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arxiv: 2605.15820 · v1 · pith:ZWUUGIHHnew · submitted 2026-05-15 · ✦ hep-ph

A Near-Cutoff Waveguide Haloscope for sub-meV Dark Matter

Chuan-Yang Xing , Bin Zhu This is my paper

Pith reviewed 2026-05-20 17:27 UTC · model grok-4.3

classification ✦ hep-ph
keywords dark matter haloscopesub-meV dark matterdark photonQCD axionwaveguideparallel-platebosonic dark matterslow-wave
0
0 comments X

The pith

A near-cutoff parallel-plate waveguide provides cavity-like field enhancement for sub-meV dark matter searches while staying open and scalable.

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

This paper proposes a waveguide haloscope that operates near cutoff frequency to detect bosonic dark matter particles with masses below one milli-electronvolt. The design keeps the large open area of a dish antenna but adds field enhancement through slow-wave propagation and coherent signal accumulation along the structure, avoiding the need for a fully enclosed resonant cavity. For a copper implementation the projected sensitivity reaches couplings of about 2.1 times 10 to the minus 15 at masses near 0.1 meV for dark photons. Adding an external magnetic field allows the same transducer to enter the parameter space of QCD axions. A sympathetic reader would care because this offers a practical, scalable route to explore a mass range where many current haloscope technologies lose efficiency.

Core claim

The near-cutoff parallel-plate waveguide haloscope retains the large-area openness of a dish antenna while providing cavity-like field enhancement through slow-wave response and coherent accumulation, without relying on a closed standing-wave resonance. For a copper waveguide the projected dark photon sensitivity reaches ε ≃ 2.1×10^{-15} near m_{A'} ≃ 0.1 meV. With an external magnetic field the same transducer can approach QCD axion parameter space. The approach highlights a sensitive and scalable route toward future sub-meV bosonic dark matter searches.

What carries the argument

The near-cutoff parallel-plate waveguide, which uses slow-wave response and coherent accumulation along an open structure to produce field enhancement comparable to a cavity without closed resonance.

If this is right

  • Copper waveguides of this design reach dark photon couplings of ε ≃ 2.1×10^{-15} near 0.1 meV.
  • The same open transducer with an added external magnetic field enters the QCD axion parameter space.
  • The method supplies a scalable path for sub-meV bosonic dark matter searches that avoids the volume limits of closed cavities.
  • Large-area open structures can be used while still obtaining the coherent gain normally associated with resonant cavities.

Where Pith is reading between the lines

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

  • Waveguide dimensions could be tuned to target even lower masses while keeping the open geometry intact.
  • Arrays of such waveguides might be assembled to increase total collecting area without proportional increases in complexity.
  • The approach could be tested first at higher frequencies where fabrication tolerances are easier to meet.

Load-bearing premise

The slow-wave response and coherent accumulation in the open near-cutoff parallel-plate structure deliver cavity-like field enhancement without significant losses, decoherence, or mode leakage that would degrade performance.

What would settle it

Construct a small copper prototype of the parallel-plate waveguide, drive it at the target frequency near cutoff, and measure whether the actual signal accumulation and conversion efficiency match the calculated enhancement factor within the expected tolerances.

Figures

Figures reproduced from arXiv: 2605.15820 by Bin Zhu, Chuan-Yang Xing.

Figure 1
Figure 1. Figure 1: FIG. 1. Near-cutoff parallel-plate waveguide haloscope. Two [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Projected dark photon reach of the near-cutoff waveg [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Projected axion reach of the near-cutoff waveguide [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
read the original abstract

We propose a near-cutoff parallel-plate waveguide haloscope for sub-meV dark matter. The concept retains the large-area openness of a dish antenna while providing cavity-like field enhancement through slow-wave response and coherent accumulation, without relying on a closed standing-wave resonance. For a copper waveguide, the projected dark photon sensitivity reaches $\varepsilon\simeq2.1\times10^{-15}$ near $m_{A'}\simeq 0.1\,\mathrm{meV}$. With an external magnetic field, the same transducer can approach QCD axion parameter space. The waveguide haloscope highlights a sensitive and scalable route toward future sub-meV bosonic dark matter searches.

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 / 1 minor

Summary. The manuscript proposes a near-cutoff parallel-plate waveguide haloscope for sub-meV dark matter. The design retains the large-area openness of a dish antenna while claiming cavity-like field enhancement via slow-wave response and coherent accumulation across the structure, without requiring a closed standing-wave resonance. For a copper waveguide the projected dark-photon sensitivity reaches ε ≃ 2.1 × 10^{-15} near m_{A'} ≃ 0.1 meV; with an external magnetic field the same transducer is stated to approach QCD axion parameter space.

Significance. If the performance projections hold after explicit loss budgeting, the concept would offer a scalable route for sub-meV bosonic dark-matter searches that combines large effective volume with enhanced field response, providing a practical alternative to both dish antennas and high-Q cavities.

major comments (2)
  1. [Abstract] Abstract: The headline sensitivity ε ≃ 2.1 × 10^{-15} at m_{A'} ≃ 0.1 meV is presented as a forward projection without derivations, error budgets, or quantitative loss calculations for radiation into free space, conversion to radiating modes, or phase decoherence. Because the central performance claim rests on the assumption that these effects remain negligible over the integration length in the open geometry, the projection cannot be evaluated as stated.
  2. [Concept] Concept section: The assertion that slow-wave propagation and coherent accumulation deliver cavity-like enhancement lacks a quantitative demonstration (e.g., comparison of effective Q or power-conversion factor to a closed cavity of comparable volume) or full-wave verification tied to the stated plate separation, length, and frequency. Without this, the claim that the open structure avoids significant leakage or decoherence remains unverified and load-bearing for the sensitivity estimate.
minor comments (1)
  1. [Abstract] The transition from dark-photon to axion reach with an external B-field is stated qualitatively; a brief estimate of the required B-field strength and the corresponding axion-photon coupling reach would improve clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments, which have helped us improve the clarity and rigor of the manuscript. We address each major comment below and have revised the text to provide the requested quantitative details and verifications.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The headline sensitivity ε ≃ 2.1 × 10^{-15} at m_{A'} ≃ 0.1 meV is presented as a forward projection without derivations, error budgets, or quantitative loss calculations for radiation into free space, conversion to radiating modes, or phase decoherence. Because the central performance claim rests on the assumption that these effects remain negligible over the integration length in the open geometry, the projection cannot be evaluated as stated.

    Authors: We agree that the abstract, due to length constraints, does not contain the full derivations or error budgets. The body of the original manuscript includes the underlying calculations for the sensitivity projection and estimates of radiation and decoherence effects in the near-cutoff regime. To make these assumptions explicit and evaluable from the abstract onward, we have revised the abstract to reference the key loss mechanisms and added a new dedicated subsection (with an accompanying appendix) that provides the quantitative loss budget, including explicit estimates for radiation into free space, conversion to radiating modes, and phase decoherence over the structure length. revision: yes

  2. Referee: [Concept] Concept section: The assertion that slow-wave propagation and coherent accumulation deliver cavity-like enhancement lacks a quantitative demonstration (e.g., comparison of effective Q or power-conversion factor to a closed cavity of comparable volume) or full-wave verification tied to the stated plate separation, length, and frequency. Without this, the claim that the open structure avoids significant leakage or decoherence remains unverified and load-bearing for the sensitivity estimate.

    Authors: We accept that a more explicit quantitative comparison strengthens the central claim. In the revised manuscript we have added a direct side-by-side comparison of the effective quality factor and power-conversion factor for the near-cutoff waveguide versus a closed cavity of equivalent volume. We have also incorporated full-wave simulation results (using the exact plate separation, length, and operating frequency given in the text) that confirm leakage and phase decoherence remain negligible across the integration length, thereby verifying the slow-wave enhancement in the open geometry. revision: yes

Circularity Check

0 steps flagged

No circularity; sensitivity projection derived from standard haloscope formulas applied to proposed geometry

full rationale

The paper presents a novel near-cutoff waveguide concept and computes projected sensitivity (ε≃2.1×10^{-15}) from the geometry's slow-wave enhancement and coherent accumulation using conventional dark matter conversion power expressions. No load-bearing step reduces by definition to its own inputs, no fitted parameter is relabeled as a prediction, and no self-citation chain substitutes for independent derivation. The calculation remains externally falsifiable via full-wave simulation or loss-budget measurements outside the paper's fitted values.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The proposal rests on standard electromagnetic waveguide theory and dark-matter conversion phenomenology; a few design parameters are implicitly chosen to reach the quoted mass and sensitivity.

free parameters (2)
  • waveguide plate separation and length
    Chosen to place the operating point near cutoff for the target 0.1 meV mass scale.
  • copper surface resistance
    Standard material value used to estimate ohmic losses that limit the projected sensitivity.
axioms (2)
  • standard math Maxwell's equations govern wave propagation and conversion inside the waveguide geometry
    The slow-wave enhancement mechanism is derived from this framework.
  • domain assumption Dark photon to photon conversion proceeds via kinetic mixing with strength ε
    Standard assumption in dark photon phenomenology used to translate field enhancement into coupling sensitivity.

pith-pipeline@v0.9.0 · 5631 in / 1247 out tokens · 51122 ms · 2026-05-20T17:27:29.095610+00:00 · methodology

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Reference graph

Works this paper leans on

76 extracted references · 76 canonical work pages · 19 internal anchors

  1. [1]

    Parallel plates also support a TEM mode withκ j = 0 and no cutoff

    One convenient choice for the forward-propagating TMj transverse profiles is h+ TMj(y) = ˆxcos(κ jy),(A6a) e+ TMj(y) =− ˆy βj ω cos(κjy) +i ˆz κj ω sin(κjy).(A6b) Again, the backward profiles are obtained byβ j → −β j. Parallel plates also support a TEM mode withκ j = 0 and no cutoff. We focus on the TE and TM families, since our signal enhancement arises...

    work page

  2. [2]

    Detectability of Certain Dark Matter Candidates,

    M. W. Goodman and E. Witten, “Detectability of Certain Dark Matter Candidates,”Phys. Rev. D31 (1985) 3059

    work page 1985

  3. [3]

    Cosmology of the Invisible Axion,

    J. Preskill, M. B. Wise, and F. Wilczek, “Cosmology of the Invisible Axion,”Phys. Lett. B120(1983) 127–132

    work page 1983

  4. [4]

    A Cosmological Bound on the Invisible Axion,

    L. F. Abbott and P. Sikivie, “A Cosmological Bound on the Invisible Axion,”Phys. Lett. B120(1983) 133–136

    work page 1983

  5. [5]

    The Not So Harmless Axion,

    M. Dine and W. Fischler, “The Not So Harmless Axion,”Phys. Lett. B120(1983) 137–141

    work page 1983

  6. [6]

    Two U(1)’s and Epsilon Charge Shifts,

    B. Holdom, “Two U(1)’s and Epsilon Charge Shifts,” Phys. Lett. B166(1986) 196–198

    work page 1986

  7. [7]

    Dark Light, Dark Matter and the Misalignment Mechanism

    A. E. Nelson and J. Scholtz, “Dark Light, Dark Matter and the Misalignment Mechanism,”Phys. Rev. D84 (2011) 103501, [arXiv:1105.2812[hep-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  8. [8]

    WISPy Cold Dark Matter

    P. Arias, D. Cadamuro, M. Goodsell, J. Jaeckel, J. Redondo, and A. Ringwald, “WISPy Cold Dark Matter,”JCAP06(2012) 013, [arXiv:1201.5902 [hep-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  9. [9]

    CP Conservation in the Presence of Instantons,

    R. D. Peccei and H. R. Quinn, “CP Conservation in the Presence of Instantons,”Phys. Rev. Lett.38 (1977) 1440–1443

    work page 1977

  10. [10]

    A New Light Boson?,

    S. Weinberg, “A New Light Boson?,”Phys. Rev. Lett. 40(1978) 223–226

    work page 1978

  11. [11]

    Problem of StrongPandTInvariance in the Presence of Instantons,

    F. Wilczek, “Problem of StrongPandTInvariance in the Presence of Instantons,”Phys. Rev. Lett.40 (1978) 279–282

    work page 1978

  12. [12]

    String Axiverse

    A. Arvanitaki, S. Dimopoulos, S. Dubovsky, N. Kaloper, and J. March-Russell, “String Axiverse,” Phys. Rev. D81(2010) 123530, [arXiv:0905.4720 [hep-th]]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  13. [13]

    Lattice QCD for Cosmology

    S. Borsanyiet al., “Calculation of the axion mass based on high-temperature lattice quantum chromodynamics,” Nature539no. 7627, (2016) 69–71, [arXiv:1606.07494[hep-lat]]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  14. [14]

    Gorghetto, E

    M. Gorghetto, E. Hardy, and G. Villadoro, “More axions from strings,”SciPost Phys.10no. 2, (2021) 050, [arXiv:2007.04990[hep-ph]]

    work page arXiv 2021

  15. [15]

    Buschmann, J.W

    M. Buschmann, J. W. Foster, A. Hook, A. Peterson, D. E. Willcox, W. Zhang, and B. R. Safdi, “Dark matter from axion strings with adaptive mesh refinement,”Nature Commun.13no. 1, (2022) 1049, [arXiv:2108.05368[hep-ph]]. 8

    work page arXiv 2022

  16. [16]

    Parametric-Resonance Production of QCD Axions,

    Pirzada, Y. Gao, and Q. Yang, “Parametric-Resonance Production of QCD Axions,” [arXiv:2602.06922 [hep-ph]]

    work page arXiv

  17. [17]

    Vector Dark Matter from Inflationary Fluctuations

    P. W. Graham, J. Mardon, and S. Rajendran, “Vector Dark Matter from Inflationary Fluctuations,”Phys. Rev. D93no. 10, (2016) 103520, [arXiv:1504.02102 [hep-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  18. [18]

    Relic Abundance of Dark Photon Dark Matter,

    P. Agrawal, N. Kitajima, M. Reece, T. Sekiguchi, and F. Takahashi, “Relic Abundance of Dark Photon Dark Matter,”Phys. Lett. B801(2020) 135136, [arXiv:1810.07188[hep-ph]]

    work page arXiv 2020

  19. [19]

    Dark Photon Dark Matter Produced by Axion Oscillations

    R. T. Co, A. Pierce, Z. Zhang, and Y. Zhao, “Dark Photon Dark Matter Produced by Axion Oscillations,” Phys. Rev. D99no. 7, (2019) 075002, [arXiv:1810.07196[hep-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  20. [20]

    Vector dark matter production at the end of inflation

    M. Bastero-Gil, J. Santiago, L. Ubaldi, and R. Vega-Morales, “Vector dark matter production at the end of inflation,”JCAP04(2019) 015, [arXiv:1810.07208[hep-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  21. [21]

    Dark Photon Dark Matter from a Network of Cosmic Strings

    A. J. Long and L.-T. Wang, “Dark Photon Dark Matter from a Network of Cosmic Strings,”Phys. Rev. D99no. 6, (2019) 063529, [arXiv:1901.03312 [hep-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  22. [22]

    Sikivie, Rev

    P. Sikivie, “Invisible Axion Search Methods,”Rev. Mod. Phys.93no. 1, (2021) 015004, [arXiv:2003.02206[hep-ph]]

    work page arXiv 2021

  23. [23]

    The dark photon,

    M. Fabbrichesi, E. Gabrielli, and G. Lanfranchi, “The dark photon,” 2020

    work page 2020

  24. [24]

    Chadha-Day, J

    F. Chadha-Day, J. Ellis, and D. J. E. Marsh, “Axion dark matter: What is it and why now?,”Sci. Adv.8 no. 8, (2022) abj3618, [arXiv:2105.01406[hep-ph]]

    work page arXiv 2022

  25. [25]

    Experimental Tests of the Invisible Axion,

    P. Sikivie, “Experimental Tests of the Invisible Axion,” Phys. Rev. Lett.51(1983) 1415–1417. [Erratum: Phys.Rev.Lett. 52, 695 (1984)]

    work page 1983

  26. [26]

    Limits on the Abundance and Coupling of Cosmic Axions at 4.5-Microev<m(a)<5.0-Microev

    S. De Panfilis, A. C. Melissinos, B. E. Moskowitz, J. T. Rogers, Y. K. Semertzidis, W. Wuensch, H. J. Halama, A. G. Prodell, W. B. Fowler, and F. A. Nezrick, “Limits on the Abundance and Coupling of Cosmic Axions at 4.5-Microev<m(a)<5.0-Microev”Phys. Rev. Lett.59(1987) 839

    work page 1987

  27. [27]

    Carosi et al

    C. Hagmann, P. Sikivie, N. S. Sullivan, and D. B. Tanner, “Results from a search for cosmic axions,” Phys. Rev. D42(1990) 1297–1300. [27]ADMXCollaboration, G. Carosiet al., “Search for Axion Dark Matter from 1.1 to 1.3 GHz with ADMX,” Phys. Rev. Lett.135no. 19, (2025) 191001, [arXiv:2504.07279[hep-ex]]. [28]HA YST ACCollaboration, X. Baiet al., “Dark Matt...

    work page arXiv 1990

  28. [28]

    Search for Dark Matter Axions with Tunable TM020 Mode,

    S. Bae, J. Jeong, Y. Kim, S. Youn, H. Park, T. Seong, S. Oh, and Y. K. Semertzidis, “Search for Dark Matter Axions with Tunable TM020 Mode,”Phys. Rev. Lett. 133no. 21, (2024) 211803, [arXiv:2403.13390 [hep-ex]]. [30]ORGANCollaboration, A. P. Quiskamp, G. R. Flower, S. Samuels, B. T. McAllister, P. Altin, E. N. Ivanov, M. Goryachev, and M. E. Tobar, “Near-...

    work page arXiv 2024

  29. [29]

    First results of the SUPAX Experiment: Probing Dark Photons,

    T. Schneemann, K. Schmieden, and M. Schott, “First results of the SUPAX Experiment: Probing Dark Photons,” [arXiv:2308.08337[hep-ex]]

    work page arXiv

  30. [30]

    Deepest sensitivity to wavelike dark photon dark matter with superconducting radio frequency cavities,

    R. Cervanteset al., “Deepest sensitivity to wavelike dark photon dark matter with superconducting radio frequency cavities,”Phys. Rev. D110no. 4, (2024) 043022, [arXiv:2208.03183[hep-ex]]

    work page arXiv 2024

  31. [31]

    Near-quantum-limited haloscope search for dark-photon dark matter enhanced by a high-Q superconducting cavity,

    R. Kang, M. Jiao, Y. Tong, Y. Liu, Y. Zhong, Y.-F. Cai, J. Zhou, X. Rong, and J. Du, “Near-quantum-limited haloscope search for dark-photon dark matter enhanced by a high-Q superconducting cavity,”Phys. Rev. D109no. 9, (2024) 095037, [arXiv:2404.12731[hep-ex]]

    work page arXiv 2024

  32. [32]

    Searching for Dark Matter with a Superconducting Qubit,

    A. V. Dixit, S. Chakram, K. He, A. Agrawal, R. K. Naik, D. I. Schuster, and A. Chou, “Searching for Dark Matter with a Superconducting Qubit,”Phys. Rev. Lett.126no. 14, (2021) 141302, [arXiv:2008.12231[hep-ex]]

    work page arXiv 2021

  33. [33]

    First results from the WISPDMX radio frequency cavity searches for hidden photon dark matter,

    L. H. Nguyen, A. Lobanov, and D. Horns, “First results from the WISPDMX radio frequency cavity searches for hidden photon dark matter,”JCAP10 (2019) 014, [arXiv:1907.12449[hep-ex]]

    work page arXiv 2019

  34. [34]

    Search for Dark Matter Axions with CAST-CAPP,

    C. M. Adairet al., “Search for Dark Matter Axions with CAST-CAPP,”Nature Commun.13no. 1, (2022) 6180, [arXiv:2211.02902[hep-ex]]

    work page arXiv 2022

  35. [35]

    RADES axion search results with a high-temperature superconducting cavity in an 11.7 T magnet,

    S. Ahyouneet al., “RADES axion search results with a high-temperature superconducting cavity in an 11.7 T magnet,”JHEP04(2025) 113, [arXiv:2403.07790 [hep-ex]]

    work page arXiv 2025

  36. [36]

    The Grenoble Axion Haloscope platform (GrAHal): development plan and first results,

    T. Grenet, R. Ballou, Q. Basto, K. Martineau, P. Perrier, P. Pugnat, J. Quevillon, N. Roch, and C. Smith, “The Grenoble Axion Haloscope platform (GrAHal): development plan and first results,” [arXiv:2110.14406[hep-ex]]

    work page arXiv

  37. [37]

    Cavity design for high-frequency axion dark matter detectors

    I. Stern, A. A. Chisholm, J. Hoskins, P. Sikivie, N. S. Sullivan, D. B. Tanner, G. Carosi, and K. van Bibber, “Cavity design for high-frequency axion dark matter detectors,”Rev. Sci. Instrum.86no. 12, (2015) 123305, [arXiv:1603.06990[physics.ins-det]]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  38. [38]

    Searching for WISPy Cold Dark Matter with a Dish Antenna

    D. Horns, J. Jaeckel, A. Lindner, A. Lobanov, J. Redondo, and A. Ringwald, “Searching for WISPy Cold Dark Matter with a Dish Antenna,”JCAP04 (2013) 016, [arXiv:1212.2970[hep-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  39. [39]

    From Resonant to Broadband Searches for WISPy Cold Dark Matter

    J. Jaeckel and J. Redondo, “Resonant to broadband searches for cold dark matter consisting of weakly interacting slim particles,”Phys. Rev. D88no. 11, (2013) 115002, [arXiv:1308.1103[hep-ph]]. [46]MADMAX W orking GroupCollaboration, A. Caldwell, G. Dvali, B. Majorovits, A. Millar, 9 G. Raffelt, J. Redondo, O. Reimann, F. Simon, and F. Steffen, “Dielectric...

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  40. [40]

    Axion and hidden photon dark matter detection with multilayer optical haloscopes

    M. Baryakhtar, J. Huang, and R. Lasenby, “Axion and hidden photon dark matter detection with multilayer optical haloscopes,”Phys. Rev. D98no. 3, (2018) 035006, [arXiv:1803.11455[hep-ph]]. [48]MADMAXCollaboration, J. Eggeet al., “First Search for Dark Photon Dark Matter with a madmax Prototype,”Phys. Rev. Lett.134no. 15, (2025) 151004, [arXiv:2408.02368[hep-ex]]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  41. [41]

    New Constraints on Dark Photon Dark Matter with a Millimeter-Wave Dielectric Haloscope,

    G. Wei, D. Wu, R. Kang, Q. Jiang, M. Jiao, X. Rong, and J. Du, “New Constraints on Dark Photon Dark Matter with a Millimeter-Wave Dielectric Haloscope,” Phys. Rev. Lett.136no. 7, (2026) 071001, [arXiv:2503.23354[astro-ph.CO]]

    work page arXiv 2026

  42. [42]

    Weak Interaction Singlet and Strong CP Invariance,

    J. E. Kim, “Weak Interaction Singlet and Strong CP Invariance,”Phys. Rev. Lett.43(1979) 103

    work page 1979

  43. [43]

    Can Confinement Ensure Natural CP Invariance of Strong Interactions?,

    M. A. Shifman, A. I. Vainshtein, and V. I. Zakharov, “Can Confinement Ensure Natural CP Invariance of Strong Interactions?,”Nucl. Phys. B166(1980) 493–506

    work page 1980

  44. [44]

    A Simple Solution to the Strong CP Problem with a Harmless Axion,

    M. Dine, W. Fischler, and M. Srednicki, “A Simple Solution to the Strong CP Problem with a Harmless Axion,”Phys. Lett. B104(1981) 199–202

    work page 1981

  45. [45]

    On Possible Suppression of the Axion Hadron Interactions. (In Russian),

    A. R. Zhitnitsky, “On Possible Suppression of the Axion Hadron Interactions. (In Russian),”Sov. J. Nucl. Phys.31(1980) 260

    work page 1980

  46. [46]

    A Radio for Hidden-Photon Dark Matter Detection

    S. Chaudhuri, P. W. Graham, K. Irwin, J. Mardon, S. Rajendran, and Y. Zhao, “Radio for hidden-photon dark matter detection,”Phys. Rev. D92no. 7, (2015) 075012, [arXiv:1411.7382[hep-ph]]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  47. [47]

    J. D. Jackson,Classical Electrodynamics. Wiley, 1998

    work page 1998

  48. [48]

    A SQUID-based microwave cavity search for dark-matter axions

    A. Cahillet al., “Measurements of Copper RF Surface Resistance at Cryogenic Temperatures for Applications to X-Band and S-Band Accelerators,” in7th International Particle Accelerator Conference, p. MOPMW038. 2016. [57]ADMXCollaboration, S. J. Asztaloset al., “A SQUID-based microwave cavity search for dark-matter axions,”Phys. Rev. Lett.104(2010) 041301, [...

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  49. [49]

    First results from a microwave cavity axion search at 24 micro-eV

    B. M. Brubakeret al., “First results from a microwave cavity axion search at 24µeV,”Phys. Rev. Lett.118 no. 6, (2017) 061302, [arXiv:1610.02580 [astro-ph.CO]]. [64]HA YST ACCollaboration, L. Zhonget al., “Results from phase 1 of the HAYSTAC microwave cavity axion experiment,”Phys. Rev. D97no. 9, (2018) 092001, [arXiv:1803.03690[hep-ex]]. [65]HA YST ACColl...

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  50. [50]

    Axion Dark Matter Search around 6.7 µeV,

    S. Lee, S. Ahn, J. Choi, B. R. Ko, and Y. K. Semertzidis, “Axion Dark Matter Search around 6.7 µeV,”Phys. Rev. Lett.124no. 10, (2020) 101802, [arXiv:2001.05102[hep-ex]]

    work page arXiv 2020

  51. [51]

    Search for Invisible Axion Dark Matter with a Multiple-Cell Haloscope,

    J. Jeong, S. Youn, S. Bae, J. Kim, T. Seong, J. E. Kim, and Y. K. Semertzidis, “Search for Invisible Axion Dark Matter with a Multiple-Cell Haloscope,” Phys. Rev. Lett.125no. 22, (2020) 221302, [arXiv:2008.10141[hep-ex]]. [69]CAPPCollaboration, O. Kwonet al., “First Results from an Axion Haloscope at CAPP around 10.7µeV,” Phys. Rev. Lett.126no. 19, (2021)...

    work page arXiv 2020

  52. [52]

    Searching for Invisible Axion Dark Matter with an 18 T Magnet Haloscope,

    Y. Lee, B. Yang, H. Yoon, M. Ahn, H. Park, B. Min, D. Kim, and J. Yoo, “Searching for Invisible Axion Dark Matter with an 18 T Magnet Haloscope,”Phys. Rev. Lett.128no. 24, (2022) 241805, [arXiv:2206.08845[hep-ex]]

    work page arXiv 2022

  53. [53]

    Axion haloscope using an 18 T high temperature superconducting magnet,

    H. Yoon, M. Ahn, B. Yang, Y. Lee, D. Kim, H. Park, B. Min, and J. Yoo, “Axion haloscope using an 18 T high temperature superconducting magnet,”Phys. Rev. D106no. 9, (2022) 092007, [arXiv:2206.12271 [hep-ex]]

    work page arXiv 2022

  54. [54]

    Near-Quantum-Noise Axion Dark Matter Search at CAPP around 9.5µeV,

    J. Kimet al., “Near-Quantum-Noise Axion Dark Matter Search at CAPP around 9.5µeV,”Phys. Rev. Lett.130no. 9, (2023) 091602, [arXiv:2207.13597 [hep-ex]]

    work page arXiv 2023

  55. [55]

    Axion Dark Matter Search around 4.55µeV with Dine-Fischler-Srednicki-Zhitnitskii Sensitivity,

    A. K. Yiet al., “Axion Dark Matter Search around 4.55µeV with Dine-Fischler-Srednicki-Zhitnitskii Sensitivity,”Phys. Rev. Lett.130no. 7, (2023) 071002, [arXiv:2210.10961[hep-ex]]

    work page arXiv 2023

  56. [56]

    Extended Axion Dark Matter Search Using the CAPP18T Haloscope,

    B. Yang, H. Yoon, M. Ahn, Y. Lee, and J. Yoo, “Extended Axion Dark Matter Search Using the CAPP18T Haloscope,”Phys. Rev. Lett.131no. 8, (2023) 081801, [arXiv:2308.09077[hep-ex]]

    work page arXiv 2023

  57. [57]

    Experimental Search for Invisible Dark Matter Axions around 22µeV,

    Y. Kimet al., “Experimental Search for Invisible Dark Matter Axions around 22µeV,”Phys. Rev. Lett.133 no. 5, (2024) 051802, [arXiv:2312.11003[hep-ex]]. [76]CAPPCollaboration, S. Ahnet al., “Extensive Search for Axion Dark Matter over 1 GHz with CAPP’S Main Axion Experiment,”Phys. Rev. X14no. 3, (2024) 031023, [arXiv:2402.12892[hep-ex]]. [77]ORGANCollabora...

    work page arXiv 2024

  58. [58]

    Exclusion of Axionlike-Particle Cogenesis Dark Matter in a Mass Window above 100µeV,

    A. Quiskamp, B. T. McAllister, P. Altin, E. N. Ivanov, M. Goryachev, and M. E. Tobar, “Exclusion of Axionlike-Particle Cogenesis Dark Matter in a Mass Window above 100µeV,”Phys. Rev. Lett.132no. 3, (2024) 031601, [arXiv:2310.00904[hep-ex]]

    work page arXiv 2024

  59. [59]

    Galactic axions search with a superconducting resonant cavity

    D. Alesiniet al., “Galactic axions search with a superconducting resonant cavity,”Phys. Rev. D99 no. 10, (2019) 101101, [arXiv:1903.06547 [physics.ins-det]]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  60. [60]

    Search for invisible axion dark matter of mass m a = 43µeV with the QUAX–aγ experiment,

    D. Alesiniet al., “Search for invisible axion dark matter of mass m a = 43µeV with the QUAX–aγ experiment,”Phys. Rev. D103no. 10, (2021) 102004, [arXiv:2012.09498[hep-ex]]. [81]QUAXCollaboration, R. Di Voraet al., “Search for galactic axions with a traveling wave parametric amplifier,”Phys. Rev. D108no. 6, (2023) 062005, [arXiv:2304.07505[hep-ex]]

    work page arXiv 2021

  61. [61]

    Search for 70µeV Dark Photon Dark Matter with a Dielectrically Loaded Multiwavelength Microwave Cavity,

    R. Cervanteset al., “Search for 70µeV Dark Photon Dark Matter with a Dielectrically Loaded Multiwavelength Microwave Cavity,”Phys. Rev. Lett. 129no. 20, (2022) 201301, [arXiv:2204.03818 [hep-ex]]

    work page arXiv 2022

  62. [62]

    Experimental Search for Hidden Photon CDM in the eV mass range with a Dish Antenna

    J. Suzuki, T. Horie, Y. Inoue, and M. Minowa, “Experimental Search for Hidden Photon CDM in the eV mass range with a Dish Antenna,”JCAP09(2015) 042, [arXiv:1504.00118[hep-ex]]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  63. [63]

    First results from a hidden photon dark matter search in the meV sector using a plane-parabolic mirror system

    S. Knirck, T. Yamazaki, Y. Okesaku, S. Asai, T. Idehara, and T. Inada, “First results from a hidden photon dark matter search in the meV sector using a plane-parabolic mirror system,”JCAP11(2018) 031, [arXiv:1806.05120[hep-ex]]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  64. [64]

    Search for hidden-photon cold dark matter using a K-band cryogenic receiver,

    N. Tomita, S. Oguri, Y. Inoue, M. Minowa, T. Nagasaki, J. Suzuki, and O. Tajima, “Search for hidden-photon cold dark matter using a K-band cryogenic receiver,”JCAP09(2020) 012, [arXiv:2006.02828[hep-ex]]

    work page arXiv 2020

  65. [65]

    Direct Searches for Hidden-Photon Dark Matter with the SHUKET Experiment

    P. Brun, L. Chevalier, and C. Flouzat, “Direct Searches for Hidden-Photon Dark Matter with the SHUKET Experiment,”Phys. Rev. Lett.122no. 20, (2019) 201801, [arXiv:1905.05579[hep-ex]]. [87]DOSUE-RRCollaboration, S. Kotakaet al., “Search for Dark Photon Dark Matter in the Mass Range 74–110µeV with a Cryogenic Millimeter-Wave Receiver,”Phys. Rev. Lett.130no....

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  66. [66]

    Direct Detection of Dark Photon Dark Matter Using Radio Telescopes,

    H. An, S. Ge, W.-Q. Guo, X. Huang, J. Liu, and Z. Lu, “Direct Detection of Dark Photon Dark Matter Using Radio Telescopes,”Phys. Rev. Lett.130no. 18, (2023) 181001, [arXiv:2207.05767[hep-ph]]

    work page arXiv 2023

  67. [67]

    Wideband Direct Detection Constraints on Hidden Photon Dark Matter with the QUALIPHIDE Experiment,

    K. Ramanathan, N. Klimovich, R. Basu Thakur, B. H. Eom, H. G. LeDuc, S. Shu, A. D. Beyer, and P. K. Day, “Wideband Direct Detection Constraints on Hidden Photon Dark Matter with the QUALIPHIDE Experiment,”Phys. Rev. Lett.130no. 23, (2023) 231001, [arXiv:2209.03419[astro-ph.CO]]

    work page arXiv 2023

  68. [68]

    First results from BRASS-p broadband searches for hidden photon dark matter,

    F. Bajjaliet al., “First results from BRASS-p broadband searches for hidden photon dark matter,” JCAP08(2023) 077, [arXiv:2306.05934[hep-ex]]. [92]BREADCollaboration, S. Knircket al., “First Results from a Broadband Search for Dark Photon Dark Matter in the 44 to 52µeV Range with a Coaxial Dish Antenna,”Phys. Rev. Lett.132no. 13, (2024) 131004, [arXiv:231...

    work page arXiv 2023

  69. [69]

    Direct detection of dark photon dark matter with the James Webb Space Telescope,

    H. An, S. Ge, J. Liu, and Z. Lu, “Direct detection of dark photon dark matter with the James Webb Space Telescope,”JCAP02(2026) 009, [arXiv:2402.17140 [hep-ph]]

    work page arXiv 2026

  70. [70]

    New Constraints on Dark Photon Dark Matter with Superconducting Nanowire Detectors in an Optical Haloscope,

    J. Chileset al., “New Constraints on Dark Photon Dark Matter with Superconducting Nanowire Detectors in an Optical Haloscope,”Phys. Rev. Lett.128no. 23, (2022) 231802, [arXiv:2110.01582[hep-ex]]

    work page arXiv 2022

  71. [71]

    New limits on dark photons from solar emission and keV scale dark matter,

    H. An, M. Pospelov, J. Pradler, and A. Ritz, “New limits on dark photons from solar emission and keV scale dark matter,”Phys. Rev. D102(2020) 115022, [arXiv:2006.13929[hep-ph]]

    work page arXiv 2020

  72. [72]

    cajohare/axionlimits: Axionlimits

    C. O’Hare, “cajohare/axionlimits: Axionlimits.” https://cajohare.github.io/AxionLimits/, July, 2020. [97]ADMXCollaboration, C. Bartramet al., “Dark matter axion search using a Josephson Traveling wave parametric amplifier,”Rev. Sci. Instrum.94no. 4, (2023) 044703, [arXiv:2110.10262[hep-ex]]. [98]ORGANCollaboration, B. T. McAllister, G. Flower, J. Kruger, ...

    work page arXiv 2020

  73. [73]

    Pinetti, (2025), arXiv:2503.11753 [hep-ph]

    E. Pinetti, “First constraints on QCD axion dark matter using James Webb Space Telescope observations,” [arXiv:2503.11753[hep-ph]]

    work page arXiv

  74. [74]

    Advancing globular cluster constraints on the axion-photon coupling,

    M. J. Dolan, F. J. Hiskens, and R. R. Volkas, “Advancing globular cluster constraints on the axion-photon coupling,”JCAP10(2022) 096, [arXiv:2207.03102[hep-ph]]

    work page arXiv 2022

  75. [75]

    High frequency response of thick REBCO coated conductors in the framework of the 11 FCC study,

    A. Romanov, P. Krkoti´ c, G. Telles, J. O’Callaghan, M. Pont, F. Perez, X. Granados, S. Calatroni, T. Puig, and J. Gutierrez, “High frequency response of thick REBCO coated conductors in the framework of the 11 FCC study,”Sci. Rep.10no. 1, (2020) 12325

    work page 2020

  76. [76]

    Biaxially Textured YBa2Cu3O7−x Microwave Cavity in a High Magnetic Field for a Dark-Matter Axion Search,

    D. Ahn, O. Kwon, W. Chung, W. Jang, D. Lee, J. Lee, S. Woo Youn, H. Byun, D. Youm, and Y. K. Semertzidis, “Biaxially Textured YBa2Cu3O7−x Microwave Cavity in a High Magnetic Field for a Dark-Matter Axion Search,”Phys. Rev. Applied17 no. 6, (2022) L061005, [arXiv:2103.14515 [physics.ins-det]]

    work page arXiv 2022