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A 0.2 mg plate levitated by laser light could detect vector ultralight dark matter at sensitivities beyond current fifth-force and gravitational-wave searches.

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2026-08-03 19:32 UTC pith:GGC4C2NT

load-bearing objection A serious design study with a genuinely new quantum-noise optimization for optically trapped sensors; the headline reach to B-L ULDM is conditional on an optimistic, unquantified detection efficiency and a laser-power inconsistency that should be fixed. the 3 major comments →

arxiv 2512.00166 v2 pith:GGC4C2NT submitted 2025-11-28 hep-ph hep-exquant-ph

Searching for Ultralight Dark Matter with MOLeQuTE: a Massive Optically Levitated Quantum Tabletop Experiment

Louis Hamaide , Hannah Banks , Peter Barker , Andrew A. Geraci This is my paper
classification hep-ph hep-exquant-ph PACS 95.35.+d42.50.Wk
keywords ultralight dark mattervector B-L dark matteroptically levitated sensoroptomechanicsstandard quantum limitforce sensingtabletop experimentquantum noise optimisation
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper proposes a tabletop experiment in which a thin silica plate of about 0.2 mg is levitated by a vertical laser beam and trapped horizontally by counter-propagating beams, and argues that this sensor can reach the standard quantum limit using existing technology. Its central claim is that such a sensor would be uniquely sensitive to oscillatory forces produced by ultralight dark matter coupled to baryon minus lepton number, improving on existing bounds by up to an order of magnitude for dark matter masses around 10^-14 to 10^-13 eV. The work also provides the first consistent optimisation of quantum noises in optically trapped systems, showing that the best operating point is off resonance, and derives a simple noise floor m ω^2. A larger 0.8 g version is argued to outperform existing searches by up to three orders of magnitude over a wider mass range.

Core claim

The central discovery is a design and optimisation procedure showing that an optically trapped plate in the geometric optics regime can be tuned, at each search frequency, to the standard quantum limit with a quantum force noise floor of S_FF = m ω^2, despite the trap frequency and laser power being coupled. Using this, the paper projects a minimum detectable coupling g_min^{B-L} = 6.9e-25 (m_DM/1e-13 eV)^{3/2} (0.2mg/m)^{1/2} N^{1/4}, which for the 0.2 mg sensor exceeds fifth-force and LIGO bounds for m_DM in [1e-14, 3e-13] eV by up to an order of magnitude. The key scaling is that in the geometric optics regime the quantum noise grows linearly with mass while the dark matter force grows li

What carries the argument

The key machinery is the optical trap itself: a thin high-reflectivity plate whose weight is supported by a vertical beam, with its horizontal motion confined by counter-propagating beams focused by cylindrical lenses. The mechanical frequency Ω depends on laser power and distance, so the standard two-stage noise optimisation is replaced by a joint optimisation; the resulting SQL condition (2/5) ω_L \bar{x} Ω^2 = ω^2 yields a noise floor m ω^2. The differential acceleration between a silica sensor and a tungsten-186 reference plate, which have different neutron-to-nucleon ratios, is the readout observable.

Load-bearing premise

The projected sensitivity assumes that essentially all light scattered by the sensor is collected by the readout (η_D ≈ 1); any real loss of scattered light raises the shot noise floor and reduces the reach.

What would settle it

Build a prototype with the 0.2 mg plate and measure the force noise spectrum at a few frequencies; if the achieved noise is above m ω^2 by a factor 1/η_D, the assumed detection efficiency is not met. Also check the power scaling: if the noise does not flatten when tuning Ω and \bar{x} according to the SQL condition, the central optimisation claim fails.

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

If this is right

  • A 0.2 mg sensor operating at the SQL could probe vector B-L dark matter couplings down to g ≈ 10^-24 in the mass range 10^-14 - 10^-13 eV, exceeding Eöt-Wash, MICROSCOPE, and LIGO limits by up to an order of magnitude.
  • A future 0.8 g version with ~70 kW lasers could beat existing bounds by up to three orders of magnitude over 10^-14 - 10^-10 eV, and would also reach unexplored parameter space for scalar dark matter coupled to neutrons with a dedicated 50-300 Hz search.
  • The joint optimisation shows that it is better to operate at the SQL off resonance than on resonance above the SQL, and that the SQL is achievable at each target frequency with modest resources.
  • Because the force signal scales with mass while the quantum noise scales only linearly with mass in the geometric optics regime, larger sensors provide a sqrt(m) improvement in signal-to-noise ratio.
  • The experiment can be run at the quantum noise floor down to about 5 Hz, below which seismic noise dominates; additional differential measurements or underground operation could recover some of that low-frequency range.

Where Pith is reading between the lines

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

  • If the η_D ≈ 1 assumption fails in practice because the readout must tap off a fraction of the trapping beam, the projected reach weakens roughly as η_D^{-1/2} in coupling; a prototype measurement of the shot-noise floor would settle this directly.
  • The same joint-optimisation logic—treating trap frequency and readout power as linked—could be applied to other levitated or trapped sensors, including Paul traps and magnetic levitation, potentially revising their projected ULDM sensitivities.
  • The directional sensitivity of the trap could, in the event of a signal, be used to look for the dark matter 'wind' by comparing force amplitudes along x and y, which the paper mentions but leaves to future work.
  • Using a shorter trapping wavelength would lower the laser power needed to reach the SQL, suggesting a concrete upgrade path if high-power short-wavelength lasers become available.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The manuscript proposes a levitated optomechanical force sensor for detecting oscillatory forces from ultralight dark matter. A thin silica plate (0.2 mg benchmark, with a 0.8 g long-term version) is supported by a vertical laser beam and trapped in the transverse directions by counter-propagating beams focused by cylindrical lenses; the reflected light is read out with a balanced homodyne scheme. The core of the paper is a quantum-noise optimization for optically trapped systems in which the mechanical frequency depends on the trapping power. The authors derive an off-resonance standard quantum limit, S_FF^min ≈ mω^2, inventory the relevant classical noises (seismic, residual gas, blackbody, coating vibrations, suspension noise), and then project sensitivities to vector B-L dark matter and to a scalar coupling to neutrons. The central claims are that the 0.2 mg design can reach the SQL with off-the-shelf technology and surpass Eöt-Wash, MICROSCOPE, and LIGO bounds for m_DM in roughly [1e-14, 3e-13] eV by up to an order of magnitude, and that a future 0.8 g sensor could extend this reach by several orders of magnitude with sufficient laser power.

Significance. If the assumptions hold, this is a significant contribution. The paper gives a concrete route toward a milligram-scale optically levitated force sensor for ULDM searches, and it addresses a gap in the optomechanics literature by optimizing quantum noises under the constraint that the mechanical frequency and readout power are not independent. The geometric-optics scaling argument (SNR ∝ √m) is clearly presented and motivates the high-mass design. The manuscript is also unusually transparent: the SQL condition, the noise inventory, and the sensitivity formula are given analytically, with numerical inputs from measured spectra and laboratory references, which makes the projections falsifiable. The main weaknesses are the unquantified assumption η_D≈1 in the detection chain and a numerical/typographical inconsistency in the power requirements for the 0.8 g sensor; both are fixable and do not undermine the basic idea, but they must be addressed before the headline sensitivities can be taken at face value.

major comments (3)
  1. [Sec. IVA, Eqs. (11)-(13)] The SQL and the projected reach assume detection efficiency η_D=1. Equation (11) defines Γ_meas = η_D Γ_recoil, but Eq. (13) drops η_D from the shot-noise force term, which is equivalent to setting η_D=1. Re-optimizing Eq. (13) with the 1/η_D prefactor and fixed ar{x}=h gives S_FF^min ≈ mω^2/√η_D, hence g_min ∝ η_D^{-1/4}. No component-level loss budget is provided for the polarizing beam splitter, quarter-wave plate, AR coatings, photodiode quantum efficiency, or homodyne mode matching. This is load-bearing: at η_D=0.1, the claimed 'up to an order of magnitude' improvement over Eöt-Wash/MICROSCOPE in Sec. VI is reduced to roughly a factor of a few, and the statement that the system operates at the SQL is no longer literally correct. Please provide a quantitative loss budget or present sensitivity curves for several η_D values and state the critical efficiency needed for the stated reach
  2. [Sec. V and Figs. 3-4] The text and figure captions state that the 0.8 g sensor requires two P_L≈70 kW lasers to reach the SQL only up to f=270 Hz. However, the power formula just before this passage, P_L=250 W (m/0.2 mg)(f/1 kHz)^2, gives P_L≈73 W for m=0.8 g and f=270 Hz, and Eq. (17) with ar{x}=h yields the same. The manuscript is therefore internally inconsistent by a factor of 1000. If the intended value is 70 W, all occurrences of '70 kW' should be corrected; if 70 kW is genuinely assumed, the SQL cutoff frequency is ≈8.4 kHz, not 270 Hz, and the stated power-limited scaling g_B-L ∝ m_DM^{9/4} above 270 Hz is incorrect. This affects the long-term B-L projection in Fig. 3 and the scalar-DM projection in Fig. 4.
  3. [Sec. IVA, Eqs. (14)-(18)] The derivation of the SQL as a 'simultaneous' minimization is not a well-defined stationarity problem. Equation (14) is the conditional minimum of S_FF in Ω for fixed ar{x}; Eq. (15) is the conditional minimum in ar{x} for fixed Ω. Setting both partial derivatives to zero has no physical solution for ar{x}>0: the two equations are compatible only in the limit (2/5)ω_L ar{x}→0. The true constrained minimum over the domain ar{x}≥h occurs on the boundary ar{x}=h, and Eq. (16) follows from Eq. (14) in the large-ar{x} limit, not from combining Eqs. (14) and (15). The final value S_FF^min≈mω^2 is correct in this constrained formulation, so the result can be repaired, but the derivation as written should be restated as a constrained minimization with ar{x}=h. This is load-bearing because Eq. (18) underpins all subsequent sensitivity forecasts.
minor comments (5)
  1. [Throughout] Typos should be corrected: 'Insitut' in the first affiliation, 'analgously' (Intro), 'acheive' (Sec. IVA and VI), 'Newtownian' and 'gravtiational' (Sec. IVB5), 'mininimum' (Eq. 15), 'sensitivities' in the Fig. 3/4 captions.
  2. [Fig. 2 caption] The caption says backaction and shot noise are 'plotted according to Eq. 18', but Eq. 18 gives the total optimized quantum noise, not the individual contributions. At the SQL the two components are each half of the total; please clarify how the curves are computed.
  3. [Sec. V / Fig. 3] The LIGO/Virgo bound is shown as a constraint on g_B-L, but Refs. [134-136] are dark-photon kinetic-mixing searches. Please state explicitly how these limits are recast to the B-L gauge coupling, or cite the source of the recast bound, so that the comparison in Fig. 3 is reproducible.
  4. [Sec. IVA / Fig. 2] Eq. (19) gives the vertical-beam leakage backaction as 7.3e-39 N^2/Hz and the text says it is subdominant above f=4 Hz, yet Fig. 2 shows it nearly coincident with the quantum noise at the quantum/seismic transition. Please quantify the margin and explain the apparent proximity.
  5. [Sec. VI] The abstract and conclusion emphasize 'off-the-shelf technologies' and 'moderate resources', while the 0.8 g projection requires either 70 kW per beam as written or 70 W after the typo is fixed, plus a 1 MW intracavity levitation power. Please clarify which of these statements apply to the short-term 0.2 mg design and which are long-term projections, so that the resource claims are not overstated.

Circularity Check

0 steps flagged

No significant circularity: the central SQL sensitivity is derived from the optomechanical Hamiltonian with independent noise inputs; only minor, non-load-bearing self-citations appear.

full rationale

The paper's central claim, the projected B-L ULDM sensitivity in Eq. (34), is not circular. The derivation chain is: Eq. (9) relates the mechanical frequency to the trapping intensity and geometry; Eqs. (10)-(13) express backaction and shot noise in terms of scattered power, mass, frequency, and detection efficiency; minimizing the total quantum force noise yields the SQL condition Eq. (16) and the minimum noise Eq. (18), S_FF^{tot,min} = m omega^2. This result is then inserted into the SNR formula, Eq. (33), and converted to a coupling reach in Eq. (34). The inputs entering this chain are either derived within the paper, standard optomechanical results cited to independent literature, or externally measured quantities (seismic spectra, coating absorption, LIGO surface roughness). No parameter is fitted to the DM signal and then renamed as a prediction. The assumption eta_D ≈ 1 is explicitly stated and quantified in Eqs. (11)-(13); it is a practical efficiency assumption, not a fitted input, and an incorrect value would weaken the reach but does not make the derivation circular. The paper cites the authors' prior work for the seismic isolation system (Refs. [55,65]) and an 'in preparation' companion paper (Ref. [104]), but these are not used to force the central sensitivity result; the SQL itself is checked against independent references [74,109]. The comparison with existing Eöt-Wash, MICROSCOPE, and LIGO bounds is an external benchmark, not an internal target. Overall, the derivation is self-contained and the projected sensitivity is an honest consequence of the stated assumptions.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 0 invented entities

The central SQL result is a parameter-free derivation; the listed items are environmental or design inputs with direct impact on the projected reach. No new particles or forces are introduced.

free parameters (4)
  • Detection efficiency η_D = 1 (assumed)
    Set to unity for the SQL calculation; shot noise scales as 1/η_D, so any loss degrades the projected sensitivity. Assumed in Sec. IVA.
  • Seismic displacement spectral fit = S_xx^gnd(f) = 1e-10 (100 Hz/f)^2 m^2/Hz
    Fitted to measured ground motion at Northwestern; used to project the low-frequency seismic noise floor. If the site is noisier, the quantum-limited region shrinks.
  • Isolation transfer function parameters = 0.25, 1e-3, n=4
    Taken from Ref [55]; the 4-stage isolation provides S_FF ∝ f^{-16}, critical for sub-10 Hz operation.
  • Coating absorption coefficient = α = 6e-3 cm^-1
    From coating literature; sets the sensor equilibrium temperature T≈160 K via Eqs. 21-22.
axioms (4)
  • standard math Fluctuation-dissipation theorem and standard optomechanical quantum noise formulas (backaction and imprecision noise).
    Used in Sec. IVA and App. B to derive the SQL for the trapped system.
  • domain assumption Standard Halo Model with local DM density ρ_DM = 0.3 GeV/cm^3; DM treated as a monochromatic plane wave over coherence times, with isotropic polarization.
    Stated in Sec. II; sets the force amplitude and signal linewidth in the sensitivity analysis.
  • domain assumption Sensor and support plate behave as free test masses for the DM differential acceleration, with the plate's mechanical coupling to the suspension neglected.
    Used in Eq. 7 to compute the differential acceleration; ignores back-action of the suspension on the plate's DM response.
  • ad hoc to paper The vertical levitating beam can be recirculated without introducing additional noise, and the 0.8 g sensor can be levitated with a ~1 MW intracavity power within coating damage thresholds.
    Assumed in Sec. III to make the high-mass sensor feasible; not yet demonstrated.

pith-pipeline@v1.3.0-alltime-deepseek · 40944 in / 41823 out tokens · 365414 ms · 2026-08-03T19:32:33.455736+00:00 · methodology

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read the original abstract

Many well theoretically motivated models of ultralight dark matter are expected to give rise to feeble oscillatory forces on macroscopic objects. Optically trapped sensors have high force sensitivities but have remained relatively unexplored in this context. In this work we propose a new, tunable, optically trapped sensor specifically designed to detect such forces. Our design features a high-mass ($\sim$ mg) plate whose high aspect ratio allows its weight to be supported by a vertical beam without excessive heating. We present the first systematic analysis and optimisation of quantum noises in optically trapped systems and show that our setup has the potential to operate at the standard quantum limit with current off-the-shelf technologies. We demonstrate that our sensor could offer unique access to large regions of uncharted parameter space of vector B-L dark matter, with projected sensitivities that could advance existing limits by several orders of magnitude over a broad range of frequencies.

Figures

Figures reproduced from arXiv: 2512.00166 by Andrew A. Geraci, Hannah Banks, Louis Hamaide, Peter Barker.

Figure 1
Figure 1. Figure 1: FIG. 1. Conceptual perspective view of our proposed setup for sensing forces from dark matter (dashed line) using a silica [PITH_FULL_IMAGE:figures/full_fig_p007_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Comparison of both classical and quantum force noise spectra present in our setup for [PITH_FULL_IMAGE:figures/full_fig_p011_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Projected sensitivies to [PITH_FULL_IMAGE:figures/full_fig_p018_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Projected sensitivies to [PITH_FULL_IMAGE:figures/full_fig_p020_4.png] view at source ↗

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Reference graph

Works this paper leans on

139 extracted references · 16 canonical work pages · cited by 1 Pith paper

  1. [1]

    P. D. Group, R. L. Workman, V. D. Burkert, V. Crede, E. Klempt, U. Thoma, L. Tiator,et al., Review of particle physics, Progress of Theoret- ical and Experimental Physics2022, 083C01 (2022), https://academic.oup.com/ptep/article- pdf/2022/8/083C01/49175539/ptac097.pdf

    2022

  2. [2]

    PANTHEON: Perspectives in As- troparticle and Neutrino THEory with Old and New mes- sengers

    Alternatively, to double the scan rate across DM frequencies, we may tune each direction to detect forces at different frequencies. We also leave the torque sensing capabilities of this system (around the verticalˆz-axis), which could offer the means to probe an increased com- pendium of ULDM couplings such as pseudo-scalar DM coupling to spin, to future ...

    2022

  3. [3]

    Further, the position of the particle is estimated us- ing the optical phase

    The rate of momentum de- position per unit frequency in the trap has the power spectrum Sba FF =ℏ 2 Γrecoil x2 0 .(B3) 24 where ‘ba’ stands for backaction noise. Further, the position of the particle is estimated us- ing the optical phase. Fluctuations of the optical phase therefore lead to uncertainty in the sensor’s position. Al- though these fluctuatio...

  4. [4]

    This condition thus translates to an upper bound on the phonon num- bern ϕ

    We then impose an upper bound on the standard deviation ofϕ,σ ϕ = p ⟨ϕ2⟩at the value beyond which this motion would introduce an excessive noise on the inferred posi- tion of the sensor (in this case,σϕ,rough). This condition thus translates to an upper bound on the phonon num- bern ϕ. Using the steady state relationshipnϕ = Γϕ/γϕ 25 as discussed in Sec. ...

  5. [5]

    Cirelli, A

    M. Cirelli, A. Strumia, and J. Zupan, Dark Matter, (2024), arXiv:2406.01705 [hep-ph]

    Pith/arXiv arXiv 2024

  6. [6]

    Battaglieriet al., US Cosmic Visions: New Ideas in Dark Matter 2017: Community Report, inU.S

    M. Battaglieriet al., US Cosmic Visions: New Ideas in Dark Matter 2017: Community Report, inU.S. Cosmic Visions: New Ideas in Dark Matter(2017) arXiv:1707.04591 [hep-ph]

    Pith/arXiv arXiv 2017

  7. [7]

    Jaeckel and A

    J. Jaeckel and A. Ringwald, The Low-Energy Frontier of Particle Physics, Ann. Rev. Nucl. Part. Sci.60, 405 (2010), arXiv:1002.0329 [hep-ph]

    Pith/arXiv arXiv 2010

  8. [8]

    Antypaset al., New Horizons: Scalar and Vector Ultralight Dark Matter, (2022), arXiv:2203.14915 [hep- ex]

    D. Antypaset al., New Horizons: Scalar and Vector Ultralight Dark Matter, (2022), arXiv:2203.14915 [hep- ex]

    arXiv 2022

  9. [9]

    Jaeckel, G

    J. Jaeckel, G. Rybka, and L. Winslow, Report of the Topical Group on Wave Dark Matter for Snowmass 2021, Snowmass 2021 (2022), arXiv:2209.08125 [hep- ph]

    Pith/arXiv arXiv 2021

  10. [10]

    R. D. Peccei and H. R. Quinn,CPconservation in the presence of pseudoparticles, Phys. Rev. Lett.38, 1440 (1977)

    1977

  11. [11]

    R. D. Peccei and H. R. Quinn, Constraints Imposed by CP Conservation in the Presence of Instantons, Phys. Rev. D16, 1791 (1977)

    1977

  12. [12]

    Weinberg, A New Light Boson?, Phys

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

    1978

  13. [13]

    Wilczek, Problem of StrongPandTInvariance in the Presence of Instantons, Phys

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

    1978

  14. [14]

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

    1980

  15. [15]

    M. Dine, W. Fischler, and M. Srednicki, A Simple Solu- tion to the Strong CP Problem with a Harmless Axion, Phys. Lett. B104, 199 (1981)

    1981

  16. [16]

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

    1980

  17. [17]

    J. E. Kim, Weak Interaction Singlet and Strong CP In- variance, Phys. Rev. Lett.43, 103 (1979)

    1979

  18. [18]

    Preskill, M

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

    1983

  19. [19]

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

    1983

  20. [20]

    Dine and W

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

    1983

  21. [21]

    Svrcek and E

    P. Svrcek and E. Witten, Axions In String Theory, JHEP06, 051, arXiv:hep-th/0605206

    Pith/arXiv arXiv

  22. [22]

    March-Russell, String Axiverse, Phys

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

    Pith/arXiv arXiv 2010

  23. [23]

    Shifman, A

    M. Shifman, A. Vainshtein, and V. Zakharov, Can con- finement ensure natural cp invariance of strong interac- tions?, Nuclear Physics B166, 493 (1980)

    1980

  24. [24]

    Di Luzio, M

    L. Di Luzio, M. Giannotti, E. Nardi, and L. Visinelli, The landscape of QCD axion models, Phys. Rept.870, 1 (2020), arXiv:2003.01100 [hep-ph]

    Pith/arXiv arXiv 2020

  25. [25]

    K. Choi, S. H. Im, and C. Sub Shin, Recent Progress in the Physics of Axions and Axion-Like Particles, Ann. Rev. Nucl. Part. Sci.71, 225 (2021), arXiv:2012.05029 [hep-ph]

    Pith/arXiv arXiv 2021

  26. [26]

    B.Holdom,Twou(1)’sandepsilonchargeshifts,Physics Letters B166, 196 (1986)

    1986

  27. [27]

    Fayet, Extra u(1)’s and new forces, Nuclear Physics B347, 743 (1990)

    P. Fayet, Extra u(1)’s and new forces, Nuclear Physics B347, 743 (1990)

    1990

  28. [28]

    Fabbrichesi, E

    M. Fabbrichesi, E. Gabrielli, and G. Lanfranchi, The Dark Photon, SpringerBriefs in Physics 2020 10.1007/978-3-030-62519-1 (2020), arXiv:2005.01515 [hep-ph]

    Pith/arXiv arXiv 2020

  29. [29]

    S. A. Abel, M. D. Goodsell, J. Jaeckel, V. V. Khoze, and A. Ringwald, Kinetic Mixing of the Photon with Hidden U(1)s in String Phenomenology, JHEP07, 124, arXiv:0803.1449 [hep-ph]

    Pith/arXiv arXiv

  30. [30]

    Goodsell, J

    M. Goodsell, J. Jaeckel, J. Redondo, and A. Ring- wald, Naturally Light Hidden Photons in LARGE Volume String Compactifications, JHEP11, 027, arXiv:0909.0515 [hep-ph]

    Pith/arXiv arXiv

  31. [31]

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

    Pith/arXiv arXiv 2011

  32. [32]

    Arias, D

    P. Arias, D. Cadamuro, M. Goodsell, J. Jaeckel, J. Re- dondo, and A. Ringwald, WISPy Cold Dark Matter, JCAP06, 013, arXiv:1201.5902 [hep-ph]

    Pith/arXiv arXiv

  33. [33]

    P. W. Graham, J. Mardon, and S. Rajendran, Vector Dark Matter from Inflationary Fluctuations, Phys. Rev. D93, 103520 (2016), arXiv:1504.02102 [hep-ph]

    Pith/arXiv arXiv 2016

  34. [34]

    Agrawal, N

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

    Pith/arXiv arXiv 2020

  35. [35]

    Bastero-Gil, J

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

    Pith/arXiv arXiv

  36. [36]

    J. A. Dror, K. Harigaya, and V. Narayan, Parametric Resonance Production of Ultralight Vector Dark Mat- ter, Phys. Rev. D99, 035036 (2019), arXiv:1810.07195 [hep-ph]

    Pith/arXiv arXiv 2019

  37. [37]

    R. T. Co, A. Pierce, Z. Zhang, and Y. Zhao, Dark Pho- ton Dark Matter Produced by Axion Oscillations, Phys. Rev. D99, 075002 (2019), arXiv:1810.07196 [hep-ph]

    Pith/arXiv arXiv 2019

  38. [38]

    Caputo, A

    A. Caputo, A. J. Millar, C. A. J. O’Hare, and E. Vitagliano, Dark photon limits: A handbook, Phys. Rev. D104, 095029 (2021), arXiv:2105.04565 [hep-ph]

    Pith/arXiv arXiv 2021

  39. [39]

    Adshead, K

    P. Adshead, K. D. Lozanov, and Z. J. Weiner, Dark photon dark matter from an oscillating dilaton, Phys. Rev. D107, 083519 (2023), arXiv:2301.07718 [hep-ph]

    Pith/arXiv arXiv 2023

  40. [40]

    Cyncynates and Z

    D. Cyncynates and Z. J. Weiner, Detectable and Defect- Free Dark Photon Dark Matter, Phys. Rev. Lett.134, 211002 (2025), arXiv:2310.18397 [hep-ph]. 26

    Pith/arXiv arXiv 2025

  41. [41]

    Cyncynates and Z

    D. Cyncynates and Z. J. Weiner, Experimental targets for dark photon dark matter, Phys. Rev. D111, 103535 (2025), arXiv:2410.14774 [hep-ph]

    Pith/arXiv arXiv 2025

  42. [42]

    Dimopoulos and G

    S. Dimopoulos and G. F. Giudice, Macroscopic forces from supersymmetry, Phys. Lett. B379, 105 (1996), arXiv:hep-ph/9602350

    Pith/arXiv arXiv 1996

  43. [43]

    Arkani-Hamed, L

    N. Arkani-Hamed, L. J. Hall, D. Tucker-Smith, and N. Weiner, Solving the hierarchy problem with exponen- tially large dimensions, Phys. Rev. D62, 105002 (2000), arXiv:hep-ph/9912453

    Pith/arXiv arXiv 2000

  44. [44]

    C. P. Burgess, A. Maharana, and F. Quevedo, Uber-naturalness: unexpectedly light scalars from supersymmetric extra dimensions, JHEP05, 010, arXiv:1005.1199 [hep-th]

    Pith/arXiv arXiv

  45. [45]

    Cicoli, C

    M. Cicoli, C. P. Burgess, and F. Quevedo, Anisotropic Modulus Stabilisation: Strings at LHC Scales with Micron-sized Extra Dimensions, JHEP10, 119, arXiv:1105.2107 [hep-th]

    Pith/arXiv arXiv

  46. [46]

    Damour and A

    T. Damour and A. Polyakov, The string dilation and a leastcouplingprinciple,NuclearPhysicsB423,532–558 (1994)

    1994

  47. [47]

    Taylor and G

    T. Taylor and G. Veneziano, Dilaton couplings at large distances, Physics Letters B213, 450 (1988)

    1988

  48. [48]

    Piazza and M

    F. Piazza and M. Pospelov, Sub-eV scalar dark matter through the super-renormalizable Higgs portal, Phys. Rev. D82, 043533 (2010), arXiv:1003.2313 [hep-ph]

    Pith/arXiv arXiv 2010

  49. [49]

    Banerjee, H

    A. Banerjee, H. Kim, and G. Perez, Coherent relax- ion dark matter, Phys. Rev. D100, 115026 (2019), arXiv:1810.01889 [hep-ph]

    Pith/arXiv arXiv 2019

  50. [50]

    Fayet, Effects of the Spin 1 Partner of the Goldstino (Gravitino) on Neutral Current Phenomenology, Phys

    P. Fayet, Effects of the Spin 1 Partner of the Goldstino (Gravitino) on Neutral Current Phenomenology, Phys. Lett. B95, 285 (1980)

    1980

  51. [51]

    Fayet, On the Search for a New Spin 1 Boson, Nucl

    P. Fayet, On the Search for a New Spin 1 Boson, Nucl. Phys. B187, 184 (1981)

    1981

  52. [52]

    Badurinaet al., AION: An Atom Interferom- eter Observatory and Network, JCAP05, 011, arXiv:1911.11755 [astro-ph.CO]

    L. Badurinaet al., AION: An Atom Interferom- eter Observatory and Network, JCAP05, 011, arXiv:1911.11755 [astro-ph.CO]

    Pith/arXiv arXiv 1911

  53. [53]

    Arvanitaki, J

    A. Arvanitaki, J. Huang, and K. Van Tilburg, Searching for dilaton dark matter with atomic clocks, Phys. Rev. D91, 015015 (2015), arXiv:1405.2925 [hep-ph]

    Pith/arXiv arXiv 2015

  54. [54]

    D. W. P. Amaral, D. G. Uitenbroek, T. H. Oosterkamp, andC.D.Tunnell,FirstSearchforUltralightDarkMat- ter Using a Magnetically Levitated Particle, Phys. Rev. Lett.134, 251001 (2025), arXiv:2409.03814 [hep-ph]

    arXiv 2025

  55. [55]

    Kalia, D

    S. Kalia, D. Budker, D. F. J. Kimball, W. Ji, Z. Liu, A. O. Sushkov, C. Timberlake, H. Ulbricht, A. Vinante, and T. Wang, Ultralight dark matter detection with lev- itated ferromagnets, Phys. Rev. D110, 115029 (2024), arXiv:2408.15330 [hep-ph]

    Pith/arXiv arXiv 2024

  56. [56]

    Carney, A

    D. Carney, A. Hook, Z. Liu, J. M. Taylor, and Y. Zhao, Ultralight dark matter detection with mechan- ical quantum sensors, New J. Phys.23, 023041 (2021), arXiv:1908.04797 [hep-ph]

    Pith/arXiv arXiv 2021

  57. [57]

    Higgins, S

    G. Higgins, S. Kalia, and Z. Liu, Maglev for dark mat- ter: Dark-photon and axion dark matter sensing with levitated superconductors, Phys. Rev. D109, 055024 (2024), arXiv:2310.18398 [hep-ph]

    Pith/arXiv arXiv 2024

  58. [58]

    Deshpande, A

    T. Deshpande, A. Ionescu, N. Miller, Z. Wang, G. Gabrielse, A. A. Geraci, and T. Kovachy, Demonstra- tion that Differential Length Changes of Optical Cav- ities are a Sensitive Probe for Ultralight Dark Matter, (2024), arXiv:2412.20623 [hep-ex]

    arXiv 2024

  59. [59]

    R. Li, S. Lin, L. Zhang, C. Duan, P. Huang, and J. Du, Search for Ultralight Dark Matter with a Fre- quency Adjustable Diamagnetic Levitated Sensor, Chin. Phys. Lett.40, 069502 (2023), arXiv:2307.15758 [astro- ph.CO]

    Pith/arXiv arXiv 2023

  60. [60]

    Manley, M

    J. Manley, M. D. Chowdhury, D. Grin, S. Singh, and D. J. Wilson, Searching for vector dark matter with an optomechanical accelerometer, Phys. Rev. Lett.126, 061301 (2021), arXiv:2007.04899 [quant-ph]

    Pith/arXiv arXiv 2021

  61. [61]

    Manley, R

    J. Manley, R. Stump, D. Wilson, D. Grin, and S. Singh, Searching for scalar dark matter with compact mechan- ical resonators, Phys. Rev. Lett.124, 151301 (2020), arXiv:1910.07574 [astro-ph.IM]

    Pith/arXiv arXiv 2020

  62. [62]

    M. D. Chowdhury, J. P. Manley, C. A. Condos, A. R. Agrawal, and D. J. Wilson, Optomechanical ac- celerometer search for ultralight dark matter (2025), arXiv:2509.12175 [hep-ex]

    Pith/arXiv arXiv 2025

  63. [63]

    Tsaturyan, A

    Y. Tsaturyan, A. Barg, E. S. Polzik, and A. Schliesser, Ultracoherent nanomechanical resonators via soft clampinganddissipationdilution,NatureNanotech.12, 776 (2017), arXiv:1608.00937 [quant-ph]

    Pith/arXiv arXiv 2017

  64. [64]

    Catalini, Y

    L. Catalini, Y. Tsaturyan, and A. Schliesser, Soft- clamped phononic dimers for mechanical sensing and transduction, Phys. Rev. Appl.14, 014041 (2020)

    2020

  65. [65]

    Aspelmeyer, T

    M. Aspelmeyer, T. J. Kippenberg, and F. Marquardt, Cavity Optomechanics, Rev. Mod. Phys.86, 1391 (2014), arXiv:1303.0733 [cond-mat.mes-hall]

    Pith/arXiv arXiv 2014

  66. [66]

    Reinhardt, T

    C. Reinhardt, T. Müller, A. Bourassa, and J. C. Sankey, Ultralow-noise sin trampoline resonators for sensing and optomechanics, Phys. Rev. X6, 021001 (2016)

    2016

  67. [67]

    Matsumoto, M

    N. Matsumoto, M. Sugawara, S. Suzuki, N. Abe, K. Ko- mori, Y. Michimura, Y. Aso, S. B. Cataño-Lopez, and K. Edamatsu, Demonstration of displacement sensing of a mg-scale pendulum for mm- and mg- scale grav- ity measurements, Phys. Rev. Lett.122, 071101 (2019), arXiv:1809.05081 [quant-ph]

    Pith/arXiv arXiv 2019

  68. [68]

    A. A. Geraci, C. Bradley, D. Gao, J. Weinstein, and A. Derevianko, Searching for ultralight dark matter with optical cavities, Physical Review Letters123, 10.1103/physrevlett.123.031304 (2019)

    work page doi:10.1103/physrevlett.123.031304 2019

  69. [69]

    B. P. Abbottet al.(LIGO Scientific), LIGO: The Laser interferometer gravitational-wave observatory, Rept. Prog. Phys.72, 076901 (2009), arXiv:0711.3041 [gr-qc]

    Pith/arXiv arXiv 2009

  70. [70]

    W. P. Bowen and G. J. Milburn,Quantum Optomechan- ics(CRC Press, Boca Raton, FL, 2015)

    2015

  71. [71]

    M. G. Latorre, A. Paradkar, D. Hambraeus, G. Hig- gins, and W. Wieczorek, A chip-based superconducting magnetic trap for levitating superconducting micropar- ticles, IEEE Transactions on Applied Superconductivity 32, 1–5 (2022)

    2022

  72. [72]

    M. J. Biercuk, H. Uys, J. W. Britton, A. P. VanDevender, and J. J. Bollinger, Ultrasensitive force and displacement detection using trapped ions 10.1038/NNANO.2010.165 (2010), arXiv:1004.0780 [quant-ph]

    Pith/arXiv arXiv 2010

  73. [73]

    P. A. Ivanov, N. V. Vitanov, and K. Singer, High- precision force sensing using a single trapped ion, Sci- entific Reports6, 10.1038/srep28078 (2016)

    doi:10.1038/srep28078 2016

  74. [74]

    W. Ji, C. Xu, G. Qu, and D. Budker, Levitated sen- sor for magnetometry in ambient environment (2025), arXiv:2504.21524 [physics.ins-det]

    Pith/arXiv arXiv 2025

  75. [75]

    Millen, T

    J. Millen, T. S. Monteiro, R. Pettit, and A. N. Vami- vakas, Optomechanics with levitated particles, Reports on Progress in Physics83, 026401 (2020)

    2020

  76. [76]

    V. Jain, J. Gieseler, C. Moritz, C. Dellago, R. Quidant, and L. Novotny, Direct measurement of photon recoil 27 from a levitated nanoparticle, Phys. Rev. Lett.116, 243601 (2016)

    2016

  77. [77]

    Magrini, P

    L. Magrini, P. Rosenzweig, C. Bach, A. Deutschmann- Olek, S. G. Hofer, S. Hong, N. Kiesel, A. Kugi, and M. Aspelmeyer, Real-time optimal quantum control of mechanical motion at room temperature, Nature 10.1038/s41586-021-03602-3 (2020), arXiv:2012.15188 [quant-ph]

    Pith/arXiv arXiv 2020

  78. [78]

    D.C.MooreandA.A.Geraci,Searchingfornewphysics using optically levitated sensors, Quantum Science and Technology6, 014008 (2021)

    2021

  79. [79]

    A.Ashkin,Forcesofasingle-beamgradientlasertrapon a dielectric sphere in the ray optics regime, Biophysical Journal61, 569 (1992)

    1992

  80. [80]

    A. Ashkin, Optical trapping and manipulation of neutral particles using lasers, Proceedings of the National Academy of Sciences94, 4853 (1997), https://www.pnas.org/doi/pdf/10.1073/pnas.94.10.4853

    work page doi:10.1073/pnas.94.10.4853 1997

Showing first 80 references.