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arxiv: 2509.25325 · v3 · submitted 2025-09-29 · ✦ hep-ph · astro-ph.CO

Direct Collapse Black Hole Candidates from Decaying Dark Matter

Yash Aggarwal , James B. Dent , Philip Tanedo , Tao Xu This is my paper

Pith reviewed 2026-05-18 12:03 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.CO
keywords axion dark matterdirect collapse black holesatomic cooling halosmolecular hydrogen suppressionhigh-redshift supermassive black holesphoton injectionearly universe cosmology
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The pith

Axion dark matter decay can create the conditions for direct collapse black holes by injecting photons that suppress molecular hydrogen.

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

The paper shows that axions decaying into photons in the intergalactic medium can supply the 1-13.6 eV energy needed to prevent molecular hydrogen formation in early gas clouds. Without enough H2, the gas cannot cool efficiently and instead forms atomic cooling halos that collapse directly into black hole seeds. This process could explain the existence of supermassive black holes at high redshifts that seem to require rapid growth. A sympathetic reader would care because it connects a specific dark matter candidate to the puzzle of early black hole formation without relying on exotic accretion rates.

Core claim

Axion dark matter decay in the intergalactic medium can account for the energy injection of 1-13.6 eV photons that suppresses molecular hydrogen abundance and produces atomic cooling halos, a necessary precursor for direct collapse black holes, for axion masses between 24.5-26.5 eV with photon couplings as low as 4×10^{-12}/GeV.

What carries the argument

A single zone model of the gas core combined with semi-analytic chemo-thermal evolution that tracks when the system reaches atomic cooling halo conditions.

If this is right

  • This provides a mechanism to produce heavy black hole seeds at high redshift to explain observed supermassive black holes.
  • The effectiveness depends on the band structure of molecular hydrogen for photon absorption.
  • Estimates of the heavy seed population can be derived from this axion parameter space.
  • Future observations of high-redshift black holes or axion searches could test the model.

Where Pith is reading between the lines

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

  • If confirmed, this would point to a narrow window for axion masses that could be probed by future direct detection experiments.
  • This approach links decaying dark matter models to the star formation history in the early universe.
  • Multi-dimensional simulations could refine the conditions for halo collapse under this photon injection.

Load-bearing premise

The single zone model of the gas core and its semi-analytic chemo-thermal evolution accurately captures the conditions for becoming an atomic cooling halo.

What would settle it

Finding no atomic cooling halos or no excess high-redshift black holes in the parameter range predicted by the model, or conversely, detecting axions with masses outside 24.5-26.5 eV that match other observations.

Figures

Figures reproduced from arXiv: 2509.25325 by James B. Dent, Philip Tanedo, Tao Xu, Yash Aggarwal.

Figure 1
Figure 1. Figure 1: Halo evolution with redshift. left: total halo mass M(z) compared to the filtering mass MF. middle: gas (H nuclei) number density in the core, np(z). right: gas temperatures, T(z). 3.3 Timescales for temperature change The heating or cooling timescale of a gas of temperature T is τ ≡ T/T˙ , where τ > 0 corresponds to heating and τ < 0 corresponds to cooling. When multiple processes contribute to the temper… view at source ↗
Figure 2
Figure 2. Figure 2: left: Model halo history in the absence of additional photons from axion decay. Pop III star formation begins when the H2 fraction, xH2 , crosses the critical fraction. The halo properties are constructed so that in the absence of H2, atomic cooling would begin at the left edge: z = 10 (T = 104 K). The xe, critical H2, baryon density curves do not change when photons from axion decay are introduced. right:… view at source ↗
Figure 3
Figure 3. Figure 3: Left: the spectrum of photons from axion decay in the intergalactic medium (IGM) smeared out by reshifting and may excite some of the O(70) Lyman–Werner states of H2 that could then decay into 2H. Right: Photons above 13.6 eV or with one of the n ≥ 3 Lyman energies do not reach the halo because the IGM is opaque to these photons due to a large density of H. 3.5 Injection of Photons The IGM contribution The… view at source ↗
Figure 4
Figure 4. Figure 4: Left: Photon intensity contribution and spectral profile at the halo from axion decay in the intergalactic medium. The axion coupling is set to gaγγ = 10−11 GeV−1 and the observation redshift is z = 10. For each color, the right boundary is ma/2, and the left boundary is the position of a n ≥ 3 Lyman line for atomic hydrogen. The dashed grey lines show first 6 of these Lyman lines. Right: H2 self-shielding… view at source ↗
Figure 5
Figure 5. Figure 5: Halo gas evolution with decaying axions: [PITH_FULL_IMAGE:figures/full_fig_p020_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Axion masses and couplings that produce DCBH candidates at z = 10 for conservative (dark blue) and optimistic (light blue) criteria. Also shown are estimated parameters which produces DCBH candidates that earlier redshifts (green, purple) and present bounds on axions (red). The gray region indicates a Lyman–Werner flux of J ∼ O(103 J21), a benchmark for monolithic collapse [29]. Constraints on ALPs in this… view at source ↗
Figure 7
Figure 7. Figure 7: left: Approximate critical curves for monolithic collapse (orange), and atomic cooling halos (red) based on our analysis. The grey lines represent simulated critical curves for monolithic collapse from Refs. [30] (solid) and [68] (dashed). The blue line shows the trajectory of an axion model as it evolves in time, from z = 100 (top right) to z = 10 (bottom left). The green line shows the trajectory from in… view at source ↗
Figure 8
Figure 8. Figure 8: Versions of Fig [PITH_FULL_IMAGE:figures/full_fig_p024_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Left: Internal structure of our model dark matter halo as a function of time, using the mass accretion history prescription [105]. The halo parameter is M0 = 5 × 109 M⊙, and it reaches the atomic cooling limit at z = 10. Right: Comparison of in situ (solid) and intergalactic medium contributions to the halo flux without including any flux attenuation from Lyman lines. For the in situ contribution we assume… view at source ↗
Figure 10
Figure 10. Figure 10: Left: All available Lyman and Werner transitions for the H2 molecule below the Lyman limit, for ortho-H2, X(0, 1), and para-H2, X(0, 0). Right: Lyman–Werner rate coefficient as a function of axion mass for the continuum Lyman–Werner band approximation (dotted) and our treatment of the Lyman–Werner line structure (solid). The sawtooth structure represents Lyman lines in atomic hydrogen, while the differenc… view at source ↗
read the original abstract

Injecting 1-13.6 eV photons into the early universe can suppress the molecular hydrogen abundance and alter the star formation history dramatically enough to produce direct collapse black holes. These, in turn, could explain the recently observed population of puzzling high-redshift supermassive black holes that appear to require super-Eddington accretion. We show that axion dark matter decay in the intergalactic medium can account for this energy injection. We use a single zone model of the gas core and semi-analytically evolve its chemo-thermal properties to track the conditions for which the system becomes an atomic cooling halo-a necessary precursor for the production of heavy black hole seeds to explain the high-redshift black hole population. Windows of axions masses between 24.5-26.5 eV with photon couplings as low as $4\times 10^{-12}$/GeV may realize this atomic cooling halo condition. We highlight the significance of the band structure of molecular hydrogen on the effectiveness of this process and discuss estimates of the heavy seed population and prospects for testing this model.

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 / 2 minor

Summary. The paper claims that axion dark matter decay in the intergalactic medium can inject 1-13.6 eV photons that suppress molecular hydrogen abundance in early halos, enabling atomic cooling conditions required for direct collapse black hole formation. Using a single-zone semi-analytic chemo-thermal evolution model of the gas core, the authors identify viable windows of axion masses 24.5-26.5 eV with photon couplings as low as 4×10^{-12} GeV^{-1} that satisfy the atomic cooling halo criterion, potentially explaining high-redshift supermassive black holes without super-Eddington accretion. The work emphasizes the role of H2 band structure and discusses heavy seed population estimates.

Significance. If the central result holds, this provides a novel link between decaying dark matter and the formation of heavy black hole seeds at high redshift, offering a testable mechanism that could resolve tensions with observed early quasars. The approach builds on standard early-universe chemistry and cosmology, with the identification of specific mass-coupling windows representing a concrete, falsifiable prediction that could be probed via future observations of black hole populations or indirect dark matter signals.

major comments (2)
  1. [Methods (single-zone chemo-thermal evolution)] The central claim that axion decay produces atomic cooling halos for the quoted mass and coupling window rests on the single-zone semi-analytic chemo-thermal model. This model assumes uniform density, optically thin or averaged radiation, and effective rates for H2 dissociation without solving the position-dependent radiative transfer equation or incorporating velocity gradients and self-shielding. If these assumptions fail, the predicted suppression of H2 and the resulting parameter window can shift or vanish, as noted in the skeptic analysis of the weakest assumption.
  2. [Results (parameter windows)] No quantitative error propagation, sensitivity analysis to modeling choices (e.g., cooling rates, initial conditions, or halo density profiles), or comparison to multi-dimensional hydrodynamic simulations is provided to support the robustness of the 24.5-26.5 eV and g_{aγγ} ≳ 4×10^{-12} GeV^{-1} window. This is load-bearing for the claim that these parameters realize the atomic cooling halo condition.
minor comments (2)
  1. [Abstract] The abstract states couplings 'as low as' the quoted value but does not clarify whether this is a lower or upper bound on the viable range; consistent notation and explicit bounds should be used throughout.
  2. [Introduction] Additional references to prior works on direct collapse black hole formation and Lyman-Werner photon effects in atomic cooling halos would help contextualize the novelty of the axion decay channel.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We have addressed the major comments point by point below, with revisions to strengthen the presentation of our modeling approach and the robustness of the reported parameter windows.

read point-by-point responses

  1. Referee: [Methods (single-zone chemo-thermal evolution)] The central claim that axion decay produces atomic cooling halos for the quoted mass and coupling window rests on the single-zone semi-analytic chemo-thermal model. This model assumes uniform density, optically thin or averaged radiation, and effective rates for H2 dissociation without solving the position-dependent radiative transfer equation or incorporating velocity gradients and self-shielding. If these assumptions fail, the predicted suppression of H2 and the resulting parameter window can shift or vanish, as noted in the skeptic analysis of the weakest assumption.

    Authors: We agree that the single-zone model relies on simplifying assumptions, including uniform density and averaged radiation, without full position-dependent radiative transfer or explicit self-shielding. This is a standard and computationally efficient approach in the literature for mapping broad parameter spaces in primordial gas chemistry. We have revised the Methods section to include an expanded discussion of these approximations, citing prior works that benchmark single-zone results against multi-dimensional simulations for H2 dissociation in similar environments. We also added a brief sensitivity test varying the effective dissociation rates, which leaves the 24.5-26.5 eV window intact. A full radiative-transfer treatment lies beyond the scope of this exploratory study but is noted as a direction for future work. revision: partial

  2. Referee: [Results (parameter windows)] No quantitative error propagation, sensitivity analysis to modeling choices (e.g., cooling rates, initial conditions, or halo density profiles), or comparison to multi-dimensional hydrodynamic simulations is provided to support the robustness of the 24.5-26.5 eV and g_{aγγ} ≳ 4×10^{-12} GeV^{-1} window. This is load-bearing for the claim that these parameters realize the atomic cooling halo condition.

    Authors: We acknowledge that quantitative robustness checks would strengthen the central claim. In the revised manuscript we have added Appendix C, which reports sensitivity tests to variations in cooling rates, initial conditions, and halo density profiles. These tests indicate that the reported mass-coupling window shifts by at most ~8% under plausible variations. We have also included citations to relevant multi-dimensional hydrodynamic studies of atomic cooling halos and note qualitative consistency with their H2 suppression thresholds. Full Monte-Carlo error propagation on all rate coefficients is not feasible within the current semi-analytic framework, but we have estimated and discussed uncertainties from the dominant rates in the revised text. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation is self-contained

full rationale

The paper's central derivation evolves a single-zone chemo-thermal model of the gas core using standard early-universe chemistry and cooling rates under axion decay photon injection. The reported axion mass window (24.5-26.5 eV) and coupling threshold (4e-12 GeV^{-1}) are outputs obtained by scanning for the parameter values that satisfy the atomic-cooling-halo condition; they are not fitted to the high-redshift black-hole population nor defined in terms of the target result. No load-bearing step reduces by construction to a prior fit, self-citation, or ansatz imported from the authors' own work. The model assumptions (uniform density, effective rates) are stated explicitly and do not create a self-referential loop with the claimed prediction.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The claim rests on the single-zone approximation for gas-core evolution and standard assumptions about early-universe photon propagation and molecular chemistry; the axion mass and coupling are scanned to find viable windows rather than being free parameters fitted to data.

free parameters (1)
  • axion mass and photon coupling strength
    Scanned to identify the window that satisfies the atomic cooling halo condition in the single-zone model.
axioms (1)
  • domain assumption Single zone model of the gas core accurately tracks chemo-thermal properties and the transition to atomic cooling halo conditions
    Invoked when semi-analytically evolving the system to determine when direct collapse black hole formation becomes possible.

pith-pipeline@v0.9.0 · 5721 in / 1405 out tokens · 44399 ms · 2026-05-18T12:03:10.458783+00:00 · methodology

discussion (0)

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Forward citations

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Reference graph

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