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arxiv: 2606.26895 · v1 · pith:XJWVNYFSnew · submitted 2026-06-25 · 🌌 astro-ph.IM

Cascade adaptive optics with a second stage based on a Zernike wavefront sensor for exoplanet observations II. Validation in broadband light on the ESO/GHOST testbed

A. Rahim , M. N'Diaye , A. Vigan , M. Kasper , J. Nousiainen , B. Engler , K. Dohlen , S. Leveratto
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J. Floriot M. Marcos C. Bailet P. Bristow E. S. Douglas
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Pith reviewed 2026-06-26 03:13 UTC · model grok-4.3

classification 🌌 astro-ph.IM
keywords adaptive opticsZernike wavefront sensorhigh-contrast imagingexoplanet observationsbroadband lightcascade AOtestbed validationLyot coronagraph
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The pith

A Zernike wavefront sensor second stage improves contrast by up to a factor of ten in broadband light after static aberration removal.

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

The paper tests a cascade adaptive optics setup in which a fast second-stage loop driven by a Zernike wavefront sensor corrects the residuals left by a first-stage extreme AO system. Experiments on the GHOST testbed simulate realistic residuals and measure performance through Lyot coronagraphic images in both narrowband and broadband light. Closing the second-stage loop raises contrast inside the correction region under most tested conditions of seeing, wind speed, and stellar flux. After subtracting quasi-static aberrations the gain reaches one order of magnitude and remains independent of bandwidth and turbulence strength. Broadband and narrowband results match for bright targets while narrowband holds a small edge for faint ones.

Core claim

On the GHOST testbed, closing the Zernike wavefront sensor control loop on simulated first-stage XAO residuals consistently improves contrast in Lyot coronagraphic images within the correction region. After subtraction of quasi-static aberrations the loop delivers a contrast gain up to one order of magnitude. This gain is independent of bandwidth and turbulence strength. Broadband and narrowband performance match for bright sources, while narrowband remains slightly preferable for faint targets.

What carries the argument

The Zernike wavefront sensor (ZWFS) second-stage control loop that senses and corrects residual aberrations from a first-stage extreme AO system in cascade adaptive optics.

If this is right

  • The ZWFS-based cascade loop is feasible in polychromatic light across a wide range of seeings, wind speeds, and stellar fluxes.
  • Contrast gains remain independent of bandwidth once quasi-static aberrations are removed.
  • Narrowband operation offers only a modest advantage for the faintest targets.
  • The scheme points toward use on Extremely Large Telescopes once achromatic masks and accurate quasi-static calibration are available.

Where Pith is reading between the lines

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

  • If the testbed results translate to on-sky conditions, second-stage ZWFS loops could relax requirements on first-stage XAO speed for future high-contrast instruments.
  • Accurate subtraction of quasi-static aberrations emerges as the dominant practical limit rather than bandwidth or turbulence strength.
  • The approach could be tested on existing 8-meter-class telescopes by adding a ZWFS channel to current extreme AO systems.
  • Extending the method to even broader wavelength ranges would require verifying that the Zernike mask remains effective without chromatic errors.

Load-bearing premise

Simulated first-stage XAO residuals on the testbed accurately represent real telescope conditions and quasi-static aberrations can be subtracted without introducing new errors.

What would settle it

No measurable contrast improvement when the ZWFS loop is closed during on-sky broadband observations with an actual telescope would falsify the performance claim.

Figures

Figures reproduced from arXiv: 2606.26895 by A. Rahim, A. Vigan, B. Engler, C. Bailet, E. S. Douglas, J. Floriot, J. Nousiainen, K. Dohlen, M. Kasper, M. Marcos, M. N'Diaye, P. Bristow, S. Leveratto.

Figure 1
Figure 1. Figure 1 [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: (top and middle rows) presents the coronagraphic im￾ages under a bright star flux regime for the two spectral config￾urations. In open loop, the coronagraph exhibits a large dark re￾gion extending up to approximately 20λ/D, which corresponds to the expected frequency cutoff of the first stage XAO system. In closed loop, a new high contrast region appears inside the XAO corrected area, extending up to about… view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of contrast performance obtained in broadband and narrowband for a faint star, under standard atmospheric conditions (see￾ing of 0.7′′ and wind speed of 10 m·s−1 ). Top: coronagraphic images for the second stage AO in open loop (left) and closed loop (right) in broad￾band light. Middle: same comparison in narrowband. Bottom: contrast curves derived from the azimuthal averaged intensity of the im… view at source ↗
Figure 4
Figure 4. Figure 4: Contrast curves obtained after subtraction of NCPA for the bright star configuration, under standard atmospheric conditions (seeing of 0.7′′ and wind speed of 10 m·s −1 ). Top: azimuthally averaged corona￾graphic intensity profiles in open loop (dashed) and in closed loop after NCPA subtraction (solid), shown for the narrow spectral band (blue) and the broadband configuration (red). Bottom: corresponding g… view at source ↗
Figure 6
Figure 6. Figure 6: presents the contrast curves obtained under vari￾ous observing conditions, highlighting the residual wavefront er￾rors transmitted by the XAO first stage at different wind speeds. At moderate and high wind speeds (10 and 24 m.s−1 ), the loop operates efficiently and provides a significant contrast improve￾ment by a factor of nearly 10, respectively, inside the control ra￾dius. For a wind speed of 5 m.s−1 ,… view at source ↗
Figure 7
Figure 7. Figure 7: shows the contrast curves for different seeing con￾ditions, illustrating the residuals left by the first-stage correction that are subsequently handled by the second stage. For seeing values of 0.5” and 0.7”, the loop can be operated with high gains and provides a clear contrast gain within the 11 λ/D correction radius. When the seeing degrades to 1.0”, the injected phase vari￾ance increases substantially … view at source ↗
Figure 8
Figure 8. Figure 8: Contrast curves of the coronagraphic images obtained in broad￾band light for different flux levels, under standard atmospheric condi￾tions (seeing of 0.7′′ and wind speed of 10 m·s −1 ). Top: azimuthal av￾erages of the images in open loop (dashed lines) and closed loop (solid lines), plotted as a function of radial separation (in λ/D) for different fluxes expressed in relative magnitude. Bottom: gain curve… view at source ↗
read the original abstract

Current high-contrast facilities on the ground use extreme adaptive optics (XAO) systems to achieve contrasts down to $10^{-6}$ at 200\,mas for exoplanet observations. This performance is mainly limited by the XAO residuals due to the temporal errors in the XAO control loop. To overcome this issue, a promising solution consists in using cascade adaptive optics with a fast second stage. This approach was recently validated for a control loop based on a Zernike wavefront sensor (ZWFS) in monochromatic light. As wavefront sensors operate in broadband light to maximise photon sensitivity, this work aims to validate the ZWFS-based control loop in polychromatic light and assess its performance over a wide range of seeings, wind speeds, and stellar fluxes. Experiments were conducted on the ESO's GPU-based High-order adaptive OpticS Testbench (GHOST) testbed to probe our scheme in polychromatic light. Residual aberrations from a first-stage XAO system were simulated and our approach was evaluated in narrowband and broadband light through contrast in Lyot coronagraphic images. Closing the ZWFS-based control loop consistently improves contrast within its correction region in most tested conditions. After subtraction of quasi-static aberrations, our loop reaches a contrast gain up to one order of magnitude, independently of bandwidth and turbulence strength. The broadband and narrowband cases match in performance for bright sources, while narrowband remains slightly preferable for faint targets. These results demonstrate the feasibility of broadband ZWFS-based control loop and underline promising avenues with achromatic masks and an accurate calibration of quasi-static aberrations for future high-contrast imaging on Extremely Large Telescopes.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript experimentally validates a cascade adaptive optics scheme on the GHOST testbed in which a Zernike wavefront sensor (ZWFS) serves as the second stage. Simulated residuals from a first-stage XAO are injected into the testbed; the ZWFS loop is closed in both narrowband and broadband light across a range of seeing, wind speed, and stellar flux conditions. Contrast is measured in Lyot coronagraphic images, and the central claim is that loop closure yields contrast gains up to one order of magnitude after quasi-static aberration subtraction, with performance independent of bandwidth and turbulence strength (narrowband slightly preferred only for faint targets).

Significance. If the testbed results translate to on-sky conditions, the work would provide a practical path to mitigate the dominant temporal-error floor of current XAO systems for exoplanet imaging on ELTs. The hardware demonstration in polychromatic light is a necessary step beyond the prior monochromatic validation and directly addresses the photon-efficiency requirement of real wavefront sensors. The experimental nature supplies concrete contrast numbers rather than purely simulated predictions.

major comments (2)
  1. [Abstract and Results] Abstract and Results section: the headline claim of 'contrast gain up to one order of magnitude, independently of bandwidth and turbulence strength' is stated without error bars, standard deviations across repeated measurements, or explicit criteria for data inclusion/exclusion. Because the independence statement is load-bearing for the broadband feasibility conclusion, the absence of these statistics prevents quantitative assessment of robustness.
  2. [Methods] Methods section (description of injected residuals): the first-stage XAO residuals are described only as 'simulated' with no quantitative match provided to on-sky power spectral densities, temporal power spectra, or chromatic content (including NCPA and differential refraction). This omission directly affects the validity of the bandwidth-independence result, as any mismatch in spatial-frequency or wavelength dependence would alter ZWFS performance in ways not captured by the testbed data.
minor comments (2)
  1. [Abstract] The abstract would be clearer if it listed the precise wavelength ranges and bandwidths used for the narrowband and broadband cases.
  2. [Figures] Figure captions and axis labels should explicitly state whether contrast curves represent single realizations or averages, and whether the plotted values are raw or post-subtraction.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive feedback. The comments highlight opportunities to strengthen the statistical presentation and the description of the injected residuals. We address each point below and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [Abstract and Results] Abstract and Results section: the headline claim of 'contrast gain up to one order of magnitude, independently of bandwidth and turbulence strength' is stated without error bars, standard deviations across repeated measurements, or explicit criteria for data inclusion/exclusion. Because the independence statement is load-bearing for the broadband feasibility conclusion, the absence of these statistics prevents quantitative assessment of robustness.

    Authors: We agree that quantitative error estimates would strengthen the robustness claim. In the revised manuscript we will add standard deviations derived from repeated measurements (where available in the dataset) to the contrast-gain values reported in the Results section and abstract, and we will explicitly state the data-inclusion criteria used. This will allow readers to assess the statistical support for the reported independence from bandwidth and turbulence strength. revision: yes

  2. Referee: [Methods] Methods section (description of injected residuals): the first-stage XAO residuals are described only as 'simulated' with no quantitative match provided to on-sky power spectral densities, temporal power spectra, or chromatic content (including NCPA and differential refraction). This omission directly affects the validity of the bandwidth-independence result, as any mismatch in spatial-frequency or wavelength dependence would alter ZWFS performance in ways not captured by the testbed data.

    Authors: The injected residuals were generated from a standard first-stage XAO simulation employing Kolmogorov turbulence with parameters (seeing, wind speed, actuator count) chosen to match typical ELT conditions. The testbed experiment directly measures ZWFS performance in broadband light on those residuals; the observed bandwidth independence is therefore an empirical result under the tested conditions rather than a claim of perfect spectral fidelity. To address the concern we will expand the Methods section with the power spectral density and temporal spectrum of the injected residuals and note the absence of differential refraction and NCPA in the simulation. Full on-sky chromatic matching lies outside the scope of this controlled testbed validation. revision: partial

Circularity Check

0 steps flagged

No circularity: purely experimental validation on hardware with measured contrasts

full rationale

The paper reports testbed experiments on the GHOST facility using simulated first-stage XAO residuals injected into a ZWFS-based second-stage loop. Performance is quantified via direct contrast measurements in Lyot coronagraphic images under varying bandwidth, seeing, wind speed, and flux conditions. No derivations, first-principles predictions, fitted parameters renamed as outputs, or load-bearing self-citations appear in the abstract or described content. The central result (up to 10× contrast gain after quasi-static subtraction) is a measured hardware outcome, not a reduction to prior inputs by construction. Self-citation to prior monochromatic validation is present but not load-bearing for the broadband claims, which rest on new measurements.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

No mathematical derivation or new physical entities; the work rests on standard domain assumptions about testbed fidelity and AO simulation accuracy.

axioms (1)
  • domain assumption Testbed simulation of first-stage XAO residuals accurately represents on-sky conditions
    Invoked when stating that simulated residuals were used to evaluate the second-stage loop.

pith-pipeline@v0.9.1-grok · 5907 in / 1123 out tokens · 57440 ms · 2026-06-26T03:13:21.826908+00:00 · methodology

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Reference graph

Works this paper leans on

34 extracted references

  1. [1]

    T., & Oberti, S

    Agapito, G., Pinna, E., Esposito, S., Heritier, C. T., & Oberti, S. 2023, A&A, 677, A168

    2023

  2. [2]

    P., Bendek, E., Monacelli, B., & et al

    Bailey, V . P., Bendek, E., Monacelli, B., & et al. 2023, in Society of Photo- Optical Instrumentation Engineers (SPIE) Conference Series, V ol. 12680 (SPIE), 126800T

    2023

  3. [3]

    2019, A&A, 631, A155

    Beuzit, J.-L., Vigan, A., Mouillet, D., & et al. 2019, A&A, 631, A155

    2019

  4. [4]

    2022, in Proceedings of the SPIE, V ol

    Boccaletti, A., Chauvin, G., Wildi, F., & et al. 2022, in Proceedings of the SPIE, V ol. 12184, Ground-based and Airborne Instrumentation for Astronomy IX, ed. C. J. Evans, J. J. Bryant, & K. Motohara, 622–634

    2022

  5. [5]

    2024, in Proc

    Burgett, W., Bernstein, R., Ashby, D., et al. 2024, in Proc. SPIE 13094, Ground- based and Airborne Telescopes X, 13094E–17

    2024

  6. [6]

    2022, JATIS, 8, 019001

    Cerpa-Urra, N., Deo, V ., Kolb, J., Osborn, J., & Correia, C. 2022, JATIS, 8, 019001

    2022

  7. [7]

    Chauvin, G. 2024, C. R. Phys., 24, 139

    2024

  8. [8]

    T., et al

    Cisse, M., Muslimov, E., Heritier, C. T., et al. 2023, in AO4ELT7 Conference Proceedings, 1–6

    2023

  9. [9]

    1995, JOSA A, 12, 1559

    Conan, J.-M., Rousset, G., & Madec, P.-Y . 1995, JOSA A, 12, 1559

    1995

  10. [10]

    2023, in ASP Conf

    Currie, T., Biller, B., Lagrange, A., et al. 2023, in ASP Conf. Ser., V ol. 534, Protostars and Planets VII, ed. S. Inutsuka, Y . Aikawa, T. Muto, K. Tomida, & M. Tamura, 799

    2023

  11. [11]

    Darcis, S. et al. 2025, A&A, 701, A157

    2025

  12. [12]

    S., Fagginger Auer, F., Escuti, M

    Doelman, D. S., Fagginger Auer, F., Escuti, M. J., & Snik, F. 2019, Opt. Lett., 44, 17

    2019

  13. [13]

    2024, arXiv preprint arXiv:2411.05408 [arXiv:2411.05408]

    Engler, B., Kasper, M., Leveratto, S., et al. 2024, arXiv preprint arXiv:2411.05408 [arXiv:2411.05408]

    arXiv 2024

  14. [14]

    2022, in 2022 IEEE Workshop on Signal Processing Systems (SiPS) (IEEE), 1–6

    Ferreira, F., Bernard, J., Sevin, A., Doucet, N., & Gratadour, D. 2022, in 2022 IEEE Workshop on Signal Processing Systems (SiPS) (IEEE), 1–6

    2022

  15. [15]

    Fitzgerald, M. P. et al. 2019, BAAS, 51, 251

    2019

  16. [16]

    Fried, D. L. 1990, JOSA A, 7, 1224

    1990

  17. [17]

    2018, ARA&A, 56, 315

    Guyon, O. 2018, ARA&A, 56, 315

    2018

  18. [18]

    Haffert, S. Y . 2024, A&A, 683, A113 Héritier, C. T., Vérinaud, C., & Correia, C. 2023, OOPAO: Object Oriented Python Adaptive Optics, Proceedings of the AO for Extremely Large Tele- scopes Conference (AO4ELT)

    2024

  19. [19]

    2015, PASP, 127, 890

    Jovanovic, N., Guyon, O., Martinache, F., & et al. 2015, PASP, 127, 890

    2015

  20. [20]

    2021, The Messenger, 182, 37

    Kasper, M., Cerpa Urra, N., Pathak, P., et al. 2021, The Messenger, 182, 37

    2021

  21. [21]

    P., et al

    Kasper, M., Fedrigo, E., Looze, D. P., et al. 2004, JOSA A, 21, 1004

    2004

  22. [22]

    1932, Zeitschrift für Astrophysik, 5, 73

    Lyot, B. 1932, Zeitschrift für Astrophysik, 5, 73

    1932

  23. [23]

    R., Ingraham, P., & et al

    Macintosh, B., Graham, J. R., Ingraham, P., & et al. 2014, PNAS, 111, 12661

    2014

  24. [24]

    2024, JATIS, 10, 035004

    Mennesson, B., Belikov, R., Por, E., et al. 2024, JATIS, 10, 035004

    2024

  25. [25]

    2021, in Opti- cal Instrument Science, Technology, and Applications II (SPIE), 56–68, arXiv:2110.10263 N’Diaye, M., Dohlen, K., Fusco, T., & Paul, B

    Muslimov, E., Levraud, N., Chambouleyron, V ., et al. 2021, in Opti- cal Instrument Science, Technology, and Applications II (SPIE), 56–68, arXiv:2110.10263 N’Diaye, M., Dohlen, K., Fusco, T., & Paul, B. 2013, A&A, 555, A94 N’Diaye, M., Vigan, A., Engler, B., et al. 2024, A&A, 692, A157

    arXiv 2021

  26. [26]

    2024, JATIS, 10, 019001

    Nousiainen, J., Engler, B., Kasper, M., et al. 2024, JATIS, 10, 019001

    2024

  27. [27]

    2022, A&A, 664, A71

    Nousiainen, J., Rajani, C., Kasper, M., et al. 2022, A&A, 664, A71

    2022

  28. [28]

    Ragazzoni, R. 1996, J. Mod. Opt., 43, 289

    1996

  29. [29]

    & Farinato, J

    Ragazzoni, R. & Farinato, J. 1999, A&AS, 136, 205

    1999

  30. [30]

    & Roddier, F

    Sarazin, M. & Roddier, F. 1990, A&A, 227, 294

    1990

  31. [31]

    2019, A&A, 629, A11

    Vigan, A., N’Diaye, M., Dohlen, K., et al. 2019, A&A, 629, A11

    2019

  32. [32]

    & Smith, B

    Vilas, F. & Smith, B. A. 1987, Appl. Opt., 26, 664

    1987

  33. [33]

    K., Rao, S., Jensen-Clem, R

    Wallace, J. K., Rao, S., Jensen-Clem, R. M., & Serabyn, G. 2011, in Proceedings of the SPIE, V ol. 8126, Adaptive Optics Systems II, 81260F

    2011

  34. [34]

    1934, MNRAS, 94, 377 Article number, page 12 of 13 A

    Zernike, F. 1934, MNRAS, 94, 377 Article number, page 12 of 13 A. Rahim et al.: Cascade AO with ZWFS – Part II: Validation in broadband light Appendix A: Summary of the experiments Table A.1presents the second-stage AO loop parameters with the corresponding coronagraphic performance for all experimental configurations discussed in this paper. Table A.1.Se...

    1934