We explore the interpretation that the diffuse astrophysical neutrino flux is dominated by a single standard candle-like source class. Since recent observations favor a broken power law with a spectral break around 30 TeV, we postulate that the $p\gamma$ channel is the dominant neutrino production process creating a peak at these energies. We use a sophia-based photo-pion interaction model with a thermal target including high-energy processes, such as multipion production, which turns out to be relevant for the interpretation. We demonstrate that target photon temperatures of about 80 to 300 eV are preferred in a multiparameter fit, whereas the maximal neutrino energies can be limited by ($a$) soft injection spectra, ($b$) a maximal proton energy in the PeV range, or ($c$) magnetic field effects on the secondary muons, pions, and kaons with $B$ in the few–10 kG range. We predict that future measurements, such as readings of the neutrino flavor composition or neutrino-antineutrino ratio (Glashow resonance), can discriminate between scenarios. We also point out that the parameters obtained in our generic approach, such as in the strong magnetic field values, might be indicative for an active galactic nucleus core origin as a driver of the diffuse flux.

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• Cosmic rays & astroparticles
• Extrasolar neutrino astronomy
• Neutrinos