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arxiv: 2510.26126 · v2 · pith:2EAED2MYnew · submitted 2025-10-30 · ✦ hep-ph · astro-ph.CO

KM3-230213A and IceCube Neutrino Events from Metastable Dark Matter of Primordial Black Hole Origin

Prabhav Singh , Mansi Dhuria , Nathanael Varghese Job This is my paper

Pith reviewed 2026-05-18 03:40 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.CO
keywords ultra-high-energy neutrinosprimordial black holesdark matter decayKM3NeTIceCuberelic abundancePeV neutrinosmetastable dark matter
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The pith

Superheavy dark matter produced by primordial black hole evaporation can decay into neutrinos that explain the KM3-230213A event at 220 PeV and IceCube high-energy detections while satisfying the relic abundance limit.

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

The paper investigates whether the decay of superheavy metastable dark matter particles created during the evaporation of primordial black holes can produce the ultra-high-energy neutrinos observed in the KM3-230213A event and by IceCube. The authors first use the observed dark matter relic density to place limits on the primordial black hole abundance parameter as a function of initial black hole mass and dark matter mass. They then compute the resulting neutrino flux and show that dark matter masses between the PeV and EeV scales generate neutrinos at the right energies to account for both sets of observations. The model stays consistent with existing cosmological and astrophysical constraints across a wide range of parameters and does not predict accompanying signals in photons or other messengers.

Core claim

Dark matter masses in the PeV-EeV range produced via primordial black hole evaporation, when decaying into neutrinos with appropriate lifetime and branching ratio, generate a neutrino flux that matches the KM3-230213A event at median energy of approximately 220 PeV as well as IceCube high-energy neutrinos, all while satisfying the relic abundance constraint on the primordial black hole parameter β.

What carries the argument

Primordial black hole evaporation producing superheavy metastable dark matter whose decays yield the observed ultra-high-energy neutrinos.

If this is right

  • Neutrino energies from the decays match the observed PeV to EeV range events.
  • The model remains consistent with the dark matter relic abundance for a range of initial PBH masses and DM masses.
  • The scenario satisfies existing cosmological and astrophysical bounds over a broad parameter space.
  • No multimessenger signatures accompany the neutrino events.

Where Pith is reading between the lines

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

  • Future neutrino telescopes could search for the specific spectral shape predicted by this decay channel.
  • The mechanism connects early-universe black hole formation directly to present-day high-energy neutrino detections.
  • Absence of events in certain energy windows could further narrow the allowed dark matter mass range.

Load-bearing premise

The dark matter particles must be metastable with a lifetime and neutrino branching ratio tuned to match the observed flux once the primordial black hole abundance is fixed by the relic density constraint.

What would settle it

Detection of high-energy photons, cosmic rays, or a mismatched neutrino energy spectrum from the same sources would rule out a pure neutrino-decay origin.

Figures

Figures reproduced from arXiv: 2510.26126 by Mansi Dhuria, Nathanael Varghese Job, Prabhav Singh.

Figure 1
Figure 1. Figure 1: FIG. 1: Constraints on the PBH abundance, [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2: Phase-space distribution function of neutrinos pro [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: The energy squared differential neutrino flux per steradian with respect to the energy of the neutrinos. Figure shows [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4: The energy squared differential neutrino flux per steradian with respect to the energy of the neutrinos for a fixed [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5: The neutrino flux as a function of PBH constituting the fraction of dark matter [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
read the original abstract

We investigate a scenario in which the recently observed ultra-high-energy neutrino event KM3-230213A, with a median energy of approximately 220 PeV, as well as the high-energy neutrinos detected by IceCube Observatory, originate from the decay of superheavy dark matter (DM) particles produced through primordial black hole (PBH) evaporation. To establish this connection, we derive constraints on the PBH abundance parameter $\beta$ as a function of the initial PBH mass $M_{\mathrm{BH_0}}$ and DM mass $m_{\mathrm{DM}}$, by considering the bound from the observed relic DM abundance. Using these constraints, we compute the resulting neutrino flux and show that DM masses in the PeV-EeV range can yield neutrinos of comparable energies, capable of accounting for both the KM3-230213A and IceCube events while remaining consistent with the relic abundance constraint. Interestingly, the scenario remains viable over a broad region of parameter space while satisfying existing cosmological and astrophysical bounds. Overall, our results demonstrate that PBH evaporation followed by DM decay provides a consistent and natural explanation for the observed ultra-high-energy neutrino events in the absence of accompanying multimessenger signatures.

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

1 major / 3 minor

Summary. The manuscript proposes that the KM3-230213A ultra-high-energy neutrino event (~220 PeV) and IceCube high-energy neutrinos arise from the decay of metastable superheavy dark matter particles produced via primordial black hole evaporation. Constraints on the PBH abundance β(M_BH0, m_DM) are derived from the observed relic DM density; these normalized densities are then used to compute the present-day neutrino flux for m_DM in the PeV-EeV range, with lifetime and branching ratio chosen to reproduce the observed rates while satisfying cosmological and astrophysical bounds.

Significance. If the result holds, the work supplies a viable mechanism connecting PBH evaporation, superheavy DM, and UHE neutrinos without requiring multimessenger counterparts. It applies standard PBH-to-DM yield formulas and cosmological decay flux integrals, explicitly normalizing to relic abundance and scanning a broad parameter space consistent with stated limits. This constitutes a concrete, falsifiable extension of PBH-DM scenarios into neutrino astronomy.

major comments (1)
  1. [§4] §4: the neutrino flux is computed after fixing β from relic abundance and then selecting a metastable lifetime and neutrino branching ratio to match the KM3-230213A and IceCube rates. This post-hoc adjustment demonstrates consistency but reduces the predictive power of the central claim; an independent theoretical range or prior for the lifetime (e.g., from a concrete decay model) should be provided to show the window is not solely data-driven.
minor comments (3)
  1. [Abstract] Abstract: the phrase 'in the absence of accompanying multimessenger signatures' should cite the specific gamma-ray or other bounds used later in the text for immediate clarity.
  2. [§3] §3: the relic-abundance constraint on β assumes the DM particles account for the full observed density; a brief explicit statement confirming that evaporation products do not violate BBN or other early-universe bounds for the adopted M_BH0 range would strengthen the derivation.
  3. [§2] Notation: M_BH0 and m_DM are introduced without a consolidated table of symbols; adding one would improve readability across §§2–4.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We are grateful to the referee for their thorough review and insightful comments on our manuscript. We have carefully considered the feedback and provide our responses below.

read point-by-point responses

  1. Referee: [§4] §4: the neutrino flux is computed after fixing β from relic abundance and then selecting a metastable lifetime and neutrino branching ratio to match the KM3-230213A and IceCube rates. This post-hoc adjustment demonstrates consistency but reduces the predictive power of the central claim; an independent theoretical range or prior for the lifetime (e.g., from a concrete decay model) should be provided to show the window is not solely data-driven.

    Authors: We acknowledge the referee's observation that the lifetime and branching ratio are chosen to match the observed rates. Our primary goal is to demonstrate the consistency of the PBH-evaporated metastable DM scenario with the KM3-230213A and IceCube data, while respecting the relic abundance constraint derived from β. This is inherently a consistency check rather than a parameter-free prediction, as the decay properties of the superheavy DM are not fixed by the PBH production mechanism alone. In the absence of a specific UV-complete model for the DM decay, the lifetime remains a free parameter that can be constrained by the neutrino observations. We believe this does not diminish the predictive power in the sense that the model predicts the possibility of explaining the events for DM masses in the PeV-EeV range with appropriate lifetimes that are still allowed by other bounds. To address the concern, we have added a paragraph in the revised version of Section 4 discussing possible theoretical origins for the metastable lifetime from high-scale physics, providing some theoretical context for the parameter choices. This strengthens the presentation without requiring a full concrete decay model. revision: partial

Circularity Check

0 steps flagged

No significant circularity

full rationale

The paper's chain starts from the standard PBH evaporation yield to place an upper bound on β(M_BH0, m_DM) using the observed relic DM abundance as an external input. The resulting normalized DM density then enters the standard cosmological decay flux integral. Selection of m_DM in the PeV-EeV window and a metastable lifetime plus neutrino branching ratio simply tunes the model to reproduce the observed event rates while remaining inside the relic-allowed window; this is ordinary parameter fitting to data rather than any equation reducing to its own input by construction. No self-citation is load-bearing for the central result, and all steps rely on externally verifiable cosmological and astrophysical limits stated in the text.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 1 invented entities

The central claim rests on standard early-universe cosmology plus the postulate of metastable DM with neutrino decay channels; parameters β and m_DM are adjusted within the relic-abundance window to match neutrino energies.

free parameters (2)
  • β (PBH abundance fraction)
    Constrained as a function of initial PBH mass and DM mass by the observed relic DM density; used to normalize the neutrino flux.
  • m_DM (DM particle mass)
    Selected in the PeV-EeV range so that decay products reach the observed neutrino energies.
axioms (2)
  • standard math Standard Hawking evaporation and cosmological evolution of PBHs
    Invoked to relate initial PBH mass to the produced DM abundance and to derive the β constraint.
  • domain assumption Metastable DM decays dominantly into neutrinos with suitable lifetime
    Required to convert the constrained DM density into the predicted neutrino flux at Earth.
invented entities (1)
  • Metastable superheavy dark matter particles from PBH evaporation no independent evidence
    purpose: Source of ultra-high-energy neutrinos matching KM3-230213A and IceCube events
    Postulated to link PBH evaporation to the observed neutrinos; no independent falsifiable signature outside the neutrino flux itself is provided.

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Forward citations

Cited by 1 Pith paper

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Reference graph

Works this paper leans on

48 extracted references · 48 canonical work pages · cited by 1 Pith paper

  1. [1]

    M. G. Aartsen et al. Multimessenger observations of a flaring blazar coincident with high-energy neutrino IceCube-170922A.Science, 361(6398):eaat1378, 2018

    work page 2018

  2. [2]

    M. G. Aartsen et al. IceCube-Gen2: the window to the extreme Universe.J. Phys. G, 48(6):060501, 2021

    work page 2021

  3. [3]

    On the potential cosmogenic origin of the ultra-high-energy event km3-230213a.The Astro- physical Journal Letters, 984(2):L41, 2025

    O Adriani, S Aiello, A Albert, AR Alhebsi, M Al- shamsi, S Alves Garre, A Ambrosone, F Ameli, M Andre, L Aphecetche, et al. On the potential cosmogenic origin of the ultra-high-energy event km3-230213a.The Astro- physical Journal Letters, 984(2):L41, 2025

    work page 2025

  4. [4]

    Observation of an ultra-high-energy cosmic neutrino with km3net.Nature, 638(8050):376–382, 2025

    work page 2025

  5. [5]

    Adriani et al

    O. Adriani et al. On the Potential Galactic Origin of the Ultra-High-Energy Event KM3-230213A. 2 2025

    work page 2025

  6. [6]

    Clash of the Titans: ultra- high energy KM3NeT event versus IceCube data

    Shirley Weishi Li, Pedro Machado, Daniel Naredo-Tuero, and Thomas Schwemberger. Clash of the Titans: ultra- high energy KM3NeT event versus IceCube data. 2 2025

    work page 2025

  7. [7]

    Abbasi et al

    R. Abbasi et al. Search for Extremely-High-Energy Neu- trinos and First Constraints on the Ultrahigh-Energy Cosmic-Ray Proton Fraction with IceCube.Phys. Rev. Lett., 135(3):031001, 2025

    work page 2025

  8. [8]

    Road through Darkνess: Probing dark matter-neutrino interactions using KM3-230213A

    Ranjini Mondol, Subhadip Bouri, Akash Kumar Saha, and Ranjan Laha. Road through Darkνess: Probing dark matter-neutrino interactions using KM3-230213A. 6 2025

    work page 2025

  9. [9]

    Scrutiniz- ing the cosmogenic origin of the KM3-230213A event: A Multimessenger Perspective

    Alessandro Cermenati, Antonio Ambrosone, Roberto Aloisio, Denise Boncioli, and Carmelo Evoli. Scrutiniz- ing the cosmogenic origin of the KM3-230213A event: A Multimessenger Perspective. 7 2025

    work page 2025

  10. [10]

    Investigat- ing the uhecr characteristics from cosmogenic neutrino limits with the measurements of the pierre auger obser- vatory

    Camilla Petrucci, A Abdul Halim, P Abreu, M Agli- etta, I Allekotte, K Almeida Cheminant, A Almela, Olaf Scholten, Pierre Auger Collaboration, et al. Investigat- ing the uhecr characteristics from cosmogenic neutrino limits with the measurements of the pierre auger obser- vatory. In38th International Cosmic Ray Conference (ICRC2023)-Cosmic-Ray Physics (In...

    work page

  11. [11]

    Sissa Medialab, 2024

    work page 2024

  12. [12]

    Lua F. T. Airoldi, Gustavo F. S. Alves, Yuber F. Perez- Gonzalez, Gabriel M. Salla, and Renata Zukanovich Fun- chal. Could a Primordial Black Hole Explosion Explain the KM3NeT Event? 5 2025

    work page 2025

  13. [13]

    Cascaded Gamma-Ray Emission Associated with the KM3NeT Ultrahigh-energy Event KM3-230213A.Astrophys

    Ke Fang, Francis Halzen, and Dan Hooper. Cascaded Gamma-Ray Emission Associated with the KM3NeT Ultrahigh-energy Event KM3-230213A.Astrophys. J. Lett., 982(1):L16, 2025

    work page 2025

  14. [14]

    Interpreting the KM3-230213A PeV Neu- trino Event via Vector Dark Matter Decay and Its Multi- Messenger Signatures

    Yu-Hang Su, Si-Yu Chen, Chengfeng Cai, and Hong- Hao Zhang. Interpreting the KM3-230213A PeV Neu- trino Event via Vector Dark Matter Decay and Its Multi- Messenger Signatures. 7 2025

    work page 2025

  15. [15]

    Constraining Super-Heavy Dark Matter with the KM3-230213A Neutrino Event

    Roberto Aloisio, Antonio Ambrosone, and Carmelo Evoli. Constraining Super-Heavy Dark Matter with the KM3-230213A Neutrino Event. 8 2025

    work page 2025

  16. [16]

    Possible origin of the KM3-230213A neutrino event from dark matter decay.Phys

    Debasish Borah, Nayan Das, Nobuchika Okada, and Prantik Sarmah. Possible origin of the KM3-230213A neutrino event from dark matter decay.Phys. Rev. D, 111(12):123022, 2025

    work page 2025

  17. [17]

    Linking the KM3-230213A Neutrino Event to Dark Matter Decay and Gravitational Waves Signals

    Sarif Khan, Jongkuk Kim, and Pyungwon Ko. Linking the KM3-230213A Neutrino Event to Dark Matter Decay and Gravitational Waves Signals. 4 2025

    work page 2025

  18. [18]

    Super heavy dark matter origin of the PeV neu- trino event: KM3-230213A

    Kazunori Kohri, Partha Kumar Paul, and Narendra Sahu. Super heavy dark matter origin of the PeV neu- trino event: KM3-230213A. 3 2025

    work page 2025

  19. [19]

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

    Ivan Esteban and Alejandro Ibarra. Attenuation of the ultra-high-energy neutrino flux by dark matter scatter- ings. 8 2025

    work page 2025

  20. [20]

    The Highest- Energy Neutrino Event Constrains Dark Matter- Neutrino Interactions

    Toni Bert´ olez-Mart´ ınez, Gonzalo Herrera, Pablo Mart´ ınez-Mirav´ e, and Jorge Terol Calvo. The Highest- Energy Neutrino Event Constrains Dark Matter- Neutrino Interactions. 6 2025

    work page 2025

  21. [21]

    P. S. Bhupal Dev, Bhaskar Dutta, Aparajitha Karthikeyan, Writasree Maitra, Louis E. Strigari, and Ankur Verma. ‘Dark’ Matter Effect as a Novel Solution to the KM3-230213A Puzzle. 5 2025

    work page 2025

  22. [22]

    Explaining the KM3- 230213A Detection without Gamma-Ray Emission: Cosmic-Ray Dark Radiation

    Yuma Narita and Wen Yin. Explaining the KM3- 230213A Detection without Gamma-Ray Emission: Cosmic-Ray Dark Radiation. 3 2025

    work page 2025

  23. [23]

    Cosmo- genic Neutrino Point Source and KM3-230213A

    Qinyuan Zhang, Tian-Qi Huang, and Zhuo Li. Cosmo- genic Neutrino Point Source and KM3-230213A. 4 2025

    work page 2025

  24. [24]

    Sakharov, Rostislav Konoplich, and Merab Gogberashvili

    Alexander S. Sakharov, Rostislav Konoplich, and Merab Gogberashvili. Ultra High Energy Neutrino Event KM3- 230213A as a Signal of Electroweak Vacuum Turbulence in Merging Black Hole Binaries. 6 2025. 11

    work page 2025

  25. [25]

    An Accretion Flare In- terpretation for the UHE Neutrino Event KM3-230213A

    Chengchao Yuan, Leonard Pfeiffer, Walter Winter, Sara Buson, Federico Testagrossa, Jose Maria Sanchez Za- balla, and Alessandra Azzollini. An Accretion Flare In- terpretation for the UHE Neutrino Event KM3-230213A. 6 2025

    work page 2025

  26. [26]

    Pseudo-Goldstone dark matter from primordial black holes: gravitational wave signatures and implications for KM3-230213A event at KM3NeT.JCAP, 06:023, 2025

    Siyu Jiang and Fa Peng Huang. Pseudo-Goldstone dark matter from primordial black holes: gravitational wave signatures and implications for KM3-230213A event at KM3NeT.JCAP, 06:023, 2025

    work page 2025

  27. [27]

    Klipfel and David I

    Alexandra P. Klipfel and David I. Kaiser. Ultra-High- Energy Neutrinos from Primordial Black Holes. 3 2025

    work page 2025

  28. [28]

    A strike of luck: could the KM3-230213A event be caused by an evaporating primordial black hole? 2 2025

    Andrea Boccia and Fabio Iocco. A strike of luck: could the KM3-230213A event be caused by an evaporating primordial black hole? 2 2025

    work page 2025

  29. [29]

    Constraints on earth- mass primordial black holes from ogle 5-year microlensing events.Phys

    Hiroko Niikura, Masahiro Takada, Shuichiro Yokoyama, Takahiro Sumi, and Shogo Masaki. Constraints on earth- mass primordial black holes from ogle 5-year microlensing events.Phys. Rev. D, 99:083503, Apr 2019

    work page 2019

  30. [30]

    Chapter 4 - primordial black holes

    Albert Escriv` a, Florian K¨ uhnel, and Yuichiro Tada. Chapter 4 - primordial black holes. In Manuel Arca Sedda, Elisa Bortolas, and Mario Spera, editors,Black Holes in the Era of Gravitational-Wave Astronomy, pages 261–377. Elsevier, 2024

    work page 2024

  31. [31]

    Seven hints for primordial black hole dark matter.Physics of the Dark Universe, 22:137–146, 2018

    S´ ebastien Clesse and Juan Garc´ ıa-Bellido. Seven hints for primordial black hole dark matter.Physics of the Dark Universe, 22:137–146, 2018

    work page 2018

  32. [32]

    Primordial black hole evaporation and dark matter production

    Andrew Cheek, Lucien Heurtier, Yuber F Perez- Gonzalez, and Jessica Turner. Primordial black hole evaporation and dark matter production. i. solely hawk- ing radiation.Physical Review D, 105(1):015022, 2022

    work page 2022

  33. [33]

    Constraints on primordial black holes.Reports on Progress in Physics, 84(11):116902, 2021

    Bernard Carr, Kazunori Kohri, Yuuiti Sendouda, and Jun’ichi Yokoyama. Constraints on primordial black holes.Reports on Progress in Physics, 84(11):116902, 2021

    work page 2021

  34. [34]

    Constraints on primordial black holes from big bang nucleosynthesis revisited.Physical Review D, 102(10):103512, 2020

    Celeste Keith, Dan Hooper, Nikita Blinov, and Samuel D McDermott. Constraints on primordial black holes from big bang nucleosynthesis revisited.Physical Review D, 102(10):103512, 2020

    work page 2020

  35. [35]

    New cosmological constraints on primordial black holes.Physical Review D—Particles, Fields, Grav- itation, and Cosmology, 81(10):104019, 2010

    BJ Carr, Kazunori Kohri, Yuuiti Sendouda, and Jun’ichi Yokoyama. New cosmological constraints on primordial black holes.Physical Review D—Particles, Fields, Grav- itation, and Cosmology, 81(10):104019, 2010

    work page 2010

  36. [36]

    Black hole explosions?Nature, 248(5443):30–31, 1974

    Stephen W Hawking. Black hole explosions?Nature, 248(5443):30–31, 1974

    work page 1974

  37. [37]

    Black holes in the early universe.Monthly Notices of the Royal Astro- nomical Society, 168(2):399–415, 1974

    Bernard J Carr and Stephen W Hawking. Black holes in the early universe.Monthly Notices of the Royal Astro- nomical Society, 168(2):399–415, 1974

    work page 1974

  38. [38]

    Gravitationally collapsed objects of very low mass.Monthly Notices of the Royal Astronom- ical Society, 152(1):75–78, 04 1971

    Stephen Hawking. Gravitationally collapsed objects of very low mass.Monthly Notices of the Royal Astronom- ical Society, 152(1):75–78, 04 1971

    work page 1971

  39. [39]

    The primordial black hole mass spec- trum.Astrophysical Journal, vol

    Bernard J Carr. The primordial black hole mass spec- trum.Astrophysical Journal, vol. 201, Oct. 1, 1975, pt. 1, p. 1-19. Research supported by the Science Research Council of England, 201:1–19, 1975

    work page 1975

  40. [40]

    Warm hawking relics from primordialblack hole domination.Journal of Cosmology and Astroparticle Physics, 2025(02):026, 2025

    Christopher J Shallue, Julian B Mu˜ noz, and Gordan Z Krnjaic. Warm hawking relics from primordialblack hole domination.Journal of Cosmology and Astroparticle Physics, 2025(02):026, 2025

    work page 2025

  41. [41]

    Cosmological origin of the km3-230213a event and associated gravitational waves

    Ki-Young Choi, Erdenebulgan Lkhagvadorj, and Satyabrata Mahapatra. Cosmological origin of the km3-230213a event and associated gravitational waves. arXiv preprint arXiv:2503.22465, 2025

    work page arXiv 2025

  42. [42]

    Arcadi, M

    Giorgio Arcadi, Manfred Lindner, Jacinto P Neto, and Farinaldo S Queiroz. Ultraheavy dark matter and wimps production aided by primordial black holes.arXiv preprint arXiv:2408.13313, 2024

    work page arXiv 2024

  43. [43]

    Hooper, and Laura Lopez-Honorez

    Iason Baldes, Quentin Decant, Deanna C. Hooper, and Laura Lopez-Honorez. Non-cold dark matter from pri- mordial black hole evaporation.Journal of Cosmology and Astroparticle Physics, 2020(08):045, aug 2020

    work page 2020

  44. [44]

    High-energy and ultra-high-energy neutrinos from primordial black holes.Journal of Cosmology and Astroparticle Physics, 2025(02):059, 2025

    Quan-feng Wu and Xun-Jie Xu. High-energy and ultra-high-energy neutrinos from primordial black holes.Journal of Cosmology and Astroparticle Physics, 2025(02):059, 2025

    work page 2025

  45. [45]

    Aghanim et al

    N. Aghanim et al. Planck 2018 results. VI. Cosmological parameters.Astron. Astrophys., 641:A6, 2020. [Erratum: Astron.Astrophys. 652, C4 (2021)]

    work page 2018

  46. [46]

    Mark G Aartsen, M Ackermann, J Adams, JA Aguilar, M Ahlers, M Ahrens, I Al Samarai, D Altmann, K An- deen, T Anderson, et al. Differential limit on the extremely-high-energy cosmic neutrino flux in the pres- ence of astrophysical background from nine years of ice- cube data.Physical Review D, 98(6):062003, 2018

    work page 2018

  47. [47]

    Icecube high-energy start- ing event sample: Description and flux characterization with 7.5 years of data.Physical Review D, 104(2):022002, 2021

    R Abbasi, M Ackermann, J Adams, JA Aguilar, M Ahlers, M Ahrens, C Alispach, AA Alves Jr, NM Amin, K Andeen, et al. Icecube high-energy start- ing event sample: Description and flux characterization with 7.5 years of data.Physical Review D, 104(2):022002, 2021

    work page 2021

  48. [48]

    Foster, and Julian B

    Yitian Sun, Joshua W. Foster, and Julian B. Mu˜ noz. Constraining inhomogeneous energy injection from an- nihilating dark matter and primordial black holes with 21-cm cosmology. 9 2025

    work page 2025