Prospects for PBR detection of KM3-230213A-like events

TL;DR

This paper explores the potential of the PBR balloon experiment to detect high-energy neutrino events similar to KM3-230213A, especially those that could indicate physics beyond the Standard Model, by assessing its sensitivity and observational prospects.

Contribution

It evaluates PBR's capability to detect BSM physics signals related to KM3-230213A-like neutrino events, filling a gap in understanding the experiment's potential for new physics detection.

Findings

PBR can probe BSM physics models consistent with KM3-230213A observations.

Sensitivity analysis shows PBR's potential to detect signals not seen by IceCube/Auger.

Results suggest PBR could confirm or refute BSM explanations for high-energy neutrino events.

Abstract

POEMMA-Balloon with Radio (PBR) is a scaled-down version of the Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) design, optimized to be flown as a payload on one of NASA's sub-orbital super pressure balloons circling the Earth above the southern oceans for a mission duration of more than 20 days. One of the main science objectives of PBR is to follow up astrophysical event alerts in search of neutrinos with very high energy ($10^8 \lesssim E_\nu /{\rm GeV} \lesssim 10^{10}$). Of particular interest for anticipated PBR observations, the KM3NeT Collaboration has recently reported the detection of the neutrino KM3-230213A with $10^{7.8} \lesssim E_\nu/{\rm GeV} \lesssim 10^{9.0}$. Such an unprecedented event is in tension with upper limits on the cosmic neutrino flux from IceCube and the Pierre Auger Observatory: for a diffuse isotropic neutrino flux there is a $3.5\sigma$ tension between KM3NeT and IceCube measurements, and about $2.6\sigma$ if the neutrino flux originates in transient sources. Therefore, if KM3-230213A was not beginner's luck, it becomes compelling to consider beyond Standard Model (BSM) possibilities which could lead to a signal at KM3NeT-ARCA but not at IceCube/Auger. We calculate the PBR horizon-range sensitivity to probe BSM physics compatible with observation at KM3NeT-ARCA and non-observation at IceCube/Auger. As an illustration, we consider a particular class of BSM physics models which has been described in the literature as a possible explanation of KM3-230213A.