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This paper argues that cosmic-ray-boosted dark matter, analyzed with realistic energy-dependent cross sections, lets LUX-ZEPLIN exclude keV-scale dark matter at cross sections near 10^-40 cm^2 rather than the ~10^-33 cm^2 implied by constan

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Using LZ nuclear recoil data, the authors derive 90% CL exclusion limits on cosmic-ray-boosted sub-GeV dark matter for two U(1)' mediator models, with energy-dependent cross sections improving the lower reach versus constant cross section.

T0 review reviewed 2026-08-05 challenge →

load-bearing objection Solid recast of LZ CRBDM limits; the reader's main worry about the heavy-mediator conversion vanishes once you compute q^2 correctly. the 2 major comments →

arxiv 2509.02301 v1 pith:RHH2VNPD submitted 2025-09-02 hep-ph astro-ph.HE

A congruous approach with realistic cross section towards limiting sub-GeV dark matter from LUX-ZEPLIN

Atanu Guha , Jong-Chul Park This is my paper
classification hep-ph astro-ph.HE
keywords cosmic-ray boosted dark mattersub-GeV dark matterLUX-ZEPLINdark photonU(1)_{B-L}nuclear recoilenergy-dependent cross sectionEarth shielding
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

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 paper argues that the usual shortcut in cosmic-ray-boosted dark matter searches—treating the dark-matter–nucleon cross section as a constant—does not adequately represent what LUX-ZEPLIN data can say about sub-GeV dark matter. Working through two concrete models, a secluded dark photon and a U(1)_{B-L} gauge boson, the authors insert realistic, energy-dependent cross sections into the boosted flux, the LZ nuclear-recoil event rate, and the Earth-crust attenuation calculation. Their headline result is quantitative: at a dark-matter mass of 1 keV and a mediator mass of 1 GeV, the lower bound on the spin-independent cross section moves from about 4x10^-33 cm^2 (constant cross section) to about 6.4x10^-40 cm^2 (dark photon) or 2.5x10^-40 cm^2 (U(1)_{B-L}). If correct, this means sub-GeV dark matter of the kind described is already excluded by LZ over a much wider parameter region than constant-cross-section analyses implied, and energy dependence is not a minor refinement but the dominant effect. The same framework also sets an upper bound from Earth shielding, comparable in both scenarios.

Core claim

Using the LUX-ZEPLIN nuclear-recoil data (2–70 keV window, 5.5-tonne fiducial mass, 60 days, no excess events above background), the paper derives 90% confidence exclusion limits on cosmic-ray-boosted dark matter for the secluded dark-photon and U(1)_{B-L} models. The central move is to replace the energy-independent cross section with the full t-channel, finite-mediator cross section, so limits are set in the coupling plane and then converted to the DM–nucleon spin-independent cross section. At m_chi = 1 keV and m_A' = 1 GeV, the lower exclusion bounds are about 6.4x10^-40 cm^2 (dark photon) and 2.5x10^-40 cm^2 (B-L), versus about 4x10^-33 cm^2 for the constant-cross-section treatment; the

What carries the argument

The carrying device is the energy-dependent differential scattering cross section, whose mediator propagator makes the limits depend on recoil energy. It is fed into the cosmic-ray-boosted flux built from electron, proton, and helium cosmic-ray fluxes, and into the LZ event-rate integral with the LZ efficiency and energy window. The Earth-crust attenuation formula converts energy loss into an upper bound on the coupling. Finally, a heavy-mediator conversion formula, which the paper labels valid only in that regime, turns the coupling bound into the quoted spin-independent cross-section limit.

Load-bearing premise

The headline cross-section limits assume the heavy-mediator conversion formula, which the paper itself flags as valid only when the mediator is much heavier than the momentum transfer; at the quoted 1 GeV mediator mass that condition is not met over the LZ recoil window, and the conversion then depends on a reference momentum that is never specified.

What would settle it

Recompute the exclusion limit for m_chi = 1 keV and m_A' = 1 GeV from the published LZ data using the full momentum-dependent form factor with an explicit choice of reference momentum (for example q_ref = m_A' or q_ref = 100 MeV), instead of the heavy-mediator conversion formula. If the resulting lower bound on the spin-independent cross section moves by an order of magnitude or more, or if different reasonable reference-momentum choices disagree, the central claim that realistic energy dependence pushes the limit to about 10^-40 cm^2 is not quantitatively robust.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

If this is right

  • Sub-GeV (keV-to-GeV) dark matter with these mediator structures is excluded by LZ nuclear-recoil data above the derived cross sections—roughly 10^-40 cm^2 at 1 keV for a 1 GeV mediator—rather than only above about 10^-33 cm^2.
  • Because the lower bound tightens by about seven orders of magnitude when energy dependence is included, constant-cross-section analyses do not provide a conservative envelope; they underestimate the excluded region.
  • The Earth-shielding upper bound is comparable in the energy-dependent and constant scenarios, so the allowed parameter window is bounded above and below.
  • The reach of this method extends to dark-matter masses near 1 keV, well below the roughly 1 GeV threshold of conventional direct searches, though existing beam-dump, collider, and stellar-cooling constraints still restrict the couplings.
  • For mediator masses much heavier than the momentum transfer, the energy-dependent results reduce toward the constant-cross-section limit, making the mediator mass a key dial for future searches.

Where Pith is reading between the lines

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

  • The headline numbers assume the DM–mediator coupling g_chi = 1; rescaling that coupling shifts both the coupling limits and the cross-section bounds, so the specific excluded window is a benchmark rather than a universal ceiling.
  • A consistent treatment at m_A' = 1 GeV—where LZ momentum transfers can exceed the mediator mass—would require choosing the reference momentum q_ref of the paper's normalization equations explicitly; until that choice is made, the quantitative superiority of the energy-dependent limits over the constant scenario is not fully settled.
  • The same machinery can be applied to electron-recoil data and to future detectors; if energy dependence matters this strongly for xenon nuclear recoils, it likely shifts projected sensitivities elsewhere as well.
  • The Earth-shielding upper bound implies that deeply buried detectors cannot probe strongly interacting light dark matter at all—a generic property that would apply to any model predicting large cross sections, not only the two studied here.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. The paper derives 90% CL exclusion limits on sub-GeV dark matter (DM) from LUX-ZEPLIN nuclear-recoil data under the cosmic-ray boosted dark matter (CRBDM) mechanism, using two U(1)' models: a secluded dark photon and U(1)_{B-L}. The authors compute the CRBDM flux from cosmic-ray protons, electrons, and helium, include an approximate Earth-shielding attenuation, and translate LZ's null result into bounds on the mediator–nucleon coupling and then on the DM–nucleon spin-independent cross section. Their central quantitative claim is that energy-dependent, mediator-mediated cross sections improve the lower bound by about seven orders of magnitude compared with the constant-cross-section scenario: for m_chi = 1 keV and m_A' = 1 GeV they quote lower bounds of ~6.4e-40 cm^2 (secluded) and ~2.5e-40 cm^2 (U(1)_{B-L}) versus ~4e-33 cm^2 for the constant-cross-section case. I verified the heavy-mediator condition for the headline mass: with m_N ~ 122 GeV and E_R <= 70 keV, q^2 = 2 m_N E_R <= 0.017 GeV^2, which is two orders of magnitude below m_A'^2 = 1 GeV^2, so Eq. (5.15) is applicable for the quoted numbers and the q_ref ambiguity cancels in that limit.

Significance. If the quoted limits are correct, the paper would substantially strengthen CRBDM constraints for keV-to-GeV DM and would demonstrate that model-dependent energy dependence matters greatly for the interpretation of direct-detection null results. The approach is standard: it recasts published LZ data using an analytic flux calculation, and the heavy-mediator conversion for the headline m_A' = 1 GeV is internally consistent. The main strength is the use of two concrete, physically motivated mediator models rather than a phenomenological constant cross section. The main weaknesses are a lack of clarity in the nuclear-coherence convention between the event-rate formula and the cross-section conversion, and a qualitative criterion for the Earth-shielding upper bound. Neither issue necessarily invalidates the qualitative conclusion, but the quantitative limits in Sec. 6 and Fig. 4 need clarification or recomputation before the result can be accepted as stated.

major comments (2)
  1. [§5.1–5.3, Eqs. (5.5), (5.6), (5.15)] The convention for g_i is inconsistent. In §5.2, g_i is defined as the coupling between the SM nucleon and the mediator, but Eq. (5.5) is written for a xenon nucleus without displaying the coherent enhancement factor (Z^2 for the secluded model, A^2 for U(1)_{B-L}). If Eq. (5.5) is intended to be a DM–nucleus cross section with per-nucleon g_i, then the right-hand side is missing the nuclear coherence factor. If, instead, g_i in Eq. (5.5) is meant to be the effective nuclear coupling, then Eq. (5.15), which converts g_i into a per-nucleon σ_SI, is not correct unless g_i is first divided by Z or A. These two readings lead to quoted σ_SI limits that differ by a factor of Z (secluded) or A (B–L). The manuscript never states which convention is used, and the event-rate formula in Eq. (5.6), the flux in Eq. (4.1), and the cross-section conversion in Eq. (5.15) all depend on this point. Since
  2. [§4.2 and §5.2 (Earth-shielding upper bound)] The upper bound from Earth shielding is defined only by 'the value ... at which the suppression starts' (Sec. 5.2) and 'drops to a significantly lower value' (Sec. 4.2). No quantitative criterion is given, so the dotted upper-edge curves in Fig. 4 are not reproducible from the text. Even if the lower-bound claim is unaffected, the abstract and conclusion present the shielding bound as part of the results. Please replace the qualitative threshold with an operational definition (e.g., attenuation by a stated factor at the minimum recoil energy), or clearly label the upper edge as an approximate band.
minor comments (5)
  1. [Abstract / Sec. 1] The sentence 'Without the mechanism of boosted dark matter, sub-GeV DM particles are cold enough to produce detectable nuclear recoil' appears to say the opposite of what is meant. Sub-GeV DM is generally too light to produce observable nuclear recoils above threshold; please reword.
  2. [Eqs. (5.11)–(5.14)] The reference momentum q_ref is never specified. Although q_ref cancels in the heavy-mediator limit used for the headline m_A'=1 GeV numbers, the paper should state this explicitly so readers do not misinterpret the intermediate formulas.
  3. [§5.2, Eq. (5.9)] The alternative calibration route uses the approximation m_CDM >> m_N with m_CDM = 36 GeV and m_N ~ 122 GeV, which is not satisfied. Since the authors state they do not use this route for the reported limits, this should either be corrected or removed to avoid confusion.
  4. [General] The manuscript does not mention whether the numerical code or tabulated limits will be released. For a paper whose main product is an updated exclusion plot, making the limits available in machine-readable form would increase its value and reproducibility.
  5. [Typos and formatting] There are several typos: 'covert' should be 'convert' in Sec. 5.3, 'a a new' in Sec. 1, 'sub-Ge V' in the title, and the coupling notation in Eq. (4.2) is typeset awkwardly. Please also ensure that all subscripts such as A' are consistently formatted.

Circularity Check

0 steps flagged

No significant circularity: the central LZ limits are computed from external LZ data and standard CR flux inputs; self-citations to [47] are method-level and not load-bearing.

full rationale

The derivation chain is: (i) external CR flux parameterizations [61,63,72,73]; (ii) standard U(1)' t-channel cross sections (Eqs. 3.1–3.3, 4.2); (iii) LZ null observation setting 2.3 events at 90% CL (Sec. 5.1); (iv) coupling limit g_i = (2.3/N_R)^{1/4} (Eq. 5.6); (v) mapping to σ_SI via Eq. 5.15. None of these steps restates its own output: the coupling limit is a direct Poisson rescaling of the LZ non-observation, and the cross-section conversion is a model definition. The heavy-mediator condition for Eq. 5.15 is satisfied for the quoted mA'=1 GeV: with the LZ recoil window ending at E_R=70 keV, q^2 ≤ 2 m_N E_R ≈ 0.017 GeV^2 << m_A'^2, so |F_DM| = 1 and the never-specified q_ref drops out. The constant-cross-section limit is benchmarked against the external LZ CRBDM result [116], so the model-dependent limits are not a renaming of a known result. The self-citations to [47] concern the Earth-attenuation upper bound (Sec. 4.2) and detailed flux maps; [47] was cross-checked against [46], and the attenuation treatment is explicitly built on independent work [112]. The central lower-bound claim therefore does not reduce to a self-citation chain or to a fitted input. The only explicit limitation in the text is that 'Rigorous monte carlo simulation is beyond the scope of this work' (Sec. 4.2), which affects the qualitative upper (attenuation) bound, not the headline lower bound. Consequently no circular step is exhibited.

Axiom & Free-Parameter Ledger

3 free parameters · 6 axioms · 0 invented entities

The central limits rest on the CRBDM flux model, the LZ null-event count, and the model cross sections. The main added assumptions beyond standard CRBDM practice are the heavy-mediator conversion applied at mA' = 1 GeV and the qualitative Earth-shielding criterion; both are author-chosen and only partially specified.

free parameters (3)
  • gχ = 1 = 1
    The DM-mediator coupling is fixed to 1 by hand (Sec. 5.2), and all coupling bounds scale as g_i = (2.3/NR)^{1/4} with gχ = 1; the final σ limits depend on this choice.
  • q_ref
    Reference momentum transfer in the DM form factor definition, Eqs. (5.11)-(5.14); never given a numerical value, which changes the light-mediator σ limits and is needed for reproducibility.
  • Earth-shielding 'suppression starts' threshold
    The upper bound on the cross section is set where the attenuated CRBDM flux 'drops to a significantly lower value' (Sec. 4.2); no quantitative criterion is given, so the upper edge of each exclusion region is not precisely defined.
axioms (6)
  • domain assumption CRBDM flux formula Eq. (4.1) with D_eff = 10 kpc and ρ_local = 0.3 GeV cm^-3
    Sec. 4.1: the boosted DM flux factorizes as an effective diffusion zone times local DM density divided by mχ, times CR fluxes and scattering cross sections.
  • domain assumption Cosmic ray flux parameterizations from Refs. [61,63,72,73]
    Sec. 2: electron, proton, and helium fluxes are taken from published fits; the proton/helium fit parameters are not reproduced in the text.
  • domain assumption LZ null result corresponds to 2.3 events at 90% CL over efficiency-weighted {2,70} keV, 5.5 t, 60 days
    Sec. 5.1: the recast uses the published LZ exposure and zero-background Poisson limit; this is a simplified likelihood treatment.
  • ad hoc to paper Cross section conversion Eq. (5.15) is applied for mA' = 1 GeV despite the 'valid only for heavy mediator' caveat
    Sec. 5.3 defines σ via the heavy-mediator formula, and Sec. 6 quotes headline numbers for mA' = 1 GeV, where q^2 = 2 m_N E_R can exceed mA'^2 over the LZ window.
  • domain assumption Earth crust composition and constant electron density n_e = 8e23 cm^-3 with exponential attenuation Eq. (4.8)
    Sec. 4.2: crust composition from Ref. [113] and electron density from Ref. [39]; a single exponential attenuation approximation replaces a Monte Carlo simulation, which the paper explicitly states is beyond scope.
  • domain assumption Deep inelastic cutoff q_p < 2 GeV for proton-DM scattering
    Eq. (4.7): the maximum momentum transfer for elastic proton scattering is restricted to avoid deep inelastic scattering; a similar explicit cutoff is not given for helium.

reviewed 2026-08-05 · how reviews work

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Cite this review

Pith. "Pith review of A congruous approach with realistic cross section towards limiting sub-GeV dark matter from LUX-ZEPLIN." pith.science (2026). https://pith.science/paper/RHH2VNPD

@misc{pith2026250902301,
  author       = {Pith},
  title        = {Pith review of: A congruous approach with realistic cross section towards limiting sub-GeV dark matter from LUX-ZEPLIN},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/RHH2VNPD}},
  note         = {Machine review of arXiv:2509.02301}
}
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abstract

We present constraints on sub-GeV dark matter (DM) through the mechanism of being boosted by cosmic rays (CRs). We utilize the nuclear recoil data from the LUX-ZEPLIN (LZ) experiment for this purpose. Without the mechanism of boosted dark matter (BDM), sub-GeV DM particles are cold enough to produce detectable nuclear recoil in the LZ experiment above the detector threshold. We choose to work with the leading components of cosmic rays to take into account the boost due to them towards the cold DM. In the present discussion we worked on models consisting of a Dirac fermion $\chi$ with a new $U(1)'$ gauge symmetry and DM particles have non-zero coupling to the nucleons as per the model parameters. Specific examples of the energy dependence of the scattering cross section have been invoked through the secluded dark photon model and $U(1)_{B-L}$ model. Additionally, we present the upper bound on the interaction cross section due to the Earth shielding effect in the light of a systematic analysis of the energy loss by the BDM while traveling to the underground detector through the Earth's crust.

Figures

Figures reproduced from arXiv: 2509.02301 by Atanu Guha, Jong-Chul Park.

Figure 1
Figure 1. Figure 1: Cosmic ray electron, proton and Helium nuclei boosted DM flux for various DM mass and mediator mass considering gχ = 1, eε cos θW = 10−3 (left panel) and gχ = 1, gB−L = 10−3 (right panel). The + and − sign in Eq. (4.6) stand for the scenario where Tχ > 2mi and Tχ < 2mi , respectively. For two different benchmark models, the corresponding coupling schemes used in Eq. (4.2) are defined as • Secluded U(1)′ [… view at source ↗
Figure 2
Figure 2. Figure 2: Exclusion limits at 90% confidence level for gχ = 1, in the coupling vs mχ plane for secluded dark photon model (left) and U(1)B−L model (right) with different values of the mediator mass. Dotted lines with the same color code stands for the upper limit due to the earth shielding effect. In general this expression is dependent on the mass of the mediator. We found that the two different approaches to const… view at source ↗
Figure 3
Figure 3. Figure 3: Exclusion limits at 90% confidence level for gχ = 1, in the coupling vs mA′ plane for secluded dark photon model (left) and U(1)B−L model (right) with different values of the DM mass. Dotted lines with the same color code stands for the upper limit due to the earth shielding effect. In the upper and lower panel we show our results along with the existing limits. Invisible decay denotes the scenario where t… view at source ↗
Figure 4
Figure 4. Figure 4: Exclusion limits at 90% confidence level in the σ SI χ vs mχ plane for secluded dark photon model (left) and U(1)B−L model (right) with different values of the mediator mass. The constant cross section scenario is defined by the consideration of energy independent cross section without any underlying model, dσχn dTχ = σχn T max χ and dσχn dTN = σχn T max N . For comparison we also show the bounds obtained … view at source ↗

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This paper was first reviewed by deepseek-v4-flash on August 5, 2026.