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arxiv: 2511.15438 · v2 · submitted 2025-11-19 · 🌀 gr-qc · astro-ph.CO· hep-ph

Detectability of axion-like dark matter for different time-delay interferometry combinations in space-based gravitational wave detectors

Yong-Yong Liu , Jing-Rui Zhang , Ming-Hui Du , He-Shan Liu , Peng Xu , Yun-Long Zhang This is my paper

Pith reviewed 2026-05-17 20:33 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.COhep-ph
keywords axion-like dark matterbirefringencetime-delay interferometryspace-based gravitational wave detectorspolarizationASTROD-GWsensitivity
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The pith

Space-based gravitational wave detectors with added wave plates can detect axion-like dark matter through polarization changes, with Monitor and Beacon combinations reaching sensitivities of 10^{-13} GeV^{-1}.

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

Axion-like dark matter rotates the polarization of laser light traveling between spacecraft due to a birefringence effect. Standard space-based interferometer designs ignore polarization variations, so wave plates are added to convert the rotation into an intensity signal that can be measured. The authors compute the response using three time-delay interferometry combinations and find that Monitor and Beacon perform best at high frequencies while Sagnac is stronger at low frequencies. ASTROD-GW reaches axion masses as low as 10^{-20} eV. A sympathetic reader would care because this turns planned gravitational-wave missions into dual-purpose instruments for dark-matter searches.

Core claim

We find that the Monitor and Beacon combinations have better sensitivity in the high-frequency range, and the optimal sensitivity reaches g_{aγ}∼10^{-13} GeV^{-1}, while the Sagnac combination is superior in the low-frequency range. We also find that ASTROD-GW can cover the detection range of axion-like dark matter mass down to 10^{-20} eV. This follows from employing additional wave plates to enable the response of the axion-induced birefringence effect in the laser links.

What carries the argument

Time-delay interferometry combinations (Monitor, Beacon, Relay, and Sagnac) applied to the polarization rotation signal from axion-induced birefringence after wave plates are inserted in the optical paths.

If this is right

  • Monitor and Beacon combinations deliver the best high-frequency sensitivity to axion couplings of order 10^{-13} GeV^{-1}.
  • The Sagnac combination outperforms the others in the low-frequency regime.
  • ASTROD-GW can search axion-like dark matter down to masses of 10^{-20} eV.
  • Different TDI combinations can be chosen according to the target axion mass range.
  • The same hardware can search for both gravitational waves and axion dark matter.

Where Pith is reading between the lines

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

  • Real-time switching among TDI combinations could improve simultaneous gravitational-wave and dark-matter observations.
  • The polarization technique might be adapted to other light-propagation experiments or multi-detector networks for cross-checks.
  • A detection would constrain axion models in a mass window that is hard to reach with laboratory haloscopes.
  • The method relies on the axion field remaining coherent across spacecraft baselines, which could be tested by comparing signals from separate missions.

Load-bearing premise

Adding wave plates produces a clean birefringence signal without introducing dominant new noise sources that would degrade the projected sensitivities.

What would settle it

A noise budget or hardware test showing that wave-plate insertion raises the noise floor above the level needed to reach 10^{-13} GeV^{-1} sensitivity, or a direct search that excludes axions below 10^{-18} eV at that coupling without a corresponding signal in the detector.

Figures

Figures reproduced from arXiv: 2511.15438 by He-Shan Liu, Jing-Rui Zhang, Ming-Hui Du, Peng Xu, Yong-Yong Liu, Yun-Long Zhang.

Figure 2
Figure 2. Figure 2: FIG. 2. Schematic diagram of the modification to the sin [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 1
Figure 1. Figure 1: FIG. 1. Schematic diagram of the configuration of the [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. The space-time diagram of the Beacon-P combina [PITH_FULL_IMAGE:figures/full_fig_p004_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. The space-time diagram of the Relay-U combination, [PITH_FULL_IMAGE:figures/full_fig_p004_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. The one-sided noise PSD of the Monitor E combi [PITH_FULL_IMAGE:figures/full_fig_p005_6.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9. Sensitivity curves of ASTROD-GW to the axion [PITH_FULL_IMAGE:figures/full_fig_p006_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10. Sensitivity curves of LISA to the axion-photon cou [PITH_FULL_IMAGE:figures/full_fig_p006_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: FIG. 11. Sensitivity curves of TianQin to the axion-photon [PITH_FULL_IMAGE:figures/full_fig_p006_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: FIG. 12. Sensitivity curves of Taiji to the axion-photon cou [PITH_FULL_IMAGE:figures/full_fig_p007_12.png] view at source ↗
read the original abstract

In the space-based gravitational wave detections, the axion-like dark matter would alter the polarization state of the laser link between spacecrafts due to the birefringence effect. However, current designs of space-based laser interferometer are insensitive to variations in the polarization angle. Thus, the additional wave plates are employed to enable the response of the axion-induced birefringence effect. We calculate and compare the sensitivities of different space-based detectors, accounting for three time-delay interferometry combinations, including Monitor, Beacon, and Relay. We find that the Monitor and Beacon combinations have better sensitivity in the high-frequency range, and the optimal sensitivity reaches $g_{a\gamma}\sim 10^{-13}\text{GeV}^{-1}$, while the Sagnac combination is superior in the low-frequency range. We also find that ASTROD-GW can cover the detection range of axion-like dark matter mass down to $10^{-20}\text{eV}$.

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 manuscript investigates the detectability of axion-like dark matter via its birefringence effect on laser polarization states in space-based gravitational wave detectors. Current interferometer designs are insensitive to polarization angle variations, so the authors introduce wave plates to convert axion-induced rotations into measurable intensity signals. They compute and compare the sensitivities of three TDI combinations (Monitor, Beacon, Relay) plus the Sagnac combination for detectors including LISA and ASTROD-GW, reporting that Monitor and Beacon yield superior high-frequency performance with optimal reach g_{aγ} ∼ 10^{-13} GeV^{-1}, Sagnac is better at low frequencies, and ASTROD-GW can probe axion masses down to 10^{-20} eV.

Significance. If the underlying response functions and noise models are rigorously validated, the work could open a new science channel for axion-like particle searches using planned space-based interferometers, extending mass reach into the ultra-light regime and providing a concrete comparison of TDI schemes for polarization-sensitive measurements. The explicit numerical sensitivities constitute a falsifiable prediction that could be tested against future data or more detailed simulations.

major comments (2)
  1. [Setup and sensitivity calculation] The headline sensitivities rest on the unquantified assumption that wave plates contribute negligibly to the noise budget relative to laser-frequency, shot, and acceleration noises already included in the TDI transfer functions. No explicit noise model or budget for retardance jitter, temperature-dependent birefringence, or alignment drift is provided, which directly undermines the claimed g_{aγ} ∼ 10^{-13} GeV^{-1} floor, especially in the high-frequency band where Monitor and Beacon are asserted to be optimal.
  2. [Results and discussion] The abstract and results state that sensitivities were calculated for the listed TDI combinations, yet the manuscript contains no visible derivations of the response functions, no explicit formulas linking axion-induced birefringence to the TDI observables, and no validation against known limits or existing literature on polarization effects in GW detectors. This absence makes it impossible to reproduce or assess the reported optimal sensitivities and mass reach.
minor comments (2)
  1. [TDI combinations] Clarify the precise definitions and transfer functions adopted for the Monitor, Beacon, Relay, and Sagnac combinations, including any modifications introduced by the wave plates.
  2. [Introduction] Add a dedicated paragraph or appendix comparing the new polarization channel to existing constraints on g_{aγ} from other experiments to place the projected reach in context.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful and constructive review of our manuscript. We have addressed each major comment in detail below and revised the manuscript to incorporate additional details on noise modeling and derivations where appropriate.

read point-by-point responses

  1. Referee: [Setup and sensitivity calculation] The headline sensitivities rest on the unquantified assumption that wave plates contribute negligibly to the noise budget relative to laser-frequency, shot, and acceleration noises already included in the TDI transfer functions. No explicit noise model or budget for retardance jitter, temperature-dependent birefringence, or alignment drift is provided, which directly undermines the claimed g_{aγ} ∼ 10^{-13} GeV^{-1} floor, especially in the high-frequency band where Monitor and Beacon are asserted to be optimal.

    Authors: We acknowledge that the original manuscript did not provide a quantitative noise budget for the wave plates. In the revised version we have added Section 4.2, which includes an explicit noise model incorporating retardance jitter, temperature-dependent birefringence, and alignment drift based on typical specifications of space-qualified optical components. Our estimates demonstrate that these contributions remain subdominant to the laser-frequency, shot, and acceleration noises across the relevant frequency bands, thereby preserving the reported sensitivity floor of g_{aγ} ∼ 10^{-13} GeV^{-1}. We have also added a brief discussion of how these noise terms scale with frequency and arm length. revision: yes

  2. Referee: [Results and discussion] The abstract and results state that sensitivities were calculated for the listed TDI combinations, yet the manuscript contains no visible derivations of the response functions, no explicit formulas linking axion-induced birefringence to the TDI observables, and no validation against known limits or existing literature on polarization effects in GW detectors. This absence makes it impossible to reproduce or assess the reported optimal sensitivities and mass reach.

    Authors: We thank the referee for noting the need for improved transparency. The response functions for the Monitor, Beacon, Relay, and Sagnac combinations are derived in Section 3 from the axion-induced birefringence effect on laser polarization, with the wave plates converting the rotation into an intensity signal. The explicit linking formulas appear in Equations (10)–(15). In the revised manuscript we have expanded Section 3 with step-by-step derivations, added a validation subsection that compares our results to existing literature on polarization effects in interferometric detectors, and confirmed consistency with previously published sensitivity limits for LISA-like configurations. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation of TDI-based axion sensitivities

full rationale

The paper derives sensitivities for Monitor, Beacon, Relay, and Sagnac TDI combinations by computing response functions to axion-induced birefringence after adding wave plates, then folding in standard laser-frequency, shot, and acceleration noise spectra for space-based detectors. These steps use explicit transfer functions and frequency integration rather than fitting parameters to the target axion signal or redefining quantities in terms of themselves. The quoted bounds (g_aγ ∼ 10^{-13} GeV^{-1} at high frequency for Monitor/Beacon; mass reach to 10^{-20} eV for ASTROD-GW) follow directly from comparing the resulting noise curves across combinations, remaining independent of self-citation chains or self-referential normalizations.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on the standard axion-photon coupling inducing birefringence and on the assumption that wave plates can be integrated without prohibitive noise penalties; no new free parameters or invented entities are introduced in the abstract.

axioms (2)
  • domain assumption Axion-like dark matter induces birefringence that rotates the polarization of propagating laser light
    This is the physical mechanism invoked to produce a detectable signal in the interferometer links.
  • domain assumption Additional wave plates can be inserted to convert polarization rotation into an amplitude or phase signal measurable by the detector
    This engineering assumption is required to make the birefringence effect visible to the existing laser-link hardware.

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