A search for extremely-high-energy neutrinos with IceCube and implications for the ultra-high-energy cosmic-ray proton fraction

When ultra-high-energy cosmic rays (UHECRs) interact with ambient photon backgrounds, a flux of extremely-high-energy (EHE), so-called cosmogenic, neutrinos is produced. The observation of these neutrinos with IceCube can probe the nature of UHECRs. We present a search for EHE neutrinos using $12.6\mathrm{y}\mathrm{e}\mathrm{a}\mathrm{r}\mathrm{s}$ of IceCube data. The non-observation of neutrinos with energies $\gtrsim 10\mathrm{P}\mathrm{e}\mathrm{V}$ constrains the all-flavor neutrino flux at $1\mathrm{E}\mathrm{e}\mathrm{V}$ to be below $E^2{\mathrm{\Phi }}_{{\nu }_e+{\nu }_{\mu }+{\nu }_{\tau }}\simeq {10}^{-8}\mathrm{G}\mathrm{e}\mathrm{V}{\mathrm{c}\mathrm{m}}^{-2}{\mathrm{s}}^{-1}{\mathrm{s}\mathrm{r}}^{-1}$, the most stringent limit to date. This constrains the proton fraction in UHECRs of energy above $30\mathrm{E}\mathrm{e}\mathrm{V}$ to be $\lesssim 70\mathrm{\%}$ if the evolution of the UHECR sources is similar to the star formation rate. Our analysis circumvents uncertainties associated with hadronic interaction models in studies of UHECR air showers, which also suggest a heavy composition at such energies.