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arxiv: 1907.08690 · v1 · pith:M2DZGZX4new · submitted 2019-07-19 · 🌌 astro-ph.HE · hep-ex· hep-ph· hep-th

Fundamental physics with high-energy cosmic neutrinos today and in the future

Carlos A. Arg\"uelles (MIT) , Mauricio Bustamante (Bohr Inst. & DARK Cosmology Ctr.) , Ali Kheirandish (Wisconsin U. , Madison) , Sergio Palomares-Ruiz (Valencia U. , Ific) , Jordi Salvado (Barcelona U. , ECM & ICC
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Barcelona U.) Aaron C. Vincent (Queen's U. Kingston & Perimeter Inst. Theor. Phys.)
This is my paper

Pith reviewed 2026-05-24 18:48 UTC · model grok-4.3

classification 🌌 astro-ph.HE hep-exhep-phhep-th
keywords high-energy neutrinosIceCubebeyond the Standard Modelastrophysical neutrinosneutrino propagationfundamental physicscosmic neutrinosnew physics tests
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The pith

High-energy cosmic neutrinos detected by IceCube test fundamental particle physics at scales unreachable by accelerators.

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

The paper claims that neutrinos arriving at Earth with energies from TeV to PeV after traveling distances up to a few gigaparsecs can expose tiny departures from standard physics because both the energy and baseline are far larger than anything achievable in laboratories. It reviews how pre-IceCube theoretical proposals for such tests have now been carried out on real data, yielding some of the tightest existing limits on physics beyond the Standard Model even after astrophysical uncertainties are taken into account. Concrete applications include searches for violations of Lorentz invariance, neutrino decay, and non-standard interactions through the measured energy spectrum, flavor ratios, and arrival directions. Future instruments sensitive to tens of EeV will push these tests to still higher energies.

Core claim

The astrophysical neutrinos discovered by IceCube, carrying the highest detected energies from TeV to PeV and traveling the longest distances up to a few Gpc, function as probes of fundamental particle-physics properties at energy scales unreachable by any other means, allowing current data to realize earlier proposals for beyond-Standard-Model tests in neutrino propagation and interactions.

What carries the argument

High-energy astrophysical neutrino fluxes observed over cosmological baselines, used to extract beyond-Standard-Model effects by comparing measured spectrum, flavor composition, and timing against standard expectations after marginalizing astrophysical variables.

If this is right

  • Current IceCube observations already deliver some of the most stringent constraints on certain beyond-Standard-Model scenarios involving neutrinos.
  • Measurements of flavor ratios at high energies can distinguish among competing new-physics models such as decay or non-standard interactions.
  • Limits on Lorentz invariance violation derived from these neutrinos exceed those from other experiments because of the extreme energies and distances involved.
  • Detectors reaching tens of EeV will extend the same tests to still higher energy scales and longer baselines.

Where Pith is reading between the lines

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

  • Combining neutrino data with gamma-ray or cosmic-ray observations from the same sources could reduce astrophysical uncertainties and sharpen the particle-physics constraints.
  • If a specific beyond-Standard-Model effect predicts a characteristic energy-dependent flavor transition, dedicated IceCube analyses targeting that transition could provide a direct test independent of overall flux normalization.
  • The same long-baseline, high-energy regime could be used to bound hypothetical new particles that couple only weakly to neutrinos, an avenue left implicit in the review.

Load-bearing premise

Astrophysical uncertainties about neutrino sources and propagation can be controlled or marginalized so that particle-physics signals remain extractable from the data.

What would settle it

A global fit to IceCube data showing that every observed deviation from standard neutrino expectations is fully accounted for by plausible variations in source properties or propagation, with no residual that improves when new-physics parameters are added, would indicate that the signals cannot yet be isolated.

Figures

Figures reproduced from arXiv: 1907.08690 by Aaron C. Vincent (Queen's U., Ali Kheirandish (Wisconsin U., Barcelona U.), Carlos A. Arg\"uelles (MIT), ECM & ICC, Ific), Jordi Salvado (Barcelona U., Kingston & Perimeter Inst. Theor. Phys.), Madison), Mauricio Bustamante (Bohr Inst. & DARK Cosmology Ctr.), Sergio Palomares-Ruiz (Valencia U..

Figure 1
Figure 1. Figure 1: Energy and distance scales of neutrinos from different sources. For comparison, GZK (Greisen￾Zatsepin-Kuzmin) refers to the maximum distance and energy that ultra-high-energy cosmic rays can reach. Figure adapted from Ref. [4]. However, new-physics effects could change this. The absence of standard interactions during propagation removes one layer of uncertainty when looking for new physics. • They have a … view at source ↗
Figure 2
Figure 2. Figure 2: Flavor composition of high-energy cosmic neutrinos at Earth. Left: Regions expected from different energy scales of Lorentz-invariance violation, starting from different flavor compositions at the sources [20]. Right: Regions expected from neutrino decay, for any composition at the sources, with D the fraction of non-decaying neutrinos that survive until reaching Earth [21]. In the sources, protons with en… view at source ↗
Figure 3
Figure 3. Figure 3: Measurements and predictions of the high￾energy neutrino-nucleon cross section using IceCube data [22, 23]; see also Ref. [24]. Updated versions of the color glass condensate model [25] still show sig￾nificant differences. Figure extracted from Ref. [4] [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Classification of models of new neutrino physics, according to at what stage they act — produc￾tion, propagation, detection — and what observables they affect — energy spectrum, arrival directions, flavor composition, arrival times — shown as lines connected to the models. The list of models is representative. Given the wide spread of models of new neutrino physics, it is useful to organize them [PITH_FUL… view at source ↗
read the original abstract

The astrophysical neutrinos discovered by IceCube have the highest detected neutrino energies --- from TeV to PeV --- and likely travel the longest distances --- up to a few Gpc, the size of the observable Universe. These features make them naturally attractive probes of fundamental particle-physics properties, possibly tiny in size, at energy scales unreachable by any other means. The decades before the IceCube discovery saw many proposals of particle-physics studies in this direction. Today, those proposals have become a reality, in spite of astrophysical unknowns. We will showcase examples of doing fundamental neutrino physics at these scales, including some of the most stringent tests of physics beyond the Standard Model. In the future, larger neutrino energies --- up to tens of EeV --- could be observed with larger detectors and further our reach.

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

0 major / 2 minor

Summary. The manuscript is a review paper arguing that IceCube-detected astrophysical neutrinos (TeV–PeV energies, Gpc-scale baselines) enable unique tests of fundamental physics beyond the Standard Model, including neutrino decay, secret interactions, and Lorentz violation. It states that many pre-IceCube theoretical proposals have now been realized with real data despite astrophysical unknowns, and outlines prospects for EeV neutrinos with future detectors.

Significance. If the central framing holds, the review is a useful synthesis that correctly credits the transition from proposals to actual constraints using existing IceCube data. It provides a clear overview of the field without introducing new derivations, which is appropriate for its scope.

minor comments (2)
  1. [Abstract] The abstract and introduction would benefit from a brief explicit statement of the energy and distance ranges used for each BSM test discussed later in the text.
  2. A small number of figure captions could more clearly distinguish between current IceCube limits and projected future sensitivities.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of the manuscript, recognition of its synthesis of the field, and recommendation to accept. The report accurately captures the central framing that pre-IceCube proposals have been realized with existing data.

Circularity Check

0 steps flagged

Review paper presents no original derivations or predictions

full rationale

This is a review article that summarizes prior proposals and existing IceCube results on using astrophysical neutrinos for BSM tests. No new equations, fits, or predictions are derived within the paper itself; all content references external work. The abstract and structure explicitly frame the text as showcasing examples from the literature rather than advancing a self-contained derivation chain. Consequently there are no load-bearing steps that reduce to self-definition, fitted inputs, or self-citation chains.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Review paper with no new derivations, free parameters, or invented entities introduced by the authors.

pith-pipeline@v0.9.0 · 5742 in / 963 out tokens · 14369 ms · 2026-05-24T18:48:49.898475+00:00 · methodology

discussion (0)

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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.

  1. Astrophysical bounds on the high-energy evolution of neutrino mixing

    hep-ph 2026-04 unverdicted novelty 5.0

    High-energy astrophysical neutrinos can constrain the running of neutrino mixing parameters with energy, with future multi-detector setups forecast to set strong bounds despite astrophysical uncertainties.

Reference graph

Works this paper leans on

44 extracted references · 44 canonical work pages · cited by 1 Pith paper · 36 internal anchors

  1. [1]

    T. K. Gaisser, F. Halzen and T. Stanev, Phys. Rept. 258 (1995) 173 [hep-ph/9410384]

    work page internal anchor Pith review Pith/arXiv arXiv 1995

  2. [2]

    I CECUBE collaboration, Science 342 (2013) 1242856 [1311.5238]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  3. [3]

    Probing Particle Physics with IceCube

    M. Ahlers, K. Helbing and C. Pérez de los Heros, Eur . Phys. J. C78 (2018) 924 [1806.05696]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  4. [4]

    Fundamental Physics with High-Energy Cosmic Neutrinos

    M. Ackermann et al., Bull. Am. Astron. Soc. 51 (2019) 215 [1903.04333]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  5. [5]

    N UTEV collaboration, Phys. Rev. D 74 (2006) 012008 [hep-ex/0509010]

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  6. [6]

    O. Mena, S. Palomares-Ruiz and A. C. Vincent, Phys. Rev. Lett. 113 (2014) 091103 [1404.0017]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  7. [7]

    Spectral analysis of the high-energy IceCube neutrinos

    S. Palomares-Ruiz, A. C. Vincent and O. Mena, Phys. Rev. D 91 (2015) 103008 [1502.02649]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  8. [8]

    S. W. Li, M. Bustamante and J. F. Beacom, Phys. Rev. Lett. 122 (2019) 151101 [1606.06290]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  9. [9]

    G. B. Gelmini, S. Nussinov and M. Roncadelli, Nucl. Phys. B 209 (1982) 157. 6 High-Energy Fundamental Neutrino Physics Mauricio Bustamante

    work page 1982

  10. [10]

    Neutrino Decays over Cosmological Distances and the Implications for Neutrino Telescopes

    P. Baerwald, M. Bustamante and W. Winter, JCAP 1210 (2012) 020 [1208.4600]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  11. [11]

    Lorentz-Violating Extension of the Standard Model

    D. Colladay and V . A. Kostelecky, Phys. Rev. D 58 (1998) 116002 [hep-ph/9809521]

    work page internal anchor Pith review Pith/arXiv arXiv 1998

  12. [12]

    V . A. Kostelecky and M. Mewes, Phys. Rev. D 69 (2004) 016005 [hep-ph/0309025]

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  13. [13]

    Neutrino Interferometry for High-Precision Tests of Lorentz Symmetry with IceCube

    I CECUBE collaboration, Nature Phys. 14 (2018) 961 [1709.03434]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  14. [14]

    I CECUBE collaboration, Phys. Rev. Lett. 113 (2014) 101101 [1405.5303]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  15. [15]

    L. A. Anchordoqui et al., JHEAp 1-2 (2014) 1 [1312.6587]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  16. [16]

    Cosmic-Ray and Neutrino Emission from Gamma-Ray Bursts with a Nuclear Cascade

    D. Biehl, D. Boncioli, A. Fedynitch and W. Winter, Astron. Astrophys. 611 (2018) A101 [1705.08909]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  17. [17]

    I CECUBE collaboration, Eur . Phys. J.C79 (2019) 234 [1811.07979]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  18. [18]

    I CECUBE , FERMI -LAT, MAGIC, AGILE, ASAS-SN, HAWC, H.E.S.S., INTEGRAL, K ANATA, K ISO , KAPTEYN , LIVERPOOL TELESCOPE , SUBARU , SWIFT NUSTAR, VERITAS, VLA/17B-403 collaboration, Science 361 (2018) eaat1378 [1807.08816]

    work page arXiv 2018

  19. [19]

    I CECUBE collaboration, Science 361 (2018) 147 [1807.08794]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  20. [20]

    C. A. Argüelles, T. Katori and J. Salvadó, Phys. Rev. Lett. 115 (2015) 161303 [1506.02043]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  21. [21]

    Testing decay of astrophysical neutrinos with incomplete information

    M. Bustamante, J. F. Beacom and K. Murase, Phys. Rev. D 95 (2017) 063013 [1610.02096]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  22. [22]

    Extracting the Energy-Dependent Neutrino-Nucleon Cross Section Above 10 TeV Using IceCube Showers

    M. Bustamante and A. Connolly, Phys. Rev. Lett. 122 (2019) 041101 [1711.11043]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  23. [23]

    I CECUBE collaboration, Nature 551 (2017) 596 [1711.08119]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  24. [24]

    I CECUBE collaboration, Phys. Rev. D 99 (2019) 032004 [1808.07629]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  25. [25]

    C. A. Argüelles, F. Halzen, L. Wille, M. Kroll and M. H. Reno, Phys. Rev. D 92 (2015) 074040 [1504.06639]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  26. [26]

    C. A. Argüelles, A. Kheirandish and A. C. Vincent, Phys. Rev. Lett. 119 (2017) 201801 [1703.00451]

    work page arXiv 2017

  27. [27]

    K. C. Y . Ng and J. F. Beacom, Phys. Rev. D 90 (2014) 065035 [1404.2288]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  28. [28]

    U. K. Dey, D. Kar, M. Mitra, M. Spannowsky and A. C. Vincent, Phys. Rev. D 98 (2018) 035014 [1709.02009]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  29. [29]

    J. F. Cherry, A. Friedland and I. M. Shoemaker, 1411.1071

    work page internal anchor Pith review Pith/arXiv arXiv

  30. [30]

    Theoretically palatable flavor combinations of astrophysical neutrinos

    M. Bustamante, J. F. Beacom and W. Winter, Phys. Rev. Lett. 115 (2015) 161302 [1506.02645]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  31. [31]

    Unitarity Bounds of Astrophysical Neutrinos

    M. Ahlers, M. Bustamante and S. Mu, Phys. Rev. D 98 (2018) 123023 [1810.00893]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  32. [32]

    Flavor of cosmic neutrinos preserved by ultralight dark matter

    Y . Farzan and S. Palomares-Ruiz, Phys. Rev. D 99 (2019) 051702 [1810.00892]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  33. [33]

    Murase and I

    K. Murase and I. M. Shoemaker, 1903.08607

    work page arXiv 1903

  34. [34]

    I CECUBE collaboration, 1412.5106

    work page internal anchor Pith review Pith/arXiv arXiv

  35. [35]

    KM3N ET collaboration, J. Phys. G 43 (2016) 084001 [1601.07459]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  36. [36]

    B AIKAL collaboration, J. Phys. Conf. Ser .1263 (2019) 012005

    work page 2019

  37. [37]

    A. V . Olinto et al., PoS ICRC2017 (2018) 542 [1708.07599]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  38. [38]

    The Giant Radio Array for Neutrino Detection (GRAND): Science and Design

    GRAND collaboration, Sci. China-Phys. Mech. Astron. 63 (2020) 219501 [1810.09994]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  39. [39]

    Nelles, Presented at the XVIII International Workshop on Neutrino Telescopes, March 18–22, 2019, https://indico.cern.ch/event/768000/

    A. Nelles, Presented at the XVIII International Workshop on Neutrino Telescopes, March 18–22, 2019, https://indico.cern.ch/event/768000/

    work page 2019

  40. [40]

    I CECUBE collaboration, JINST 9 (2014) P03009 [1311.4767]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  41. [41]

    I CECUBE collaboration, Phys. Rev. Lett. 114 (2015) 171102 [1502.03376]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  42. [42]

    I CECUBE collaboration, Astrophys. J. 809 (2015) 98 [1507.03991]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  43. [43]

    Halzen and A

    F. Halzen and A. Kheirandish, Front. Astron. Space Sci. 6 (2019) 32

    work page 2019

  44. [44]

    Mészáros, D

    P. Mészáros, D. B. Fox, C. Hanna and K. Murase, 1906.10212. 7

    work page arXiv 1906