/1/0/all/0/1">O. A. Gress</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haungs_A/0/1/0/all/0/1">A. Haungs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hiller_R/0/1/0/all/0/1">R. Hiller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huege_T/0/1/0/all/0/1">T. Huege</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kazarina_Y/0/1/0/all/0/1">Y. Kazarina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kleifges_M/0/1/0/all/0/1">M. Kleifges</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korosteleva_E/0/1/0/all/0/1">E. E. Korosteleva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuzmichev_L/0/1/0/all/0/1">L. A. Kuzmichev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lenok_V/0/1/0/all/0/1">V. Lenok</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lubsandorzhiev_N/0/1/0/all/0/1">N. Lubsandorzhiev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshalkina_T/0/1/0/all/0/1">T. Marshalkina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monkhoev_R/0/1/0/all/0/1">R. Monkhoev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Osipova_E/0/1/0/all/0/1">E. Osipova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pakhorukov_A/0/1/0/all/0/1">A. Pakhorukov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pankov_L/0/1/0/all/0/1">L. Pankov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prosin_V/0/1/0/all/0/1">V. V. Prosin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schroder_F/0/1/0/all/0/1">F. G. Schröder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shipilov_D/0/1/0/all/0/1">D. Shipilov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zagorodnikov_A/0/1/0/all/0/1">A. Zagorodnikov</a>
The Tunka Radio Extension (Tunka-Rex) is a digital radio array operating in
the frequency band of 30-80 MHz and detecting radio emission from air-showers
produced by cosmic rays with energies above 100 PeV. The experiment is
installed at the site of the TAIGA (Tunka Advanced Instrument for cosmic rays
and Gamma Astronomy) observatory and performs joint measurements with the
co-located particle and air-Cherenkov detectors in passive mode receiving a
trigger from the latter. Tunka-Rex collects data since 2012, and during the
last five years went through several upgrades. As a result the density of the
antenna field was increased by three times since its commission. In this
contribution we present the latest results of Tunka-Rex experiment,
particularly an updated analysis and efficiency study, which have been applied
to the measurement of the mean shower maximum as a function of energy for
cosmic rays of energies up to EeV. The future plans are also discussed:
investigations towards an energy spectrum of cosmic rays with Tunka-Rex and
their mass composition using a combination of Tunka-Rex data with muon
measurements by the particle detector Tunka-Grande.
The Tunka Radio Extension (Tunka-Rex) is a digital radio array operating in
the frequency band of 30-80 MHz and detecting radio emission from air-showers
produced by cosmic rays with energies above 100 PeV. The experiment is
installed at the site of the TAIGA (Tunka Advanced Instrument for cosmic rays
and Gamma Astronomy) observatory and performs joint measurements with the
co-located particle and air-Cherenkov detectors in passive mode receiving a
trigger from the latter. Tunka-Rex collects data since 2012, and during the
last five years went through several upgrades. As a result the density of the
antenna field was increased by three times since its commission. In this
contribution we present the latest results of Tunka-Rex experiment,
particularly an updated analysis and efficiency study, which have been applied
to the measurement of the mean shower maximum as a function of energy for
cosmic rays of energies up to EeV. The future plans are also discussed:
investigations towards an energy spectrum of cosmic rays with Tunka-Rex and
their mass composition using a combination of Tunka-Rex data with muon
measurements by the particle detector Tunka-Grande.
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