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arxiv: 2508.02869 · v3 · submitted 2025-08-04 · ✦ hep-ph · astro-ph.CO· astro-ph.HE

Attenuation of the ultra-high-energy neutrino flux by dark matter scatterings

Ivan Esteban , Alejandro Ibarra This is my paper

Pith reviewed 2026-05-19 00:06 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.COastro-ph.HE
keywords ultra-high-energy neutrinosdark matter scatteringneutrino attenuationMilky Way halointergalactic mediumneutrino-dark matter cross sectionKM3230213A
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The pith

Neutrino-dark matter scatterings can attenuate ultra-high-energy neutrinos and allow limits on their interaction strength even without knowing the sources.

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

The paper examines how ultra-high-energy neutrinos traveling from distant astrophysical sources can lose energy or change direction by scattering off dark matter particles both in the vast spaces between galaxies and inside our own Milky Way. This scattering process would reduce the overall number of neutrinos that reach Earth, modify their energy distribution, and create detectable differences in arrival directions depending on the observer's location relative to the galactic dark matter halo. A key insight is that even with limited knowledge of where the neutrinos originated, simple assumptions about dark matter distribution let observers set upper bounds on the scattering strength using data from a single high-energy event like KM3230213A. Detectors at different latitudes on Earth would see complementary patterns from the Milky Way's dark matter, providing a practical way to test these interactions.

Core claim

Scatterings of ultra-high-energy neutrinos with dark matter in the intergalactic medium and the Milky Way halo affect the total flux, energy spectrum, and arrival directions of these neutrinos. With mild astrophysical assumptions about dark matter densities, limits on the neutrino-dark matter scattering cross section can be derived even when the neutrino sources remain unknown, as demonstrated using the recent event KM3230213A. Detectors at different latitudes can probe the directional anisotropies induced by scattering in the Milky Way dark matter halo.

What carries the argument

The neutrino-dark matter scattering cross section, which sets the interaction rate that produces flux attenuation, spectral distortion, and directional anisotropies from the Milky Way halo.

If this is right

  • Detectors at different Earth latitudes can measure complementary anisotropies caused by neutrinos scattering with Milky Way dark matter.
  • Limits on the neutrino-dark matter cross section become possible without precise knowledge of neutrino source locations.
  • Both intergalactic and galactic scatterings contribute to changes in the observed energy spectrum and arrival directions.
  • The recent KM3230213A event can already be used to derive concrete bounds under standard dark matter density assumptions.

Where Pith is reading between the lines

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

  • Future multi-detector networks could map the dark matter halo shape through neutrino arrival directions if scattering is confirmed.
  • The same attenuation logic might apply to other cosmic messengers like high-energy gamma rays if they interact similarly with dark matter.
  • Stronger limits would follow from accumulating more ultra-high-energy neutrino events rather than relying on a single detection.

Load-bearing premise

Standard dark matter density profiles hold for the Milky Way halo and enough dark matter exists in the intergalactic medium to cause observable attenuation of the neutrino flux.

What would settle it

Detection of several ultra-high-energy neutrinos showing no reduction in flux, no spectral softening, and no latitude-dependent directional bias that would be expected from scattering with the modeled dark matter distributions.

Figures

Figures reproduced from arXiv: 2508.02869 by Alejandro Ibarra, Ivan Esteban.

Figure 1
Figure 1. Figure 1: Effective integrated DM column density of a high-redshift source, for different energy [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Integrated Milky Way DM column density at different directions, for an NFW (left) [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Neutrino-flux attenuation due to DM-neutrino scatterings in the Milky Way halo as [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Left panel: Current landscape of UHE astrophysical neutrino fluxes, together with the Waxman-Bahcall upper bound. All limits and measurements are at 90% CL. Right panel: χ 2 of each experiment as well as the joint χ 2 from KM3NeT, IceCube and the Pierre Auger Observatory. this is the renowned Waxman-Bahcall bound [26]. The actual flux is likely smaller, as the bound assumes strong redshift evolution and a … view at source ↗
Figure 5
Figure 5. Figure 5: Sky-averaged neutrino-flux, attenuated by the Milky Way DM, for an unattenuated [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Unatennuated flux for different energy-independent DM-neutrino interaction cross [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Limits on DM-ν scattering from the KM3-230213A event and from previous works. We assume that KM3-230213A has a diffuse origin, although the results are similar for a point source (under different assumptions, see text). We also show the extrapolation of the limits to other energies assuming simple energy dependence of the cross section. 9 [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Diffuse neutrino flux for different energy-dependent cross sections over DM mass: [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Day-averaged effective area of IceCube, the Pierre Auger Observatory and KM3NeT, [PITH_FULL_IMAGE:figures/full_fig_p012_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Effective sensitivity of IceCube and the Pierre Auger Observatory, relative to [PITH_FULL_IMAGE:figures/full_fig_p012_10.png] view at source ↗
read the original abstract

A flux of ultra-high-energy (UHE) neutrinos, produced by astrophysical sources at cosmological distances, is anticipated to exist and reach Earth. In this paper, we investigate the impact on the total flux, energy spectrum, and arrival directions of UHE neutrinos of neutrino-dark matter (DM) scatterings. We study scatterings both in the intergalactic medium and in the Milky Way. We emphasize the complementarity among neutrino detectors at different latitudes, that can probe anisotropies induced by neutrinos scattering with the Milky Way DM halo. We also discuss that, with mild astrophysical assumptions, limits on the DM-$\nu$ scattering cross section can be placed even if the neutrino sources are unknown. Finally, we explore all this phenomenology with the recent UHE neutrino event KM3230213A, and place the corresponding limits on the DM-$\nu$ scattering cross section.

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 paper investigates the attenuation of ultra-high-energy (UHE) neutrinos due to scattering with dark matter (DM) in both the intergalactic medium (IGM) and the Milky Way halo. It examines effects on the total flux, energy spectrum, and arrival directions, highlights complementarity between neutrino detectors at different latitudes for detecting halo-induced anisotropies, and claims that limits on the DM-ν scattering cross section can be placed using the recent event KM3230213A even when source locations are unknown, relying on mild astrophysical assumptions about DM density profiles.

Significance. If the calculations hold, the work offers a novel approach to constraining DM-neutrino interactions at ultra-high energies using observed events, independent of specific source identification. The discussion of detector complementarity and application to real data like KM3230213A strengthens its potential impact, though robustness depends on handling of cosmological integrals.

major comments (2)
  1. [§4] §4 (limits from unknown sources): The optical depth τ = σ ∫ n_DM dl for IGM scattering is computed under a fixed or average source redshift assumption to derive the upper bound on the cross section from KM3230213A. This choice is load-bearing for the central claim that 'mild astrophysical assumptions' suffice without knowing sources; the bound is sensitive to the redshift distribution (e.g., star-formation-rate weighted vs. uniform), and the paper should show explicit marginalization or sensitivity tests to confirm robustness.
  2. [§3.2] §3.2 (IGM modeling): The mean DM density is fixed by Ω_DM, but the proper distance and clumping factor in the line-of-sight integral still depend on unknown z; without a concrete prior or demonstration that the limit is stable across plausible distributions, the 'parameter-free' or assumption-light character of the bound is not fully established.
minor comments (2)
  1. [Figure 3] Figure 3 (anisotropy maps): The color scale and latitude dependence could be clarified with explicit labels for detector positions to better illustrate the complementarity claim.
  2. [Eq. (12)] Eq. (12) (cross-section parametrization): The energy dependence is introduced without a reference to the underlying model; adding a brief justification or citation would improve clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading and constructive comments on our manuscript. The points raised regarding the sensitivity of the IGM optical depth to source redshift assumptions are well taken, and we address them directly below with plans to strengthen the presentation.

read point-by-point responses

  1. Referee: [§4] §4 (limits from unknown sources): The optical depth τ = σ ∫ n_DM dl for IGM scattering is computed under a fixed or average source redshift assumption to derive the upper bound on the cross section from KM3230213A. This choice is load-bearing for the central claim that 'mild astrophysical assumptions' suffice without knowing sources; the bound is sensitive to the redshift distribution (e.g., star-formation-rate weighted vs. uniform), and the paper should show explicit marginalization or sensitivity tests to confirm robustness.

    Authors: We agree that the optical depth and resulting cross-section limit depend on the source redshift distribution. Our manuscript employed a representative average redshift to illustrate the bound under mild assumptions without requiring source identification. To address the referee's concern, we will add explicit sensitivity tests in the revised version, comparing the derived limits for a star-formation-rate weighted distribution against a uniform distribution in redshift. These tests will quantify the variation and support the robustness of the central claim. revision: yes

  2. Referee: [§3.2] §3.2 (IGM modeling): The mean DM density is fixed by Ω_DM, but the proper distance and clumping factor in the line-of-sight integral still depend on unknown z; without a concrete prior or demonstration that the limit is stable across plausible distributions, the 'parameter-free' or assumption-light character of the bound is not fully established.

    Authors: We acknowledge that, although the mean DM density is fixed by Ω_DM, the line-of-sight integral for proper distance introduces a dependence on source redshift z. In the revision we will include a dedicated discussion (or short appendix) demonstrating the stability of the upper limit by evaluating the optical depth across a range of plausible redshifts motivated by UHE neutrino observations. This will make the assumption-light character of the bound more explicit without requiring a full marginalization over an arbitrary prior. revision: yes

Circularity Check

0 steps flagged

No circularity: limits derived from observed event plus external DM density profiles

full rationale

The paper computes attenuation optical depth τ = σ ∫ n_DM dl using standard Milky Way halo profiles and mean IGM density fixed by Ω_DM, then applies the result to the single observed event KM3230213A to set upper bounds on the DM-ν cross section. These steps rely on external astrophysical inputs and the measured event rather than re-deriving any fitted parameter or self-referential quantity as a prediction. No self-definitional equations, fitted-input predictions, or load-bearing self-citations appear in the derivation chain; the central claim remains independent of its own outputs.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

Review performed on abstract only; full text unavailable. The analysis rests on standard assumptions about dark-matter distributions and source distances that are not independently verified here.

free parameters (1)
  • DM-neutrino scattering cross section
    The quantity being bounded by the analysis of attenuation effects.
axioms (2)
  • domain assumption Standard Navarro-Frenk-White or similar density profile for Milky Way DM halo
    Invoked to compute galactic scattering contribution (abstract).
  • domain assumption Neutrino sources lie at cosmological distances
    Required for intergalactic-medium scattering to be relevant.

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

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    IceCube diffuse neutrino data constrains neutrino loss from new physics via energy conservation, yielding bounds that vary with attenuation energy dependence and source redshift assumptions while potentially affecting...

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