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arxiv: 2512.20594 · v2 · submitted 2025-12-23 · 🌌 astro-ph.HE

Recognition: 2 theorem links

· Lean Theorem

The Sensitivity of PUEO to Cosmogenic Neutrinos and Exotic Physics Scenarios

Angelina Sherman , Ke Fang , Dan Hooper
Authors on Pith no claims yet

Pith reviewed 2026-05-16 20:04 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords PUEOultrahigh-energy neutrinoscosmogenic neutrinosultraheavy dark mattercosmic stringsultrahigh-energy cosmic raysproton fraction
0
0 comments X

The pith

PUEO will set the strongest neutrino-detector limits above 10^19 eV on ultraheavy dark matter decays and some cosmic string models.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

PUEO is a planned long-duration balloon experiment that will detect ultrahigh-energy neutrinos in the 1-1000 EeV range. The paper calculates how well PUEO can observe cosmogenic neutrinos produced when ultrahigh-energy cosmic rays interact with background photons, which in turn limits the proton fraction in the cosmic-ray population. It also computes the reach for neutrinos from ultraheavy dark matter particle decays and from cosmic strings. A reader would care because these measurements test the origin of the highest-energy cosmic rays and probe exotic physics that gamma-ray data alone cannot fully address. If the calculated sensitivities hold, PUEO would tighten bounds in energy ranges where existing detectors have limited exposure.

Core claim

PUEO will be able to constrain the proton composition of ultrahigh-energy cosmic rays in scenarios that feature very strong source evolution and in which protons are accelerated to extremely high energies. Although gamma-ray observations are generally more sensitive to decaying particles than neutrino observations, PUEO is expected to set the strongest neutrino-detector constraints above 10^19 eV on decaying ultraheavy dark matter and will provide the strongest constraints on some models of cosmic strings.

What carries the argument

PUEO's projected neutrino flux sensitivity in the EeV range, obtained from its balloon-borne detector geometry and exposure calculations for cosmogenic and exotic neutrino signals.

If this is right

  • PUEO will limit the allowed proton fraction in ultrahigh-energy cosmic rays if sources evolve strongly and protons reach extreme energies.
  • PUEO will deliver the leading neutrino-based upper limits on ultraheavy dark matter decay above 10^19 eV.
  • PUEO will tighten constraints on certain cosmic string models beyond current limits from other experiments.
  • Neutrino limits from PUEO will add independent information to gamma-ray bounds on dark matter decay scenarios.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • A null result from PUEO on cosmogenic neutrinos would point toward either low proton fractions or milder source evolution than the baseline assumptions.
  • The projected reach could guide target selection and exposure goals for future ground-based ultrahigh-energy neutrino arrays.
  • Neutrino constraints on cosmic strings may complement gravitational-wave searches for string-related signals.

Load-bearing premise

The projected constraints on the proton fraction assume very strong source evolution and protons accelerated to extremely high energies.

What would settle it

A measurement of ultrahigh-energy cosmic-ray composition dominated by heavy nuclei or evidence for weak source evolution would substantially weaken the expected sensitivity to the proton fraction.

Figures

Figures reproduced from arXiv: 2512.20594 by Angelina Sherman, Dan Hooper, Ke Fang.

Figure 1
Figure 1. Figure 1: FIG. 1. The spectra of UHECR protons (brown) and their [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. The spectrum of ultrahigh-energy neutrinos from the [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. The spectra of ultrahigh-energy neutrinos from [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. The regions of the UHECR parameter space [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. The projected limit from PUEO (assuming no events [PITH_FULL_IMAGE:figures/full_fig_p005_5.png] view at source ↗
read the original abstract

Several observatories designed to detect ultrahigh-energy neutrinos are planned for the next decade. The most imminent of these is the Payload for Ultrahigh Energy Observations (PUEO), a long-duration balloon-based experiment that will provide unprecedented sensitivity to neutrinos with energies in the range of ~ 1 - 1000 EeV. In this work, we assess the scientific reach of PUEO. In particular, we evaluate the sensitivity of this observatory to cosmogenic neutrinos and, in turn, to the proton fraction of the ultrahigh-energy cosmic-ray spectrum. We also consider the potential of PUEO to probe scenarios in which neutrinos are produced through the decays of ultraheavy dark matter particles or are radiated from cosmic strings. We find that PUEO will be able to constrain the proton composition of ultrahigh-energy cosmic rays in scenarios that feature very strong source evolution and in which protons are accelerated to extremely high energies. Although gamma-ray observations are generally more sensitive to decaying particles than neutrino observations, PUEO is expected to set the strongest neutrino-detector constraints above 10^19 eV. PUEO will also provide the strongest constraints on some models of cosmic strings.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript evaluates the projected sensitivity of the PUEO long-duration balloon experiment to ultrahigh-energy neutrinos (1–1000 EeV). It focuses on cosmogenic neutrinos from ultrahigh-energy cosmic rays, deriving constraints on the UHECR proton fraction under assumptions of very strong source evolution and extreme maximum proton energies. It further assesses reach for neutrinos from ultraheavy dark matter decays and cosmic string radiation, concluding that PUEO will set the strongest neutrino-detector limits above 10^19 eV on certain decaying DM models and on some cosmic string scenarios.

Significance. If the sensitivity calculations are robust, the work supplies timely forecasts for an imminent experiment in a rapidly developing field. Explicitly conditioning the proton-fraction reach on strong evolution (m ≳ 5) and E_max ≳ 10^20 eV is a strength, as is the direct comparison of neutrino versus gamma-ray constraints for ultraheavy DM. The absence of a parameter scan, however, limits the immediate utility of the cosmogenic-neutrino results.

major comments (2)
  1. [§4 (cosmogenic neutrino fluxes and proton fraction)] The central claim that PUEO constrains the UHECR proton fraction (abstract and §4) is shown only for the optimistic corner of parameter space (strong source evolution m > 5 and E_max ≳ 10^20 eV). No systematic variation with milder evolution indices or lower cutoff energies is presented, so the rate at which the projected sensitivity disappears cannot be quantified from the manuscript.
  2. [§5 (decaying ultraheavy DM)] The statement that PUEO provides the strongest neutrino-detector constraints on ultraheavy DM above 10^19 eV (abstract and §5) requires explicit overlay of PUEO’s projected limit with the projected sensitivities of IceCube-Gen2, GRAND, and other planned neutrino arrays in the same energy decade; the current comparison appears limited to existing instruments.
minor comments (2)
  1. [Figures 3–5] Figure captions for the sensitivity curves should state the exact source-evolution index m and E_max values adopted for each line; this information is only implicit in the text.
  2. [§1] The introduction would benefit from a brief quantitative comparison of PUEO’s effective area and livetime to those of ANITA and other balloon or ground-based UHE neutrino experiments.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading of our manuscript and the constructive comments. We address each major point below and will revise the paper to incorporate the suggested improvements.

read point-by-point responses

  1. Referee: [§4 (cosmogenic neutrino fluxes and proton fraction)] The central claim that PUEO constrains the UHECR proton fraction (abstract and §4) is shown only for the optimistic corner of parameter space (strong source evolution m > 5 and E_max ≳ 10^20 eV). No systematic variation with milder evolution indices or lower cutoff energies is presented, so the rate at which the projected sensitivity disappears cannot be quantified from the manuscript.

    Authors: We agree that the proton-fraction constraints are presented primarily for the regime of strong source evolution (m ≳ 5) and high E_max (≳ 10^20 eV). This focus reflects the fact that only in this corner of parameter space does PUEO achieve meaningful sensitivity to cosmogenic neutrinos; milder evolution produces substantially lower fluxes that fall below the projected PUEO threshold. To make the dependence explicit, we will add a supplementary figure (or expanded discussion in §4) that scans over a range of evolution indices m and cutoff energies, showing how the proton-fraction reach weakens and ultimately disappears for lower values. This will allow readers to quantify the rate at which sensitivity is lost. revision: yes

  2. Referee: [§5 (decaying ultraheavy DM)] The statement that PUEO provides the strongest neutrino-detector constraints on ultraheavy DM above 10^19 eV (abstract and §5) requires explicit overlay of PUEO’s projected limit with the projected sensitivities of IceCube-Gen2, GRAND, and other planned neutrino arrays in the same energy decade; the current comparison appears limited to existing instruments.

    Authors: We accept this suggestion. While the current text compares PUEO to existing detectors, we will revise §5 (and the associated figure) to include projected sensitivity curves for IceCube-Gen2, GRAND, and other planned neutrino arrays. These overlays will explicitly confirm that PUEO sets the strongest neutrino-detector limits above 10^19 eV for the ultraheavy DM decay models under consideration. revision: yes

Circularity Check

0 steps flagged

No significant circularity; sensitivity from external propagation models

full rationale

The paper derives PUEO sensitivity curves for cosmogenic neutrinos using standard UHECR propagation codes and neutrino production calculations that take source evolution index and E_max as explicit external inputs. These are not fitted to PUEO data nor redefined in terms of the target observables. No self-definitional steps, fitted-input predictions, or load-bearing self-citations appear in the central chain; the optimistic (m ≳ 5, E_max ≳ 10^20 eV) cases are presented as parameter choices rather than derived results. The derivation remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Only abstract available, so ledger is inferred from typical assumptions in the field; no explicit free parameters or invented entities stated.

free parameters (1)
  • source evolution strength
    Assumed very strong to achieve proton fraction constraints
axioms (1)
  • domain assumption Standard ultrahigh-energy cosmic ray propagation and interaction models
    Required for cosmogenic neutrino flux calculations

pith-pipeline@v0.9.0 · 5511 in / 1230 out tokens · 31093 ms · 2026-05-16T20:04:39.824102+00:00 · methodology

discussion (0)

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Reference graph

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