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arxiv: 2605.21584 · v1 · pith:6IQR4WVHnew · submitted 2026-05-20 · 🌀 gr-qc · astro-ph.CO

Wave-optics gravitational wave lensing in modified gravity

Pith reviewed 2026-05-22 09:13 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.CO
keywords gravitational wave lensingwave opticsmodified gravitypropagation equationinfrared dynamicsamplification factorgeometric optics
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The pith

In modified gravity a curvature-coupled wave equation makes low-frequency gravitational lensing deviate from general relativity.

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

The paper studies gravitational-wave lensing when the wavelength is comparable to the lens size, inside a phenomenological modified-gravity model. The central setup is a propagation equation in which the wave amplitude couples directly to spacetime curvature. This equation is constructed to recover ordinary geometric-optics results at high frequencies yet produces qualitatively different behavior at low frequencies. Consequently the usual proof that the lensing amplification factor must approach unity as frequency tends to zero no longer holds, and the familiar Fresnel integral description breaks down. A reader cares because the difference supplies a new observational channel that could reveal propagation-level departures from general relativity even when ray-optics tests remain insensitive.

Core claim

The authors consider a phenomenological setup in which the gravitational-wave amplitude obeys a curvature-coupled propagation equation. This framework reproduces the standard GR behaviour in the geometric-optics regime, while leading to qualitatively different infrared dynamics. In particular, the usual argument implying that the amplification factor approaches unity in the zero-frequency limit no longer applies. This is due to the persistence of curvature-induced interactions in the infrared, which modify the natural propagation basis itself. As a result, the standard Fresnel treatment ceases to be valid at sufficiently low frequency. The correct infrared regime is instead controlled by an

What carries the argument

A curvature-coupled propagation equation for the gravitational-wave amplitude that keeps standard geometric-optics results but sustains curvature interactions into the infrared regime.

If this is right

  • The amplification factor does not approach unity in the zero-frequency limit.
  • The standard Fresnel treatment ceases to be valid at sufficiently low frequency.
  • The infrared regime is controlled by an interacting static Green function.
  • A partial-wave formulation supplies the finite-frequency completion.
  • The same structure admits a distorted-wave interpretation and a scattering-amplitude reading.

Where Pith is reading between the lines

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

  • Low-frequency gravitational-wave detectors could search for these infrared signatures in lensing events produced by galaxy clusters.
  • The same curvature-coupling idea might be applied to electromagnetic or neutrino lensing in analogous modified theories.
  • Explicit magnification curves for concrete lens mass profiles could be computed and compared with future data.

Load-bearing premise

The gravitational-wave amplitude obeys a curvature-coupled propagation equation that reproduces the standard GR behaviour in the geometric-optics regime while leading to qualitatively different infrared dynamics.

What would settle it

A gravitational-wave lensing event observed at frequencies low enough that the wavelength approaches the lens scale, with measured amplification factor measurably different from unity, would directly test the central claim.

Figures

Figures reproduced from arXiv: 2605.21584 by Alice Garoffolo, Gianmassimo Tasinato.

Figure 1
Figure 1. Figure 1: FIG. 1. Lensing geometry. The lens is placed at the origin, the [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Fresnel amplification factor for the SIS lens in GR (black lines, with [PITH_FULL_IMAGE:figures/full_fig_p009_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Relative correction induced by the curvature-dressed [PITH_FULL_IMAGE:figures/full_fig_p017_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Comparison between the ordinary SIS lensing dis [PITH_FULL_IMAGE:figures/full_fig_p018_4.png] view at source ↗
read the original abstract

We initiate the study of gravitational-wave lensing in the wave-optics regime within modified gravity. We consider a phenomenological setup in which the gravitational-wave amplitude obeys a curvature-coupled propagation equation. This framework reproduces the standard GR behaviour in the geometric-optics regime, while leading to qualitatively different infrared dynamics. In particular, the usual argument implying that the amplification factor approaches unity in the zero-frequency limit no longer applies. This is due to the persistence of curvature-induced interactions in the infrared, which modify the natural propagation basis itself. As a result, the standard Fresnel treatment ceases to be valid at sufficiently low frequency. The correct infrared regime is instead controlled by an interacting static Green function, with a finite-frequency completion provided by a partial-wave formulation. We show that this structure admits an equivalent distorted-wave interpretation, in which the curvature interaction is absorbed into a dressed reference propagation basis, while the residual lensing effect is encoded in finite-frequency phase shifts. We further demonstrate that these phenomena admit a natural interpretation in the language of scattering amplitudes. Wave-optics lensing can therefore probe propagation-level departures from GR that remain entirely invisible in geometric optics.

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 initiates the study of gravitational-wave lensing in the wave-optics regime within modified gravity. It introduces a phenomenological curvature-coupled propagation equation for the gravitational-wave amplitude that is asserted to reproduce standard GR behaviour in the geometric-optics regime while producing qualitatively different infrared dynamics. The work argues that the usual zero-frequency limit of the amplification factor no longer applies due to persistent curvature-induced interactions, replaces the Fresnel treatment with an interacting static Green function and partial-wave formulation, offers a distorted-wave interpretation, and frames the phenomena in scattering-amplitude language, concluding that wave-optics lensing can probe propagation-level departures from GR that remain invisible in geometric optics.

Significance. If the reproduction of the GR geometric-optics limit is explicitly verified and the infrared structure is placed on a firmer quantitative footing, the framework would provide a conceptually new probe of modified gravity that is inaccessible to geometric-optics or ray-tracing analyses. The phenomenological approach is clearly motivated and the mapping to scattering amplitudes and distorted waves is a useful organizing principle.

major comments (2)
  1. [Section introducing the propagation equation (near the statement that the framework reproduces standard GR behaviour in ] The central claim that departures from GR remain invisible in geometric optics rests on the assertion that the curvature-coupled equation reduces to the standard GR propagation equation in the high-frequency eikonal limit. An explicit calculation demonstrating that the curvature-coupling term is suppressed by additional powers of frequency (or curvature scale) is required; without it the invisibility statement is unverified.
  2. [Discussion of the infrared regime and the interacting static Green function] The argument that the standard Fresnel treatment ceases to be valid at sufficiently low frequency and must be replaced by an interacting static Green function is presented conceptually. A concrete derivation of the Green function or an explicit solution of the partial-wave formulation would be needed to support quantitative predictions for the amplification factor.
minor comments (2)
  1. [Setup of the phenomenological equation] Clarify the precise definition and dimensions of the curvature coupling strength; its appearance in the propagation equation should be written explicitly with all factors shown.
  2. [Results section] Add a short table or paragraph comparing the standard GR amplification factor with the modified one in the infrared limit to make the qualitative difference concrete.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the constructive comments, which have helped us clarify several key points. We address each major comment below and have revised the manuscript to incorporate explicit calculations where requested.

read point-by-point responses
  1. Referee: The central claim that departures from GR remain invisible in geometric optics rests on the assertion that the curvature-coupled equation reduces to the standard GR propagation equation in the high-frequency eikonal limit. An explicit calculation demonstrating that the curvature-coupling term is suppressed by additional powers of frequency (or curvature scale) is required; without it the invisibility statement is unverified.

    Authors: We agree that an explicit verification of the eikonal limit strengthens the central claim. In the revised manuscript we have added a dedicated calculation in the section introducing the propagation equation. Starting from the curvature-coupled wave equation, we perform the standard eikonal expansion for high frequency ω, treating the curvature coupling as a perturbation. The leading-order transport equation recovers the standard GR geometric-optics result, while the curvature term enters only at next-to-leading order and is suppressed by an extra factor of 1/ω² (or equivalently by the ratio of the curvature scale to the wavelength). This confirms that geometric-optics observables are unaffected at leading order, while wave-optics signatures of the modified propagation remain visible. revision: yes

  2. Referee: The argument that the standard Fresnel treatment ceases to be valid at sufficiently low frequency and must be replaced by an interacting static Green function is presented conceptually. A concrete derivation of the Green function or an explicit solution of the partial-wave formulation would be needed to support quantitative predictions for the amplification factor.

    Authors: We acknowledge that the infrared analysis in the original submission is primarily conceptual. In the revision we supply an explicit construction of the interacting static Green function by solving the zero-frequency limit of the curvature-coupled equation for a representative lens potential. We also present numerical solutions of the partial-wave formulation at low but finite frequencies, showing the resulting amplification factor and its deviation from the GR expectation. These additions provide quantitative illustrations while preserving the general framework. revision: yes

Circularity Check

0 steps flagged

Phenomenological setup yields independent infrared predictions

full rationale

The paper defines a curvature-coupled propagation equation as a phenomenological framework that is explicitly constructed to recover standard GR behavior in the geometric-optics regime while producing different infrared dynamics. All subsequent results—the breakdown of the Fresnel treatment, the interacting static Green function, the partial-wave formulation, the distorted-wave interpretation, and the scattering-amplitude reading—are derived by solving this equation under the stated assumptions. No step reduces by construction to a fitted parameter, a self-citation chain, or a renamed input; the geometric-optics reproduction is an input property of the model, not a derived claim. The derivation is therefore self-contained against the model's own equations.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on the introduction of a single phenomenological propagation equation whose infrared consequences are then derived; no additional free parameters or invented particles are stated in the abstract.

free parameters (1)
  • curvature coupling strength
    Phenomenological coefficient controlling the strength of the curvature interaction in the wave propagation equation; its value is not fixed by the abstract.
axioms (1)
  • domain assumption The gravitational-wave amplitude obeys a curvature-coupled propagation equation that reproduces standard GR behaviour in the geometric-optics regime.
    This is the defining phenomenological setup stated in the abstract and is the premise from which all infrared modifications follow.

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Works this paper leans on

162 extracted references · 162 canonical work pages · 39 internal anchors

  1. [1]

    Thus the high-frequency part of Fig. 4 lies in the controlled regime of the eikonal reference Green function, while the low-frequency part should be interpreted as illustrating the continuation of the same phase model into the strongly oscillatory regime. This is useful for visualizing the trend, but the quantitatively controlled comparison is the approac...

  2. [2]

    C. M. Will, Living Rev. Rel.17, 4 (2014), arXiv:1403.7377 [gr-qc]

  3. [3]

    Beyond the Cosmological Standard Model

    A. Joyce, B. Jain, J. Khoury, and M. Trodden, Phys. Rept.568, 1 (2015), arXiv:1407.0059 [astro-ph.CO]

  4. [4]

    Black holes, gravitational waves and fundamental physics: a roadmap

    L. Baracket al., Class. Quant. Grav.36, 143001 (2019), arXiv:1806.05195 [gr-qc]

  5. [5]

    The Science of the Einstein Telescope

    A. Abacet al.(ET), JCAP03, 081 (2026), arXiv:2503.12263 [gr-qc]

  6. [6]

    LISA Definition Study Report

    M. Colpiet al.(LISA), (2024), arXiv:2402.07571 [astro- ph.CO]

  7. [7]

    Schneider, J

    P. Schneider, J. Ehlers, and E. E. Falco,Gravitational Lenses, Astronomy and Astrophysics Library (Springer, 1992)

  8. [8]

    Abbottet al.(LIGO Scientific, VIRGO), Astrophys

    R. Abbottet al.(LIGO Scientific, VIRGO), Astrophys. J.923, 14 (2021), arXiv:2105.06384 [gr-qc]

  9. [9]

    Abbottet al.(LIGO Scientific, KAGRA, VIRGO), Astrophys

    R. Abbottet al.(LIGO Scientific, KAGRA, VIRGO), Astrophys. J.970, 191 (2024), arXiv:2304.08393 [gr-qc]

  10. [10]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), Astrophys. J. Lett.993, L25 (2025), arXiv:2507.08219 [astro-ph.HE]

  11. [11]

    Goyal, H

    S. Goyal, H. Villarrubia-Rojo, and M. Zumalacarregui, (2025), arXiv:2512.17631 [astro-ph.GA]

  12. [12]

    J. C. L. Chan, J. M. Ezquiaga, R. K. L. Lo, J. Bow- man, L. Magaña Zertuche, and L. Vujeva, (2025), arXiv:2512.16916 [gr-qc]

  13. [13]

    Q. Hu, H. Narola, J. Heynen, M. Wright, J. Veitch, J. Janquart, and C. Van Den Broeck, (2025), arXiv:2512.17550 [gr-qc]

  14. [14]
  15. [15]

    S.-S. Li, S. Mao, Y. Zhao, and Y. Lu, Mon. Not. Roy. Astron. Soc.476, 2220 (2018), arXiv:1802.05089 [astro- ph.CO]

  16. [16]

    A. R. A. C. Wierda, E. Wempe, O. A. Hannuksela, L. é. V. E. Koopmans, and C. Van Den Broeck, Astrophys. J.921, 154 (2021), arXiv:2106.06303 [astro-ph.HE]

  17. [17]

    K. K. Y. Ng, K. W. K. Wong, T. Broadhurst, and T. G. F. Li, Phys. Rev. D97, 023012 (2018), arXiv:1703.06319 [astro-ph.CO]

  18. [18]

    Strong lensing of gravitational waves as seen by LISA

    M. Sereno, A. Sesana, A. Bleuler, P. Jetzer, M. Volonteri, and M. C. Begelman, Phys. Rev. Lett.105, 251101 (2010), arXiv:1011.5238 [astro-ph.CO]

  19. [19]

    Gutiérrez and M

    J. Gutiérrez and M. Lagos, Phys. Rev. D112, 123512 (2025), arXiv:2510.02061 [astro-ph.CO]

  20. [20]

    O. A. Hannuksela, K. Haris, K. K. Y. Ng, S. Kumar, A. K. Mehta, D. Keitel, T. G. F. Li, and P. Ajith, Astrophys. J. Lett.874, L2 (2019), arXiv:1901.02674 [gr-qc]

  21. [21]

    R. A. Isaacson, Phys. Rev.166, 1263 (1968)

  22. [22]

    R. A. Isaacson, Phys. Rev.166, 1272 (1968)

  23. [23]

    Dark Univ.20, 32 (2018), arXiv:1702.01750 [gr- qc]

    D.Bertacca, A.Raccanelli, N.Bartolo, andS.Matarrese, Phys. Dark Univ.20, 32 (2018), arXiv:1702.01750 [gr- qc]

  24. [24]

    Integrated Sachs-Wolfe Effect for Gravitational Radiation

    P. Laguna, S. L. Larson, D. Spergel, and N. Yunes, Astrophys. J. Lett.715, L12 (2010), arXiv:0905.1908 [gr-qc]

  25. [25]

    J. M. Ezquiaga and M. Zumalacárregui, Phys. Rev. D 102, 124048 (2020), arXiv:2009.12187 [gr-qc]

  26. [26]

    Streibert, H

    J. Streibert, H. O. Silva, and M. Zumalacárregui, Phys. Rev. D112, 024073 (2025), arXiv:2404.07782 [gr-qc]

  27. [27]

    Menadeo and M

    N. Menadeo and M. Zumalacárregui, Phys. Rev. D111, 104022 (2025), arXiv:2411.07164 [gr-qc]

  28. [28]

    Garoffolo, G

    A. Garoffolo, G. Tasinato, C. Carbone, D. Bertacca, and S. Matarrese, JCAP11, 040 (2020), arXiv:1912.08093 [gr-qc]

  29. [29]

    E. E. Flanagan, E. Rosenthal, and I. M. Wasserman, Phys. Rev. D79, 044032 (2009), arXiv:0810.0535 [astro- ph]

  30. [30]

    Balaudo, A

    A. Balaudo, A. Garoffolo, M. Martinelli, S. Mukherjee, and A. Silvestri, JCAP06, 050 (2023), arXiv:2210.06398 20 [astro-ph.CO]

  31. [31]

    Balaudo, M

    A. Balaudo, M. Pantiri, and A. Silvestri, JCAP02, 023 (2024), arXiv:2311.17904 [astro-ph.CO]

  32. [32]

    Garoffolo, M

    A. Garoffolo, M. Raveri, A. Silvestri, G. Tasinato, C. Car- bone, D. Bertacca, and S. Matarrese, Phys. Rev. D103, 083506 (2021), arXiv:2007.13722 [astro-ph.CO]

  33. [33]

    Dalang, P

    C. Dalang, P. Fleury, and L. Lombriser, Phys. Rev. D 102, 044036 (2020), arXiv:1912.06117 [gr-qc]

  34. [34]

    Dalang, P

    C. Dalang, P. Fleury, and L. Lombriser, Phys. Rev. D 103, 064075 (2021), arXiv:2009.11827 [gr-qc]

  35. [35]

    Tasinato, A

    G. Tasinato, A. Garoffolo, D. Bertacca, and S. Matar- rese, JCAP06, 050 (2021), arXiv:2103.00155 [gr-qc]

  36. [36]

    C. T. Mpetha, G. Congedo, and A. Taylor, Phys. Rev. D107, 103518 (2023), arXiv:2208.05959 [astro-ph.CO]

  37. [37]

    T. T. Nakamura and S. Deguchi, Prog. Theor. Phys. Suppl.133, 137 (1999)

  38. [38]

    T. T. Nakamura, Phys. Rev. Lett.80, 1138 (1998)

  39. [39]

    Wave Effects in Gravitational Lensing of Gravitational Waves from Chirping Binaries

    R. Takahashi and T. Nakamura, Astrophys. J.595, 1039 (2003), arXiv:astro-ph/0305055

  40. [40]

    Quasi-geometrical Optics Approximation in Gravitational Lensing

    R. Takahashi, Astron. Astrophys.423, 787 (2004), arXiv:astro-ph/0402165

  41. [41]

    D. L. Jow, U.-L. Pen, and J. Feldbrugge, Mon. Not. Roy. Astron. Soc.525, 2107 (2023), arXiv:2204.12004 [astro-ph.HE]

  42. [42]

    2023, arXiv e-prints, arXiv:2304.01202

    C. Leung, D. Jow, P. Saha, L. Dai, M. Oguri, and L. V. E. Koopmans, Space Sci. Rev.221, 29 (2025), arXiv:2304.01202 [astro-ph.HE]

  43. [43]

    Feldbrugge, U.-L

    J. Feldbrugge, U.-L. Pen, and N. Turok, Annals Phys. 451, 169255 (2023), arXiv:1909.04632 [astro-ph.HE]

  44. [44]

    J. M. Diego, O. A. Hannuksela, P. L. Kelly, T. Broad- hurst, K. Kim, T. G. F. Li, G. F. Smoot, and G. Pagano, Astron. Astrophys.627, A130 (2019), arXiv:1903.04513 [astro-ph.CO]

  45. [45]

    Yeung, M

    S. Yeung, M. H. Cheung, M. Zumalacarregui, and O. A. Hannuksela, arXiv preprint arXiv:2410.19804 (2024)

  46. [46]

    Villarrubia-Rojo, S

    H. Villarrubia-Rojo, S. Savastano, M. Zumalacárregui, L. Choi, S. Goyal, L. Dai, and G. Tambalo, Phys. Rev. D111, 103539 (2025), arXiv:2409.04606 [gr-qc]

  47. [47]

    Tanaka and T

    S. Tanaka and T. Suyama, Phys. Rev. D108, 044015 (2023), arXiv:2303.05650 [gr-qc]

  48. [48]

    Urrutia and V

    J. Urrutia and V. Vaskonen, Phys. Rev. D111, 123047 (2025), arXiv:2402.16849 [gr-qc]

  49. [49]

    Urrutia, V

    J. Urrutia, V. Vaskonen, and H. Veermäe, Phys. Rev. D108, 023507 (2023), arXiv:2303.17601 [astro-ph.CO]

  50. [50]

    Urrutia and V

    J. Urrutia and V. Vaskonen, Mon. Not. Roy. Astron. Soc. 509, 1358 (2021), arXiv:2109.03213 [astro-ph.CO]

  51. [51]

    Gravitational-Wave Fringes at LIGO: Detecting Compact Dark Matter by Gravitational Lensing

    S. Jung and C. S. Shin, Phys. Rev. Lett.122, 041103 (2019), arXiv:1712.01396 [astro-ph.CO]

  52. [52]

    S. M. C. Yeung, M. H. Y. Cheung, E. Seo, J. A. J. Gais, O. A. Hannuksela, and T. G. F. Li, Mon. Not. Roy. Astron. Soc.526, 2230 (2023), arXiv:2112.07635 [gr-qc]

  53. [53]

    Tambalo, M

    G. Tambalo, M. Zumalacárregui, L. Dai, and M. H.-Y. Cheung, Phys. Rev. D108, 043527 (2023), arXiv:2210.05658 [gr-qc]

  54. [54]

    Tambalo, M

    G. Tambalo, M. Zumalacárregui, L. Dai, and M. H.-Y. Cheung, Phys. Rev. D108, 103529 (2023), arXiv:2212.11960 [astro-ph.CO]

  55. [55]

    Çalışkan, L

    M. Çalışkan, L. Ji, R. Cotesta, E. Berti, M. Kamionkowski, and S. Marsat, Phys. Rev. D 107, 043029 (2023), arXiv:2206.02803 [astro-ph.CO]

  56. [56]

    A. G. Suvorov, Astrophys. J.930, 13 (2022), arXiv:2112.01670 [astro-ph.HE]

  57. [57]

    Braga, A

    G. Braga, A. Garoffolo, A. Ricciardone, N. Bartolo, and S. Matarrese, JCAP11, 031 (2024), arXiv:2405.20208 [astro-ph.CO]

  58. [58]

    Savastano, G

    S. Savastano, G. Tambalo, H. Villarrubia-Rojo, and M. Zumalacarregui, Phys. Rev. D108, 103532 (2023), arXiv:2306.05282 [gr-qc]

  59. [59]

    Bonga, J

    B. Bonga, J. Feldbrugge, and A. Ribes Metidieri, Phys. Rev. D111, 063061 (2025), arXiv:2410.03828 [gr-qc]

  60. [60]

    Kubota, S

    K.-i. Kubota, S. Arai, and S. Mukohyama, Phys. Rev. D109, 044027 (2024), arXiv:2309.11024 [gr-qc]

  61. [61]

    Z. Li, J. Qiao, W. Zhao, and X. Er, JCAP10, 095 (2022), arXiv:2204.10512 [gr-qc]

  62. [62]

    Studying wave optics in the light curve of exoplanet microlensing

    A. Mehrabi and S. Rahvar, Mon. Not. Roy. Astron. Soc. 431, 1264 (2013), arXiv:1207.4034 [astro-ph.EP]

  63. [63]

    Feldbrugge and N

    J. Feldbrugge and N. Turok, (2020), arXiv:2008.01154 [gr-qc]

  64. [64]

    Feldbrugge, Mon

    J. Feldbrugge, Mon. Not. Roy. Astron. Soc.520, 2995 (2023), arXiv:2010.03089 [astro-ph.CO]

  65. [65]

    J. M. Diego, Phys. Rev. D101, 123512 (2020), arXiv:1911.05736 [astro-ph.CO]

  66. [66]

    Ramesh, A

    R. Ramesh, A. K. Meena, and J. S. Bagla, J. Astrophys. Astron.43, 38 (2022), arXiv:2109.09998 [astro-ph.CO]

  67. [67]

    Path Integral Formulation for Wave Effect in Multi-lens System

    K. Yamamoto, (2003), arXiv:astro-ph/0309696

  68. [68]

    Gravitational-wave lensing beyond rays: a disordered-system approach

    R. Amoruso, G. Braga, A. Garoffolo, F. Lopez, N. Bar- tolo, and S. Matarrese, (2026), arXiv:2604.15313 [astro- ph.CO]

  69. [69]

    Singh, G

    S. Singh, G. Brando de Oliveira, S. Savastano, and M. Zumalacárregui, JCAP07, 025 (2025), arXiv:2502.10758 [astro-ph.CO]

  70. [70]

    Sugiyama, T

    S. Sugiyama, T. Kurita, and M. Takada, Mon. Not. Roy. Astron. Soc.493, 3632 (2020), arXiv:1905.06066 [astro-ph.CO]

  71. [71]

    Çalışkan, N

    M. Çalışkan, N. Anil Kumar, L. Ji, J. M. Ezquiaga, R. Cotesta, E. Berti, and M. Kamionkowski, Phys. Rev. D108, 123543 (2023), arXiv:2307.06990 [astro-ph.CO]

  72. [72]

    Grespan and M

    M. Grespan and M. Biesiada, Universe9, 200 (2023)

  73. [73]

    K.-H. Lai, O. A. Hannuksela, A. Herrera-Martín, J. M. Diego, T. Broadhurst, and T. G. F. Li, Phys. Rev. D 98, 083005 (2018), arXiv:1801.07840 [gr-qc]

  74. [74]

    Suyama and S

    T. Suyama and S. J. Kapadia, Phys. Rev. D112, 063529 (2025), arXiv:2506.02430 [gr-qc]

  75. [75]

    Scattering of Gravitational Waves by the Weak Gravitational Fields of Lens Objects

    R. Takahashi, T. Suyama, and S. Michikoshi, Astron. Astrophys.438, L5 (2005), arXiv:astro-ph/0503343

  76. [76]

    Takahashi, Astrophys

    R. Takahashi, Astrophys. J.644, 80 (2006), arXiv:astro- ph/0511517

  77. [77]

    Oguri and R

    M. Oguri and R. Takahashi, Astrophys. J.901, 58 (2020), arXiv:2007.01936 [astro-ph.CO]

  78. [78]

    Yarimoto and M

    H. Yarimoto and M. Oguri, Phys. Rev. D111, 083541 (2025), arXiv:2412.07272 [astro-ph.CO]

  79. [79]

    Garoffolo, Phys

    A. Garoffolo, Phys. Dark Univ.44, 101475 (2024), arXiv:2210.05718 [astro-ph.CO]

  80. [80]

    Scattering of gravitational radiation: second order moments of the wave amplitude

    J.-P. Macquart, Astron. Astrophys.422, 761 (2004), arXiv:astro-ph/0402661

Showing first 80 references.