Pith. sign in

REVIEW 3 major objections 4 minor 41 references

A MeV-Scale Dark QCD Solution to the Axion Domain Wall Problem

T0 review · 3 major / 4 minor · reviewed 2026-07-11 · grok-4.5

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read A cold MeV-scale dark QCD sector lifts axion domain-wall degeneracy while keeping the strong-CP angle small enough to solve the problem.

desk verdict A clean MeV-window idea for tilting axion walls with dark instantons; the balance is real but the collapse and DIGA inputs leave the window only order-of-magnitude controlled. read the letter →

arxiv 2607.04137 v1 pith:CRQ6HZGC submitted 2026-07-05 hep-ph

Jun Guo , Zhaofeng Kang , Jiang Zhu This is my paper · ORCID
classification hep-ph
keywords axiondomainwallproblemdarkQCDstrongCPgravitationalwavespulsartimingarraysglueballsMeVtelescopes
topics The Strong CP Problem
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

The Peccei-Quinn axion that solves the strong CP problem can form cosmologically dangerous domain walls whenever its potential has more than one vacuum. This paper shows that a mixed anomaly between the PQ symmetry and a hidden SU(Nc) color force generates an extra cosine potential from dark instantons. That potential tilts the vacua enough to collapse the walls before Big-Bang nucleosynthesis, yet the dark scale can still sit low enough (0.1–3 MeV) that the effective QCD theta angle remains below 10^{-10}. The same setup predicts gravitational waves already within reach of pulsar-timing arrays and a faint di-photon line from axion–dark-glueball mixing that next-generation MeV telescopes could see. A cooler dark sector is preferred so that dark glueballs do not overclose the universe.

What carries the argument

The dark cosine potential Vd = −χ0 cos(Ad θeff + δ) generated by the mixed U(1)PQ–SU(Nc)^{2} anomaly; its temperature-dependent topological susceptibility supplies the vacuum bias ΔV ∼ χ0 that lifts the NDW-fold degeneracy while the upper bound χ0/χQCD ≲ 10^{-10}/δ keeps θeff safe.

What would settle it

A stochastic gravitational-wave background whose peak frequency and doubly-broken power-law shape match the domain-wall collapse prediction for Teq ∼ few–tens of MeV and fa ∼ 10^{12} GeV, already testable by current PTA data and definitively by SKA.

Watch

Extended reading notes

Core claim

When the PQ symmetry also has a mixed anomaly with a pure Yang-Mills dark SU(Nc), the resulting dark-instanton potential explicitly breaks the residual Z_NDW symmetry. For a dark critical temperature Tc inside the narrow window 0.1–3 MeV (and a temperature ratio ξ ≲ 0.5), the vacuum bias is large enough to drive domain-wall collapse before BBN while the induced shift in the effective theta angle stays below the neutron-EDM bound, thereby solving the domain-wall problem without reintroducing the strong CP problem.

Load-bearing premise

The temperature dependence of the dark topological susceptibility is assumed to follow continuum lattice results for pure Yang-Mills even at MeV scales and for a cooler dark sector.

Editorial extensions

If this is right

  • Current PTA signals at nHz frequencies can already be interpreted as axion domain-wall collapse for NDW ≳ 5 and fa ∼ 10^{12} GeV.
  • Future SKA will reconstruct the doubly-broken power-law spectrum and distinguish it from supermassive black-hole binaries.
  • Next-generation MeV telescopes (COSI, AMEGO-X, e-ASTROGAM) can search for the di-photon line from the lightest dark glueball near 15 MeV in the most optimistic corners of parameter space.
  • A cold dark sector (ξ ≲ 0.01) automatically satisfies dark-glueball relic-density bounds while enlarging the viable Tc window.
  • A possible double-line gamma-ray signature (from 0++–0−+ mixing controlled by the dark theta term) would uniquely fingerprint the scenario.

Reading between the lines

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

  • If PTA data firm up a domain-wall-like spectrum, the required cold dark QCD sector becomes a concrete target for lattice studies of MeV-scale pure Yang-Mills.
  • The same mixed anomaly that solves the domain-wall problem automatically supplies a portal for freeze-in production of dark glueballs, linking two otherwise separate dark-matter candidates.
  • The opposite dependence of the GW amplitude and the glueball lifetime on fa and Tc means a joint detection would over-constrain the model and either confirm or kill it cleanly.
  • Models with Ad = NDW and vanishing relative theta would evade the MeV upper bound entirely, recovering a high-scale mirror-QCD limit that the paper only briefly notes.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper proposes that a mixed U(1)_PQ–SU(N_c) anomaly with a hidden dark QCD sector generates an additional cosine potential for the axion (Eqs. 2.3–2.4). This explicitly breaks the residual Z_NDW symmetry, lifting vacuum degeneracy and allowing domain walls to collapse. A delicate balance is claimed: the dark critical temperature must lie in a narrow MeV window (0.1–3 MeV, with temperature ratio ξ ≲ 0.01–0.5) so that the induced bias ΔV ∼ χ0 collapses walls before BBN (Teq ≳ 1 MeV) while keeping |NDW ⟨θ_eff⟩| ≲ 10^{-10} and preserving the PQ solution to strong CP (Eqs. 2.6–2.12 and Figs. 1–2). Two signatures are developed: a stochastic GW background from wall collapse (using published lattice templates, Eqs. 3.1–3.5) already touching current PTA sensitivity, and di-photon lines from axion–dark-glueball mixing (Eqs. 3.9–3.11) that may be accessible to next-generation MeV telescopes. The scenario prefers a cold dark sector consistent with glueball relic-density bounds.

Significance. If the claimed window is robust, the work supplies a simple, dynamical alternative to higher-dimensional PQ-breaking operators for solving the axion domain-wall problem while remaining compatible with the strong-CP solution. The GW prediction is falsifiable with existing and near-future PTA data (NANOGrav/EPTA already probe the benchmark region; SKA can reconstruct the doubly-broken spectrum), and the di-photon channel offers a complementary, albeit more challenging, probe. The analysis re-uses continuum-extrapolated lattice susceptibilities and published domain-wall GW simulations rather than inventing new non-perturbative inputs, and it cleanly links the solution to cold dark-glueball dark matter. These concrete, multi-messenger predictions constitute a genuine strength even if the precise boundaries of the MeV window require refinement.

major comments (3)
  1. [Sec. II.C, Eqs. (2.9)–(2.12); Figs. 1–2; Sec. III.A] Sec. II.C and Eqs. (2.9)–(2.12) convert the vacuum bias ΔV ∼ χ0 into a collapse temperature Teq via the simple acceleration-balance condition |a| ≃ ΔV/σ ∼ H(Teq). Later, Sec. III.A cites the 3+1 lattice results of Ref. [24] showing that GW emission continues until Hend ≈ 0.1 H(Teq), so the actual collapse occurs at a lower temperature Tend = Cs Teq with Cs ≈ 0.3. This correction is applied only to the GW amplitude (enhancing it by ∼100 while lowering ε to 0.07) and is never fed back into the (Tc, ξ) windows of Figs. 1–2. Because those windows are already only a few MeV wide and sit against the Teq > 1 MeV BBN edge, an O(1) downward shift in Teq can empty the region that simultaneously satisfies both the strong-CP bound (Eq. 2.7) and successful wall collapse. The viable parameter space must be re-mapped with the lattice-calibrated Cs factor before the central claim can be considered contr
  2. [Sec. II.B, Eq. (2.5); Sec. II.C, Eq. (2.10); Fig. 2] For the pre-transition channel the temperature dependence of χ_top(T) is taken from the DIGA form (Eq. 2.5) normalized to the lattice jump χ(Tc+)/χ0 ≈ 0.23 e^{-0.45 Nc}. The text itself notes (Sec. II.B) that DIGA overestimates the dilute-gas density by an order of magnitude even near Tc for Nc = 3, and the exponential e^{-SI} becomes extreme for Nc ≥ 4 and T/Tc ≳ 2. The post-transition channel (preferred for ξ ≪ 1) is less sensitive, yet the paper still presents both channels as viable. An O(1)–O(10) uncertainty in the effective χ_top therefore propagates directly into the claimed 0.1–3 MeV window. A quantitative error band on Figs. 1–2 (or an explicit statement that only the post-transition, lattice-normalized χ0 channel is robust) is required for the balance to be trustworthy.
  3. [Sec. II.C, Eq. (2.7)] The strong-CP bound (Eq. 2.7) is written as χ0/χQCD ≲ 10^{-10}/δ. The text invokes a “reasonably small” δ ∼ 10^{-3} to push Tc up to ∼3 MeV, but never quantifies how natural such a cancellation between Θ and Θd is, nor how the bound degrades for generic O(1) phases. Because the upper edge of the window is set by this bound, the naturalness assumption on δ is load-bearing and should be stated as an explicit free-parameter scan or justified by a symmetry argument.
minor comments (4)
  1. [Abstract; Sec. I] Abstract and Introduction contain several typos (“re-incuring”, “vaccuum”, “midly”, “axiondark-glueball”). A careful proof-read is needed.
  2. [Fig. 1 caption; Sec. II.C] Fig. 1 caption states “0.001 GeV < T_SM_eq < 0.17 GeV” while the text uses 1 MeV; units and numerical thresholds should be made consistent throughout.
  3. [Sec. II.B; Sec. III.B] The relation Λd ≈ 0.5 √σ s and m0 ≈ 6–7 Λd is used without citing the precise lattice sources for general Nc; a short table or explicit references would improve reproducibility.
  4. [Sec. III.A, Eq. (3.4)] Eq. (3.4) and the subsequent GW spectra assume g_*s(Teq) ≈ 20; for Teq near 1 MeV this is only approximate and should be stated with the corresponding uncertainty.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: MeV window and observables derived from external lattice/DIGA inputs plus free-parameter scan, not by construction from the targets.

full rationale

The load-bearing chain (Secs. II.B–C) starts from the mixed-anomaly dark cosine potential Vd = −χ0 cos(𝒜d θeff + δ), takes χ0 ≃ A0 Tc^4 and the DIGA form χtop(T) (Eq. 2.5) from continuum-extrapolated pure-YM lattice results of independent groups, then imposes the external strong-CP bound |NDW ⟨θeff⟩| ≲ 10^{-10} (Eq. 2.7) against the acceleration-balance collapse criterion ΔV ∼ H(Teq)σ that yields Teq > 1 MeV (Eqs. 2.9–2.12). Free parameters Tc, ξ, fa, NDW are scanned; the resulting window and the GW peak (Eq. 3.4) / glueball lifetime (Eq. 3.11) are therefore predictions, not tautologies. Self-citations ([17], [18], [33]) supply only ancillary technical statements (undetectable dark-PT GWs, UV freeze-in for small ξ) that are not required to close the central argument. No equation reduces a claimed observable to a quantity defined by the same data, and no uniqueness theorem or ansatz is imported from the authors’ prior work as an external fact. The derivation is therefore self-contained against external benchmarks.

Assumptions & free parameters 7 free parameters · 4 assumptions · 2 invented entities

The central claim rests on the standard PQ anomaly structure, lattice-normalized topological susceptibilities of pure Yang-Mills, the dilute-instanton-gas temperature dependence above Tc, and the usual domain-wall tension and collapse estimates. Free parameters (Tc, xi, fa, NDW, Ad, δ, Nc) are scanned; the only new entity is the dark SU(Nc) sector itself, introduced solely to generate the bias potential.

free parameters (7)
  • Tc (dark critical temperature)
    Scanned in 0.1–3 MeV window; sets both the bias strength and the glueball mass scale.
  • xi = Td / TSM
    Temperature ratio of the dark sector; must be ≲ 0.01–0.5 to open the post-transition collapse window and satisfy glueball relic density.
  • fa (axion decay constant)
    Free within the usual 10^9–10^12 GeV range; controls wall tension and GW amplitude.
  • NDW (domain-wall number)
    Integer set by the visible color anomaly; scanned (e.g., 5) to illustrate spectra.
  • Ad (dark anomaly coefficient)
    Integer controlling the dark cosine potential; assumed non-integer multiple of NDW so that ΔV ≠ 0.
  • δ (relative dark θ phase)
    Can be O(10^{-3}) to mildly relax the upper bound on Tc; treated as free.
  • Nc (dark colors)
    Integer (2 or 4 shown); enters the DIGA exponent and the jump in χ_top.
assumptions (4)
  • domain assumption The mixed U(1)_PQ–SU(3)_c anomaly coefficient A3 is an integer, so the low-energy axion potential is Z_NDW-symmetric with NDW = |A3|.
    Standard result used in Sec. II.A to define the domain-wall problem (Eq. 2.1).
  • domain assumption Zero-temperature topological susceptibility of pure Yang-Mills is χ0 ≃ A0 Tc^4 with A0 ≈ 0.2, and above Tc it follows the DIGA form with n_YM = 11 Nc/3 − 4 and a jump factor ∼ 0.23 e^{-0.45 Nc}.
    Taken from continuum-extrapolated lattice data (Refs. [12,14]) and used throughout Sec. II.B–C to compute the bias and collapse temperature.
  • domain assumption Domain-wall tension σ ≃ 9 NDW χ_QCD^{1/2} fa and collapse occurs when ΔV ∼ H(Teq) σ.
    Standard estimates (Refs. [10,16,21]) employed to derive Teq (Eqs. 2.9–2.12).
  • domain assumption Dark glueball relic density is given by the 3→2 freeze-out formula Ω h^2 ≃ (g_d*s ξ^3 / g*s) Tf / 3.6 eV with Tf ∼ Λd.
    Used in Sec. III.B (Eq. 3.8) to argue that ξ ≲ 10^{-2} is required.
invented entities (2)
  • Hidden SU(Nc) dark QCD sector with mixed U(1)_PQ anomaly
    purpose: Generates the extra cosine potential that explicitly breaks Z_NDW and supplies the vacuum bias ΔV ∼ χ0.
    Introduced in Sec. II.B; no independent experimental evidence is claimed beyond the GW and di-photon signatures derived inside the paper.
  • Dark glueballs (0++ and 0−+) as possible dark-matter components
    purpose: Provide the MeV-scale states that mix with the axion and can produce di-photon lines; also set the relic-density constraint that favors a cold sector.
    Standard pure-Yang-Mills spectrum, but their cosmological role and axion mixing are specific to this construction (Sec. III.B).

how reviews work

0 comments
Cite this review

Pith. "Pith review of A MeV-Scale Dark QCD Solution to the Axion Domain Wall Problem." pith.science (2026). https://pith.science/paper/CRQ6HZGC

@misc{pith2026260704137,
  author       = {Pith},
  title        = {Pith review of: A MeV-Scale Dark QCD Solution to the Axion Domain Wall Problem},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/CRQ6HZGC}},
  note         = {Machine review of arXiv:2607.04137}
}
abstract

PQ solution to the strong CP problem probably encounters the axion domain wall problem. In this article, we propose a simple and testable solution, assuming that the $U(1)_{\rm PQ}$ possesses mixed anomaly to a hidden $SU(N_c)$ color. Then, the axion field receives a new cosine potential from the hidden instantons, which breaks the $Z_{N_{\rm DW}}$ subgroup explicitly. The new potential lifts the vacua degeneracy, but also drives the effective $\theta$ angle away from the origin, re-incuring the strong CP problem. However, we find that the dark QCD scale within the 0.1 to 3 MeV window survives, maintaining a delicate balance. Two observational signatures are explored: gravitational waves from domain wall collapse, already probed by current PTAs, and di-photon signals from axion-dark-glueball mixing, which require next-generation MeV telescopes. The scenario favors a cold dark QCD sector consistent with dark glueball relic constraints.

Figures

Figures reproduced from arXiv: 2607.04137 by the authors.

Figure 1
Figure 1. FIG. 1: The wall-collapse temperature [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2: The wall-collapse temperature [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3: Gravitational-wave spectra from axion domain wall collapse as functions of [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

41 extracted references

  1. [24]

    The spectrum of gravitational waves from annihilating domain walls

    Alessio Notari, Fabrizio Rompineve, and Francisco Torrenti. The spectrum of gravitational waves from annihilating domain walls. JCAP, 07:049, 2025

    2025

  2. [1]

    R. D. Peccei and Helen R. Quinn. CP Conservation in the Presence of Instantons. Phys. Rev. Lett., 38:1440–1443, 1977. 13

    1977

  3. [2]

    R. D. Peccei and Helen R. Quinn. Constraints Imposed by CP Conservation in the Presence of Instan- tons. Phys. Rev. D, 16:1791–1797, 1977

    1977

  4. [3]

    P. Sikivie. Of Axions, Domain Walls and the Early Universe. Phys. Rev. Lett., 48:1156–1159, 1982

    1982

  5. [4]

    P. Sikivie. Of axions, domain walls and the new inflationary universe. Phys. Rev. D, 32:776–788, 1985

    1985

  6. [5]

    Beyer and Subir Sarkar

    Konstantin A. Beyer and Subir Sarkar. Ruling out light axions: The writing is on the wall. SciPost Phys., 15:003, 2023

    2023

  7. [6]

    Jihn E. Kim. Weak interaction singlet and strong cp invariance. Phys. Rev. Lett., 43:103, 1979

    1979

  8. [7]

    M. A. Shifman, A. I. Vainshtein, and V . I. Zakharov. Can confinement ensure natural cp invariance of strong interactions? Nucl. Phys. B, 166:493–506, 1980

    1980

Show all 41 references
  1. [8]

    A Simple Solution to the Strong CP Problem with a Harmless Axion

    Michael Dine, Willy Fischler, and Mark Srednicki. A Simple Solution to the Strong CP Problem with a Harmless Axion. Phys. Lett. B, 104:199–202, 1981

    1981

  2. [9]

    A. R. Zhitnitsky. On Possible Suppression of the Axion Hadron Interactions. (In Russian). Sov. J. Nucl. Phys., 31:260, 1980

    1980

  3. [10]

    Studies of the motion and decay of axion walls bounded by strings

    Sanghyeon Chang, Christian Hagmann, and Pierre Sikivie. Studies of the motion and decay of axion walls bounded by strings. Phys. Rev. D, 59:023505, 1999

    1999

  4. [11]

    The high temperature phase transition in SU(N) gauge theories

    Biagio Lucini, Michael Teper, and Urs Wenger. The high temperature phase transition in SU(N) gauge theories. Phys. Lett. B, 545:197–206, 2002

    2002

  5. [12]

    The 𝜃-dependence of the 𝑆𝑈 (𝑁) critical temperature at large 𝑁

    Claudio Bonanno, Massimo D’Elia, and Lorenzo Verzichelli. The 𝜃-dependence of the 𝑆𝑈 (𝑁) critical temperature at large 𝑁. JHEP, 02:156, 2024

    2024

  6. [13]

    Gross, R

    David J. Gross, R. David Pisarski, and Laurence G. Yaffe. Qcd and the finite temperature phase tran- sition. Phys. Rev. D, 25:330, 1982

    1982

  7. [14]

    Topological Susceptibility and QCD at Finite Theta Angle

    Claudio Bonanno, Claudio Bonati, and Massimo D’Elia. Topological Susceptibility and QCD at Finite Theta Angle. 4 2026. Invited chapter for the Encyclopedia of Nuclear Physics

    2026

  8. [15]

    High Quality QCD Axion and the LHC

    Anson Hook, Soubhik Kumar, Zhen Liu, and Raman Sundrum. High Quality QCD Axion and the LHC. Phys. Rev. Lett., 124(22):221801, 2020

    2020

  9. [16]

    Big bang nucleosynthesis and physics beyond the standard model

    Subir Sarkar. Big bang nucleosynthesis and physics beyond the standard model. Rept. Prog. Phys., 59:1493–1610, 1996

    1996

  10. [17]

    Dark confinement-deconfinement phase transition: a roadmap from Polyakov loop models to gravitational waves

    Zhaofeng Kang, Jiang Zhu, and Shinya Matsuzaki. Dark confinement-deconfinement phase transition: a roadmap from Polyakov loop models to gravitational waves. JHEP, 09:060, 2021

    2021

  11. [18]

    Confinement bubble wall velocity via quasiparticle determination

    Zhaofeng Kang and Jiang Zhu. Confinement bubble wall velocity via quasiparticle determination. JHEP, 05:056, 2025

    2025

  12. [19]

    David J. E. Marsh. Axion Cosmology. Physics Reports, 643:1–79, 07 2016

    2016

  13. [20]

    Domain walls in the scaling regime: Equal Time Correlator and Gravitational Waves

    Simone Blasi, Alberto Mariotti, Aäron Rase, and Miguel Vanvlasselaer. Domain walls in the scaling regime: Equal Time Correlator and Gravitational Waves. 11 2025

    2025

  14. [22]

    On the estimation of gravitational wave spectrum from cosmic domain walls

    Takashi Hiramatsu, Masahiro Kawasaki, and Ken’ichi Saikawa. On the estimation of gravitational wave spectrum from cosmic domain walls. JCAP, 02:031, 2014

    2014

  15. [23]

    A review of gravitational waves from cosmic domain walls

    Ken’ichi Saikawa. A review of gravitational waves from cosmic domain walls. Universe, 3(2):40, 2017

    2017

  16. [25]

    The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background

    Gabriella Agazie et al. The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background. Astrophys. J. Lett., 951(1):L8, 2023

    2023

  17. [26]

    Janssen et al

    G. Janssen et al. Gravitational wave astronomy with the SKA. PoS, AASKA14:037, 2015. 14

    2015

  18. [27]

    Glueballs and k-strings in SU(N) gauge theories: Calculations with improved operators

    Biagio Lucini, Michael Teper, and Urs Wenger. Glueballs and k-strings in SU(N) gauge theories: Calculations with improved operators. JHEP, 06:012, 2004

    2004

  19. [28]

    SU(N) gauge theories in 3+1 dimensions: glueball spec- trum, string tensions and topology

    Andreas Athenodorou and Michael Teper. SU(N) gauge theories in 3+1 dimensions: glueball spec- trum, string tensions and topology. JHEP, 12:082, 2021

    2021

  20. [29]

    Carlson, Marie E

    Eric D. Carlson, Marie E. Machacek, and Lawrence J. Hall. Self-interacting dark matter. Astrophys. J., 398:43–52, 1992

    1992

  21. [30]

    Nelson, and Fabian Ruehle

    James Halverson, Brent D. Nelson, and Fabian Ruehle. String theory and the dark glueball problem. Phys. Rev. D, 95(4):043527, 2017

    2017

  22. [31]

    Morrissey, and Kris Sigurdson

    Lindsay Forestell, David E. Morrissey, and Kris Sigurdson. Cosmological Bounds on Non-Abelian Dark Forces. Phys. Rev. D, 97(7):075029, 2018

    2018

  23. [32]

    Glueball dark matter revis- ited

    Pierluca Carenza, Roman Pasechnik, Gustavo Salinas, and Zhi-Wei Wang. Glueball dark matter revis- ited. Phys. Rev. Lett., 129:261302, 2022

    2022

  24. [33]

    Slightly Ultra-violet Freeze-in a Hidden Gluonic Sector

    Zhaofeng Kang. Slightly Ultra-violet Freeze-in a Hidden Gluonic Sector. Phys. Lett. B, 801:135149, 2020

    2020

  25. [34]

    Y. Chen, A. Alexandru, S. J. Dong, T. Draper, I. Horváth, F. X. Lee, K. F. Liu, N. Mathur, C. Morn- ingstar, M. Peardon, S. Tamhankar, B. L. Young, and J. B. Zhang. Glueball spectrum and matrix elements on anisotropic lattices. Phys. Rev. D, 73:014516, 2006

    2006

  26. [35]

    Composite Heavy Axionlike Dark Matter

    Pierluca Carenza, Roman Pasechnik, and Zhi-Wei Wang. Composite Heavy Axionlike Dark Matter. Phys. Rev. Lett., 135(2):021001, 2025

    2025

  27. [36]

    Fischer, D

    S. Fischer, D. Malyshev, L. Ducci, and A. Santangelo. New constraints on decaying dark matter from INTEGRAL/SPI. Mon. Not. Roy. Astron. Soc., 520(4):6322–6334, 2023

    2023

  28. [37]

    Constraints on light decaying dark matter candidates from 16 yr of INTEGRAL/SPI observations

    Francesca Calore, Ariane Dekker, Pasquale Dario Serpico, and Thomas Siegert. Constraints on light decaying dark matter candidates from 16 yr of INTEGRAL/SPI observations. Mon. Not. Roy. Astron. Soc., 520(3):4167–4172, 2023. [Erratum: Mon.Not.Roy.Astron.Soc. 538, 132 (2025)]

    2023

  29. [38]

    Tomsick et al

    John A. Tomsick et al. The Compton Spectrometer and Imager. 8 2019

    2019

  30. [39]

    Dark matter prospects with COSI: ALPs, PBHs and sub-GeV dark matter

    Andrea Caputo, Michela Negro, Marco Regis, and Marco Taoso. Dark matter prospects with COSI: ALPs, PBHs and sub-GeV dark matter. JCAP, 02:006, 2023

    2023

  31. [40]

    All-sky Medium Energy Gamma-ray Observatory eXplorer mission concept

    Regina Caputo et al. All-sky Medium Energy Gamma-ray Observatory eXplorer mission concept. J. Astron. Telesc. Instrum. Syst., 8(4):044003, 2022

    2022

  32. [41]

    Tavani et al

    M. Tavani et al. Science with e-ASTROGAM: A space mission for MeV–GeV gamma-ray astrophysics. JHEAp, 19:1–106, 2018

    2018

  33. [42]

    O’Donnell and Tracy R

    Kayla E. O’Donnell and Tracy R. Slatyer. Constraints on dark matter with future MeV gamma-ray telescopes. Phys. Rev. D, 111(8):083037, 2025. 15

    2025

Pith tools

Reviewed July 11, 2026 · model on record in the stance chip above.