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TOrsion-Bar Antenna: A Ground-Based Detector for Low-Frequency Gravity Gradient Measurement

T0 review · 3 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read A ground-based torsion-pendulum pair aims to detect gravitational waves from 1 mHz to 10 Hz.

desk verdict A candid status report on the TOBA program: useful as a review, honest about unresolved technical gaps, but the final sensitivity is a design target resting on unproven loss values; the appendix has a sign typo that should be fixed. read the letter →

arxiv 2412.01323 v1 pith:4BYTH3YW submitted 2024-12-02 gr-qc astro-ph.IMphysics.ins-det

Satoru Takano , Tomofumi Shimoda , Yuka Oshima , Ching Pin Ooi , Perry William Fox Forsyth , Mengdi Cao , Kentaro Komori , Yuta Michimura
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Ryosuke Sugimoto Nobuki Kame Shingo Watada Takaaki Yokozawa Shinji Miyoki Tatsuki Washimi Masaki Ando
This is my paper · ORCID
classification gr-qcastro-ph.IMphysics.ins-det PACS 04.30.-w04.80.Nn
keywords torsion-barantennalow-frequencygravitationalwavestorsionpendulumgravitygradiometerintermediate-massblackholebinariesstochasticwavebackgroundNewtoniannoisecryogenicsuspension
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper proposes the Torsion-Bar Antenna (TOBA), a ground-based detector that uses the very low resonant frequency of a torsion pendulum to sense gravity gradients in the 1 mHz–10 Hz band, a range normally reserved for space missions. Its stated final goal is a strain sensitivity of $10^{-19}/\sqrt{\mathrm{Hz}}$ at 0.1 Hz with a 10 m detector, sufficient to see intermediate-mass black hole binary mergers out to 10 Gpc and to place a one-year constraint on the stochastic gravitational-wave background of $\Omega_{\mathrm{GW}}\simeq 10^{-7}$. The intermediate Phase-III prototype targets $10^{-15}/\sqrt{\mathrm{Hz}}$ at 0.1 Hz, which would directly measure Newtonian noise and could detect large earthquakes about 10 seconds before seismic waves. The paper reviews prototype results: a magnetically levitated proof of concept, a two-bar wire-suspended prototype, a seismic cross-coupling reduction experiment, a cryogenic suspension that cooled a bar to 6.1 K, and a cryogenic monolithic interferometer operated at 12 K. A sympathetic reader should take this as a status report on a technically demanding but partially demonstrated path to a new ground-based gravitational-wave window.

What carries the argument

The load-bearing element is the torsion pendulum: a long bar suspended by a thin wire, with rotational resonant frequency near 1 mHz. A gravitational wave along the detector axis exerts a tidal torque through the quadrupole moment $q_\times=\int dV\,\rho(x^2-y^2)$, causing a rotation read out by Fabry–Pérot cavities. The two bars are matched and oriented orthogonally so that common noises (seismic motion, suspension fluctuations, temperature drift) cancel in the differential signal. The design noise budget is assembled from radiation-pressure shot noise, suspension thermal noise, and internal bar thermal noise, with quantum noise and bar thermal noise ending up as the limiting contributions.

What would settle it

Measure the mechanical loss angle of a full-scale 10 m aluminium torsion bar suspended by a single silicon fibre at 4 K; if the wire loss angle exceeds $10^{-10}$ or the bar loss exceeds $10^{-7}$, the thermal noise floor would sit above the design curve and the target sensitivity could not be reached.

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Extended reading notes

Core claim

The central claim is that two orthogonally suspended torsion bars, read out by interferometry, form a ground-based gravity-gradient detector whose low-frequency response is set by the torsional transfer function $H_\times(f) \simeq \frac{1}{2} \frac{f^2}{f_0^2(1+i\phi_{\mathrm{rot}})-f^2}$, with $f_0 \sim 1$ mHz and $\phi_{\mathrm{rot}}$ the suspension loss angle. Because the resonant frequency is so low, the detector is sensitive near 0.1 Hz, where conventional ground interferometers are limited by seismic and Newtonian noise, and the differential readout of two identical bars rejects common-mode disturbances. The paper's design target is $10^{-19}/\sqrt{\mathrm{Hz}}$ at 0.1 Hz for the 10 m Final TOBA, with a noise budget dominated by quantum noise and bar thermal noise (wire loss angle $10^{-10}$, internal bar loss $10^{-7}$, at 4 K), and a near-term Phase-III goal of $10^{-15}/\sqrt{\mathrm{Hz}}$ for scientific applications. It reports that each subsystem has been demonstrated separately, but not yet at the level required for the final sensitivity.

Load-bearing premise

The final sensitivity relies on achieving material losses and seismic isolation roughly three orders of magnitude better than anything demonstrated, specifically a wire loss angle of $10^{-10}$, an internal bar loss of $10^{-7}$ at 4 K, and vertical vibration suppression below $10^{-7}$ m/$\sqrt{\mathrm{Hz}}$ at 0.1 Hz.

Editorial extensions

If this is right

  • A 10 m detector at the target sensitivity would let ground-based instruments search for intermediate-mass black hole binary mergers out to redshift $z\sim 2.4$.
  • The same sensitivity would constrain the stochastic gravitational-wave background to $\Omega_{\mathrm{GW}}\simeq 10^{-7}$ after one year of observation, improving on the Big Bang nucleosynthesis bound.
  • At the Phase-III sensitivity, TOBA would directly measure Newtonian noise around 0.1 Hz, providing the first test of the models used to cancel this noise in future ground detectors.
  • Two such instruments separated by about 75 km could locate a magnitude-7 earthquake and issue a warning roughly 10 seconds before the P-wave arrival.
  • The demonstrated components—cryogenic suspension, active isolation, and monolithic interferometric readout—together form a concrete scaling path toward the 10 m final detector.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • An extension implicit in the design: at the Phase-III sensitivity the instrument is effectively a gravity gradiometer, so it could be used for local seismic hazard monitoring, volcanic deformation studies, and other geophysical applications beyond earthquake early warning.
  • The required loss values ($10^{-10}$ wire, $10^{-7}$ bar) have not been demonstrated on a 10 m scale; a prudent next step would be a 1-m cryogenic bar experiment to verify the thermal noise floor before committing to the full design.
  • Because TOBA's band overlaps with the proposed space-based detectors, a ground-based detector reaching $10^{-19}$ could serve as a cross-check or trigger for space missions, though the paper does not discuss such coordination.
  • A null test of the common-mode rejection scheme is to build two bars with deliberately different arm lengths; if the differential signal vanishes for non-tidal common noise but persists for a known tidal source, the rejection model is confirmed.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper is a review/status report on the Torsion-Bar Antenna (TOBA), a ground-based detector concept for gravitational waves in the 1 mHz–10 Hz band. It describes the operating principle of twin torsion pendulums, the design sensitivity of a proposed 10-m 'Final TOBA' (10^-19/√Hz at 0.1 Hz), and the expected astrophysical and geophysical targets (IMBH mergers, stochastic background, Newtonian noise, early earthquake detection). It then summarizes the Phase-I and Phase-II prototype experiments and their upper limits, the seismic cross-coupling studies, and the current Phase-III developments: cryogenic suspension, active vibration isolation, and a cryogenic monolithic interferometer. The paper concludes with a discussion of scaling issues for the 10-m detector.

Significance. TOBA occupies a distinctive niche among proposed ground-based low-frequency gravitational-wave detectors, and this manuscript provides a useful, consolidated description of the program's current status. Its strengths are honesty about demonstrated performance (e.g., the AVIS result is explicitly 'still not sufficient') and the inclusion of specific achieved sensitivities and upper limits from earlier publications. The scientific motivation is well presented, particularly the possibility of directly measuring Newtonian noise at ~0.1 Hz. If the Phase-III sensitivity of ~10^-15/√Hz is reached, the geophysical applications are credible. The claims about the Final TOBA's reach, however, are design projections that depend on loss and isolation parameters not yet demonstrated at the required scale, and the paper's own appendix contains a sign error in the response derivation.

major comments (3)
  1. [VI.B, Eq. (17)] Equation (17) has the response denominator written as κ(1+iφ_rot)+(2πf)^2 I, i.e., +f^2, while Eq. (3), Eq. (21), and Eq. (25) use (1+iφ_rot)f0^2 - f^2. Fourier-transforming Eq. (16) gives I[-(2πf)^2 θ] + κθ = N, so the denominator must contain -f^2. The following expression in Eq. (17) also drops the 'i' before φ_rot. This is a straightforward but load-bearing error in the derivation of the detector response; please correct Eq. (17) (and the sign in Eq. (19) if it follows from this step).
  2. [II.B and IV.C.2] The Final TOBA noise budget in Fig. 2 is controlled by the assumed suspension loss angle φ_wire=10^-10 and bar loss φ_bar=10^-7 at 4 K, but the only measured loss cited for silicon flexures at cryogenic temperatures is φ<10^-8 (Section IV.A.1). In addition, the AVIS prototype's measured suppression is 10^3 vertically at 0.7 Hz and 3×10^-2 horizontally at 1.7 Hz, which the text itself says is 'still not sufficient' (Section IV.C.2). The paper should either provide a quantitative development path (or citations) from these demonstrated values to the Final TOBA assumptions, or explicitly label the Section II.C scientific-reach estimates as conditional on those unvalidated parameters.
  3. [IV.C.3] The demonstrated readout sensitivity of the cryogenic monolithic interferometer, 3.6×10^-14 m/√Hz at 0.1 Hz, is about 600 times worse than the Phase-III requirement of 6×10^-17 m/√Hz. Since the paper identifies this interferometer as a key subsystem and the result was limited by seismic noise rather than fundamental noise, please state the planned improvements (e.g., the AVIS) that would close this gap, or clarify why the requirement can still be met.
minor comments (5)
  1. [III.B] The compiled manuscript contains visible text corruption around Section III.B (e.g., the phrase '5 Experiments 5.1 Setup') and in the Figure 5 caption; please ensure the submitted version is the clean PDF.
  2. [V] The funding statement misspells 'Funding' as 'Fundiwding'; this should be corrected.
  3. [II.B and Fig. 2] The loss-angle symbol is introduced as φ_rot in Eq. (3) but appears as φ_wire in Fig. 2 and Section II.B; please use one symbol or explicitly define both with distinct names.
  4. [Fig. 3 caption] In the caption of Fig. 3, the axis labels appear as '10□1' and '10□10' rather than proper superscripts; please check the rendered figure for missing negative signs and format the exponents correctly.
  5. [VI] The appendix is labeled 'VI. DERIVATION...' but referred to as 'Appendix VI' in Section II.A; if the journal places appendices at the end, please renumber or re-label for consistency.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity; the paper is an overview whose design targets are attributed to prior work and whose one derivation is parameter-free.

full rationale

This paper is an overview and design review, not a derivation of new results from fitted data. The only first-principles derivation is Appendix VI, which computes the torsion-pendulum response from the gravitational force equation, the quadrupole definition, and the damped harmonic oscillator equation (Eqs. 4-16); no parameter is adjusted to match the claimed H_A(f). The final sensitivity of 10^-19/sqrt(Hz) and the IMBH/SGWB reach are explicitly attributed to prior work [9] and are stated as design goals, not as predictions validated here; the noise budget in Fig. 2 is labeled 'The design sensitivity of the Final TOBA [9]'. Phase-III expectations likewise cite prior studies [16,29,32]. Thus the self-citations are frequent but not load-bearing in the sense of hiding a reduction: they are ordinary references to the group's own program rather than an unverified premise smuggled in as external support. The AVIS shortfall (vertical suppression by 10^3 versus the requirement) and the unmeasured loss angles (phi_wire = 10^-10, phi_bar = 10^-7) are validation gaps and correctness risks, not circularity, especially because the paper explicitly states the performance 'was still not sufficient'. The sign inconsistency between Eq. (17) and Eq. (21) is a typographical/correctness issue in an otherwise standard derivation, not a circular step. No equation in this paper is fitted to the quantity it claims to predict, so there is no reduction of a 'prediction' to its own input.

Assumptions & free parameters 0 free parameters · 3 assumptions · 0 invented entities

The paper rests on standard linearized gravity and mechanics, plus design assumptions about achievable mechanical losses and vibration isolation. No free parameters are fitted to data in this review.

assumptions (3)
  • standard math The gravitational wave can be treated as a small perturbation of flat spacetime, and tidal forces act on each element of the bar with dF_i = (1/2) m h_ddot_ij x_j.
    Invoked in Appendix VI A, Eq. (4), from Maggiore [40].
  • domain assumption The bar is small compared to the gravitational wave wavelength, so the quadrupole approximation holds.
    Used in deriving the torque in Appendix VI; the paper states 'Within a region whose scale is small enough compared to the wavelength of the GW'.
  • domain assumption The two torsion pendulums can be made with sufficiently matched mechanical parameters that common-mode noise is rejected.
    Section II A claims common mode rejection is 'one of the significant advantages' but this relies on matching parameters; no tolerance analysis is given.

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Cite this review

Pith. "Pith review of TOrsion-Bar Antenna: A Ground-Based Detector for Low-Frequency Gravity Gradient Measurement." pith.science (2026). https://pith.science/paper/4BYTH3YW

@misc{pith2026241201323,
  author       = {Pith},
  title        = {Pith review of: TOrsion-Bar Antenna: A Ground-Based Detector for Low-Frequency Gravity Gradient Measurement},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/4BYTH3YW}},
  note         = {Machine review of arXiv:2412.01323}
}
read the original abstract

The Torsion-Bar Antenna (TOBA) is a torsion pendulum-based gravitational detector developed to observe gravitational waves in frequencies between 1 mHz and 10 Hz. The low resonant frequency of the torsion pendulum enables observation in this frequency band on the ground. The final target of TOBA is to observe gravitational waves with a 10 m detector and expand the observation band of gravitational waves. In this paper, an overview of TOBA, including the previous prototype experiments and the current ongoing development, is presented.

Figures

Figures reproduced from arXiv: 2412.01323 by the authors.

Figure 1
Figure 1. FIG. 1. Principle of TOBA. Two test mass bars are suspended in the horizontal plane independently and orthogonally. Dashed lines indicate [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. The design sensitivity of the Final TOBA [9]. The blue and green lines show the photon shot noise and radiation pressure noise, [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. The sensitivity of prototype experiments. The blue and red curves are the achieved sensitivities of Phase-I [30] and Phase-II [31]. [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: FIG. 4. The configuration of Phase-I TOBA. ( [PITH_FULL_IMAGE:figures/full_fig_p005_4.png]
Figure 5.2
Figure 5.2. Figure 5.2: A picure of the FIG. 5. The configuration of Phase-II TOBA. ( [PITH_FULL_IMAGE:figures/full_fig_p006_5_2.png]
Figure 6
Figure 6. Figure 6: FIG. 6. Thes etup for research on seismic cross-coupling reduction. ( [PITH_FULL_IMAGE:figures/full_fig_p007_6.png]
Figure 7
Figure 7. Figure 7: FIG. 7. Configuration of Phase-III TOBA. Inside a vacuum chamber, two radiation shields are connected to the cryocooler surrounding the [PITH_FULL_IMAGE:figures/full_fig_p008_7.png]
Figure 8
Figure 8. Figure 8: FIG. 8. The designed noise budget of Phase-III TOBA. The green line shows photon shot noise. The red line is the thermal noise of the [PITH_FULL_IMAGE:figures/full_fig_p009_8.png]
Figure 9
Figure 9. Figure 9: FIG. 9. The cooling curve of the cryogenic torsion pendulum measured in [29]. The sky blue curve shows the temperature of the test mass [PITH_FULL_IMAGE:figures/full_fig_p010_9.png]
Figure 10
Figure 10. Figure 10: FIG. 10. The achieved performance of AVIS. The gray line indicates the requirement for AVIS. The red, blue, and green dashed lines are the [PITH_FULL_IMAGE:figures/full_fig_p011_10.png]
Figure 11
Figure 11. Figure 11: FIG. 11. The achieved sensitivity of the cryogenic monolithic interferometer [38]. The sensitivity shown as the black curve is limited [PITH_FULL_IMAGE:figures/full_fig_p012_11.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

50 extracted references · 46 canonical work pages

  1. [9]

    The achieved performance is shown in Figure 10

    Active Vibration Isolation System A prototype of the vibration isolation system was developed and the performance was tested in 2019 without the suspension system. The achieved performance is shown in Figure 10. The vertical seismic vibration was suppressed by 10 3 around 0.7 Hz and the horizontal vibration by 3× 10−2 around 1.7 Hz. The performance was st...

    work page 2019

  2. [1]

    For future ground-based GW detectors, NN is assumed to be the dominant noise source in frequency bands below 10 Hz [17, 18], and its mitigation method is discussed in [19, 20]

    Newtonian Noise Measurement NN is a fundamental noise source for GW detectors. For future ground-based GW detectors, NN is assumed to be the dominant noise source in frequency bands below 10 Hz [17, 18], and its mitigation method is discussed in [19, 20]. Several models describe the mechanism of NN generation [21–24]. However, so far, NN has not been meas...

    work page

  3. [2]

    This scheme pays attention to the change that occurs on the timescale of ∼10 s–100 s, which corresponds to the frequency band of TOBA

    Early Earthquake Detection It is proposed that transient changes in gravitational fields introduced by large earthquakes can be detected by gravimeters and gravity gradiometers [26]. This scheme pays attention to the change that occurs on the timescale of ∼10 s–100 s, which corresponds to the frequency band of TOBA. Because the change in the gravitational...

    work page 2010

  4. [3]

    The required temperature for Phase-III TOBA is set to 4 K, and it is also desirable to finish the cooling within an acceptable time for operation

    Cryogenic Suspension System The cryogenic system is one of the essential parts of Phase-III TOBA for reducing thermal noise. The required temperature for Phase-III TOBA is set to 4 K, and it is also desirable to finish the cooling within an acceptable time for operation. Another important point is to suppress additional noises introduced by the cooling sy...

    work page

  5. [4]

    A VIS is a feedback system that consists of multiple sensors and hexapod actuators

    Active Vibration Isolation System To suppress the seismic vibration, an active vibration isolation system (A VIS) is implemented at the suspension point. A VIS is a feedback system that consists of multiple sensors and hexapod actuators. Six seismometers are arranged to monitor all degrees of freedom of the suspension table. The signals from the seismomet...

    work page

  6. [5]

    The surface of the test mass bar is polished and coated so that it works as mirrors, to reduce the relative tilt of the mirrors which introduces the cross-coupling

    Interferometric Readout System To achieve the target sensitivity, we use Fabry–P´erot cavities to measure the motion of the bars. The surface of the test mass bar is polished and coated so that it works as mirrors, to reduce the relative tilt of the mirrors which introduces the cross-coupling. The other mirrors, which form Fabry–P´erot cavities with the s...

    work page

  7. [6]

    Therefore, it is expected that Phase-III TOBA can measure NN directly with the target sensitivity

    Newtonian Noise Measurement The estimated level of NN is in the order of 10 −15/ √ Hz around 0.1 Hz. Therefore, it is expected that Phase-III TOBA can measure NN directly with the target sensitivity. Although the frequency band in which Phase-III TOBA can observe NN is below the observation band of the ground-based interferometric detectors, measurement w...

    work page

  8. [7]

    It has been shown that for earthquakes with a magnitude of 𝑀w 7, we can detect them∼10 s faster than the current warning system if they happen∼100 km away

    Gravity Gradient Fluctuation Induced by Earthquakes Previous research investigated the detectability of earthquakes with Phase-III TOBA’s target sensitivity [16, 29]. It has been shown that for earthquakes with a magnitude of 𝑀w 7, we can detect them∼10 s faster than the current warning system if they happen∼100 km away. To identify the location of the ce...

    work page

Show all 50 references
  1. [8]

    The measured cooling curve is shown in Figure 9

    Cryogenic Suspension System The basic cryogenic suspension system was demonstrated in 2020 [29]. The measured cooling curve is shown in Figure 9. The test mass bars were successfully cooled down to 6.1 K in 10 days. Because the silicon suspension wire is still under developmen...

    2020

  2. [10]

    Interferometric Readout System The cryogenic monolithic interferometer was demonstrated in 2024 [38]. In this demonstration, the readout optics made of silicon were glued on a silicon breadboard and consisted of a monolithic interferometer with one test mass bar fixed on the b...

    2024

  3. [11]

    B. P. Abbott et al. (LIGO Scientific Collaboration and Virgo Collaboration), Observation of gravitational waves from a binary black hole merger, Phys. Rev. Lett.116, 061102 (2016)

    2016

  4. [12]

    Abbott et al

    R. Abbott et al. (LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration), GWTC-3: Compact binary coales- cences observed by ligo and virgo during the second part of the third observing run, Phys. Rev. X13, 041039 (2023)

    2023

  5. [13]

    Danzmann and the LISA study team, Lisa: laser interferometer space antenna for gravitational wave measurements, Classical and Quantum Gravity 13, A247 (1996)

    K. Danzmann and the LISA study team, Lisa: laser interferometer space antenna for gravitational wave measurements, Classical and Quantum Gravity 13, A247 (1996)

    1996

  6. [14]

    Kawamura et al., The japanese space gravitational wave antenna: Decigo, Classical and Quantum Gravity 28, 094011 (2011)

    S. Kawamura et al., The japanese space gravitational wave antenna: Decigo, Classical and Quantum Gravity 28, 094011 (2011)

    2011

  7. [15]

    M.-S. Zhan, J. Wang, W.-T. Ni, D.-F. Gao, G. Wang, L.-X. He, R.-B. Li, L. Zhou, X. Chen, J.-Q. Zhong, B. Tang, Z.-W. Yao, L. Zhu, Z.-Y. Xiong, S.-B. Lu, G.-H. Yu, Q.-F. Cheng, M. Liu, Y.-R. Liang, P. Xu, X.-D. He, M. Ke, Z. Tan, and J. Luo, Zaiga: Zhaoshan long-baseline atom i...

    2020 doi

  8. [16]

    Canuel, A

    B. Canuel, A. Bertoldi, L. Amand, E. Pozzo di Borgo, T. Chantrait, C. Danquigny, M. Dovale´Alvarez, B. Fang, A. Freise, R. Geiger,et al., Exploring gravity with the miga large scale atom interferometer, Scientific Reports8, 14064 (2018), https://doi.org/10.1038/s41598-018- 32165-z

    2018 doi

  9. [17]

    M. V. Moody, H. J. Paik, and E. R. Canavan, Three-axis superconducting gravity gradiometer for sensitive gravity experiments, Review of Scientific Instruments 73, 3957 (2002), https://pubs.aip.org/aip/rsi/article-pdf/73/11/3957/19004064/3957 1 online.pdf

    2002

  10. [18]

    H. J. Paik, C. E. Griggs, M. V. Moody, K. Venkateswara, H. M. Lee, A. B. Nielsen, E. Majorana, and J. Harms, Low-frequency terrestrial tensor gravitational-wave detector, Classical and Quantum Gravity33, 075003 (2016)

    2016

  11. [19]

    M. Ando, K. Ishidoshiro, K. Yamamoto, K. Yagi, W. Kokuyama, K. Tsubono, and A. Takamori, Torsion-bar antenna for low-frequency gravitational-wave observations, Phys. Rev. Lett.105, 161101 (2010)

    2010

  12. [20]

    V. B. Braginskii, Y. B. Zel’dovich, and V. N. Rudenko, Reception of gravitational radiation of extraterrestrial origin, ZhETF Pisma Redaktsiiu 10, 437 (1969)

    1969

  13. [21]

    V. B. Braginsky and V. S. Nazarenko, Heterodyne method for detecting gravitational radiation, Moscow University Physics Bulletin1, 89 (1971)

    1971

  14. [22]

    Matsubayashi, H

    T. Matsubayashi, H. aki Shinkai, and T. Ebisuzaki, Gravitational waves from merging intermediate-mass black holes, The Astrophysical Journal 614, 864 (2004)

    2004

  15. [23]

    Reisswig, C

    C. Reisswig, C. D. Ott, E. Abdikamalov, R. Haas, P. M¨osta, and E. Schnetter, Formation and coalescence of cosmological supermassive- black-hole binaries in supermassive-star collapse, Phys. Rev. Lett.111, 151101 (2013)

    2013

  16. [24]

    Maggiore, Gravitational wave experiments and early universe cosmology, Physics Reports331, 283 (2000)

    M. Maggiore, Gravitational wave experiments and early universe cosmology, Physics Reports331, 283 (2000)

    2000

  17. [25]

    P. R. Saulson, Terrestrial gravitational noise on a gravitational wave antenna, Phys. Rev. D30, 732 (1984)

    1984

  18. [26]

    Shimoda, K

    T. Shimoda, K. Juhel, J.-P. Ampuero, J.-P. Montagner, and M. Barsuglia, Early earthquake detection capabilities of different types of future-generation gravity gradiometers, Geophysical Journal International 224, 533 (2020)

    2020

  19. [27]

    Punturo et al., The einstein telescope: a third-generation gravitational wave observatory, Classical and Quantum Gravity 27, 194002 (2010)

    M. Punturo et al., The einstein telescope: a third-generation gravitational wave observatory, Classical and Quantum Gravity 27, 194002 (2010)

    2010

  20. [28]

    B. P. Abbott et al. (LIGO Scientific Collaboration), Exploring the sensitivity of next generation gravitational wave detectors, Classical and Quantum Gravity 34, 044001 (2017)

    2017

  21. [29]

    J. C. Driggers, J. Harms, and R. X. Adhikari, Subtraction of newtonian noise using optimized sensor arrays, Phys. Rev. D 86, 102001 (2012)

    2012

  22. [30]

    Harms and K

    J. Harms and K. Venkateswara, Newtonian-noise cancellation in large-scale interferometric gw detectors using seismic tiltmeters, Classical and Quantum Gravity 33, 234001 (2016)

    2016

  23. [31]

    S. A. Hughes and K. S. Thorne, Seismic gravity-gradient noise in interferometric gravitational-wave detectors, Phys. Rev. D 58, 122002 (1998)

    1998

  24. [32]

    Somiya and (for the KAGRA Collaboration), Detector configuration of KAGRA–the Japanese cryogenic gravitational-wave detector, Classical and Quantum Gravity 29, 124007 (2012)

    K. Somiya and (for the KAGRA Collaboration), Detector configuration of KAGRA–the Japanese cryogenic gravitational-wave detector, Classical and Quantum Gravity 29, 124007 (2012). 16

    2012

  25. [33]

    Creighton, Tumbleweeds and airborne gravitational noise sources for ligo, Classical and Quantum Gravity 25, 125011 (2008)

    T. Creighton, Tumbleweeds and airborne gravitational noise sources for ligo, Classical and Quantum Gravity 25, 125011 (2008)

    2008

  26. [34]

    Bajpai, T

    R. Bajpai, T. Tomaru, T. Suzuki, K. Yamamoto, T. Ushiba, and T. Honda, Estimation of newtonian noise from the kagra cooling system, Phys. Rev. D107, 042001 (2023)

    2023

  27. [35]

    S. S. Y. Chua, N. A. Holland, P. W. F. Forsyth, A. Kulur Ramamohan, Y. Zhang, J. Wright, D. A. Shaddock, D. E. McClelland, and B. J. J. Slagmolen, The torsion pendulum dual oscillator for low-frequency Newtonian noise detection, Applied Physics Letters 122, 201102 (2023)

    2023

  28. [36]

    Harms, J.-P

    J. Harms, J.-P. Ampuero, M. Barsuglia, E. Chassande-Mottin, J.-P. Montagner, S. N. Somala, and B. F. Whiting, Transient gravity perturbations induced by earthquake rupture, Geophysical Journal International 201, 1416 (2015)

    2015

  29. [37]

    Kame and M

    N. Kame and M. Kimura, The fundamental nature of a transient elastic response to prompt gravity perturbations, Geophysical Journal International 218, 1136 (2019)

    2019

  30. [38]

    N. Kame, Pre-p gravity signals from dynamic earthquake rupture: modelling and observations, Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 379, 20200136 (2021)

    2021

  31. [39]

    Shimoda, Cryogenic Torsion Pendulum for Observing Low-frequency Gravity Gradient Fluctuation , Ph.D

    T. Shimoda, Cryogenic Torsion Pendulum for Observing Low-frequency Gravity Gradient Fluctuation , Ph.D. thesis, The University of Tokyo (2020)

    2020

  32. [40]

    Ishidoshiro, M

    K. Ishidoshiro, M. Ando, A. Takamori, H. Takahashi, K. Okada, N. Matsumoto, W. Kokuyama, N. Kanda, Y. Aso, and K. Tsubono, Upper limit on gravitational wave backgrounds at 0.2 hz with a torsion-bar antenna, Phys. Rev. Lett.106, 161101 (2011)

    2011

  33. [41]

    Shoda, Development of a High-Angular-Resolution Antenna for Low-Frequency Gravitational-Wave Observation , Ph.D

    A. Shoda, Development of a High-Angular-Resolution Antenna for Low-Frequency Gravitational-Wave Observation , Ph.D. thesis, The University of Tokyo (2015)

    2015

  34. [42]

    Shimoda, N

    T. Shimoda, N. Aritomi, A. Shoda, Y. Michimura, and M. Ando, Seismic cross-coupling noise in torsion pendulums, Phys. Rev. D 97, 104003 (2018)

    2018

  35. [43]

    Ishidoshiro, Search for low-frequency gravitational waves using a superconducting magnetically-levitated torsion antenna , Ph.D

    K. Ishidoshiro, Search for low-frequency gravitational waves using a superconducting magnetically-levitated torsion antenna , Ph.D. thesis, The University of Tokyo (2010)

    2010

  36. [44]

    Kuwahara, A

    Y. Kuwahara, A. Shoda, K. Eda, and M. Ando, Search for a stochastic gravitational wave background at 1–5 hz with a torsion-bar antenna, Phys. Rev. D94, 042003 (2016)

    2016

  37. [45]

    S. Reid, G. Cagnoli, D. Crooks, J. Hough, P. Murray, S. Rowan, M. Fejer, R. Route, and S. Zappe, Mechanical dissipation in silicon flexures, Physics Letters A 351, 205 (2006)

    2006

  38. [46]

    Shimoda and M

    T. Shimoda and M. Ando, Nonlinear vibration transfer in torsion pendulums, Classical and Quantum Gravity 36, 125001 (2019)

    2019

  39. [47]

    Matichard and M

    F. Matichard and M. Evans, Review: Tilt-Free Low-Noise Seismometry, Bulletin of the Seismological Society of America 105, 497 (2015)

    2015

  40. [48]

    Takano, Cryogenic Monolithic Interferometer for Low-frequency Gravitational Wave Observation , Ph.D

    S. Takano, Cryogenic Monolithic Interferometer for Low-frequency Gravitational Wave Observation , Ph.D. thesis, The University of Tokyo (2024)

    2024

  41. [49]

    Shimoda, Y

    T. Shimoda, Y. Miyazaki, Y. Enomoto, K. Nagano, and M. Ando, Coherent angular signal amplification using an optical cavity, Appl. Opt. 61, 3901 (2022)

    2022

  42. [50]

    Maggiore, Gravitational Waves: Volume 1: Theory and Experiments (Oxford University Press, 2007)

    M. Maggiore, Gravitational Waves: Volume 1: Theory and Experiments (Oxford University Press, 2007)

    2007

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Reviewed August 12, 2026 · model on record in the stance chip above.