Probing the origins of ultrahigh-energy cosmic rays with the Pierre Auger Observatory

The methodology comprised two main analysis branches: 1. Large-Scale Analyses: The data were processed to calculate the dipole and quadrupole moments of the cosmic-ray flux. The tables display the number of events across different energy ranges (E), harmonic orders, Fourier coefficients, Rayleigh amplitudes and phases, and the Rayleigh probability (statistical significance) for each dataset. 2.

Correlations with Starburst Galaxies: Application of a test statistic (TS) maximisation for flux mapping and calculation of confidence level contours (1 σ and 2 σ). The data encompass the modelled flux separation, accounting for parameters such as anisotropic fraction, smearing angles, and attenuation factors. The figures provide visual representations of the outcomes of these methodological analyses (e.g., skymaps in galactic coordinates using a Hammer projection and test-statistic colour maps), while the tables provide the exact values and their respective uncertainties found during the statistical calculations.