Ultraheavy nuclei have longer energy loss lengths at ≲300 EeV than lighter nuclei, allowing them to explain UHECRs above 100 EeV from sources like collapsars and neutron star mergers while predicting distinct shower maxima.
The Pierre Auger Cosmic Ray Observatory
11 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The Pierre Auger Observatory, located on a vast, high plain in western Argentina, is the world's largest cosmic ray observatory. The objectives of the Observatory are to probe the origin and characteristics of cosmic rays above $10^{17}$ eV and to study the interactions of these, the most energetic particles observed in nature. The Auger design features an array of 1660 water-Cherenkov particle detector stations spread over 3000 km$^2$ overlooked by 24 air fluorescence telescopes. In addition, three high elevation fluorescence telescopes overlook a 23.5 km$^2$, 61-detector infilled array with 750 m spacing. The Observatory has been in successful operation since completion in 2008 and has recorded data from an exposure exceeding 40,000 km$^2$ sr yr. This paper describes the design and performance of the detectors, related subsystems and infrastructure that make up the Auger Observatory.
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A reconstruction algorithm using the radio emission maximum X_radio_max distinguishes deeply developing neutrino-induced air showers from cosmic rays, enhancing sensitivity above 1 EeV for inclined events.
Calculations indicate AMEGO-X could detect PBH transits within 0.1 AU while HAWC and LHAASO could observe explosions out to 0.1-0.5 pc, with future events at ~1000 AU potentially producing measurable electromagnetic signals unlike the 2023 KM3NeT neutrino candidate.
Updated Xmax measurements reveal a transition to heavier cosmic-ray mass composition above 10^18.4 eV with decreasing elemental diversity.
Transformers trained on cosmic ray simulations learn physically plausible features in positional encodings for symmetric air showers and in attention mechanisms for galaxy-origin particles.
SKA-Low is projected to reconstruct cosmic-ray air-shower depth of maximum with better than 8 g/cm² resolution and enable full reconstruction down to PeV energies via radio detection.
BL Lacs remain consistent with UHECR observations while FSRQs are disfavoured by anisotropy and source density mismatches after propagation modeling.
Minimal UHECR flux models from the Telescope Array predict cosmogenic neutrino fluxes consistent with the KM3-230213A event at the 2σ level.
With 2013-2023 exposure, the as-built ARA achieves world-leading UHE neutrino sensitivity above ~10^19 eV and predicts up to 13 trigger-level events under optimistic flux models, with secondaries contributing up to 30% of acceptance.
Information Field Theory is presented as a framework for full-information reconstruction and near-field interferometry of air-shower radio emission.
Alternative ISRF models produce only modest changes to the LHAASO diffuse gamma-ray fit; the associated pp neutrinos remain consistent with IceCube all-sky data and compatible with ANTARES/KM3NeT limits.
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Electromagnetic Signatures From Primordial Black Holes in the Solar System
Calculations indicate AMEGO-X could detect PBH transits within 0.1 AU while HAWC and LHAASO could observe explosions out to 0.1-0.5 pc, with future events at ~1000 AU potentially producing measurable electromagnetic signals unlike the 2023 KM3NeT neutrino candidate.