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Prospects for probing dark matter particles and primordial black holes with the Hongmeng mission using the 21 cm global spectrum at cosmic dawn

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Pith's one-line read This paper forecasts that the Hongmeng lunar-orbit 21 cm global spectrum, under ideal observing conditions, can detect dark-matter annihilation, decay, and primordial black holes at sensitivities roughly two orders of magnitude better…

desk verdict A competent, internally consistent Fisher forecast for Hongmeng, but the headline two-order sensitivity gain rests on an idealized noise model and a deep cosmic-dawn trough that SARAS 3 has put in doubt. read the letter →

arxiv 2412.19257 v3 pith:ZLOTCG5C submitted 2024-12-26 astro-ph.CO astro-ph.HEgr-qchep-ph

Meng-Lin Zhao , Sai Wang , Xin Zhang This is my paper · ORCID
classification astro-ph.COastro-ph.HEgr-qchep-ph
keywords 21cmcosmologycosmicdawndarkmatterannihilationdecayprimordialblackholesHawkingradiationFishermatrixforecastHongmengmission
topics 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

Here the authors assess whether the Hongmeng mission—an upcoming lunar-orbit interferometer that will measure the sky-averaged 21 cm spectrum from cosmic dawn—can reveal dark matter (DM) particles and primordial black holes (PBHs). The physical idea is that DM annihilation, DM decay, and PBH Hawking evaporation deposit exotic energy into the intergalactic medium, heating and ionizing it, and thereby reshaping the 21 cm brightness temperature in a frequency-dependent way. Using a Fisher-matrix forecast built on a fiducial 21 cm signal from a standard semi-numerical simulation, the paper finds that with 1000 hours of integration and negligible foreground residuals Hongmeng could reach annihilation cross-sections of order $10^{-28}\,\mathrm{cm^3\,s^{-1}}$, decay lifetimes of order $10^{28}\,\mathrm{s}$ for 10 GeV DM, and PBH abundances of order $10^{-6}$ for $10^{16}\,\mathrm{g}$ holes. These numbers would improve current constraints by nearly two orders of magnitude and would open windows, such as sub-GeV DM and PBHs above $10^{17}\,\mathrm{g}$, that present experiments cannot reach. The caveat is that the forecast assumes a deep cosmic-dawn absorption trough in the astrophysical model, a feature that only one contested measurement supports.

What carries the argument

The engine of the forecast is a Fisher information matrix evaluated on the sky-averaged 21 cm signal. The observable is the antenna temperature $T_{\rm sky}(\nu)=T_{\rm fg}(\nu)+T_{21}(\nu)$, with a power-law foreground and a diagonal noise covariance whose noise factor $f_{\rm noise}$ combines foreground residuals $\epsilon_0$ and thermal noise $1/(t_{\rm int}B)$; the Fisher matrix marginalizes over six astrophysical parameters describing star formation, photon escape, and X-ray heating. The signal itself comes from solving the coupled ionization and gas-temperature equations with Lyman-$\alpha$ coupling, using a standard 21 cm simulation code, and adding exotic energy-injection terms whose deposition efficiencies are taken from a dedicated early-universe injection code; annihilation and decay spectra come from a particle-physics package and Hawking spectra from a black-hole evaporation package. This machinery converts an assumed noise level into marginalized $1\sigma$ contours for $\langle\sigma v\rangle$, $\tau$, or $f_{\rm PBH}$ while accounting for degeneracies with astrophysics.

What would settle it

Take the same Fisher-matrix code and rerun it with a fiducial 21 cm spectrum consistent with the SARAS 3 upper limits (no deep trough) while keeping Hongmeng's noise model. If the resulting $\langle\sigma v\rangle$, $\tau$, and $f_{\rm PBH}$ sensitivities no longer exceed current bounds by two orders of magnitude, the paper's central quantitative claim is falsified for realistic astrophysics.

Watch

Extended reading notes

Core claim

The discovery claim, stated as the authors state it, is that the Hongmeng 21 cm global spectrum is a powerful future probe for three classes of exotic energy injection. For dark-matter annihilation into $e^+e^-$, the projected $1\sigma$ sensitivity at $m_\chi=10$ GeV reaches $\langle\sigma v\rangle\sim10^{-28}$ cm$^3$ s$^{-1}$; for decay, $\tau\sim10^{28}$ s; and for monochromatic PBHs, $f_{\rm PBH}\simeq10^{-6}$ at $M_{\rm PBH}=10^{16}$ g. In all three cases the reach improves on existing CMB, gamma-ray, cosmic-ray, and neutrino bounds by about two orders of magnitude, and it extends into sub-GeV DM masses and PBH masses above $10^{17}$ g that are currently inaccessible. The authors emphasize that the $e^+e^-$ channel is the most sensitive, and that matching current best constraints requires foreground residual fractions near $10^{-4}$ for annihilation and $10^{-3}$ for decay and PBHs, with integration times of hundreds to a thousand hours.

Load-bearing premise

The forecast assumes a fiducial astrophysical model that produces a deep cosmic-dawn absorption trough of about $-100$ mK; if the real 21 cm signal is weaker or absent, as the SARAS 3 non-detection suggests against the EDGES measurement, all the projected sensitivities weaken, and the paper does not say by how much.

Editorial extensions

If this is right

  • At 1000 hours integration and foreground residual fraction $10^{-4}$ or better, Hongmeng can test the current most-stringent dark-matter annihilation limits near the 10 GeV mass scale.
  • For DM decay, with noise factor near $10^{-9}$ the sensitivity already matches today's tightest bounds; a factor-of-$10^{-13}$ noise reaches lifetimes of $10^{28}$ s and probes sub-GeV masses beyond Fermi-LAT and Voyager.
  • For PBHs, the projected sensitivity reaches $f_{\rm PBH}\simeq10^{-6}$ at $10^{16}$ g, $f_{\rm PBH}\simeq10^{-9}$ at $10^{15}$ g, and extends to masses above $10^{17}$ g that are not constrained by current cosmological observations.
  • The forecast shows only weak degeneracies between the DM/PBH parameters and the six astrophysical parameters, so the mission can simultaneously constrain the cosmic-dawn astrophysics and the particle/PBH physics.
  • The same Fisher machinery with different noise factors can be used to compare Hongmeng's potential with ground-based 21 cm global experiments.

Reading between the lines

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

  • The paper fixes a monochromatic PBH mass function and an s-wave annihilation channel; extending the analysis to extended mass functions or p-wave/velocity-dependent annihilation would likely blur the sharp $f_{\rm PBH}$ and $\langle\sigma v\rangle$ contours, so the quoted reach should be read as an idealized best case.
  • Because the forecast is built on derivatives of $T_{21}$ with respect to parameters, the projected sensitivities scale roughly with the amplitude of the cosmic-dawn trough. If the true global signal is much weaker than the $\sim-100$ mK fiducial feature, as the SARAS 3 non-detection suggests could be the case, the two-orders-of-magnitude claim would degrade correspondingly; the paper does not quan
  • The same Fisher-matrix framework could be reused to compare any proposed lunar or ground-based global 21 cm experiment by plugging in its own $t_{\rm int}$, $B$, $\epsilon_0$, and $f_{\rm sky}$, producing a direct sensitivity ladder across missions.
  • A detection-like deviation in $T_{21}$ would be degenerate in channel: the paper's weak-degeneracy result suggests parameter constraints can separate DM and astrophysics, but it does not provide an explicit criterion for telling DM annihilation, DM decay, and PBH evaporation apart from the shape of the spectrum alone.
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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. The paper assesses the ability of the Hongmeng lunar-orbit mission to constrain dark-matter annihilation, dark-matter decay, and primordial black hole Hawking radiation through measurements of the global 21-cm brightness temperature at cosmic dawn. The 21-cm signal is computed with 21cmFAST, with exotic energy injection handled through PPPC4DMID and DarkHistory for dark matter and BlackHawk for PBHs, and the projected sensitivities are derived from a Fisher-matrix forecast whose noise model includes both thermal noise and foreground residuals. The headline results are 1-sigma sensitivities to <sigma v> ~ 1e-28 cm^3/s and tau ~ 1e28 s for 10 GeV dark matter, and f_PBH ~ 1e-6 for 1e16 g PBHs, under 1000 hours of integration and zero foreground residual, which the authors claim improves current constraints by nearly two orders of magnitude. The fiducial astrophysical model used for the forecast produces a deep cosmic dawn absorption trough around -100 mK.

Significance. If the quoted sensitivities are robust, the forecast would be valuable for mission planning and for comparing a 21-cm global-signature probe with current CMB, gamma-ray, cosmic-ray, and neutrino bounds, particularly for sub-GeV dark matter and for PBHs heavier than about 1e17 g. The paper is technically careful: the Fisher-matrix algebra in Eq. (4.6) follows from the standard Gaussian likelihood, the noise model in Eqs. (4.4)-(4.5) is transparent, the energy-injection calculations use established external codes, and the results are compared with independent observational limits. The main weakness is astrophysical rather than technical: the fiducial model that generates the forecast is in tension with SARAS 3, and the paper does not quantify how the quoted sensitivities depend on that assumption.

major comments (2)
  1. [Sec. 4, Fig. 1] The headline sensitivities are evaluated at the fiducial astrophysical point (t_* = 0.5, a_* = 0.5, a_esc = -0.5, log10 f_* = -1.3, log10 f_esc = -1.0, log10 L_X = 40.0), whose 21-cm spectrum has a trough near -100 mK, even though Sec. 1 notes that SARAS 3 excludes the EDGES-like profile at 95.3% confidence. Because Eq. (4.6) contains only local derivatives of log T_sky with respect to the model parameters, the projected constraints on <sigma v>, tau, and f_PBH will degrade if the true cosmic dawn signal is shallower or absent. The paper does not provide a forecast for a fiducial model consistent with SARAS 3, nor any scaling of the projected sensitivity with the amplitude or spectral shape of the 21-cm signal. I request such a robustness analysis, or at minimum an explicit statement that the quoted improvement applies only to the adopted fiducial astrophysics.
  2. [Secs. 5.1-5.2, Figs. 3, 5, 7] The projected Hongmeng curves are 1-sigma uncertainties, while the comparison limits from Planck, Fermi-LAT, Voyager-1, Super-Kamiokande, and the extragalactic photon experiments are 2-sigma upper limits. Plotting these on the same axes without converting to a common confidence level makes the 'improvement by nearly two orders of magnitude' claim appear stronger than a like-for-like comparison. Please convert the projected sensitivities to 2-sigma, or the existing limits to 1-sigma, or explicitly state the confidence-level mismatch in the text and figure captions.
minor comments (5)
  1. [Sec. 5.1] The sentence after Fig. 3 contains a duplicated clause: 'From eq. (4.5), we find that for the red dashed curve that for the red dashed curve, a foreground residual ...' should be edited.
  2. [Fig. 1] The body text quotes the 600-second noise factor as 1.6 x 10^-9, while the embedded figure label shows 1.7 x 10^-9; these values should be made consistent.
  3. [Figs. 3 and 5 captions] The Voyager-1 electron-positron constraint is cited as Refs. [69,70] in the body text but as Refs. [71,72] in the figure captions; please unify the references.
  4. [Sec. 5.2] The phrase 'According eq. (4.5)' is missing 'to', and later in the same section 'contribute equally tothe total error' should read 'to the total error'.
  5. [Sec. 4, Eq. (4.7)] The parameter vector lists '<sigma v> or Gamma or f_PBH', and each Fisher forecast treats only one exotic parameter at a time; it would be helpful to state explicitly that simultaneous constraints on two exotic parameters are not attempted and could differ due to degeneracies between them.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the Hongmeng sensitivity forecasts are Fisher-matrix projections built on external simulation tools and independent comparison limits, with no fitted target parameters and no load-bearing self-citation chain.

full rationale

The paper's central claim is a projected sensitivity, not a measurement: the Fisher-matrix forecast (Eq. 4.6) evaluates derivatives of the modeled 21 cm brightness temperature with respect to DM/PBH and astrophysical parameters at a stated fiducial model produced with 21cmFAST and DarkHistory. None of the target parameters (⟨σv⟩, τ, f_PBH) are fitted to data; they are scanned in the forecast, and the resulting sensitivity curves are compared against independent external limits from Planck, Fermi-LAT, H.E.S.S., Voyager-1, Super-Kamiokande, and related observations. The paper explicitly flags its main limitations: the cosmic-dawn trough in its fiducial model is of the kind SARAS 3 has contradicted (Sec. 1), and foreground residuals, which the paper itself notes typically reach ϵ0 ~ 0.01 rather than the ideal 10^-3-10^-4 needed for the best sensitivities, introduce biases that are deferred to future work (Sec. 6). These are model-dependence and observational-tension caveats, not circular derivations. Self-citations such as Refs. [31], [62], and [81] appear as background references or as entries in the comparison data; they do not supply the load-bearing step that converts inputs into the forecast, and no uniqueness theorem or prior ansatz by the same authors is invoked to force the result. Therefore no step in the derivation reduces, by the paper's own equations or by self-citation, to its own inputs.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The forecast rests on a fiducial astrophysical model from 21cmFAST, a specific foreground model with residual fractions, and the reliability of external simulation tools (DarkHistory, PPPC4DMID, BlackHawk). The strongest assumptions are that the cosmic dawn 21 cm signal is well described by the fiducial model and that foreground contamination can be controlled at the 10^-3 level or better. These are domain assumptions rather than fitted parameters, but they are load-bearing for the headline sensitivity.

free parameters (3)
  • Fiducial astrophysical parameters (t*, a*, aesc, log10 f*, log10 fesc, log10 LX) = (0.5, 0.5, -0.5, -1.3, -1.0, 40.0)
    Chosen by hand following 21cmFAST conventions; they set the amplitude and shape of the cosmic dawn 21 cm absorption signal, which directly sets the sensitivity to DM/PBH energy injection.
  • Foreground residual fraction epsilon_0 = 0 (optimistic), 1e-4, 1e-3, 0.1 (conservative)
    Scenario parameter chosen by hand; the headline two-orders-of-magnitude improvement requires epsilon_0 = 0, while Section 6 notes current foreground subtraction achieves ~0.01.
  • Sky coverage f_sky and foreground angular resolution theta_fg = f_sky = 0.8, theta_fg = 5 deg
    Fixed by hand following Ref. [59]; appears in the noise factor and modestly affects the forecast.
assumptions (5)
  • domain assumption The fiducial 21cmFAST astrophysical model accurately represents the cosmic dawn 21 cm global signal.
    The projected sensitivity scales with the amplitude of the absorption trough; no validation exists because the only claimed detection (EDGES) is disputed by SARAS 3 (Section 1).
  • domain assumption Foreground emission is a power law with fixed amplitude and slope, with uncertainty captured only by a residual fraction epsilon_0 and no marginalization over foreground spectral parameters.
    Used in Eq. (4.3) and the Fisher matrix; in practice foreground spectral shape is uncertain and would enlarge parameter errors.
  • standard math Fisher matrix Gaussian approximation with diagonal covariance in frequency bins is adequate for forecasting.
    Standard in the 21 cm forecasting literature (Refs. [57-59]); the Gaussian approximation can overestimate sensitivity for low signal-to-noise.
  • domain assumption Deposition efficiencies from DarkHistory and particle spectra from PPPC4DMID/PYTHIA/BlackHawk are reliable.
    Central to the energy injection calculation (Section 2); these tools have their own uncertainties but are community standards.
  • domain assumption A monochromatic PBH mass function is assumed.
    Section 2.2; extended mass functions would alter the mapping from f_PBH to Hawking radiation signal.

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Pith. "Pith review of Prospects for probing dark matter particles and primordial black holes with the Hongmeng mission using the 21 cm global spectrum at cosmic dawn." pith.science (2026). https://pith.science/paper/ZLOTCG5C

@misc{pith2026241219257,
  author       = {Pith},
  title        = {Pith review of: Prospects for probing dark matter particles and primordial black holes with the Hongmeng mission using the 21 cm global spectrum at cosmic dawn},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZLOTCG5C}},
  note         = {Machine review of arXiv:2412.19257}
}
abstract

Probing dark matter particles and primordial black holes remains a pivotal challenge in modern cosmology. Exotic energy injections from dark matter annihilation, decay, and PBH Hawking evaporation can alter the thermal and ionization histories of the early universe, leaving distinctive imprints on the 21 cm global spectrum. We assess the potential of the upcoming space project, the Hongmeng mission, to probe dark matter particles and PBHs using the 21 cm global spectrum. Under ideal conditions with 1000 hours of integration time and negligible foreground residuals, the Hongmeng project can reach sensitivities to dark matter annihilation cross sections and decay lifetimes to $\langle \sigma v \rangle \sim 10^{-28}\,\mathrm{cm^3\,s^{-1}}$ and $\tau \sim 10^{28}\,\mathrm{s}$, respectively, for dark matter particles with a mass of $10\,\mathrm{GeV}$. It can also probe PBHs with masses of $10^{16}\,\mathrm{g}$ and abundances as low as $f_{\mathrm{PBH}} \simeq 10^{-6}$. These results indicate that the Hongmeng mission can improve current constraints on dark matter annihilation, decay, and PBH Hawking radiation by nearly two orders of magnitude. Moreover, the Hongmeng mission surpasses current limits on sub-GeV dark matter probing and enables the probing of Hawking radiation from PBHs with masses above $10^{17}\,\mathrm{g}$, which remain undetectable through conventional cosmological means. Overall, the upcoming Hongmeng project holds great promise for advancing the investigation of both dark matter and PBHs, potentially deepening our understanding of the nature of dark matter.

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