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2025
article
A search for extremely-high-energy neutrinos with IceCube and implications for the ultra-high-energy cosmic-ray proton fraction
IceCube Collaboration, Rasha Abbasi, Markus Ackermann, Jenni Adams, Sanjib Kumar Agarwalla, Juanan Aguilar, Markus Ahlers, Jean-Marco Alameddine, Shoukat Ali, Najia Moureen Binte Amin, K. Andeen, Carlos Argüelles, Y. Ashida, Sofia Athanasiadou, Spencer Axani, Rishi Babu, Xinhua Bai, Joe Baines-Holmes, Aswathi Balagopal V., Simeon Bash, Vedant Basu, Ryan Bay, James Beatty, Philipp Behrens, Jakob Beise, Chiara Bellenghi, B. Benkel, Segev Y. BenZvi, David Berley, Elisa Bernardini, Dave Besson, E. Blaufuss, Lucas Bloom, Summer Blot, Ilya Bodo, Julia Book Motzkin, Caterina Boscolo Meneguolo, Olga Botner, Jakob Bottcher, Jim Braun, Bennett Brinson, Zoe Brisson-Tsavoussis, Ryan T. Burley, Delaney Butterfield, Michael Campana, Kiara Carloni, Jose Carpio, Sharmistha Chattopadhyay, Zheyang Chen, Dmitry Chirkin, Seowon Choi, Brian A. Clark, Alan Coleman, Peter John Cusack Coleman, Gabriel Collin, Diego Alberto Coloma Borja, A. Connolly, Janet M. Conrad, Rebecca Corley, D.F. Cowen, Catherine DE CLERCQ, James DeLaunay, Diyaselis Delgado, Thomas Delmeulle, Paolo Desiati, Krijn D. de Vries, Gwenhaël de Wasseige, Tyce DeYoung, Juan Carlos Diaz-Velez, Stephen DiKerby, Markus Dittmer, Alba Domi, Lincoln Draper, Lasse Dueser, Daniel Durnford, Kaustav Dutta, Michael A. DuVernois, Thomas Ehrhardt, Leonhard Eidenschink, Anna Eimer, Philipp Eller, Enrico Ellinger, Dominik Elsässer, Ralph Engel, Hannah Erpenbeck, Waleed Esmail, Steven Young Eulig, John Evans, P. Evenson, Kwok Lung Fan, Ke Fang, Kareem Ramadan Farrag, Ali R. Fazely
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Le résumé fourni par la source
When ultra-high-energy cosmic rays (UHECRs) interact with ambient photon backgrounds, a flux of extremely-high-energy (EHE), so-called cosmogenic, neutrinos is produced. The observation of these neutrinos with IceCube can probe the nature of UHECRs. We present a search for EHE neutrinos using 12.6 years of IceCube data. The non-observation of neutrinos with energies ≳10PeV constrains the all-flavor neutrino flux at 1EeV to be below E$^2$Φ$_{νe+νμ+ντ}$ ≃ 10$^{−8}$ GeVcm$^{−2}$ sr$^{−1}$ s$^{−1}$, the most stringent limit to date. This constrains the proton fraction in UHECRs of energy above 30EeV to be ≲70% if the evolution of the UHECR sources is similar to the star formation rate. Our analysis circumvents uncertainties associated with hadronic interaction models in studies of UHECR air showers, which also suggest a heavy composition at such energies.
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Les sujets associés
Astrophysics and Cosmic PhenomenaEarth Systems and Cosmic EvolutionInsects and Parasite Interactions