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Related Experiment Video

Updated: Jun 30, 2026

Angle-resolved Photoemission Spectroscopy At Ultra-low Temperatures

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Published on: October 9, 2012

Features of the Energy Spectrum of Cosmic Rays above 2.5×10^{18} eV Using the Pierre Auger Observatory.

A Aab¹, P Abreu², M Aglietta^3,4

¹IMAPP, Radboud University Nijmegen, Nijmegen, The Netherlands.

Physical Review Letters

|October 5, 2020

Summary

Cosmic ray energy spectrum measurements reveal significant spectral index changes above 1.3×10^19 eV. These findings support models with energy-dependent mass composition for ultra-high-energy cosmic rays.

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Last Updated: Jun 30, 2026

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Published on: January 30, 2020

Area of Science:

Astrophysics
Particle Physics
Cosmic Ray Physics

Background:

The origin and spectrum of ultra-high-energy cosmic rays (UHECRs) are key questions in astrophysics.
Previous studies have indicated spectral features at high energies, but precise measurements are crucial.

Purpose of the Study:

To precisely measure the energy spectrum of cosmic rays above 2.5×10^18 eV.
To identify spectral index changes and their implications for cosmic ray composition and origin.

Main Methods:

Analysis of a large dataset of 215,030 cosmic ray events.
Detailed measurement of the cosmic ray energy spectrum and its spectral index.

Main Results:

Observed a change in the spectral index from 2.51±0.03(stat)±0.05(syst) to 3.05±0.05(stat)±0.10(syst) around 1.3×10^19 eV.
Further evolution of the spectral index to 5.1±0.3(stat)±0.1(syst) beyond 5×10^19 eV.
No significant dependence of spectral features on declination was found.

Conclusions:

The observed spectral features are consistent with models incorporating energy-dependent mass composition.
The energy density of cosmic rays above 5×10^18 eV was determined to be (5.66±0.03(stat)±1.40(syst))×10^53 erg Mpc⁻³.