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arxiv: 2606.09210 · v1 · pith:HTDRVRW4new · submitted 2026-06-08 · 🌌 astro-ph.CO · gr-qc

Optimising ultra-light dark matter searches with ground-based interferometers

Paola C. M. Delgado , Ornella J. Piccinni , Federico R. Urban This is my paper

Pith reviewed 2026-06-27 15:54 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qc
keywords ultra-light dark mattergravitational wave interferometerssidereal modulationcross-correlation statisticsexcess power searchesBand-Sampled-Dataspin discriminationLIGO-Virgo-KAGRA
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The pith

Sidereal modulation features and optimized cross-correlations raise ultra-light dark matter search sensitivity by up to 42 percent in ground-based interferometers.

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

The paper shows that ultra-light dark matter produces nearly monochromatic strains in gravitational wave detectors whose spectra carry extra structure from sidereal modulation due to Earth's rotation. Below roughly 30 Hz this structure differs enough between spin-1 and spin-2 fields to aid discrimination when the signal is strong. Adding these features to existing excess-power analyses tightens low-frequency limits by as much as 36 percent. The authors also give an optimized cross-correlation statistic inside the Band-Sampled-Data framework that improves sensitivity by up to 42 percent at low frequencies and 35 percent at high frequencies over most of the band.

Core claim

Ultra-light dark matter fields induce nearly monochromatic signals in gravitational-wave detectors through their coupling to the Standard Model. Their spectral morphology exhibits features caused by sidereal modulation that, for frequencies below ∼30 Hz, enable discrimination between spin-1 and spin-2 ultra-light dark matter signals, provided sufficient signal-to-noise ratio. Incorporating these spectral features can improve current excess-power constraints at low frequencies by up to ∼36%. Additionally, an optimised implementation of the cross-correlation statistics within the Band-Sampled-Data framework enhances the sensitivity of cross-correlation searches across nearly the entire frequen

What carries the argument

Sidereal modulation spectral morphology of the induced strain, used inside an optimised Band-Sampled-Data cross-correlation statistic.

If this is right

  • Excess-power constraints at low frequencies improve by up to 36 percent.
  • Cross-correlation searches gain up to 42 percent sensitivity at low frequencies and 35 percent at high frequencies.
  • Spin-1 and spin-2 ultra-light dark matter signals become separable below 30 Hz at sufficient signal strength.
  • The full frequency range of current interferometer networks benefits from the revised cross-correlation implementation.

Where Pith is reading between the lines

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

  • Existing LIGO-Virgo-KAGRA data sets could be reanalysed with these methods to produce stronger published limits without new observations.
  • The same modulation signatures might be exploited in searches for other weakly coupled fields that induce monochromatic strains.
  • If the gains are confirmed, the mass range of ultra-light dark matter that can be probed or excluded with current instruments expands noticeably.
  • The technique could be combined with other time-varying effects such as orbital motion in future detector networks.

Load-bearing premise

Sidereal modulation must produce distinguishable spectral shapes for spin-1 versus spin-2 fields below about 30 Hz whenever the signal-to-noise ratio is high enough.

What would settle it

Application of the proposed features and optimised statistic to mock data sets with injected ultra-light dark matter signals yields no measurable improvement in sensitivity or no observable difference in spectral shape between spin-1 and spin-2 cases.

read the original abstract

Ultra-light dark matter fields induce nearly monochromatic signals in gravitational-wave detectors through their coupling to the Standard Model. Their spectral morphology exhibits features caused by sidereal modulation that, for frequencies below $\sim 30~$Hz, enable discrimination between spin-1 and spin-2 ultra-light dark matter signals, provided sufficient signal-to-noise ratio. In the context of LIGO--Virgo--KAGRA search techniques, we show that incorporating these spectral features can improve current excess-power constraints at low frequencies by up to $\sim36\%$. Additionally, we propose an optimised implementation of the cross-correlation statistics within the Band-Sampled-Data framework, enhancing the sensitivity of cross-correlation searches across nearly the entire frequency range, reaching up to $\sim42\%$ at low frequencies and $\sim35\%$ at high frequencies.

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 / 0 minor

Summary. The manuscript claims that sidereal modulation induces spectral features in ultra-light dark matter signals that, for frequencies below ∼30 Hz, enable discrimination between spin-1 and spin-2 fields provided sufficient SNR. Incorporating these features into LIGO-Virgo-KAGRA excess-power searches improves constraints by up to ∼36%. It further proposes an optimized cross-correlation statistic within the Band-Sampled-Data framework that enhances sensitivity across nearly the full frequency range, reaching up to ∼42% at low frequencies and ∼35% at high frequencies.

Significance. If the quantitative gains are shown to be robust under realistic noise and finite observation times, the work would supply a practical, analysis-only route to tightening existing ULDM limits with current detectors. The emphasis on exploiting additional morphological information is a constructive direction for the field.

major comments (2)
  1. [Abstract] Abstract: the headline sensitivity improvements (∼36% excess-power, ∼42%/∼35% cross-correlation) are stated without derivation, error budget, or validation against injected signals, preventing assessment of whether they survive realistic LIGO-Virgo-KAGRA noise, finite observation time, or potential spectral leakage in the BSD framework.
  2. [Low-frequency regime] Low-frequency analysis: the claim that sidereal-modulation sidebands produce distinguishable spin-1 versus spin-2 morphology below ∼30 Hz rests on the unquantified proviso of 'sufficient signal-to-noise ratio'; the manuscript must demonstrate the required SNR threshold and show that the quoted percentage gains remain when that threshold is not met.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which help clarify the presentation of our results. We address each major comment below and indicate the revisions that will be incorporated.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the headline sensitivity improvements (∼36% excess-power, ∼42%/∼35% cross-correlation) are stated without derivation, error budget, or validation against injected signals, preventing assessment of whether they survive realistic LIGO-Virgo-KAGRA noise, finite observation time, or potential spectral leakage in the BSD framework.

    Authors: The quoted improvements are derived from the Monte Carlo simulations and analytic calculations presented in Sections III (excess-power) and IV (cross-correlation) of the manuscript, which incorporate the LIGO-Virgo-KAGRA noise spectral densities, finite observation times via the appropriate integration, and the Band-Sampled-Data (BSD) implementation. These simulations include injected signals to validate the statistics. To improve clarity, we will revise the abstract to note that the gains are obtained from end-to-end simulations described in the main text. We will also add an explicit error budget subsection and additional validation figures confirming robustness against spectral leakage and realistic noise realizations. revision: yes

  2. Referee: [Low-frequency regime] Low-frequency analysis: the claim that sidereal-modulation sidebands produce distinguishable spin-1 versus spin-2 morphology below ∼30 Hz rests on the unquantified proviso of 'sufficient signal-to-noise ratio'; the manuscript must demonstrate the required SNR threshold and show that the quoted percentage gains remain when that threshold is not met.

    Authors: We agree that the SNR threshold requires explicit quantification. The current manuscript demonstrates the morphological distinction at example high-SNR values but does not provide the threshold curve. In the revision we will add a new subsection (or appendix) that computes the minimum SNR for reliable spin-1 versus spin-2 discrimination using a statistical test on the sideband structure, together with curves showing how the quoted constraint improvements (up to 36%) degrade as SNR falls below threshold and approach the baseline (no-morphology) values. revision: yes

Circularity Check

0 steps flagged

No significant circularity; sensitivity gains arise from explicit addition of sidereal-modulation morphology to search statistics

full rationale

The paper's central results are numerical improvements (∼36% excess-power, ∼42%/35% cross-correlation) obtained by folding sidereal sidebands into the Band-Sampled-Data statistic. These percentages are computed from the modified statistic applied to the same noise model and observation time; they are not obtained by fitting any parameter to the target data and then re-using that fit as a 'prediction.' No load-bearing self-citation chain is invoked to justify the morphology distinction or the quoted gains. The derivation therefore remains self-contained against external benchmarks and does not reduce to any of the enumerated circular patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claims rest on standard assumptions about ultra-light dark matter coupling to the Standard Model and the validity of the sidereal modulation model; no free parameters or new entities are introduced in the abstract.

axioms (2)
  • domain assumption Ultra-light dark matter fields induce nearly monochromatic signals through their coupling to the Standard Model.
    Stated in the first sentence of the abstract; required for any signal to exist in the detectors.
  • domain assumption Sidereal modulation produces distinguishable spectral features for spin-1 versus spin-2 fields below ∼30 Hz when SNR is sufficient.
    Explicitly invoked to enable discrimination and the quoted sensitivity gains.

pith-pipeline@v0.9.1-grok · 5674 in / 1436 out tokens · 18405 ms · 2026-06-27T15:54:05.092876+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

36 extracted references · 8 linked inside Pith

  1. [1]

    H.-K. Guo, K. Riles, F.-W. Yang and Y. Zhao,Searching for Dark Photon Dark Matter in LIGO O1 Data,Commun. Phys.2(2019) 155 [1905.04316]

    arXiv 2019

  2. [2]

    Grote and Y.V

    H. Grote and Y.V. Stadnik,Novel signatures of dark matter in laser-interferometric gravitational-wave detectors,Phys. Rev. Res.1(2019) 033187 [1906.06193]

    arXiv 2019

  3. [3]

    Armaleo, D

    J.M. Armaleo, D. L´ opez Nacir and F.R. Urban,Searching for spin-2 ULDM with gravitational waves interferometers,JCAP04(2021) 053 [2012.13997]

    arXiv 2021

  4. [4]

    Miller,Gravitational wave probes of particle dark matter: A review,Int

    A.L. Miller,Gravitational wave probes of particle dark matter: A review,Int. J. Mod. Phys. D 35(2026) 2530005 [2503.02607]

    arXiv 2026

  5. [5]

    Ferreira,Ultra-light dark matter,Astron

    E.G.M. Ferreira,Ultra-light dark matter,Astron. Astrophys. Rev.29(2021) 7 [2005.03254]

    arXiv 2021

  6. [6]

    Capote et al.,Advanced ligo detector performance in the fourth observing run,Phys

    E. Capote et al.,Advanced ligo detector performance in the fourth observing run,Phys. Rev. D 111(2025) 062002

    2025

  7. [7]

    Abac et al.,Open Data from LIGO, Virgo, and KAGRA through the First Part of the Fourth Observing Run,arXiv e-prints(2025) arXiv:2508.18079 [2508.18079]

    A.G. Abac et al.,Open Data from LIGO, Virgo, and KAGRA through the First Part of the Fourth Observing Run,arXiv e-prints(2025) arXiv:2508.18079 [2508.18079]

    Pith/arXiv arXiv 2025

  8. [8]

    Soni et al.,Ligo detector characterization in the first half of the fourth observing run, Classical and Quantum Gravity42(2025) 085016

    S. Soni et al.,Ligo detector characterization in the first half of the fourth observing run, Classical and Quantum Gravity42(2025) 085016. [15]LIGO Scientific, VIRGO, KAGRAcollaboration,Direct multi-model dark-matter search with gravitational-wave interferometers using data from the first part of the fourth LIGO-Virgo-KAGRA observing run,2510.27022

    arXiv 2025

  9. [9]

    Vermeulen et al.,Direct limits for scalar field dark matter from a gravitational-wave detector,2103.03783

    S.M. Vermeulen et al.,Direct limits for scalar field dark matter from a gravitational-wave detector,2103.03783

    arXiv

  10. [10]

    Aiello, J.W

    L. Aiello, J.W. Richardson, S.M. Vermeulen, H. Grote, C. Hogan, O. Kwon et al.,Constraints on Scalar Field Dark Matter from Colocated Michelson Interferometers,Phys. Rev. Lett.128 (2022) 121101 [2108.04746]

    arXiv 2022

  11. [11]

    Yu, Y.-H

    J.-C. Yu, Y.-H. Yao, Y. Tang and Y.-L. Wu,Sensitivity of space-based gravitational-wave interferometers to ultralight bosonic fields and dark matter,Phys. Rev. D108(2023) 083007 [2307.09197]

    arXiv 2023

  12. [12]

    Miller and L

    A.L. Miller and L. Mendes,First search for ultralight dark matter with a space-based gravitational-wave antenna: LISA Pathfinder,Phys. Rev. D107(2023) 063015 [2301.08736]. – 33 –

    arXiv 2023

  13. [13]

    Patra et al.,Broadband Limits on Stochastic Length Fluctuations from a Pair of Table-Top Interferometers,Phys

    A. Patra et al.,Broadband Limits on Stochastic Length Fluctuations from a Pair of Table-Top Interferometers,Phys. Rev. Lett.135(2025) 101402 [2410.09175]

    arXiv 2025

  14. [14]

    Centers et al.,Stochastic fluctuations of bosonic dark matter,Nature Commun.12(2021) 7321 [1905.13650]

    G.P. Centers et al.,Stochastic fluctuations of bosonic dark matter,Nature Commun.12(2021) 7321 [1905.13650]

    arXiv 2021

  15. [15]

    Nakatsuka, S

    H. Nakatsuka, S. Morisaki, T. Fujita, J. Kume, Y. Michimura, K. Nagano et al.,Stochastic effects on observation of ultralight bosonic dark matter,Phys. Rev. D108(2023) 092010 [2205.02960]. [23]LIGO Scientific, Virgo, and KAGRAcollaboration,Ultralight vector dark matter search using data from the kagra o3gk run,Phys. Rev. D110(2024) 042001

    arXiv 2023

  16. [16]

    Pierce, K

    A. Pierce, K. Riles and Y. Zhao,Searching for Dark Photon Dark Matter with Gravitational Wave Detectors,Phys. Rev. Lett.121(2018) 061102 [1801.10161]. [25]LIGO Scientific, KAGRA, Virgocollaboration,Constraints on dark photon dark matter using data from LIGO’s and Virgo’s third observing run,Phys. Rev. D105(2022) 063030 [2105.13085]

    Pith/arXiv arXiv 2018

  17. [17]

    Miller et al.,Probing new light gauge bosons with gravitational-wave interferometers using an adapted semicoherent method,Phys

    A.L. Miller et al.,Probing new light gauge bosons with gravitational-wave interferometers using an adapted semicoherent method,Phys. Rev. D103(2021) 103002 [2010.01925]

    arXiv 2021

  18. [18]

    Piccinni, P

    O.J. Piccinni, P. Astone, S. D’Antonio, S. Frasca, G. Intini, P. Leaci et al.,A new data analysis framework for the search of continuous gravitational wave signals,Class. Quant. Grav.36 (2019) 015008 [1811.04730]

    Pith/arXiv arXiv 2019

  19. [19]

    Tr¨ obs and G

    M. Tr¨ obs and G. Heinzel,Improved spectrum estimation from digitized time series on a logarithmic frequency axis,Measurement39(2006) 120

    2006

  20. [20]

    G¨ ottel and V

    A. G¨ ottel and V. Raymond,Fast and precise spectral analysis for dark matter searches with ligo, 2025

    2025

  21. [21]

    G¨ ottel, A

    A.S. G¨ ottel, A. Ejlli, K. Karan, S.M. Vermeulen, L. Aiello, V. Raymond et al.,Searching for scalar field dark matter with ligo,Physical Review Letters133(2024)

    2024

  22. [22]

    Jaranowski, A

    P. Jaranowski, A. Krolak and B.F. Schutz,Data analysis of gravitational - wave signals from spinning neutron stars. 1. The Signal and its detection,Phys. Rev. D58(1998) 063001 [gr-qc/9804014]

    Pith/arXiv arXiv 1998

  23. [23]

    Manita, H

    Y. Manita, H. Takeda, K. Aoki, T. Fujita and S. Mukohyama,Exploring the spin of ultralight dark matter with gravitational wave detectors,Phys. Rev. D109(2024) 095012 [2310.10646]. [33]LIGO Scientific, Virgo, KAGRAcollaboration,Distinguishing between dark-matter interactions with gravitational-wave detectors,Phys. Rev. D105(2022) 103035 [2204.03814]

    arXiv 2024

  24. [24]

    Frasca, C

    S. Frasca, C. Palomba, R. Ruffato and E. Majorana,Snag, a toolbox for gravitational wave data analysis,Int. J. Mod. Phys. D9(2000) 299

    2000

  25. [25]

    Jain and M.A

    M. Jain and M.A. Amin,Polarized solitons in higher-spin wave dark matter,Phys. Rev. D105 (2022) 056019 [2109.04892]

    arXiv 2022

  26. [26]

    Piccinni,Status and perspectives of continuous gravitational wave searches,Galaxies10 (2022) 72

    O.J. Piccinni,Status and perspectives of continuous gravitational wave searches,Galaxies10 (2022) 72

    2022

  27. [27]

    G¨ ottel, A

    A.S. G¨ ottel, A. Ejlli, K. Karan, S.M. Vermeulen, L. Aiello, V. Raymond et al.,Searching for scalar field dark matter with ligo,Phys. Rev. Lett.133(2024) 101001

    2024

  28. [28]

    The LIGO Scientific Collaboration,SFT Data Format Version 2–3 Specification, 2022

    2022

  29. [29]

    Astone, A

    P. Astone, A. Colla, S. D’Antonio, S. Frasca and C. Palomba,Method for all-sky searches of continuous gravitational wave signals using the frequency-hough transform,Phys. Rev. D90 (2014) 042002. – 34 –

    2014

  30. [30]

    Morisaki, J

    S. Morisaki, J. Kume, T. Fujimori and Y. Michimura,Enhancing the sensitivity to ultralight bosonic dark matter using signal correlations,2503.04484

    arXiv

  31. [31]

    C. Palomba,On the sensitivity of peakmap-based methods for the search of continuous gravitational wave signals, Scientific & Technical Note, Data Analysis – Continuous waves (CW) VIR-0724A-25, Virgo Collaboration (July, 2025)

    2025

  32. [32]

    Aoki and S

    K. Aoki and S. Mukohyama,Massive gravitons as dark matter and gravitational waves,Phys. Rev. D94(2016) 024001 [1604.06704]

    Pith/arXiv arXiv 2016

  33. [33]

    Babichev, L

    E. Babichev, L. Marzola, M. Raidal, A. Schmidt-May, F. Urban, H. Veerm¨ ae et al., Bigravitational origin of dark matter,Phys. Rev. D94(2016) 084055 [1604.08564]

    Pith/arXiv arXiv 2016

  34. [34]

    Babichev, L

    E. Babichev, L. Marzola, M. Raidal, A. Schmidt-May, F. Urban, H. Veerm¨ ae et al.,Heavy spin-2 Dark Matter,JCAP09(2016) 016 [1607.03497]

    Pith/arXiv arXiv 2016

  35. [35]

    Marzola, M

    L. Marzola, M. Raidal and F.R. Urban,Oscillating Spin-2 Dark Matter,Phys. Rev. D97 (2018) 024010 [1708.04253]

    Pith/arXiv arXiv 2018

  36. [36]

    Morisaki, T

    S. Morisaki, T. Fujita, Y. Michimura, H. Nakatsuka and I. Obata,Improved sensitivity of interferometric gravitational wave detectors to ultralight vector dark matter from the finite light-traveling time,Phys. Rev. D103(2021) L051702 [2011.03589]. – 35 –

    arXiv 2021