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REVIEW 3 major objections 6 minor 37 references

Adjustable picometer-stable interferometers for testing space-based gravitational wave detectors

T0 review · 3 major / 6 minor · reviewed 2026-08-09 · deepseek-v4-flash

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Pith's one-line read A clamp-mounted optical bench keeps cavity length noise below 1 pm/√Hz down to 3 mHz, reaching LISA ground-test stability for most frequencies.

desk verdict A genuinely useful engineering demonstration of reconfigurable picometer-stable interferometers, but the abstract's 'verified' overstates what a single non-stationary, detrended beat record can establish. read the letter →

arxiv 2502.01212 v1 pith:STJPRSCK submitted 2025-02-03 physics.ins-det gr-qc

Marcel Beck , Shreevathsa Chalathadka Subrahmanya , Oliver Gerberding This is my paper · ORCID
classification physics.ins-detgr-qc
keywords laserinterferometrygravitationalwavedetectorsLISAopticalgroundsupportequipmentultra-stablebenchPound-Drever-Halllockingheterodynefrequencystabilizationpicometerlengthstability
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 argues that a laser interferometer used for ground-testing space-based gravitational wave detectors does not have to be a permanently bonded assembly. The authors built a toolset, TAPSI, in which optics are clamped and screwed onto a Zerodur plate, freely repositionable like components on an optical table. Locking a laser to a 10 cm cavity built this way, they measured cavity length noise below $1\,\mathrm{pm}/\sqrt{\mathrm{Hz}}$ down to $3\,\mathrm{mHz}$ using Pound-Drever-Hall locking, below the LISA requirement for most frequencies. That means a given interferometer configuration can be set up and aligned in under an hour instead of weeks or months, which would make flexible optical ground support equipment practical.

What carries the argument

The central object is the toolset for adjustable picometer-stable interferometers (TAPSI): a Zerodur optical bench on which optics sit on posts held by clamps and screws, with Newport ZeroDrift mirror mounts chosen for low tilt-to-length coupling and an Invar compensation plate placed between mount and post so that the thermal expansions of mount and plate cancel at the mirror center. The argument is carried by measuring the length change of a 10 cm prototype cavity built with these mounts, comparing its beat frequency against a 21 cm ULE reference cavity with known $7.5\,\mathrm{fm}/\sqrt{\mathrm{Hz}}$ stability, using two locking schemes (heterodyne stabilization and Pound-Drever-Hall). The PDH result is the carrier of the central claim: it stays below the LISA requirement curve except for a slight excess at 0.8-3 mHz.

What would settle it

Directly measure the coefficient of thermal expansion of the ZeroDrift mirror-mount and Invar compensation-plate assembly, then compute the resulting 10 cm cavity length drift; if the drift projected onto the noise spectrum rises above the LISA requirement curve in the 0.1-3 mHz band, the assumed thermal cancellation fails.

Watch

Extended reading notes

Core claim

The central demonstrated claim is that adjustable, clamp-mounted optics on a low-expansion Zerodur bench can be picometer-stable at the low frequencies relevant to LISA. Using a prototype 10 cm cavity with finesse 627 assembled entirely with the TAPSI concept, a 1064 nm laser locked by the Pound-Drever-Hall technique showed relative cavity length noise below $1\,\mathrm{pm}/\sqrt{\mathrm{Hz}}$ down to $3\,\mathrm{mHz}$, below the LISA requirement curve except for a small excess between 0.8 and 3 mHz. The same cavity probed with heterodyne laser frequency stabilization was limited by an analogue demodulation delay effect, not by the mounting concept. The authors therefore conclude that the concept is suitable for flexible, reusable optical ground support equipment for LISA and future space interferometry missions.

Load-bearing premise

The whole approach rests on the assumption that the thermal expansion of the mirror mounts and the Invar plate underneath them cancel well enough to keep the mirror position stable, but that cancellation is never measured directly in the paper.

Editorial extensions

If this is right

  • Interferometers for ground testing of LISA can be assembled in hours rather than weeks or months, because components are clamped and repositionable rather than bonded.
  • The same bench and components can be reused across different experiments, reducing the cost of optical ground support equipment.
  • The concept extends to other future low-frequency space interferometry missions such as Taiji and DECIGO, which need picometer-stable ground testbeds.
  • The remaining gap at 0.8-3 mHz in the PDH lock is attributed to stray light and readout effects rather than the mounting concept, so higher cavity finesse and digital demodulation should close it.

Reading between the lines

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

  • If the mount-plate thermal cancellation holds more generally, the concept could be portable to other low-expansion benches and to testbeds where bonding is impractical; the paper only demonstrates one cavity geometry, so this portability is an inference.
  • The unmeasured coefficient of thermal expansion of the ZeroDrift mounts means the compensation plate is currently matched by assumption; a direct CTE characterization would let the design be tuned, and thermal cycling tests would reveal whether the stability is robust across temperature ranges.
  • The sub-hour assembly time suggests a workflow where candidate interferometer layouts for LISA ground support are prototyped and compared on one bench before a final bonded design is committed; the paper does not explicitly propose this workflow.
  • Because the heterodyne approach was limited by an analogue demodulation delay rather than by the optics, moving to digital demodulation could let the simpler heterodyne scheme itself reach LISA stability on the same bench; the paper plans this but has not demonstrated it.
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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 / 6 minor

Summary. The paper presents TAPSI, an opto-mechanical concept in which mirrors and other optics are placed on a Zerodur bench with adjustable, clamped Invar posts and thermally compensated mirror mounts, rather than being bonded or glued. A 10 cm prototype cavity built with this concept is characterized against a ULE reference cavity using two locking schemes, heterodyne stabilization (HS) and Pound-Drever-Hall (PDH) locking. The authors report a temperature stability of 10 µK/√Hz down to 10 mHz, an initial alignment time under one hour, and a PDH cavity-length noise that they state is below the LISA requirement for most frequencies and only slightly above at 0.8–3 mHz. The abstract goes further, claiming that the cavity length noise is verified to be below 1 pm/√Hz down to 3 mHz. The paper concludes that TAPSI is suitable for flexible optical ground support equipment for LISA and future missions.

Significance. If the central claim holds, TAPSI would be a practically valuable alternative to permanently bonded optical benches for ground-based testing of space interferometers: it promises reconfigurability and much faster assembly while maintaining picometer-level length stability. The paper has notable strengths: the length measurement is made against an external reference cavity, the thermal floor of the Zerodur bench is estimated forward from measured temperature noise and literature CTE values, two locking schemes are compared, and the authors are candid about known limitations such as stray light and the unmeasured mount CTE. However, the headline 'verified below 1 pm/√Hz down to 3 mHz' is not fully supported by the evidence presented, and the paper's own Section 5 appears to contradict the abstract at the 3 mHz point. The underlying concept is credible and the measurement is a useful upper bound, but the verification claim needs either additional data or more careful wording.

major comments (3)
  1. [Abstract; Section 5; Eq. (1)] The abstract states that 'we verified that the cavity length noise is below 1 pm/sqrt(Hz) for frequencies down to 3 mHz,' but Section 5 says the PDH trace 'is below the LISA requirements for most frequencies and only slightly above at 0.8 to 3 mHz.' Since Eq. (1) gives u(3 mHz) ≈ 1.09 pm/sqrt(Hz), being above the LISA requirement at 3 mHz implies the noise is not below 1 pm/sqrt(Hz) at that frequency. Please reconcile these statements by specifying the exact frequency at which the trace crosses 1 pm/sqrt(Hz) and clarify whether the claim applies to 3 mHz inclusive.
  2. [Section 5, Figs. 7 and 8, Eq. (8)] The central verification rests on a single beat-note ASD. Figure 8 shows a linear temperature drift removed via Eq. (8) and a quadratic drift removed before spectral estimation, and the residual is described as containing non-stationary noise attributed to parasitic beams. The paper gives no run-to-run statistics, no uncertainty bars on the ASD, and no analysis of how the detrending affects the value at 3 mHz. The plotted trace is therefore a favorable processed upper bound from one non-stationary record, not a statistical verification of the stated stability. Please provide at least two independent records, error bars or segment-to-segment scatter, and a statement of the detrending procedure's effect at the lowest reported frequency.
  3. [Section 2] The thermal-compensation mechanism is central to the design: the mirror mount and Invar compensation plate are intended to cancel each other's expansion, yet the CTE of the ZeroDrift mount is stated to be unknown and the authors note that a future study is needed to optimize the plate. The demonstrated picometer stability is therefore shown for one specific geometry and thermal environment, not as a property of the adjustable mounting concept in general. Either measure the mount's effective CTE or demonstrate repeatability after reassembly or in a different configuration before claiming that TAPSI provides adjustable picometer-stable interferometers as a general toolset.
minor comments (6)
  1. [Section 5, Eq. (8)] Equation (8) is typographically ambiguous: 'dL/dT = d f/fLaser LCavity · 1/dT' should be written as (df/f_laser) * L_cavity / dT, with units specified for each quantity.
  2. [Section 4] The phrase '7.5 fm/sqrt(Hz) (20 Hz sqrt(Hz)) down to 3 mHz' appears malformed; please clarify whether the reference cavity stability is 7.5 fm/sqrt(Hz) at 20 Hz or some other specification.
  3. [References] References [20] and [21] are the same paper (Korth et al., 'Passive, free-space heterodyne laser gyroscope'); one should be removed and citations renumbered.
  4. [List of Abbreviations] The abbreviation list contains 'ASD' twice; please deduplicate.
  5. [Figure 7 caption] The caption mentions 'the free-running laser noise of a 10 cm cavity' but the text does not define how this curve was measured or modeled; please add a brief explanation.
  6. [Section 3] The text refers to 'Johnsen-Nyquist noise'; this should be 'Johnson-Nyquist noise.'

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the central pm-stability claim is a beat-note measurement against an external ULE reference cavity, not a fitted or self-cited construction.

full rationale

The paper's central claim is an experimental measurement: the prototype cavity length ASD is obtained by locking two lasers to cavities and measuring the beat frequency, converted by Eq. 2 (dL = dnu/nu * L). The benchmark is external (LISA requirement, Eq. 1), and the reference-cavity stability is cited from an independent prior measurement [37], far below the claimed 1 pm/sqrt(Hz) level. The only fitted parameter, dL/dT ~ 4e-8 m/K (Eq. 8), is extracted from the same beat and temperature records but is used diagnostically to show that linear temperature coupling is not limiting; it is not used to generate the stability number. The theoretical Zerodur thermal floor is computed forward from the literature CTE and measured temperature noise. The one self-citation, [7], is invoked only to note that the analogue-HS delay-beat problem has been overcome digitally elsewhere, and the authors explicitly state their analogue implementation is still constrained; it is not load-bearing for the PDH result. The strongest caveat is non-circular: the low-frequency endpoint relies on a single detrended, non-stationary beat record, so the abstract's word 'verified' may overstate reproducibility; that is a robustness and statistics concern, not circularity.

Assumptions & free parameters 1 free parameters · 4 assumptions · 0 invented entities

The central claim is experimental and adds no free parameters beyond the diagnostic dL/dT fit. The load-bearing inputs are the prior reference cavity stability measurement, the unmeasured mount-CTE assumption behind the compensation plate, and standard cavity and beat-note relations. No new physical entities are postulated.

free parameters (1)
  • dL/dT linear temperature-to-length coupling = 4e-8 m/K
    Fitted in Eq. (8) from the linear rise of beat frequency and temperature, then used to project the temperature-limited noise floor; the attribution of the drift to temperature is assumed, since the paper reports no correlation between temperature and length fluctuations.
assumptions (4)
  • domain assumption The ULE reference cavity delivers 7.5 fm/sqrt(Hz) stability down to 3 mHz as measured in Ref [37].
    Introduced in Section 4 to justify attributing the entire relative beat noise to the prototype cavity; the reference is a 2005 thesis measurement and is not re-verified in the current facility.
  • domain assumption The ZeroDrift mirror mounts have small CTE and the Invar compensation plate cancels the mount's thermal expansion.
    Section 2 states the mount CTE 'was unknown but expected to be small'; the compensation plate material and length were chosen on this basis with no measurement or thermal cycling test.
  • standard math The beat-frequency ASD maps to cavity length noise through dL = (dv/v) L with v = 282 THz.
    Eq. (2) in Section 4; assumes the lock suppresses laser frequency noise and that all measured beat fluctuation originates in the prototype cavity length.
  • standard math Zerodur's nominal CTE, multiplied by the measured temperature noise, bounds the bench's thermal length noise.
    Section 5's theoretical minimum length noise curve uses the standard CTE of Zerodur as a material property without a dedicated measurement.

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Cite this review

Pith. "Pith review of Adjustable picometer-stable interferometers for testing space-based gravitational wave detectors." pith.science (2026). https://pith.science/paper/STJPRSCK

@misc{pith2026250201212,
  author       = {Pith},
  title        = {Pith review of: Adjustable picometer-stable interferometers for testing space-based gravitational wave detectors},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/STJPRSCK}},
  note         = {Machine review of arXiv:2502.01212}
}
read the original abstract

Space-based gravitational wave detectors, such as the Laser Interferometer Space Antenna (LISA), use picometer-precision laser interferometry to detect gravitational waves at frequencies from 1 Hz down to below 0.1 mHz. Laser interferometers used for on-ground prototyping and testing of such instruments are typically constructed by permanently bonding or gluing optics onto an ultra-stable bench made of low-expansion glass ceramic. This design minimizes temperature coupling to length and tilt, which dominates the noise at low frequencies due to finite temperature stability achievable in laboratories and vacuum environments. Here, we present the study of an alternative opto-mechanical concept where optical components are placed with adjustable and freely positionable mounts on an ultra-stable bench, while maintaining picometer length stability. With this concept, a given interferometer configuration can be realised very quickly due to a simplified and speed-up assembly process, reducing the realisation time from weeks or months to a matter of hours. We built a corresponding test facility and verified the length stability of our concept by measuring the length change in an optical cavity that was probed with two different locking schemes, heterodyne laser frequency stabilisation and Pound-Drever-Hall locking. We studied the limitations of both locking schemes and verified that the cavity length noise is below 1 pm/sqrt(Hz) for frequencies down to 3 mHz. We thereby demonstrate that our concept can simplify the testing of interferometer configurations and opto-mechanical components and is suitable to realise flexible optical ground support equipment for space missions that use laser interferometry, such as future space-based gravitational wave detectors and satellite geodesy missions.

Figures

Figures reproduced from arXiv: 2502.01212 by the authors.

Figure 1
Figure 1. CAD model of the toolset for adjustable picometer-stable interferometers [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Vertical cross-sectional view of the optical test facility with the toolset [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Time series of two parallel measurements of temperature inside and outside [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: ASD plot (calculated with LPSD [38] after removing the linear trend from the [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: The Heterodyne laser frequency Stabilization scheme uses the beat-note from [PITH_FULL_IMAGE:figures/full_fig_p009_5.png]
Figure 6
Figure 6. Figure 6: (a) PDH locking scheme with fiber-coupled EOMs and free space setup inside [PITH_FULL_IMAGE:figures/full_fig_p010_6.png]
Figure 7
Figure 7. Figure 7: The length stability of the prototype cavity was measured with the Heterodyne [PITH_FULL_IMAGE:figures/full_fig_p011_7.png]
Figure 8
Figure 8. Figure 8: The upper subplot shows the time series of parallel measurements of the beat [PITH_FULL_IMAGE:figures/full_fig_p011_8.png]

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Reference graph

Works this paper leans on

37 extracted references · 37 canonical work pages

  1. [1]

    Advanced ligo

    J Aasi, B P Abbott, R Abbott, T Abbott, M R Abernathy, K Ackley, C Adams, T Adams, P Addesso, R X Adhikari, V Adya, C Affeldt, N Aggarwal, O D Aguiar, A Ain, P Ajith, A Alemic, B Allen, D Amariutei, S B Anderson, W G Anderson, K Arai, M C Araya, C Arceneaux, J S Areeda, G Ashton, S Ast, S M Aston, P Aufmuth, C Aulbert, B E Aylott, S Babak, P T Baker, S W ...

    work page 2015

  2. [2]

    Advanced virgo: a second-generation interferometric gravitational wave detector

    F Acernese, M Agathos, K Agatsuma, D Aisa, N Allemandou, A Allocca, J Amarni, P Astone, G Balestri, G Ballardin, F Barone, J-P Baronick, M Barsuglia, A Basti, F Basti, Th S Bauer, V Bavigadda, M Bejger, M G Beker, C Belczynski, D Bersanetti, A Bertolini, M Bitossi, M A Bizouard, S Bloemen, M Blom, M Boer, G Bogaert, D Bondi, F Bondu, L Bonelli, R Bonnand,...

    work page 2014

  3. [3]

    Archibald, Paul T

    Gabriella Agazie, Akash Anumarlapudi, Anne M. Archibald, Paul T. Baker, Bence B´ ecsy, Laura Blecha, Alexander Bonilla, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, Rand Burnette, Robin Case, J. Andrew Casey-Clyde, Maria Charisi, Shami Chatterjee, Katerina Chatziioannou, Belinda D. Cheeseboro, Siyuan Chen, Tyler Cohen, James M. Cordes, Neil J. Cornis...

    work page 2023

  4. [4]

    Barke, Peter L

    John Baker, Simon F. Barke, Peter L. Bender, Emanuele Berti, Robert Caldwell, John W. Conklin, Neil Cornish, Elizabeth C. Ferrara, Kelly Holley-Bockelmann, Brittany Kamai, Shane L. Larson, Jeff Livas, Sean T. McWilliams, Guido Mueller, Priyamvada Natarajan, Norman Rioux, Shannon R Sankar, Jeremy Schnittman, Deirdre Shoemaker, Jacob Slutsky, Robin Stebbins...

    work page 2019

  5. [5]

    Eric D. Black. An introduction to pound–drever–hall laser frequency stabilization. American Journal of Physics , 69(1):79–87, January 2001

    work page 2001

  6. [6]

    Bogenstahl, C

    J. Bogenstahl, C. Diekmann, E. D. Fitzsimons, R. Fleddermann, E. Granova, C. J. Killow, J. Pijnenburg, D. I. Robertson, A. Shoda, A. Sohmer, M. Tr¨ obs, H. Ward, D. Weise, L. d’Arcio, M. Dehne, G. Heinzel, H. Hogenhuis, M. Perreur-Lloyd, A. Taylor, and G. Wanner. Optical bench development for lisa. In Naoto Kadowaki, editor, International Conference on Sp...

    work page 2010

  7. [7]

    Integrating high-precision and fringe-scale displacement sensing using heterodyne cavity- tracking

    Shreevathsa Chalathadka Subrahmanya, Christian Darsow-Fromm, and Oliver Gerberding. Integrating high-precision and fringe-scale displacement sensing using heterodyne cavity- tracking. Optics Express, 33(3):4044, January 2025

    work page 2025

  8. [8]

    Design and construction of an optical test bed for lisa imaging systems and tilt- to-length coupling

    M Chwalla, K Danzmann, G Fern´ andez Barranco, E Fitzsimons, O Gerberding, G Heinzel, C J Killow, M Lieser, M Perreur-Lloyd, D I Robertson, S Schuster, T S Schwarze, M Tr¨ obs, H Ward, and M Zwetz. Design and construction of an optical test bed for lisa imaging systems and tilt- to-length coupling. Classical and Quantum Gravity , 33(24):245015, November 2016

    work page 2016

Show all 37 references
  1. [9]

    Corsi, I

    C. Corsi, I. Liontos, S. Cavalieri, M. Bellini, G. Venturi, and R. Eramo. An ultrastable michelson interferometer for high-resolution spectroscopy in the xuv. Optics Express, 23(4):4106, February 2015

    2015

  2. [10]

    Lisa technology concept, status, prospects

    Karsten Danzmann and Albrecht Ruediger. Lisa technology concept, status, prospects. Classical and Quantum Gravity , 20(10):S1–S9, April 2003

    2003

  3. [11]

    Construction and noise behaviour of ultra-stable optical systems for space interferometers

    Marina Dehne. Construction and noise behaviour of ultra-stable optical systems for space interferometers. 2012

    2012

  4. [12]

    Tanner, and Guido Mueller

    Johannes Eichholz, David B. Tanner, and Guido Mueller. Heterodyne laser frequency stabilization for long baseline optical interferometry in space-based gravitational wave detectors. Phys. Rev. D, 92:022004, Jul 2015

    2015

  5. [13]

    Sub-pm √ Hz −1 non-reciprocal noise in the lisa backlink fiber

    Roland Fleddermann, Christian Diekmann, Frank Steier, Michael Tr¨ obs, Gerhard Heinzel, and Karsten Danzmann. Sub-pm √ Hz −1 non-reciprocal noise in the lisa backlink fiber. Classical and Quantum Gravity , 35(7):075007, February 2018

    2018

  6. [14]

    Concepts and status of chinese space gravitational wave detection projects

    Yungui Gong, Jun Luo, and Bin Wang. Concepts and status of chinese space gravitational wave detection projects. Nature Astronomy, 5(9):881–889, September 2021

    2021

  7. [15]

    Residual amplitude modulation mechanisms in modulation transfer spectroscopy that use electro-optic modulators

    Esa Jaatinen, David J Hopper, and Julian Back. Residual amplitude modulation mechanisms in modulation transfer spectroscopy that use electro-optic modulators. Measurement Science and Technology, 20(2):025302, December 2008

    2008

  8. [16]

    Picometer sensitive prototype of the optical truss interferometer for lisa, 2024

    Kylan Jersey, Harold Hollis, Han-Yu Chia, Jose Sanjuan, Paul Fulda, Guido Mueller, and Felipe Guzman. Picometer sensitive prototype of the optical truss interferometer for lisa, 2024

    2024

  9. [17]

    J. B. Johnson. Thermal agitation of electricity in conductors. Physical Review, 32(1):97–109, July 1928

    1928

  10. [18]

    Current status of space gravitational wave antenna decigo and b-decigo

    Seiji Kawamura, Masaki Ando, Naoki Seto, Shuichi Sato, Mitsuru Musha, Isao Kawano, Jun’ichi Yokoyama, Takahiro Tanaka, Kunihito Ioka, Tomotada Akutsu, Takeshi Takashima, Kazuhiro Agatsuma, Akito Araya, Naoki Aritomi, Hideki Asada, Takeshi Chiba, Satoshi Eguchi, Motohiro Enoki,...

    2021

  11. [19]

    Korth, Nicolas Smith-Lefebvre, Koji Arai, and Rana X

    Keiko Kokeyama, Kiwamu Izumi, William Z. Korth, Nicolas Smith-Lefebvre, Koji Arai, and Rana X. Adhikari. Residual amplitude modulation in interferometric gravitational wave detectors. Journal of the Optical Society of America A , 31(1):81, December 2013

    2013

  12. [21]

    Passive, free-space heterodyne laser gyroscope

    W Z Korth, A Heptonstall, E D Hall, K Arai, E K Gustafson, and R X Adhikari. Passive, free-space heterodyne laser gyroscope. Classical and Quantum Gravity , 33(3):035004, January 2016

    2016

  13. [22]

    Ultrastable optical components using adjustable commercial mirror mounts anchored in a ule spacer

    Soham Kulkarni, Ada Umi´ nska, Joseph Gleason, Simon Barke, Reid Ferguson, Jose Sanju´ an, Paul Fulda, and Guido Mueller. Ultrastable optical components using adjustable commercial mirror mounts anchored in a ule spacer. Applied Optics, 59(23):6999, August 2020

    2020

  14. [23]

    Springer Berlin Heidelberg, 2024

    Alexey Kupriyanov, Arthur Reis, Annike Knabe, Nina Fletling, Alireza HosseiniArani, Mohsen Romeshkani, Manuel Schilling, Vitali M¨ uller, and J¨ urgen M¨ uller.Analysis of Novel Sensors and Satellite Formation Flights for Future Gravimetry Missions . Springer Berlin Heidelberg, 2024

    2024

  15. [24]

    Tianqin: a space-borne gravitational wave detector

    Jun Luo, Li-Sheng Chen, Hui-Zong Duan, Yun-Gui Gong, Shoucun Hu, Jianghui Ji, Qi Liu, Jianwei Mei, Vadim Milyukov, Mikhail Sazhin, Cheng-Gang Shao, Viktor T Toth, Hai-Bo Tu, Yamin Wang, Yan Wang, Hsien-Chi Yeh, Ming-Sheng Zhan, Yonghe Zhang, Vladimir Zharov, and Ze-Bing Zhou. ...

    2016

  16. [25]

    Ultra-stable and versatile high- energy resolution setup for attosecond photoelectron spectroscopy

    Sizuo Luo, Robin Weissenbilder, Hugo Laurell, Mattias Ammitzb¨ oll, V´ enus Poulain, David Busto, Lana Neoriˇ ci´ c, Chen Guo, Shiyang Zhong, David Kroon, Richard J Squibb, Raimund Feifel, Mathieu Gisselbrecht, Anne L’Huillier, and Cord L Arnold. Ultra-stable and versatile hig...

    2023

  17. [26]

    Annealed proton exchanged optical waveguides in lithium niobate: differences between the x- and z-cuts

    Pavla Nekvindov´ a, JarmilaˇSpirkov´ a, JarmilaˇCerven´ a, Milos Budnar, Alenka Razpet, Benjamin Zorko, and Primoˇ z Pelicon. Annealed proton exchanged optical waveguides in lithium niobate: differences between the x- and z-cuts. Optical Materials, 19(2):245–253, April 2002

    2002

  18. [27]

    Suprema ® zerodrift™ thermally compensated mirror mounts - su100tw-f2k

    Newport. Suprema ® zerodrift™ thermally compensated mirror mounts - su100tw-f2k. Technical report, Spectra-Physics GmbH, 2020

    2020

  19. [28]

    H. Nyquist. Thermal agitation of electric charge in conductors. Physical Review, 32(1):110–113, July 1928

    1928

  20. [29]

    Diaz Ortiz, J

    M. Diaz Ortiz, J. Gleason, H. Grote, A. Hallal, M. T. Hartman, H. Hollis, K. S. Isleif, A. James, K. Karan, T. Kozlowski, A. Lindner, G. Messineo, G. Mueller, J. H. Poeld, R. C. G. Smith, A. D. Spector, D. B. Tanner, L. W. Wei, and B. Willke. Design of the alps ii optical system, 2020

    2020

  21. [30]

    Construction and testing of the optical bench for lisa pathfinder

    D I Robertson, E D Fitzsimons, C J Killow, M Perreur-Lloyd, H Ward, J Bryant, A M Cruise, G Dixon, D Hoyland, D Smith, and J Bogenstahl. Construction and testing of the optical bench for lisa pathfinder. Classical and Quantum Gravity , 30(8):085006, March 2013

    2013

  22. [31]

    Resistive- based micro-kelvin temperature resolution for ultra-stable space experiments

    David Roma-Dollase, Vivek Gualani, Martin Gohlke, Klaus Abich, Jordan Morales, Alba Gonzalvez, Victor Mart ´ ın, Juan Ramos-Castro, Josep Sanjuan, and Miquel Nofrarias. Resistive- based micro-kelvin temperature resolution for ultra-stable space experiments. Sensors, 23(1):145,...

    2022

  23. [32]

    Sanju´ an, A

    J. Sanju´ an, A. Lobo, M. Nofrarias, J. Ramos-Castro, and P. J. Riu. Thermal diagnostics front-end electronics for lisa pathfinder. Review of Scientific Instruments , 78(10), October 2007

    2007

  24. [33]

    C P Sasso, G Mana, and S Mottini. The lisa interferometer: impact of stray light on the phase of Adjustable picometer-stable interferometers for testing space-based gravitational wave detectors20 the heterodyne signal. Classical and Quantum Gravity , 36(7):075015, March 2019

    2019

  25. [34]

    Roberts, Lucie Cros, Ben T

    Etienne Savalle, Aur´ elien Hees, Florian Frank, Etienne Cantin, Paul-Eric Pottie, Benjamin M. Roberts, Lucie Cros, Ben T. McAllister, and Peter Wolf. Searching for dark matter with an optical cavity and an unequal-delay interferometer. Phys. Rev. Lett. , 126:051301, Feb 2021

    2021

  26. [35]

    B. S. Sheard, G. Heinzel, K. Danzmann, D. A. Shaddock, W. M. Klipstein, and W. M. Folkner. Intersatellite laser ranging instrument for the grace follow-on mission. Journal of Geodesy , 86(12):1083–1095, May 2012

    2012

  27. [36]

    Construction of the lisa back-side fibre link interferometer prototype

    F Steier, R Fleddermann, J Bogenstahl, C Diekmann, G Heinzel, and K Danzmann. Construction of the lisa back-side fibre link interferometer prototype. Classical and Quantum Gravity , 26(17):175016, August 2009

    2009

  28. [37]

    Laser development and stabilization for the spaceborne interferometric gravitational wave detector lisa

    Michael Tr¨ obs. Laser development and stabilization for the spaceborne interferometric gravitational wave detector lisa. 2005

    2005

  29. [38]

    Improved spectrum estimation from digitized time series on a logarithmic frequency axis

    Michael Tr¨ obs and Gerhard Heinzel. Improved spectrum estimation from digitized time series on a logarithmic frequency axis. Measurement, 39(2):120–129, February 2006

    2006

Pith tools

Reviewed August 9, 2026 · model on record in the stance chip above.