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Constraining the Prompt Atmospheric Neutrino Flux Combining IceCube's Cascade and Track Samples
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Constraining the Prompt Atmospheric Neutrino Flux Combining IceCube's Cascade and Track Samples

R Abbasi, M Ackermann, J Adams, S. K Agarwalla, J. A Aguilar, M Ahlers, J. M Alameddine, S Ali, N. M Amin, K Andeen, …
ArXiv.org
Cornell University
12/19/2025
DOI: 10.48550/arxiv.2512.17760
url
https://doi.org/10.48550/arxiv.2512.17760View
Preprint (Author's original) This preprint has not been evaluated by subject experts through peer review. Preprints may undergo extensive changes and/or become peer-reviewed journal articles. Open Access

Abstract

The IceCube Neutrino Observatory has observed a diffuse flux of high-energy astrophysical neutrinos for more than a decade. A relevant background to the astrophysical flux is prompt atmospheric neutrinos, originating from the decay of charmed mesons produced in cosmic-ray-induced air showers. The production rate of charmed mesons in the very forward phase space of hadronic interactions, and consequently, the prompt neutrino flux, remains uncertain and has not yet been observed by neutrino detectors. An accurate measurement of this flux would enhance our understanding of fundamental particle physics such as hadronic interactions in high-energy cosmic-ray-induced air showers and the nucleon structure. Furthermore, an experimental characterization of this background flux will improve the precision of astrophysical neutrino flux spectral measurements. In this work, we perform a combined fit of cascade-like and track-like neutrino events in IceCube to constrain the prompt atmospheric neutrino flux. Given that the prompt flux is a sub-dominant contribution, treating systematic uncertainties arising from the potential mis-modeling of the conventional and astrophysical neutrino fluxes is critical for its measurement. Our analysis yields a non-zero best-fit result, which is, however, consistent with the null hypothesis of no prompt flux within one standard deviation. Consequently, we establish an upper bound on the flux at 4 × 10−16 (GeV m2 s sr)−1 at 10 TeV.
 Physics - High Energy Astrophysical Phenomena

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