0603271 - FZÚ 2025 RIV IT eng C - Konferenční příspěvek (zahraniční konf.)
Abdul Halim, A. - Abreu, P. - Aglietta, M. - Bakalová, Alena - Blažek, Jiří - Boháčová, Martina - Chudoba, Jiří - Denner, Nikolas - Ebr, Jan - Hamal, Petr - Janeček, Petr - Jílek, Vlastimil - Juryšek, Jakub - Majerčáková, Margita - Mandát, Dušan - Müller, Ana Laura - Negi, Shefali - Palatka, Miroslav - Panja, Shayoni - Pech, Miroslav - Prouza, Michael - Řídký, Jan - dos Santos, Eva M. Martins - Schovánek, Petr - Stadelmaier, Maximilian Klaus - Svozilíková, Zuzana - Tobiška, Petr - Trávníček, Petr - Vícha, Jakub - Yushkov, Alexey … celkem 380 autorů
Highlights from the Pierre Auger Observatory.
Proceedings of Science. Vol. 444. Trieste: Sissa Medilab srl, 2024 - (Saito, T.), č. článku 016. ISSN 1824-8039.
[International Cosmic Ray Conference ICRC2023 /38./. Nagoya (JP), 26.07.2023-03.08.2023]
Grant CEP: GA MŠMT LTT18004; GA MŠMT LM2015038; GA MŠMT(CZ) LM2018102; GA MŠMT EF16_013/0001402; GA MŠMT(CZ) EF18_046/0016010; GA MŠMT LM2023032
Institucionální podpora: RVO:68378271
Klíčová slova: ultra-high-energy cosmic rays * AugerPrime detector
Obor OECD: Particles and field physics
Web výsledku:
https://pos.sissa.it/444/016/pdf
DOI: https://doi.org/10.22323/1.444.0016

The Pierre Auger Observatory is a unique facility designed to study ultra-high energy cosmic rays, with energies up to 1020 eV and beyond. The Observatory is located in Argentina and comprises more than 1600 water Cherenkov detectors spread over an area of 3000 square kilometers overlooked by Fluorescence detectors. The first phase of the Observatory's data-taking began in 2004 and continued until the end of 2021. In this contribution, the results from the Phase I data analysis of the Pierre Auger Observatory are presented. They include, among others, measurements of the cosmic-ray energy spectrum, composition, and arrival direction anisotropy. The Phase I results from the Pierre Auger Observatory provide major advances in the understanding of the ultra-high energy cosmic ray phenomena and lay the foundation for second-phase studies with the upgraded AugerPrime detector. The status of the AugerPrime upgrade and its performance will be also discussed.
Trvalý link: https://hdl.handle.net/11104/0360486