Detection of Cosmic-Ray Ensembles with CREDO. (arXiv:1811.10248v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wozniak_K/0/1/0/all/0/1">Krzysztof W. Woźniak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Almeida_Cheminant_K/0/1/0/all/0/1">Kevin Almeida-Cheminant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bratek_L/0/1/0/all/0/1">Łukasz Bratek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castillo_D/0/1/0/all/0/1">David Edwin Alvarez Castillo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dhital_N/0/1/0/all/0/1">Niraj Dhital</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duffy_A/0/1/0/all/0/1">Alan R. Duffy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gora_D/0/1/0/all/0/1">Dariusz Góra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hnatyk_B/0/1/0/all/0/1">Bohdan Hnatyk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Homola_P/0/1/0/all/0/1">Piotr Homola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jagoda_P/0/1/0/all/0/1">Paweł Jagoda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jalocha_Bratek_J/0/1/0/all/0/1">Joanna Jałocha-Bratek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kasztelan_M/0/1/0/all/0/1">Marcin Kasztelan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lemanski_D/0/1/0/all/0/1">Dawid Lemański</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kovacs_P/0/1/0/all/0/1">Peter Kovács</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nazari_V/0/1/0/all/0/1">Vahab Nazari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niedzwiecki_M/0/1/0/all/0/1">Michał Niedźwiecki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smelcerz_K/0/1/0/all/0/1">Katarzyna Smelcerz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smolek_K/0/1/0/all/0/1">Karel Smolek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stasielak_J/0/1/0/all/0/1">Jarosław Stasielak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stuglik_S/0/1/0/all/0/1">Sławomir Stuglik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sushchov_O/0/1/0/all/0/1">Oleksandr Sushchov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zamora_Saa_J/0/1/0/all/0/1">Jilberto Zamora-Saá</a> (for the CREDO Collaboration)
One of the main objectives of cosmic-ray studies are precise measurements of
energy and chemical composition of particles with extreme energies. Large and
sophisticated detectors are used to find events seen as showers starting in the
Earth’s atmosphere with recorded energies larger than 100 EeV. However, a
Cosmic-Ray Ensemble (CRE) developing before reaching the Earth as a bunch of
correlated particles may spread over larger areas and requires an extended set
of detectors to be discovered. The Cosmic-Ray Extremely Distributed Observatory
(CREDO) is a solution to find such phenomena. Even simple detectors measuring
the particle arrival time only are useful in this approach, as they are
sufficient both to provide candidate CRE events and to determine the direction
from which they are arriving.
One of the main objectives of cosmic-ray studies are precise measurements of
energy and chemical composition of particles with extreme energies. Large and
sophisticated detectors are used to find events seen as showers starting in the
Earth’s atmosphere with recorded energies larger than 100 EeV. However, a
Cosmic-Ray Ensemble (CRE) developing before reaching the Earth as a bunch of
correlated particles may spread over larger areas and requires an extended set
of detectors to be discovered. The Cosmic-Ray Extremely Distributed Observatory
(CREDO) is a solution to find such phenomena. Even simple detectors measuring
the particle arrival time only are useful in this approach, as they are
sufficient both to provide candidate CRE events and to determine the direction
from which they are arriving.
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