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arxiv: 2606.09986 · v1 · pith:MWM5ZOVEnew · submitted 2026-06-08 · ✦ hep-ex · hep-ph

Testing Heavy Dark Matter Decay as the Origin of KM3-230213A

KM3NeT Collaboration: O. Adriani , J. A. Aguilar , A. Albert , A. R. Alhebsi , S. Alshalloudi , F. Ameli , M. Andre , L. Aphecetche
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M. Ardid S. Ardid J. Aublin F. Badaracco B. Baret A. Bariego-Quintana L. Barigione M. Barnard Y. Becherini M. Bendahman F. Benfenati Gualandi M. Benhassi D. M. Benoit Z. Be\v{n}u\v{s}ov\'a E. Berbee C. van Bergen E. Berti V. Bertin P. Betti S. Biagi M. Boettcher D. Bonanno M. Bond\`i M. Bongi S. Bottai J. Boumaaza M. Bouta C. Bozza R. M. Bozza F. Bretaudeau M. Breuhaus R. Bruijn J. Brunner R. Bruno E. Buis R. Buompane B. Caiffi D. Calvo E.G.J. van Campenhout A. Capone F. Carenini V. Carretero T. Cartraud P. Castaldi V. Cecchini S. Celli M. Chabab A. Chen S. Cherubini M. Chianese T. Chiarusi W. Chung M. Circella R. Clark R. Cocimano J. A. B. Coelho A. Coleiro A. Condorelli R. Coniglione P. Coyle A. Creusot G. Cuttone R. Dallier A. De Benedittis G. De Wasseige V. Decoene P. Deguire I. Del Rosso L. S. Di Mauro I. Di Palma A. F. D\'iaz D. Diego-Tortosa C. Distefano A. Domi C. Donzaud D. Dornic E. Drakopoulou D. Drouhin J.-G. Ducoin P. Duverne R. Dvornick\'y T. Eberl E. Eckerov\'a A. Eddymaoui M. Eff D. van Eijk I. El Bojaddaini S. El Hedri S. El Mentawi V. Ellajosyula A. Enzenh\"ofer M. Farino A. Ferrara G. Ferrara M. D. Filipovi\'c F. Filippini A. Foisseau D. Franciotti C. Frosin L. A. Fusco T. Gal J. Garc\'ia M\'endez A. Garcia Soto C. Gatius Oliver N. Gei{\ss}elbrecht H. Ghaddari L. Gialanella B. K. Gibson E. Giorgio I. Goos P. Goswami S. R. Gozzini R. Gracia M. Guelfand B. Guillon C. Hanna H. van Haren E. Hazelton A. Heijboer L. Hennig J. J. Hern\'andez-Rey A. Idrissi W. Idrissi Ibnsalih G. Illuminati R. Jaimes O. Janik D. Joly M. de Jong P. de Jong B. J. Jung P. Kalaczy\'nski G. Kalaitzidakis C. Karagiannis U. F. Katz J. Keegans T. Khvichia G. Kistauri C. Kopper A. Kouchner Y. Y. Kovalev L. Krupa V. Kueviakoe V. Kulikovskiy R. Kvatadze M. Labalme R. Lahmann M. Lamoureux A. Langella G. Larosa C. Lastoria J. Lazar G. Lehaut V. Lema\^itre E. Leonora N. Lessing G. Levi I. Lhenry-Yvon M. Lincetto M. Lindsey Clark F. Longhitano M. Loup A. Luashvili S. Madarapu F. Magnani V. A. Makeev L. Malerba F. Mamedov P. M\'anek A. Manfreda A. Manousakis M. Marconi A. Margiotta A. Marinelli C. Markou L. Martin M. Mastrodicasa S. Mastroianni J. Mauro K. C. K. Mehta G. Miele P. Migliozzi E. Migneco M. L. Mitsou C. M. Mollo L. Morales-Gallegos N. Mori A. Mosbrugger A. Moussa I. Mozun Mateo S. Mugnier R. Muller M. R. Musone M. Musumeci S. Navas C. A. Nicolau B. Nkosi B. \'O Fearraigh V. Oliviero A. Orlando E. Oukacha L. Pacini D. Paesani P. Papini V. Parisi G. Pascua B. Pascual-Estrugo A. M. P\u{a}un G. E. P\u{a}v\u{a}la\v{s} S. Pe\~na Mart\'inez M. Perrin-Terrin V. Pestel M. Petropavlova L. Pfeiffer P. Piattelli A. Plavin C. Poir\`e V. Poireau T. Pradier J. Prado S. Pulvirenti N. Randazzo A. Ratnani S. Razzaque I. C. Rea D. Real G. Riccobene J. Robinson A. Romanov E. Ros F. Salesa Greus D. F. E. Samtleben A. S\'anchez Losa S. Sanfilippo M. Sanguineti D. Santonocito P. Sapienza M. Scaringella M. Scarnera J. Schnabel J. Schumann M. Senniappan P. A. Sevle Myhr I. Sgura R. Shanidze Y. Shitov F. \v{S}imkovic A. Simonelli A. Sinopoulou C. Sironneau M. Spurio O. Starodubtsev I. \v{S}tekl D. Stocco M. Taiuti Y. Tayalati J. Tena H. Thiersen S. Thoudam I. Tosta e Melo B. Trocm\'e V. Tsourapis C. Tully E. Tzamariudaki A. Ukleja A. Vacheret V. Valsecchi V. Van Elewyck G. Vannoye E. Vannuccini G. Vasileiadis F. Vazquez de Sola A. Veutro S. Viola D. Vivolo A. van Vliet L. Voorend E. de Wolf S. Zavatarelli D. Zito J. D. Zornoza J. Z\'u\~niga
This is my paper

Pith reviewed 2026-06-27 14:26 UTC · model grok-4.3

classification ✦ hep-ex hep-ph
keywords dark matter decayultra-high-energy neutrinosKM3-230213AKM3NeTPeV-scale dark matterneutrino lifetime boundsGalactic versus extragalactic dark matter
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The pith

If the KM3-230213A neutrino came from heavy dark matter decay, the particle mass would need to exceed 100 PeV with a lifetime of 10^26 to 10^27 seconds, but these values conflict with other observations.

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

The paper tests whether one ultra-high-energy neutrino event detected by KM3NeT could be produced by the decay of a dark matter particle heavier than a PeV. It combines the measured energy deposit and arrival direction with full detector simulations to predict the expected signals from different possible decay channels. The fit under the dark matter assumption requires masses above roughly 100 PeV at 95 percent , with lifetimes in a narrow window around 10^26 to 10^27 seconds. Both Galactic and extragalactic dark matter contributions are included, yet the favored region remains excluded by limits from other neutrino telescopes and by gamma-ray data. This outcome indicates that dark matter decay is disfavored as the explanation for the observed event.

Core claim

Assuming a dark matter origin of the event, we find that the preferred mass at 95% C.L. is larger than about 100 PeV in all scenarios considered, with best-fit lifetimes in the range 10^{26}-10^{27} s. These preferred regions are in tension with existing bounds from other neutrino telescopes and gamma-ray observations.

What carries the argument

Detector Monte Carlo simulation that maps the event's deposited energy and arrival direction onto expected signal distributions for different decay channels while separating Galactic and extragalactic dark matter contributions.

If this is right

  • Dark matter masses above 100 PeV are required at 95 percent confidence level for every decay channel examined.
  • Lifetimes between 10^{26} and 10^{27} seconds provide the best match to the event properties.
  • The same parameter region is already excluded by gamma-ray flux limits.
  • Constraints from other neutrino telescopes independently rule out the preferred lifetimes and masses.
  • Inclusion of both Galactic and extragalactic dark matter does not remove the tension with existing bounds.

Where Pith is reading between the lines

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

  • The tension favors an astrophysical explanation for this particular neutrino event over a dark matter origin.
  • Repeating the same energy-direction analysis on any future ultra-high-energy neutrino detections could tighten limits on heavy decaying dark matter.
  • Multi-messenger follow-up observations that search for accompanying gamma rays at the predicted level could directly test the decay hypothesis.
  • The method can be extended to other high-energy events to place model-independent bounds on dark matter lifetime at extreme masses.

Load-bearing premise

The observed event originates from dark matter decay rather than an astrophysical source or background.

What would settle it

An independent analysis that attributes KM3-230213A to a known astrophysical source such as a blazar or cosmic-ray interaction would remove the premise needed to derive the mass and lifetime constraints.

Figures

Figures reproduced from arXiv: 2606.09986 by A. Albert, A. Bariego-Quintana, A. Capone, A. Chen, A. Coleiro, A. Condorelli, A. Creusot, A. De Benedittis, A. Domi, A. Eddymaoui, A. Enzenh\"ofer, A. F. D\'iaz, A. Ferrara, A. Foisseau, A. Garcia Soto, A. Heijboer, A. Idrissi, A. Kouchner, A. Langella, A. Luashvili, A. Manfreda, A. Manousakis, A. Margiotta, A. Marinelli, A. Mosbrugger, A. Moussa, A. M. P\u{a}un, A. Orlando, A. Plavin, A. R. Alhebsi, A. Ratnani, A. Romanov, A. S\'anchez Losa, A. Simonelli, A. Sinopoulou, A. Ukleja, A. Vacheret, A. van Vliet, A. Veutro, B. Baret, B. Caiffi, B. Guillon, B. J. Jung, B. K. Gibson, B. Nkosi, B. \'O Fearraigh, B. Pascual-Estrugo, B. Trocm\'e, C. A. Nicolau, C. Bozza, C. Distefano, C. Donzaud, C. Frosin, C. Gatius Oliver, C. Hanna, C. Karagiannis, C. Kopper, C. Lastoria, C. Markou, C. M. Mollo, C. Poir\`e, C. Sironneau, C. Tully, C. van Bergen, D. Bonanno, D. Calvo, D. Diego-Tortosa, D. Dornic, D. Drouhin, D. F. E. Samtleben, D. Franciotti, D. Joly, D. M. Benoit, D. Paesani, D. Real, D. Santonocito, D. Stocco, D. van Eijk, D. Vivolo, D. Zito, E. Berbee, E. Berti, E. Buis, E. De Wolf, E. Drakopoulou, E. Eckerov\'a, E. Giorgio, E.G.J. van Campenhout, E. Hazelton, E. Leonora, E. Migneco, E. Oukacha, E. Ros, E. Tzamariudaki, E. Vannuccini, F. Ameli, F. Badaracco, F. Benfenati Gualandi, F. Bretaudeau, F. Carenini, F. Filippini, F. Longhitano, F. Magnani, F. Mamedov, F. Salesa Greus, F. Vazquez de Sola, F. \v{S}imkovic, G. Cuttone, G. de Wasseige, G. E. P\u{a}v\u{a}la\v{s}, G. Ferrara, G. Illuminati, G. Kalaitzidakis, G. Kistauri, G. Larosa, G. Lehaut, G. Levi, G. Miele, G. Pascua, G. Riccobene, G. Vannoye, G. Vasileiadis, H. Ghaddari, H. Thiersen, H. van Haren, I. C. Rea, I. Del Rosso, I. Di Palma, I. El Bojaddaini, I. Goos, I. Lhenry-Yvon, I. Mozun Mateo, I. Sgura, I. Tosta e Melo, I. \v{S}tekl, J. A. Aguilar, J. A. B. Coelho, J. Aublin, J. Boumaaza, J. Brunner, J. D. Zornoza, J. Garc\'ia M\'endez, J.-G. Ducoin, J. J. Hern\'andez-Rey, J. Keegans, J. Lazar, J. Mauro, J. Prado, J. Robinson, J. Schnabel, J. Schumann, J. Tena, J. Z\'u\~niga, K. C. K. Mehta, KM3NeT Collaboration: O. Adriani, L. A. Fusco, L. Aphecetche, L. Barigione, L. Gialanella, L. Hennig, L. Krupa, L. Malerba, L. Martin, L. Morales-Gallegos, L. Pacini, L. Pfeiffer, L. S. Di Mauro, L. Voorend, M. Andre, M. Ardid, M. Barnard, M. Bendahman, M. Benhassi, M. Boettcher, M. Bond\`i, M. Bongi, M. Bouta, M. Breuhaus, M. Chabab, M. Chianese, M. Circella, M. de Jong, M. D. Filipovi\'c, M. Eff, M. Farino, M. Guelfand, M. Labalme, M. Lamoureux, M. Lincetto, M. Lindsey Clark, M. L. Mitsou, M. Loup, M. Marconi, M. Mastrodicasa, M. Musumeci, M. Perrin-Terrin, M. Petropavlova, M. R. Musone, M. Sanguineti, M. Scaringella, M. Scarnera, M. Senniappan, M. Spurio, M. Taiuti, N. Gei{\ss}elbrecht, N. Lessing, N. Mori, N. Randazzo, O. Janik, O. Starodubtsev, P. A. Sevle Myhr, P. Betti, P. Castaldi, P. Coyle, P. Deguire, P. De Jong, P. Duverne, P. Goswami, P. Kalaczy\'nski, P. M\'anek, P. Migliozzi, P. Papini, P. Piattelli, P. Sapienza, R. Bruijn, R. Bruno, R. Buompane, R. Clark, R. Cocimano, R. Coniglione, R. Dallier, R. Dvornick\'y, R. Gracia, R. Jaimes, R. Kvatadze, R. Lahmann, R. M. Bozza, R. Muller, R. Shanidze, S. Alshalloudi, S. Ardid, S. Biagi, S. Bottai, S. Celli, S. Cherubini, S. El Hedri, S. El Mentawi, S. Madarapu, S. Mastroianni, S. Mugnier, S. Navas, S. Pe\~na Mart\'inez, S. Pulvirenti, S. Razzaque, S. R. Gozzini, S. Sanfilippo, S. Thoudam, S. Viola, S. Zavatarelli, T. Cartraud, T. Chiarusi, T. Eberl, T. Gal, T. Khvichia, T. Pradier, U. F. Katz, V. A. Makeev, V. Bertin, V. Carretero, V. Cecchini, V. Decoene, V. Ellajosyula, V. Kueviakoe, V. Kulikovskiy, V. Lema\^itre, V. Oliviero, V. Parisi, V. Pestel, V. Poireau, V. Tsourapis, V. Valsecchi, V. Van Elewyck, W. Chung, W. Idrissi Ibnsalih, Y. Becherini, Y. Shitov, Y. Tayalati, Y. Y. Kovalev, Z. Be\v{n}u\v{s}ov\'a.

Figure 1
Figure 1. Figure 1: FIG. 1. Expected distributions of the deposited energy (top) and of the angle with respect to the Galactic center (bottom) [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. The Feldman–Cousins 95% and 99% C.L. contours (solid and dashed lines, respectively) for DM decaying into [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Each panel shows the neutrino energy flux per flavor as a function of neutrino energy for the different DM decay [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
read the original abstract

This work explores the hypothesis that the ultra-high-energy neutrino event KM3-230213A originates from the decay of a heavy dark matter particle with a mass above PeV scale. The analysis exploits the deposited energy and arrival direction of the event as well as a complete detector Monte Carlo simulation to compute the expected signal distributions for different decay channels and assesses the relative contributions from Galactic and extragalactic dark matter. Assuming a dark matter origin of the event, we find that the preferred mass at 95% C.L. is larger than about 100 PeV in all scenarios considered, with best-fit lifetimes in the range $10^{26}$-$10^{27}$ s. These preferred regions are in tension with existing bounds from other neutrino telescopes and gamma-ray observations.

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 tests whether the ultra-high-energy neutrino event KM3-230213A originates from heavy dark matter decay above the PeV scale. It employs the event's deposited energy and arrival direction together with a complete detector Monte Carlo simulation to derive expected signal distributions across decay channels, while separating Galactic and extragalactic dark matter contributions. Assuming a dark matter origin for the event, the analysis reports a preferred mass larger than about 100 PeV at 95% C.L. with best-fit lifetimes in the range 10^{26}–10^{27} s; these regions are stated to be in tension with existing neutrino telescope and gamma-ray bounds.

Significance. If the result holds, the work supplies a concrete conditional constraint on heavy dark matter by mapping a single observed event onto mass and lifetime parameter space via full detector Monte Carlo. Credit is due for the explicit separation of Galactic and extragalactic contributions and the use of complete detector Monte Carlo, both of which strengthen the signal modeling. The analysis adds a falsifiable test of the dark matter hypothesis for this ultra-high-energy neutrino within a multi-messenger framework.

minor comments (2)
  1. [Abstract] Abstract: the phrase 'in all scenarios considered' is left unspecified; listing the decay channels or models examined would improve immediate clarity for readers.
  2. [Section on statistical analysis] The likelihood construction and treatment of systematic uncertainties on the single-event fit are referenced but would benefit from an expanded description to confirm how the 95% C.L. mass lower limit is obtained.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for the positive assessment of our work, the recognition of the value of the full detector Monte Carlo and the Galactic/extragalactic separation, and the recommendation for minor revision. No specific major comments were raised in the report.

Circularity Check

0 steps flagged

No significant circularity

full rationale

The paper conditions explicitly on the hypothesis that the single observed event originates from heavy DM decay, then uses deposited energy, direction, and full detector MC to derive conditional best-fit mass (>~100 PeV at 95% C.L.) and lifetime ranges (10^26-10^27 s) across channels, plus Galactic/extragalactic decomposition. These are standard likelihood fits to data under the premise; the tension statement references independent external neutrino and gamma-ray bounds. No step reduces by construction to its own inputs, no self-citation chain is load-bearing for the central claim, and no ansatz or uniqueness theorem is smuggled in. The derivation is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on two fitted parameters to a single event plus standard domain assumptions about decay channels and detector response; no new entities are postulated.

free parameters (2)
  • dark matter mass = >100 PeV
    Fitted parameter whose lower bound is derived from matching simulated energy deposits to the observed event under the dark matter hypothesis
  • dark matter lifetime = 10^{26}-10^{27} s
    Fitted parameter whose best-fit range is obtained from the likelihood analysis assuming dark matter origin
axioms (2)
  • domain assumption The neutrino event originates from dark matter decay
    Explicit premise stated in the abstract that enables derivation of mass and lifetime constraints
  • domain assumption Monte Carlo simulation correctly reproduces detector response and signal distributions for decay channels
    Required to compute expected signals for Galactic and extragalactic contributions

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discussion (0)

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Reference graph

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