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arxiv: 2605.20117 · v1 · pith:AFKX4VUJnew · submitted 2026-05-19 · 🌌 astro-ph.HE · astro-ph.GA· hep-ph

The potential of diffuse Galactic Ridge neutrino measurements to constrain dark matter

Jaume Zuriaga-Puig , Pedro de la Torre Luque , Viviana Gammaldi This is my paper

Pith reviewed 2026-05-20 03:36 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GAhep-ph
keywords dark matterneutrino astronomyGalactic RidgeANTARESindirect detectionWIMPsterile neutrinos
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The pith

ANTARES Galactic Ridge neutrino data can constrain both annihilating and decaying dark matter over wide mass ranges and final states.

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

The paper applies the most recent ANTARES measurements of neutrinos from the Galactic Ridge to indirect dark matter searches. It evaluates signals expected from both annihilation and decay of dark matter particles across many masses and particle channels, while subtracting the predicted astrophysical neutrino background. Different dark matter density profiles are tested, ranging from cuspy to cored distributions, and the analysis is extended to concrete models such as branons and heavy sterile neutrinos. The work shows what current limits look like and what sensitivity future neutrino telescopes could reach. A reader would care because a clean separation of any dark matter neutrino signal would give an independent handle on the nature and distribution of dark matter in the Milky Way.

Core claim

The latest ANTARES Galactic Ridge neutrino measurements can be used to constrain both annihilating and decaying dark matter scenarios across a wide range of masses and final states, after systematic comparison with astrophysical Galactic diffuse emission and for different allowed dark matter density profiles, including in the WIMP model-independent case and for branon and very heavy sterile neutrino models.

What carries the argument

Direct comparison of dark matter neutrino flux predictions, computed for annihilation and decay channels with varied galactic density profiles, against ANTARES data after subtraction of the modeled astrophysical diffuse background.

Load-bearing premise

The astrophysical Galactic diffuse neutrino emission can be accurately modeled and subtracted without significant contamination or uncertainty that would affect the isolation of any dark matter contribution.

What would settle it

A future measurement showing a neutrino flux in the Galactic Ridge that matches the astrophysical background prediction exactly, with no room for an additional component at the level predicted by any dark matter density profile or channel, would remove the claimed constraining power.

Figures

Figures reproduced from arXiv: 2605.20117 by Jaume Zuriaga-Puig, Pedro De la Torre Luque, Viviana Gammaldi.

Figure 1
Figure 1. Figure 1: ANTARES 2022 neutrino flux of the Galactic Ridge region (light [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: ANTARES 2022 neutrino flux (light blue bands) compared with the expected neutrino flux in the Galactic Ridge from DM annihilation to the [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Top panel: different Galactic DM density profiles used in this work, ranging from cuspy profiles (gNFW with γ = 1.4 (solid yellow line), Stars￾Spike (dotted green), NFW (solid blue) and Einasto (dot-dashed purple)) and the Burkert cored profile (dashed red). The vertical dotted lines represent the boundaries of the ANTARES Galactic Ridge (|b| ⩽ 2 ◦ , |l| ⩽ 30◦ ). Bottom panel: same color scheme as the top … view at source ↗
Figure 4
Figure 4. Figure 4: 90% C.L. lower limits on the annihilation decay lifetime [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: 90% C.L. lower limits on the annihilation decay lifetime [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: 90% C.L. (yellow thick line) lower limits on the decay lifetime [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: 2σ flux uncertainty needed for a future neutrino telescope to be sensitive to a decay lifetime τ = 1029 s (left panel) and the thermal relic cross-section ⟨σv⟩th (right panel) for different annihilation channels. The horizontal grey lines represent the expected ideal maximum precision for KMN3Net. The constraints are computed with PPPC and assuming an NFW profile. Given the differences of the flux peaks am… view at source ↗
Figure 8
Figure 8. Figure 8: Left panel: branon annihilation branching ratios into di [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Lower limits to the branon tension f , where the black solid line rep￾resents the precise f value for branons to be the entire DM content. With the same color scheme as the right panel of [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Lower limits (90% C.L.) for the decay lifetime of sterile neutrino DM for the total model (left panel: blue normal ordering, green inverted) and separated [PITH_FULL_IMAGE:figures/full_fig_p012_10.png] view at source ↗
read the original abstract

We use the latest ANTARES Galactic Ridge neutrino measurements to investigate their implications for indirect dark matter (DM) searches. We consider both annihilating and decaying DM scenarios, spanning a wide range of masses and final states, and systematically compare the resulting neutrino fluxes with the expected astrophysical Galactic diffuse emission. Furthermore, we compare the results for different DM density profiles allowed by the observations, from spike and cuspy to cored profiles. We do so for the WIMP model-independent scenario and explore two more specific models: branons and very heavy sterile neutrinos, where a cold DM candidate arises naturally from the theory. We show the potential neutrino measurements in the Galactic Ridge for DM and make predictions for future neutrino observatories.

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 / 3 minor

Summary. The paper uses the latest ANTARES Galactic Ridge neutrino measurements to constrain both annihilating and decaying dark matter across a range of masses and final states. It systematically compares predicted DM neutrino fluxes to modeled astrophysical Galactic diffuse emission for multiple DM density profiles (spike, cuspy, cored) and explores WIMP model-independent cases plus specific models (branons, very heavy sterile neutrinos). Predictions for future neutrino observatories are also provided.

Significance. If the background modeling holds, the work provides a useful exploration of how Galactic Ridge neutrino data can probe DM parameter space, with explicit comparisons across profiles and models that highlight differences between annihilating and decaying scenarios. The inclusion of theory-motivated candidates like branons adds value beyond generic WIMP limits.

major comments (2)
  1. [§3] §3 (background modeling): The astrophysical Galactic diffuse neutrino flux is subtracted using a fixed model based on cosmic-ray interactions with gas; the manuscript does not propagate the 20-50% uncertainties arising from cosmic-ray propagation parameters, gas maps, and hadronic cross sections into the final DM limits. This omission is load-bearing for the central claim, as these uncertainties can absorb or mimic the smoother DM-induced component, particularly for decaying DM or cored profiles.
  2. [§4.2] §4.2 (results for decaying DM): The derived upper limits on the DM lifetime for cored profiles rely on the assumption that the subtracted background leaves a clean residual; without a dedicated sensitivity study varying the background normalization within its uncertainty range, it is unclear whether the reported constraints remain robust or become consistent with zero DM signal.
minor comments (3)
  1. [Figure 2] Figure 2: The legend for different DM profiles is difficult to distinguish in grayscale; adding line styles or markers would improve readability.
  2. [§2.1] §2.1: The notation for the neutrino yield per annihilation/decay (dN/dE) is introduced without an explicit reference to the PYTHIA or similar simulation settings used for the spectra.
  3. References: Several recent ANTARES publications on diffuse emission are cited, but the specific data release or public likelihood files used for the Ridge analysis should be stated explicitly for reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the thorough review and constructive feedback on our manuscript. The comments highlight important aspects of background modeling that we will address to improve the robustness of our dark matter constraints. We respond to each major comment below.

read point-by-point responses

  1. Referee: [§3] §3 (background modeling): The astrophysical Galactic diffuse neutrino flux is subtracted using a fixed model based on cosmic-ray interactions with gas; the manuscript does not propagate the 20-50% uncertainties arising from cosmic-ray propagation parameters, gas maps, and hadronic cross sections into the final DM limits. This omission is load-bearing for the central claim, as these uncertainties can absorb or mimic the smoother DM-induced component, particularly for decaying DM or cored profiles.

    Authors: We agree that a more detailed treatment of the background uncertainties would strengthen the analysis. The current work uses the best available central model for the astrophysical flux as provided in the ANTARES publication. However, to address this concern, we will revise the manuscript to include a sensitivity study where the background normalization is varied within the quoted 20-50% range. This will demonstrate how the DM limits shift and confirm that the constraints remain informative even under conservative assumptions. The revised section 3 will incorporate these variations and discuss their implications for annihilating versus decaying DM scenarios. revision: yes

  2. Referee: [§4.2] §4.2 (results for decaying DM): The derived upper limits on the DM lifetime for cored profiles rely on the assumption that the subtracted background leaves a clean residual; without a dedicated sensitivity study varying the background normalization within its uncertainty range, it is unclear whether the reported constraints remain robust or become consistent with zero DM signal.

    Authors: We acknowledge the validity of this point for the cored profiles in the decaying DM case, where the signal is more diffuse and thus more susceptible to background uncertainties. In the revised version, we will add a dedicated sensitivity analysis in section 4.2, varying the background by its estimated uncertainties and showing the resulting range of lifetime limits. This will clarify the robustness and indicate under which conditions the limits could be consistent with no DM signal. We believe this addition will resolve the concern while preserving the main conclusions for cuspy and spiked profiles where the DM signal is more distinct. revision: yes

Circularity Check

0 steps flagged

No significant circularity; constraints derived from external data comparison

full rationale

The paper computes neutrino fluxes from annihilating and decaying DM using standard halo profiles and annihilation/decay channels, then directly compares these predictions to ANTARES Galactic Ridge measurements after subtracting an independently modeled astrophysical diffuse background from cosmic-ray interactions. No step defines a DM parameter in terms of the final constraint, renames a fitted background as a DM prediction, or relies on a self-citation chain for a uniqueness theorem. Background modeling draws from external cosmic-ray propagation and gas maps; future observatory predictions are straightforward extrapolations of the same flux formulas. The derivation chain remains independent of its own outputs and uses external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The analysis rests on standard assumptions about DM density profiles and neutrino yields from annihilation/decay drawn from prior literature, plus the separability of astrophysical and DM neutrino components.

axioms (1)
  • domain assumption The Galactic diffuse neutrino emission can be modeled independently of dark matter contributions.
    Invoked when comparing predicted DM neutrino fluxes against the expected astrophysical background.

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discussion (0)

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Works this paper leans on

84 extracted references · 84 canonical work pages · 28 internal anchors

  1. [1]

    Planck 2018 results. VI. Cosmological parameters

    N. Aghanim, et al., Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys. 641 (2020) A6, [Erratum: Astron.Astrophys. 652, C4 (2021)].arXiv:1807.06209, doi:10.1051/0004-6361/201833910

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833910 2018

  2. [2]

    Benito, F

    M. Benito, F. Iocco, A. Cuoco, Uncertainties in the Galac- tic Dark Matter distribution: An update, Physics of the 15 Region NFW Burkert Einasto Stars-Spike gNFW (γ=1.4) ANTARES Galactic Ridge 2.30×10 22 1.52×10 21 4.14×10 22 2.90×10 23 4.64×10 23 θGC <2 ◦ 1.02×10 22 9.31×10 19 1.82×10 22 2.77×10 23 4.09×10 23 l∈[15 ◦,125 ◦] b∈[−5 ◦,5 ◦] 4.15×10 21 2.59×1...

    work page doi:10.1016/j.dark.2021.100826 2021

  3. [3]

    P. J. McMillan, The mass distribution and gravita- tional potential of the Milky Way, Monthly Notices of the Royal Astronomical Society 465 (2017) 76–94. doi:10.1093/mnras/stw2759. URLhttps://academic.oup.com/mnras/ article-lookup/doi/10.1093/mnras/stw2759

    work page internal anchor Pith review doi:10.1093/mnras/stw2759 2017

  4. [4]

    Big Bang Nucleosynthesis and Particle Dark Matter

    K. Jedamzik, M. Pospelov, Big Bang nucleosynthesis and particle dark matter, New Journal of Physics 11 (10) (2009) 105028.arXiv:0906.2087,doi:10.1088/ 1367-2630/11/10/105028

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  5. [5]

    Dark Matter

    M. Cirelli, A. Strumia, J. Zupan, Dark Matter, arXiv e-prints (2024) arXiv:2406.01705arXiv:2406.01705, doi:10.48550/arXiv.2406.01705

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2406.01705 2024

  6. [6]

    M. D. Mauro, Characteristics of the Galactic Cen- ter excess measured with 11 years of Fermi-LAT data, Physical Review D 103 (2021) 063029. doi:10.1103/PhysRevD.103.063029. URLhttps://journals.aps.org/prd/abstract/ 10.1103/PhysRevD.103.063029

    work page doi:10.1103/physrevd.103.063029 2021

  7. [7]

    A. Acharyya, et al., Sensitivity of the Cherenkov Tele- scope Array to a dark matter signal from the Galactic centre, JCAP 01 (2021) 057.arXiv:2007.16129,doi: 10.1088/1475-7516/2021/01/057

    work page doi:10.1088/1475-7516/2021/01/057 2021

  8. [8]

    J. A. R. Cembranos, V . Gammaldi, A. L. Maroto, Possi- 16 103 104 105 106 mDM [GeV] 0.0 0.5 1.0 1.5 2.0 2.5 3.0 % 2 σ uncertaintyτ = 10 29s PPPC CosmiXs HDMS νe ¯νe νµ ¯νµ ντ ¯ντ µ+µ□ τ +τ □ 103 104 105 106 mDM [GeV] 0 2 4 6 8 10 12 14% 2 σ uncertainty ⟨σv⟩ = 3 × 10□26cm3s□1 PPPC CosmiXs HDMS νe ¯νe νµ ¯νµ ντ ¯ντ µ+µ□ τ +τ □ Figure C.14: 2σflux uncertaint...

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  9. [9]

    Zuriaga-Puig, V

    J. Zuriaga-Puig, V . Gammaldi, D. Gaggero, T. Lacroix, M. A. Sánchez-Conde, Multi-TeV dark matter density in the inner Milky Way halo: spectral and dynamical constraints, JCAP 2023 (11) (2023) 063.arXiv:2307. 06823,doi:10.1088/1475-7516/2023/11/063

    work page doi:10.1088/1475-7516/2023/11/063 2023

  10. [12]

    Abbasi, et al., Search for neutrino lines from dark matter annihilation and decay with IceCube, Phys

    R. Abbasi, et al., Search for neutrino lines from dark matter annihilation and decay with IceCube, Phys. Rev. D108 (10) (2023) 102004.arXiv:2303. 13663,doi:10.1103/PhysRevD.108.102004

    work page doi:10.1103/physrevd.108.102004 2023

  11. [13]

    R. Abbasi, et al., Search for GeV-scale Dark Matter from the Galactic Center with IceCube-DeepCore, arXiv e-prints (2025) arXiv:2511.00918arXiv:2511.00918, doi:10.48550/arXiv.2511.00918. 17 105 106 107 mDM [GeV] 10□56 10□55 |yν|2 DM-only DM + GDE Normal ordering Inverted ordering 105 106 107 mDM [GeV] 10□56 10□55 10□54 |yl ν|2 DM-only DM + GDE e µ τ Figur...

    work page doi:10.48550/arxiv.2511.00918 2025

  12. [14]

    Jeong, C

    M. Jeong, C. Rott, Search for Dark Matter Decay in Nearby Galaxy Clusters and Galaxies with IceCube, arXiv e-prints (2023) arXiv:2308.04833arXiv:2308.04833, doi:10.48550/arXiv.2308.04833

    work page doi:10.48550/arxiv.2308.04833 2023

  13. [15]

    A. Albert, et al., Search for dark matter towards the galactic centre with 11 years of antares data, Physics Letters B 805 (2020) 135439.doi:https: //doi.org/10.1016/j.physletb.2020.135439. URLhttps://www.sciencedirect.com/science/ article/pii/S0370269320302434 18

    work page doi:10.1016/j.physletb.2020.135439 2020

  14. [16]

    Aiello, et al., First searches for dark matter with the KM3NeT neutrino telescopes, J

    S. Aiello, et al., First searches for dark matter with the KM3NeT neutrino telescopes, J. Cosmology Astropart. Phys.2025 (3) (2025) 058.arXiv:2411.10092,doi: 10.1088/1475-7516/2025/03/058

    work page doi:10.1088/1475-7516/2025/03/058 2025

  15. [17]

    K. Abe, et al., Indirect Search for Dark Matter from the Galactic Center and Halo with the Super-Kamiokande Detector, arXiv e-prints (2020) arXiv:2005.05109arXiv: 2005.05109,doi:10.48550/arXiv.2005.05109

    work page doi:10.48550/arxiv.2005.05109 2020

  16. [19]

    M. G. Aartsen, et al., All-flavour search for neutrinos from dark matter annihilations in the Milky Way with IceCube/DeepCore, European Physical Journal C 76 (10) (2016) 531.arXiv:1606.00209,doi:10.1140/epjc/ s10052-016-4375-3

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1140/epjc/ 2016

  17. [20]

    Cao, et al., Constraints on Heavy Decaying Dark Matter from 570 Days of LHAASO Observations, Phys

    Z. Cao, et al., Constraints on Heavy Decaying Dark Matter from 570 Days of LHAASO Observations, Phys. Rev. Lett.129 (26) (2022) 261103.arXiv:2210. 15989,doi:10.1103/PhysRevLett.129.261103

    work page doi:10.1103/physrevlett.129.261103 2022

  18. [21]

    M. G. Baring, T. Ghosh, F. S. Queiroz, K. Sinha, New limits on the dark matter lifetime from dwarf spheroidal galaxies using Fermi-LAT, Phys. Rev. D93 (10) (2016) 103009.arXiv:1510.00389,doi: 10.1103/PhysRevD.93.103009

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.93.103009 2016

  19. [22]

    Albert, et al., Search for decaying dark mat- ter in the Virgo cluster of galaxies with HAWC, Phys

    A. Albert, et al., Search for decaying dark mat- ter in the Virgo cluster of galaxies with HAWC, Phys. Rev. D109 (4) (2024) 043034.arXiv:2309. 03973,doi:10.1103/PhysRevD.109.043034

    work page doi:10.1103/physrevd.109.043034 2024

  20. [23]

    Albert, et al., An optimized search for dark matter in the galactic halo with HAWC, J

    A. Albert, et al., An optimized search for dark matter in the galactic halo with HAWC, J. Cosmology Astropart. Phys.2023 (12) (2023) 038.arXiv:2305.09861,doi: 10.1088/1475-7516/2023/12/038

    work page doi:10.1088/1475-7516/2023/12/038 2023

  21. [24]

    Cao, et al., Constraints on Ultraheavy Dark Matter Properties from Dwarf Spheroidal Galaxies with LHAASO Observations, Phys

    Z. Cao, et al., Constraints on Ultraheavy Dark Matter Properties from Dwarf Spheroidal Galaxies with LHAASO Observations, Phys. Rev. Lett.133 (6) (2024) 061001.arXiv:2406.08698,doi:10.1103/ PhysRevLett.133.061001

    work page arXiv 2024

  22. [25]

    Rocamora, P

    M. Rocamora, P. De La Torre Luque, M. A. Sánchez- Conde, Constraints on Ultra-heavy DM from TeV-PeV gamma-ray diffuse measurements, arXiv e-prints (2025) arXiv:2509.09609arXiv:2509.09609,doi:10.48550/ arXiv.2509.09609

    work page arXiv 2025

  23. [27]

    Abdalla, et al., Search for Dark Matter An- nihilation Signals in the H.E.S.S

    H. Abdalla, et al., Search for Dark Matter An- nihilation Signals in the H.E.S.S. Inner Galaxy Survey, Phys. Rev. Lett. 129 (2022) 111101. doi:10.1103/PhysRevLett.129.111101. URLhttps://link.aps.org/doi/10.1103/ PhysRevLett.129.111101

    work page doi:10.1103/physrevlett.129.111101 2022

  24. [28]

    The incorrect rotation curve of the Milky Way

    L. Chemin, F. Renaud, C. Soubiran, Incorrect rotation curve of the Milky Way, A&A 578 (2015) A14.arXiv: 1504.01507,doi:10.1051/0004-6361/201526040

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201526040 2015

  25. [30]

    Pinpointing Extragalactic Neutrino Sources in Light of Recent IceCube Observations

    M. Ahlers, F. Halzen, Pinpointing extragalactic neu- trino sources in light of recent IceCube observations, Phys. Rev. D90 (4) (2014) 043005.arXiv:1406.2160, doi:10.1103/PhysRevD.90.043005

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.90.043005 2014

  26. [31]

    IceCube Collaboration, et al., Observation of high-energy neutrinos from the galactic plane, Science 380 (6652) (2023) 1338–1343, publisher Copyright:©2023 Amer- ican Association for the Advancement of Science.doi: 10.1126/science.adc9818

    work page doi:10.1126/science.adc9818 2023

  27. [32]

    ANTARES Collaboration, et al., Antares: the first under- sea neutrino telescope, Nuclear Instruments and Methods in Physics Research A 656 (2011) 11–38, aNTARES Col- laboration overview of detector design, construction and performance.doi:10.1016/j.nima.2011.06.103

    work page doi:10.1016/j.nima.2011.06.103 2011

  28. [33]

    Albert, et al., The ANTARES detector: Two decades of neutrino searches in the Mediterranean Sea, Phys

    A. Albert, et al., The ANTARES detector: Two decades of neutrino searches in the Mediterranean Sea, Phys. Rep.1121-1124 (2025) 1–46.arXiv:2504.09473, doi:10.1016/j.physrep.2025.04.001

    work page doi:10.1016/j.physrep.2025.04.001 2025

  29. [34]

    Albert, et al., Search for Diffuse Galactic Neutri- nos with the Full ANTARES Telescope Dataset, Jour- nal of High Energy Astrophysics (11 2025).arXiv: 2511.01687

    A. Albert, et al., Search for Diffuse Galactic Neutri- nos with the Full ANTARES Telescope Dataset, Jour- nal of High Energy Astrophysics (11 2025).arXiv: 2511.01687

    work page arXiv 2025

  30. [36]

    J. A. Cembranos, A. Dobado, A. L. Maroto, Brane- World Dark Matter, Phys. Rev. Lett.90 (24) (2003) 241301.arXiv:hep-ph/0302041,doi:10.1103/ PhysRevLett.90.241301

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  31. [37]

    Neutrinoful Universe

    T. Higaki, R. Kitano, R. Sato, Neutrinoful universe, Jour- nal of High Energy Physics 2014 (2014) 44.arXiv: 1405.0013,doi:10.1007/JHEP07(2014)044

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/jhep07(2014)044 2014

  32. [38]

    K. Fang, J. S. Gallagher, F. Halzen, The milky way revealed to be a neutrino desert by the ice- cube galactic plane observation, Nature Astronomy 8 (2024) 241–246.arXiv:2303.02128,doi:10.1038/ s41550-023-02128-0

    work page arXiv 2024

  33. [39]

    De la Torre Luque, D

    P. De la Torre Luque, D. Gaggero, D. Grasso, O. Fornieri, K. Egberts, C. Steppa, C. Evoli, Galactic diffuse gamma rays meet the pev frontier, Astronomy & Astrophysics 672 (2023) A58.doi:10.1051/0004-6361/202243714

    work page doi:10.1051/0004-6361/202243714 2023

  34. [40]

    De la Torre Luque, D

    P. De la Torre Luque, D. Gaggero, D. Grasso, A. Marinelli, Prospects for detection of a galactic dif- fuse neutrino flux, Frontiers in Astronomy and Space Sci- ences 9 (2022) 1041838.doi:10.3389/fspas.2022. 1041838

    work page doi:10.3389/fspas.2022 2022

  35. [41]

    F. A. Aharonian, A. Dar, High-energy neutrinos from 19 galactic cosmic rays, Physical Review D 72 (4) (2005) 043005.arXiv:astro-ph/0506099,doi:10.1103/ PhysRevD.72.043005

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  36. [42]

    The gamma-ray and neutrino sky: A consistent picture of Fermi-LAT, Milagro, and IceCube results

    D. Gaggero, A. Urbano, M. Valli, P. Ullio, The gamma- ray and neutrino sky: A consistent picture of cosmic- ray transport in the galaxy, The Astrophysical Journal Letters 815 (2) (2015) L25.arXiv:1504.00227,doi: 10.1088/2041-8205/815/2/L25

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/815/2/l25 2015

  37. [43]

    J. A. Cembranos, A. Dobado, A. L. Maroto, Cosmo- logical and astrophysical limits on brane fluctuations, Phys. Rev. D68 (10) (2003) 103505.arXiv:hep-ph/ 0307062,doi:10.1103/PhysRevD.68.103505

    work page doi:10.1103/physrevd.68.103505 2003

  38. [44]

    J. A. Cembranos, A. Dobado, A. L. Maroto., Bra- non radiative corrections to collider physics and precision observables, Phys. Rev. D73 (3) (2006) 035008.arXiv:hep-ph/0510399,doi:10.1103/ PhysRevD.73.035008

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  39. [45]

    Cirelli, G

    M. Cirelli, G. Corcella, A. Hektor, G. Hütsi, M. Kadastik, P. Panci, M. Raidal, F. Sala, A. Strumia, PPPC 4 DM ID: a poor particle physicist cookbook for dark matter indirect detection, Journal of Cosmol- ogy and Astroparticle Physics 2011 (2011) 051. doi:10.1088/1475-7516/2011/03/051. URLhttps://iopscience.iop.org/article/ 10.1088/1475-7516/2011/03/051ht...

    work page doi:10.1088/1475-7516/2011/03/051 2011

  40. [46]

    Weak Corrections are Relevant for Dark Matter Indirect Detection

    P. Ciafaloni, D. Comelli, A. Riotto, F. Sala, A. Strumia, A. Urbano, Weak Corrections are Relevant for Dark Mat- ter Indirect Detection, JCAP 03 (2011) 019.arXiv: 1009.0224,doi:10.1088/1475-7516/2011/03/019

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2011/03/019 2011

  41. [47]

    C. W. Bauer, N. L. Rodd, B. R. Webber, Dark matter spectra from the electroweak to the Planck scale, Jour- nal of High Energy Physics 2021 (6) (2021) 121.arXiv: 2007.15001,doi:10.1007/JHEP06(2021)121

    work page doi:10.1007/jhep06(2021)121 2021

  42. [48]

    Arina, M

    C. Arina, M. Di Mauro, N. Fornengo, J. Heisig, A. Jueid, R. Ruiz de Austri, CosmiXs: cosmic messenger spec- tra for indirect dark matter searches, J. Cosmology As- tropart. Phys.2024 (3) (2024) 035.arXiv:2312.01153, doi:10.1088/1475-7516/2024/03/035

    work page doi:10.1088/1475-7516/2024/03/035 2024

  43. [49]

    Schwefer, P

    G. Schwefer, P. Mertsch, C. Wiebusch, Diffuse high- energy gamma-ray and neutrino emission from a global fit of cosmic rays, The Astrophysical Journal 940 (1) (2022) 123.arXiv:2211.15607,doi:10.3847/1538-4357/ ac9248

    work page doi:10.3847/1538-4357/ 2022

  44. [50]

    Vecchiotti, F

    V . Vecchiotti, F. L. Villante, G. Pagliaroli, Setting an up- per limit for the total tev neutrino flux from the disk of our galaxy, Journal of Cosmology and Astroparticle Physics 2023 (09) (2023) 027.arXiv:2306.16305, doi:10.1088/1475-7516/2023/09/027

    work page doi:10.1088/1475-7516/2023/09/027 2023

  45. [51]

    De La Torre Luque, D

    P. De La Torre Luque, D. Gaggero, D. Grasso, A. Marinelli, M. Rocamora, The cosmic-ray sea explains the diffuse galactic gamma-ray and neutrino emissions from GeV to PeV, JCAP 12 (2025) 041.arXiv:2502. 18268,doi:10.1088/1475-7516/2025/12/041

    work page doi:10.1088/1475-7516/2025/12/041 2025

  46. [52]

    P. D. Marinos, T. A. Porter, G. P. Rowell, I. V . Moskalenko, G. Jóhannesson, Simulating the diffuse neu- trino emission from the milky way with GALPROP, arXiv Preprint arXiv:2511.09777, predicted Galactic dif- fuse neutrino flux from GALPROP; journal publication forthcoming (2025)

    work page arXiv 2025

  47. [53]

    Ozlati Moghadam, K

    M. Ozlati Moghadam, K. Egberts, R. Batzofin, C. Steppa, E. Bernardini, Estimating the contribution of galactic neu- trino sources, Astroparticle Physics 178 (2026) 103216. doi:10.1016/j.astropartphys.2026.103216. URLhttp://dx.doi.org/10.1016/j. astropartphys.2026.103216

    work page doi:10.1016/j.astropartphys.2026.103216 2026

  48. [54]

    M. Amenomori, et al., First detection of sub-pev dif- fuse gamma rays from the galactic disk: Evidence for ubiquitous galactic cosmic rays beyond pev ener- gies, Physical Review Letters 126 (14) (Apr. 2021). doi:10.1103/physrevlett.126.141101. URLhttp://dx.doi.org/10.1103/PhysRevLett. 126.141101

    work page doi:10.1103/physrevlett.126.141101 2021

  49. [55]

    S. S. Cerri, D. Gaggero, A. Vittino, C. Evoli, D. Grasso, A signature of anisotropic cosmic-ray transport in the gamma-ray sky, Journal of Cosmology and Astroparticle Physics 2017 (10) (2017) 019–019. doi:10.1088/1475-7516/2017/10/019. URLhttp://dx.doi.org/10.1088/1475-7516/ 2017/10/019

    work page doi:10.1088/1475-7516/2017/10/019 2017

  50. [56]

    Bertone, D

    G. Bertone, D. Hooper, History of dark matter, Reviews of Modern Physics 90 (4) (2018) 045002.arXiv:1605. 04909,doi:10.1103/RevModPhys.90.045002

    work page doi:10.1103/revmodphys.90.045002 2018

  51. [57]

    Analytical Models For Galactic Nuclei

    H. Zhao, Analytical models for galactic nu- clei, Mon. Not. Roy. Astron. Soc. 278 (1996) 488–496.arXiv:astro-ph/9509122,doi: 10.1093/mnras/278.2.488

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/278.2.488 1996

  52. [58]

    Dark matter annihilation at the galactic center

    P. Gondolo, J. Silk, Dark matter annihilation at the galactic center, Phys. Rev. Lett. 83 (1999) 1719– 1722.arXiv:astro-ph/9906391,doi:10.1103/ PhysRevLett.83.1719

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  53. [59]

    Dark matter distributions around massive black holes: A general relativistic analysis

    L. Sadeghian, F. Ferrer, C. M. Will, Dark matter distribu- tions around massive black holes: A general relativistic analysis, Phys. Rev. D 88 (6) (2013) 063522.arXiv: 1305.2619,doi:10.1103/PhysRevD.88.063522

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.88.063522 2013

  54. [60]

    Vasiliev, M

    E. Vasiliev, M. Zelnikov, Dark matter dynamics in the galactic center, Phys. Rev. D 78 (2008) 083506. doi:10.1103/PhysRevD.78.083506. URLhttps://link.aps.org/doi/10.1103/ PhysRevD.78.083506

    work page doi:10.1103/physrevd.78.083506 2008

  55. [61]

    Bertone, D

    G. Bertone, D. Merritt, DARK MATTER DY- NAMICS AND INDIRECT DETECTION, Mod- ern Physics Letters A 20 (14) (2005) 1021–1036. doi:10.1142/S0217732305017391. URLhttps://doi.org/10.1142/ S0217732305017391

    work page doi:10.1142/s0217732305017391 2005

  56. [62]

    The Structure of Dark Matter Haloes in Dwarf Galaxies

    A. Burkert, The Structure of dark matter halos in dwarf galaxies, Astrophys. J. Lett. 447 (1995) L25.arXiv: astro-ph/9504041,doi:10.1086/309560

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/309560 1995

  57. [63]

    All-flavor search for a diffuse flux of cosmic neutrinos with 9 years of ANTARES data

    A. Albert, et al., All-flavor Search for a Diffuse Flux of Cosmic Neutrinos with Nine Years of ANTARES Data, ApJ853 (1) (2018) L7.arXiv:1711.07212,doi:10. 3847/2041-8213/aaa4f6. 20

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  58. [64]

    A. Albert, et al., An algorithm for the reconstruction of high-energy neutrino-induced particle showers and its ap- plication to the ANTARES neutrino telescope, European Physical Journal C 77 (6) (2017) 419.arXiv:1708. 03649,doi:10.1140/epjc/s10052-017-4979-2

    work page doi:10.1140/epjc/s10052-017-4979-2 2017

  59. [65]

    Albert, et al., Constraints on the energy spectrum of the diffuse cosmic neutrino flux from the ANTARES neutrino telescope, J

    A. Albert, et al., Constraints on the energy spectrum of the diffuse cosmic neutrino flux from the ANTARES neutrino telescope, J. Cosmology Astropart. Phys.2024 (8) (2024) 038.arXiv:2407.00328,doi:10.1088/1475-7516/ 2024/08/038

    work page doi:10.1088/1475-7516/ 2024

  60. [66]

    Spurio, Status report (2006) of the ANTARES project, arXiv e-prints (2006) hep–ph/0611032arXiv:hep-ph/ 0611032,doi:10.48550/arXiv.hep-ph/0611032

    M. Spurio, Status report (2006) of the ANTARES project, arXiv e-prints (2006) hep–ph/0611032arXiv:hep-ph/ 0611032,doi:10.48550/arXiv.hep-ph/0611032

    work page doi:10.48550/arxiv.hep-ph/0611032 2006

  61. [67]

    J. F. Navarro, C. S. Frenk, S. D. M. White, The Structure of Cold Dark Matter Halos, ApJ462 (1996) 563.arXiv: astro-ph/9508025,doi:10.1086/177173

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/177173 1996

  62. [68]

    J. F. Navarro, C. S. Frenk, S. D. M. White, A Universal Density Profile from Hierarchical Clustering, ApJ490 (2) (1997) 493–508.arXiv:astro-ph/9611107,doi:10. 1086/304888

    work page internal anchor Pith review Pith/arXiv arXiv 1997

  63. [69]

    J. Einasto, On the Construction of a Composite Model for the Galaxy and on the Determination of the System of Galactic Parameters, Trudy Astrofizicheskogo Instituta Alma-Ata 5 (1965) 87–100

    work page 1965

  64. [70]

    K. Abd El Dayem, et al., Improving constraints on the ex- tended mass distribution in the Galactic center with stel- lar orbits, A&A692 (2024) A242.arXiv:2409.12261, doi:10.1051/0004-6361/202452274

    work page doi:10.1051/0004-6361/202452274 2024

  65. [71]

    D. Massari, et al., Proof that the Milky Way experienced a significant merger only 1.5 billion years after the Big Bang, arXiv e-prints (2026) arXiv:2601.18896arXiv: 2601.18896,doi:10.48550/arXiv.2601.18896

    work page doi:10.48550/arxiv.2601.18896 2026

  66. [72]

    Dark matter annihilation near a black hole: plateau vs. weak cusp

    E. Vasiliev, Dark matter annihilation near a black hole: Plateau vs. weak cusp, Phys. Rev. D 76 (2007) 103532.arXiv:0707.3334,doi:10.1103/PhysRevD. 76.103532

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd 2007

  67. [73]

    Abuter, et al., Mass distribution in the Galactic Cen- ter based on interferometric astrometry of multiple stel- lar orbits, Astron

    R. Abuter, et al., Mass distribution in the Galactic Cen- ter based on interferometric astrometry of multiple stel- lar orbits, Astron. Astrophys. 657 (2022) L12.arXiv: 2112.07478,doi:10.1051/0004-6361/202142465

    work page doi:10.1051/0004-6361/202142465 2022

  68. [74]

    Dynamical constraints on a dark matter spike at the Galactic Centre from stellar orbits

    T. Lacroix, Dynamical constraints on a dark matter spike at the Galactic Centre from stellar orbits, Astron. As- trophys. 619 (2018) A46.arXiv:1801.01308,doi: 10.1051/0004-6361/201832652

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201832652 2018

  69. [75]

    GRA VITY Collaboration, et al., A geometric distance measurement to the Galactic center black hole with 0.3% uncertainty, A&A625 (2019) L10.arXiv:1904.05721, doi:10.1051/0004-6361/201935656

    work page doi:10.1051/0004-6361/201935656 2019

  70. [76]

    Gillessen, F

    S. Gillessen, F. Eisenhauer, T. K. Fritz, O. Pfuhl, T. Ott, R. Genzel, The distance to the Galactic Center, in: R. de Grijs (Ed.), Advancing the Physics of Cosmic Distances, V ol. 289 of IAU Symposium, 2013, pp. 29–35.doi:10. 1017/S1743921312021060

    work page 2013

  71. [77]

    H. W. Leung, J. Bovy, J. T. Mackereth, J. A. S. Hunt, R. R. Lane, J. C. Wilson, A measurement of the distance to the Galactic centre using the kinematics of bar stars, MNRAS519 (1) (2023) 948–960.arXiv:2204.12551, doi:10.1093/mnras/stac3529

    work page doi:10.1093/mnras/stac3529 2023

  72. [78]

    A. Albert, et al., Search for secluded dark mat- ter towards the galactic centre with the antares neutrino telescope, Journal of Cosmology and Astroparticle Physics 2022 (06) (2022) 028. doi:10.1088/1475-7516/2022/06/028. URLhttp://dx.doi.org/10.1088/1475-7516/ 2022/06/028

    work page doi:10.1088/1475-7516/2022/06/028 2022

  73. [79]

    Mančinska and D

    A. Albert, et al., Search for dark matter towards the galac- tic centre with 11 years of antares data, Phys. Lett. B 805 (2020) 135439.arXiv:1912.05296,doi:10.1016/j. physletb.2020.135439

    work page doi:10.1016/j 2020

  74. [80]

    A. Albert, et al., Results from the search for dark matter in the Milky Way with 9 years of data of the ANTARES neutrino telescope, Physics Letters B 769 (2017) 249– 254.arXiv:1612.04595,doi:10.1016/j.physletb. 2017.03.063

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.physletb 2017

  75. [81]

    Filippini, KM3NeT Collaboration, Search for a diffuse astrophysical neutrino flux from the Galactic Ridge with KM3NeT/ARCA, in: 39th International Cosmic Ray Con- ference, 2025, p

    F. Filippini, KM3NeT Collaboration, Search for a diffuse astrophysical neutrino flux from the Galactic Ridge with KM3NeT/ARCA, in: 39th International Cosmic Ray Con- ference, 2025, p. 1039

    work page 2025

  76. [82]

    Aguirre-Santaella, V

    A. Aguirre-Santaella, V . Gammaldi, M. A. Sánchez- Conde, D. Nieto, Cherenkov Telescope Array sensitivity to branon dark matter models, J. Cosmology Astropart. Phys.2020 (10) (2020) 041.arXiv:2006.16706,doi: 10.1088/1475-7516/2020/10/041

    work page doi:10.1088/1475-7516/2020/10/041 2020

  77. [83]

    S. Abe, et al., Combined search in dwarf spheroidal galax- ies for branon dark matter annihilation signatures with the magic telescopes, Journal of Cosmology and As- troparticle Physics 2025 (03) (2025) 020.doi:10.1088/ 1475-7516/2025/03/020. URLhttps://doi.org/10.1088/1475-7516/2025/ 03/020

    work page doi:10.1088/1475-7516/2025/ 2025

  78. [84]

    J. A. R. Cembranos, Á. de la Cruz-Dombriz, V . Gammaldi, M. Méndez-Isla, SKA-Phase 1 sen- sitivity to synchrotron radio emission from multi- TeV Dark Matter candidates, Physics of the Dark Universe 27 (2020) 100448.arXiv:1905.11154, doi:10.1016/j.dark.2019.100448

    work page doi:10.1016/j.dark.2019.100448 2020

  79. [85]

    CMS Collaboration, Search for new phenom- ena in monophoton final states in proton- proton collisions at sqrt(s)=8 TeV, arXiv e- prints (2014) arXiv:1410.8812arXiv:1410.8812, doi:10.48550/arXiv.1410.8812

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1410.8812 2014

  80. [86]

    J. A. R. Cembranos, A. de la Cruz-Dombriz, P. K. S. Dunsby, M. Mendez-Isla, Analysis of branon dark mat- ter and extra-dimensional models with AMS-02, Phys. Lett. B 790 (2019) 345–353.arXiv:1709.09819,doi: 10.1016/j.physletb.2019.01.011

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.physletb.2019.01.011 2019

Showing first 80 references.