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We study the production of cosmogenic neutrinos and photons during theextragalactic propagation of ultra-high-energy cosmic rays (UHECRs). For a widerange of models in cosmological evolution of source luminosity, composition andmaximum energy we calculate the expected flux of cosmogenic secondaries bynormalizing our cosmic ray output to experimental spectra and comparing thediffuse flux of GeV-TeV gamma-rays to the experimental one measured by theFermi satellite. Most of these models yield significant neutrino fluxes forcurrent experiments like IceCube or Pierre Auger. Furthermore, we discuss thepossibilities of signing the presence of UHE proton sources either within oroutside the cosmic ray horizon using neutrinos or photons observations even ifthe cosmic ray composition becomes heavier at the highest energies. We discussthe possible constraints that could be brought on the UHECR origin from thedifferent messengers and energy ranges.

Constraints on the origin of ultra-high-energy cosmic rays from cosmogenic neutrinos and photons