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Composite asymmetric dark matter with a dark photon portal: Multimessenger tests

T0 review · 2 major / 5 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read Composite asymmetric dark matter in the 1-10 GeV mass range must be extremely long-lived: AMS-02 positrons require a lifetime above about 10^26 seconds, while Super-K neutrino data require at least 10^23 seconds.

desk verdict Solid multimessenger analysis of 1–10 GeV composite ADM; the headline lifetime bound is conditional on a stated but unquantified two-body decay assumption that could shift the limits by an order of magnitude. read the letter →

arxiv 2412.15641 v2 pith:P3RASCZD submitted 2024-12-20 hep-ph astro-ph.HE

Saikat Das , Ayuki Kamada , Takumi Kuwahara , Kohta Murase , Deheng Song This is my paper · ORCID
classification hep-phastro-ph.HE PACS 95.35.+d
keywords compositeasymmetricdarkmatterphotonportalQCDdecayingcosmic-rayconstraintsneutrinolineAMS-02positronsSuper-Kamiokande
topics Dark Matter
open problems Dark Matter
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Composite asymmetric dark matter aims to explain why the dark matter and baryon densities of the Universe are so similar by making dark matter a dark-sector baryon whose asymmetry is shared with the Standard Model. This paper asks how long such dark baryons can survive if they decay through a dark photon portal, and it answers with existing multimessenger data. For dark matter masses of 1-10 GeV, the most restrictive probe is the AMS-02 positron flux, which forces the dark baryon lifetime above roughly $10^{26}$ seconds for masses above about 2 GeV, corresponding to a portal cutoff scale of about $10^{8}$-$10^{9}$ GeV. Neutrino telescopes give independent, more conservative limits: Super-Kamiokande data require lifetimes above about 2 x $10^{23}$ seconds at low masses and about 6 x $10^{23}$ seconds at 10 GeV. If correct, the composite ADM framework survives only in a narrow region with very long-lived dark baryons and a very weak portal interaction.

What carries the argument

The engine of the calculation is the cascade-decay spectrum: the dark baryon n' decays through the portal operator into a neutral dark meson pi'0 plus an antineutrino; pi'0 then decays either into two on-shell dark photons when kinematically allowed, or into an off-shell dark photon plus an electron-positron pair, and each dark photon decays to e+e-(gamma) through kinetic mixing with the Standard Model photon. The primary spectra are built by boosting the rest-frame decay spectra using the final-state-radiation splitting function, with the branching fractions of dark baryons into neutral dark mesons fixed by Clebsch-Gordan coefficients, one-third in the minimal vector-like model. These spectra are then propagated with a standard cosmic-ray transport framework under four propagation scenarios, and the neutrino signal is analyzed with a three-bin chi-squared approach using Super-K effective areas and the atmospheric neutrino background.

What would settle it

A dedicated search for a monoenergetic neutrino line at an energy near half the dark matter mass in the 1-10 GeV range would settle the claim: if Super-K, Hyper-K, or DUNE sees a line flux corresponding to a lifetime below the limits claimed here, the central conclusion would be wrong. Equally decisive would be a lattice or chiral-effective-theory calculation showing that the three-body dark-baryon decay rate is comparable to the two-body rate, since that would invalidate the assumed spectra and require all limits to be recomputed.

Watch

Extended reading notes

Core claim

The paper claims that the decay of composite asymmetric dark matter in the 1-10 GeV mass window is already strongly bounded by existing cosmic-ray and neutrino observations, and that these bounds cannot be obtained by naive extrapolation from higher-mass dark matter searches. Modeling the full cascade chain, dark baryon to dark meson plus antineutrino, dark meson to dark photons (or to an off-shell dark photon plus electron-positron pair), and dark photon to e+e-(gamma), the authors compute the primary e±, gamma-ray, and neutrino spectra and compare them with positron, electron, gamma-ray, and neutrino data. The strongest limit comes from AMS-02 positrons at masses above about 2 GeV, requiring the dark matter lifetime to exceed about $10^{26}$ seconds, which translates into a portal cutoff scale of about $10^{8}$-$10^{9}$ GeV. The dedicated Super-K monoenergetic neutrino search yields tau_DM greater than about 2 x $10^{23}$ seconds at low masses and about 6 x $10^{23}$ seconds at 10 GeV. These results imply that in the viable parameter region the dark baryon must be very long-lived and the portal interaction that shares the asymmetry must be very weak.

Load-bearing premise

The entire spectral calculation rests on the assumption that dark baryons decay overwhelmingly through the two-body channels such as n' -> pi'0 + nu, with spin-one, multi-meson, and three-body final states negligible; the paper flags this in footnote 5, and if the neglected channels are comparable, the e±, gamma-ray, and neutrino spectra change and the derived lifetime limits shift.

Editorial extensions

If this is right

  • AMS-02 positron data alone place the vector-like two-body model at tau_DM above about 3 x 10^27 seconds at 1 GeV and above about 10^26 seconds across most of the 2-10 GeV range, making positrons the current strongest probe.
  • The neutrino line at roughly half the dark matter mass is robust and nearly model-independent, and Super-K already excludes lifetimes below about 2 x 10^23 seconds at low masses and about 6 x 10^23 seconds at 10 GeV.
  • Hyper-Kamiokande will improve on Super-K only if the systematic uncertainty on the atmospheric neutrino background drops to roughly 10 percent or better energy resolution is achieved.
  • Chiral composite ADM models are less constrained than vector-like models because their branching fractions into neutral dark mesons differ.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If three-body dark-baryon decay channels are comparable to the two-body ones, as the paper notes can happen in GUT nucleon decay through final-state interactions, the monochromatic neutrino line would be smeared and the e± and gamma spectra softened, shifting the quoted lifetime limits; a dedicated calculation of the three-body branching fraction would settle how much.
  • The same cascade-spectrum machinery could be applied to other portal-decay dark matter scenarios with GeV-scale masses, and the steep mass scaling of the lifetime means the bounds tighten quickly toward 10 GeV and relax toward 1 GeV.
  • A full analysis of actual Super-K event data rather than the conservative effective-area and binning approach used here could strengthen the neutrino limits by a factor of a few.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 5 minor

Summary. This paper studies decaying composite asymmetric dark matter (ADM) in the 1-10 GeV mass range, in both vector-like and chiral realizations with a dark photon portal. It computes analytic cascade spectra for dark baryon decay into a dark meson plus antineutrino, followed by two- or three-body dark meson decays into dark photons and e±/γ, and uses these spectra to derive 95% C.L. lifetime lower limits from AMS-02 e±, Voyager e±, Fermi/EGRET/COMPTEL/SMM γ-ray data, and a dedicated three-bin line search against atmospheric neutrino backgrounds for Super-K, with projections for Hyper-K. The headline result is that AMS-02 positrons provide the most stringent limit, τ_DM ≳ 10^26 s, corresponding to a portal cutoff of about 10^8-10^9 GeV, and that Super-K yields constraints around 2×10^23 s at low masses and 6×10^23 s at 10 GeV.

Significance. The paper fills a genuine gap: existing decaying-DM constraints at 1-10 GeV are not directly applicable to this scenario because the e± spectrum is softened by the cascade and the atmospheric neutrino background is large. The authors provide explicit analytic spectra for both two-body and three-body dark meson decays, use four cosmic-ray propagation scenarios, cross-check against CMB constraints, and give a concrete Hyper-K projection. The methods are transparent: Section III and Appendices A-C contain the spectrum derivations, decay-rate relations via Clebsch-Gordan coefficients, and an equivalence-theorem check for the chiral model, while the propagation uses the public GALPROP code. The derived limits are robust across propagation models for the higher end of the mass range, and the neutrino analysis is appropriately framed as conservative. If the two-body dominance assumption for dark baryon decay holds, the constraints are an important and nontrivial input to composite ADM model building.

major comments (2)
  1. [Section III, footnote 5; Eqs. (10)-(15)] The assumption that dark baryon decay is dominated by two-body channels n' → π' + ν (and analogous modes), with spin-one, multi-meson, and three-body channels negligible, is load-bearing for the entire spectrum computation. The paper itself notes in footnote 5 that in GUT nucleon decay three-body final states can be comparable via pion final-state interactions (Ref. [110]), and it defers investigation of such channels to future work. Because the monochromatic neutrino line used in the Super-K analysis (Section IV.D) and the e± injection spectrum behind the AMS-02 bound (Section IV.C) both assume precisely these initial two-body kinematics, the quoted lifetime limits in Figs. 6 and 9 are conditional on an unquantified model assumption. I request either a chiral-perturbation/final-state-interaction estimate of the three-body branching fraction in this specific model, or at least a sensitivity study showing how the τ_DM limits shift for a non-negligible three-body branching fraction (e.g., 10% and 50%). Without one of these, the caveat is not merely cosmetic but directly affects the central numerical claims.
  2. [Section IV.D, Figs. 8-9] The Super-K 'constraint' is not derived from observed event counts; it is a comparison of the predicted signal plus atmospheric background model to the HKKM model expectation, with the model used as pseudo-data. The text does state that this is intended as a conservative bound and encourages more sophisticated analyses with actual Super-K data, which is commendable. However, the abstract and figure captions present the result as a constraint from Super-K data, and the quantitative statements in the abstract ('Super-K neutrino data require...') are stronger than what the analysis actually supports. I recommend rewording the presentation to make explicit that these are expected limits from a Super-K-like background-model analysis, not limits extracted from the unbinned or event-level data set, and to state this qualification in the abstract and conclusions where the neutrino numbers are quoted.
minor comments (5)
  1. [Eq. (21)] The expression for ξ1:min is missing parentheses; as printed, the denominator is ambiguous. It should read ξ1:min = [1 + ϵ1^2 − 2ξ2 + ξ2^2]/(1 − ξ2).
  2. [Section IV.C and summary] For m_DM below about 2.4 GeV, the PD and DC propagation models produce no AMS-02 limits because the modulated flux falls below the lowest data point, as noted in the text. The summary statement that e± yield τ_DM ≳ 10^26 s 'for all ADM models' should therefore be qualified by the mass range and propagation-model dependence.
  3. [Section II.A, Eqs. (3)-(5)] The effective cutoff M_* in Eq. (5) is defined only collectively, and its relation to M and M' in Eq. (3) is not stated. A sentence or footnote explaining this connection would help readers follow the cutoff-scale interpretation of the main limit.
  4. [Fig. 4 caption] The caption uses '2mA/mπ = 0.4'; this should be '2mA′/mπ′' for consistency with the rest of the paper.
  5. [Section IV.D, Fig. 9 caption] The statement that both vector-like and chiral models lead to the same neutrino constraint is correct but should be explained at first use: the neutrino line flux is independent of the neutral-meson branching ratio because every dark baryon decay produces an antineutrino, whereas the e± and γ-ray fluxes do depend on that branching ratio.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the lifetime limits are derived by comparing independently propagated model spectra with external data, so no fitted input is renamed as a prediction.

full rationale

The paper's derivation chain is conditional rather than circular: it takes a pre-existing composite-ADM framework (Refs. [17,19,85]) as input, computes dark-baryon cascade-decay spectra using standard methods (Eqs. (10)-(27)), and derives lifetime lower limits by comparing the propagated Galactic/extragalactic fluxes with external data (AMS-02, Voyager-I, Fermi-LAT/EGRET/COMPTEL/SMM, and Super-K atmospheric-neutrino backgrounds). No parameter relevant to the target constraints is fitted to those constraints. The only fitted inputs are the cosmic-ray propagation parameters of Ref. [124], which are calibrated to other CR species and are explicitly stated not to fit the local e± data; the DM mass and dark-meson/dark-photon mass ratios are scanned as benchmark parameters rather than fitted. The self-citations (notably Ref. [17], with overlapping authorship) supply the model Lagrangian, gauge charges, and U(1)D assignments, but they do not contain the lifetime constraints, so the central claim does not reduce to them by construction. The explicit caveat in footnote 5, neglecting three-body dark-baryon decay channels such as n' -> pi' pi' nu, is a physical modeling assumption that could soften the quoted limits if relaxed; it is a correctness/robustness risk, not a circular step, because the limits are computed from that assumed spectrum and compared to data, not derived from data back into the assumption. Overall, the paper is self-contained against external benchmarks for its main multimessenger claims, and I find no equation or fitted parameter that is equivalent by definition to the claimed result.

Assumptions & free parameters 4 free parameters · 7 assumptions · 4 invented entities

The central constraints rest on a composite dark sector with several hand-chosen benchmark parameters: the dark matter mass, two mass ratios involving the dark meson and dark photon, and equal reduced matrix elements in the chiral model. The decay and propagation assumptions are standard for this type of analysis, but they carry systematic uncertainty that is not fully quantified.

free parameters (4)
  • Dark matter mass m_N' (m_DM) = 1-10 GeV (scanned)
    Treated as a free parameter; all constraints are presented as functions of m_DM. The model predicts this range from asymmetry sharing, but the paper does not fit it.
  • Dark meson to dark photon mass ratio 2 m_A'/m_pi' = 0.4 and 1.4
    Benchmark choices distinguishing two-body and three-body dark meson decay channels (Sec IV). The constraints depend on these choices.
  • Dark meson to dark baryon mass ratio m_pi'/m_N' = 0.1 (for 0.4) and 0.03 (for 1.4)
    Chosen benchmark mass spectrum; sets the dark photon mass to 20-200 MeV (Sec III).
  • Chiral reduced matrix element ratios A_Lambda(1):A_Lambda(2):A_Sigma(1):A_Sigma(2) = 1:1:1:1
    Assumed in numerical simulations (Appendix A); determines the branching into electromagnetic dark mesons in chiral models.
assumptions (7)
  • domain assumption Dark neutral mesons decay into two dark photons via the chiral anomaly in the dark sector.
    Invoked in Sec III before Eq. (10); this is the mechanism that converts dark meson decays into electron/positron and gamma-ray signals.
  • domain assumption Dark baryon decay is dominated by two-body channels into a single dark meson (or longitudinal dark photon) plus antineutrino; spin-one and multi-meson final states are negligible.
    Stated in Sec III footnote 5; the whole spectrum calculation and the monochromatic neutrino line rely on this.
  • domain assumption The dark photon decays promptly (lifetime smaller than O(1) s, kinetic mixing epsilon greater than 1e-10) and its mass lies in 20-200 MeV so only electron channels are open.
    Assumed in Sec III and Sec IV; if the dark photon lived longer or decayed to muons or pions, the electromagnetic constraints would change.
  • domain assumption The cosmic-ray propagation models from Ref [124], which were not fit to local electron/positron data, are adequate for e+ and e- in the 1-10 GeV range.
    Used in Sec IV.B and Table III; the spread among PD, DC, DRE, and DRC scenarios is the main systematic uncertainty in the electron/positron limits.
  • domain assumption The atmospheric neutrino background is described by the HKKM model (Ref [132]) with a 15% systematic uncertainty.
    Used in Sec IV.D for the Super-K and Hyper-K neutrino constraints.
  • domain assumption The extragalactic gamma-ray contribution from ADM decay is substantially lower than the Galactic component and can be neglected.
    Asserted in Sec IV.A without a quantitative demonstration; this is conservative for the gamma-ray limits.
  • standard math For the simplified boost formulas, the dark baryon is much heavier than the dark meson and dark photon (epsilon_2 much less than 1 and epsilon_tilde_1 much less than 1).
    Used to simplify Eqs. (13) to (14) and Eq. (15); valid for the benchmark mass hierarchies.
invented entities (4)
  • Dark baryons p', n' (vector-like) and Sigma', Lambda', Xi' (chiral)
    purpose: The composite asymmetric dark matter particles whose decay produces the neutrino and electromagnetic signals.
    Adopted from Refs [17,85]; no direct evidence beyond the predicted decay signals discussed in this paper.
  • Dark mesons pi'0, eta', K', pi'
    purpose: Decay products of dark baryons; neutral ones decay into dark photons and generate electron/positron and gamma-ray fluxes.
    Particles of the dark QCD sector; no independent detection.
  • Dark photon A'
    purpose: Mediator that mixes with the SM photon and converts dark hadron decay energy into electrons, positrons, and photons.
    The kinetic mixing epsilon is assumed large enough for prompt decay; no external evidence is cited.
  • Dark quarks U', D', S' and dark Higgs phi_D
    purpose: Constituents that form the dark hadrons and break U(1)_D to give the dark photon mass.
    Building blocks of the composite ADM model; not observed.

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Cite this review

Pith. "Pith review of Composite asymmetric dark matter with a dark photon portal: Multimessenger tests." pith.science (2026). https://pith.science/paper/P3RASCZD

@misc{pith2026241215641,
  author       = {Pith},
  title        = {Pith review of: Composite asymmetric dark matter with a dark photon portal: Multimessenger tests},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/P3RASCZD}},
  note         = {Machine review of arXiv:2412.15641}
}
abstract

Composite asymmetric dark matter (ADM) is the framework that naturally explains the coincidence of the baryon density and the dark matter density of the Universe. Through a portal interaction sharing particle-antiparticle asymmetries in the Standard Model and dark sectors, dark matter particles, which are dark-sector counterparts of baryons, can decay into antineutrinos and dark-sector counterparts of mesons (dark mesons) or dark photon. Subsequent cascade decay of the dark mesons and the dark photon can also provide electromagnetic fluxes at late times of the Universe. The cosmic-ray constraints on the decaying dark matter with the mass of $1$--$10$~GeV has not been well studied. We perform comprehensive studies on the decay of the composite ADM by combining the astrophysical constraints from $e^\pm$ and $\gamma$-ray. The constraints from cosmic-ray positron measurements by AMS-02 are the most stringent at $\gtrsim2$~GeV: a lifetime should be larger than the order of $10^{26}$~s, corresponding to the cutoff scale of the portal interaction of about $10^8 \text{--} 10^9 \, \mathrm{GeV}$. We also perform the dedicated analysis for the neutrino monoenergetic signals at Super-Kamiokande and Hyper-Kamiokande due to the atmospheric neutrino background in the energy range of our interest.

Figures

Figures reproduced from arXiv: 2412.15641 by the authors.

Figure 1
Figure 1. FIG. 1. Our summary plot of multimessenger constraints on [PITH_FULL_IMAGE:figures/full_fig_p001_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. DM mass as a function of the numbers of dark flavors [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. Energy fractions of the dark matter decay: electron and positron (red-solid), [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figures from the paper (6 more)
Figure 5
Figure 5. Figure 5: FIG. 5. Diffuse [PITH_FULL_IMAGE:figures/full_fig_p009_5.png]
Figure 6
Figure 6. Figure 6: FIG. 6. 95% C.L. limits on the ADM lifetime for all the modes considered in this work, including chiral models. The constraints [PITH_FULL_IMAGE:figures/full_fig_p010_6.png]
Figure 7
Figure 7. Figure 7: FIG. 7. 95% C.L. limits on the ADM decay lifetime for all [PITH_FULL_IMAGE:figures/full_fig_p011_7.png]
Figure 8
Figure 8. Figure 8: FIG. 8 [PITH_FULL_IMAGE:figures/full_fig_p012_8.png]
Figure 9
Figure 9. Figure 9: FIG. 9. 95% C.L. limits on DM decay lifetime from Super-K. [PITH_FULL_IMAGE:figures/full_fig_p013_9.png]
Figure 10
Figure 10. Figure 10: FIG. 10. Dependence of projected constraints for Hyper-K on [PITH_FULL_IMAGE:figures/full_fig_p014_10.png]

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