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Ultra-high-energy cosmic rays (UHECRs) are atomic nuclei from space withvastly higher energies than any other particles ever observed. Their origin andchemical composition remain a mystery. As we show here, the large- andintermediate-angular-scale anisotropies observed by the Pierre AugerObservatory are a powerful tool for understanding the origin of UHECRs. Withoutspecifying any particular production mechanism, but only postulating that thesource distribution follows the matter distribution of the local Universe, agood accounting of the magnitude, direction and energy dependence of the dipoleanisotropy at energies above $8 \times 10^{18}$ eV is obtained, after takinginto account the impact of energy losses during propagation (the "GZKhorizon"), diffusion in extragalactic magnetic field and deflections in theGalactic magnetic field (GMF). This is a major step toward the long-standinghope of using UHECR anisotropies to constrain UHECR composition and magneticfields. The observed dipole anisotropy is incompatible with a pure protoncomposition in this scenario. With a more accurate treatment of energy losses,it should be possible to further constrain the cosmic-ray composition andproperties of the extragalactic magnetic field, self-consistently improve theGMF model, and potentially expose individual UHECR sources.

The Imprint of Large Scale Structure on the Ultra-High-Energy Cosmic Ray Sky