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The sources of ultra-high-energy cosmic rays are still unknown, but assumingstandard physics, they are expected to lie within a few hundred megaparsecsfrom us. Indeed, over cosmological distances cosmic rays lose energy tointeractions with background photons, at a rate depending on their mass numberand energy and properties of photonuclear interactions and photon backgrounds.The universe is not homogeneous at such scales, hence the distribution of thearrival directions of cosmic rays is expected to reflect the inhomogeneities inthe distribution of galaxies; the shorter the energy loss lengths, the strongerthe expected anisotropies. Galactic and intergalactic magnetic fields can blurand distort the picture, but the magnitudes of the largest-scale anisotropies,namely the dipole and quadrupole moments, are the most robust to their effects.Measuring them with no bias regardless of any higher-order multipoles is notpossible except with full-sky coverage. In this work, we achieve this in threeenergy ranges (approximately 8--16 EeV, 16--32 EeV, and 32--$\infty$ EeV) bycombining surface-detector data collected at the Pierre Auger Observatory until2020 and at the Telescope Array (TA) until 2019, before the completion of theupgrades of the arrays with new scintillator detectors. We find that thefull-sky coverage achieved by combining Auger and TA data reduces theuncertainties on the north-south components of the dipole and quadrupole inhalf compared to Auger-only results.

The UHECR dipole and quadrupole in the latest data from the original Auger and TA surface detectors