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The Pierre Auger Observatory (PAO) has measured the spectrum and compositionof the ultrahigh energy cosmic rays with unprecedented precision. We use thesemeasurements to constrain their spectrum and composition as injected from theirsources and, in turn, use these results to estimate the spectrum of cosmogenicneutrinos generated in their propagation through intergalactic space. We findthat the PAO measurements can be well fit if the injected cosmic rays consistentirely of nuclei with masses in the intermediate (C, N, O) to heavy (Fe, Si)range. A mixture of protons and heavier species is also acceptable but (on thebasis of existing hadronic interaction models) injection of pure light nuclei(p, He) results in unacceptable fits to the new elongation rate data. Theexpected spectrum of cosmogenic neutrinos can vary considerably, depending onthe precise spectrum and chemical composition injected from the cosmic raysources. In the models where heavy nuclei dominate the cosmic ray spectrum andfew dissociated protons exceed GZK energies, the cosmogenic neutrino flux canbe suppressed by up to two orders of magnitude relative to the all-protonprediction, making its detection beyond the reach of current and plannedneutrino telescopes. Other models consistent with the data, however, areproton-dominated with only a small (1-10%) admixture of heavy nuclei andpredict an associated cosmogenic flux within the reach of upcoming experiments.Thus a detection or non-detection of cosmogenic neutrinos can assist indiscriminating between these possibilities.

Predictions for the Cosmogenic Neutrino Flux in Light of New Data from the Pierre Auger Observatory