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REVIEW 3 major objections 7 minor 23 references

An optimized classical Lyot coronagraph on ELT/ANDES reaches 10^{-3} raw contrast at 20 mas and, with molecular mapping, 10^{-7} detection limits for hot gas giants.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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T0 review · grok-4.5

2026-07-30 19:11 UTC pith:NB2XSQCG

load-bearing objection Solid ANDES-specific CLC design and first-order error budget that hits the 10^{-3} at 20 mas goal under stated SCAO residuals; APU 10^{-7} limits are promising but still preliminary. the 3 major comments →

arxiv 2607.23555 v1 pith:NB2XSQCG submitted 2026-07-26 astro-ph.IM astro-ph.EP

ANDES, the high-resolution spectrograph of the ELT: simulated performance of the CORO module and overview of the high-contrast capabilities for exoplanet observations

M. N'Diaye , A. Simonnin , A. Spang , P. Berio , A. Chiavassa , G. Agapito , C. Bailet , G. Carl\`a
show 14 more authors
Y. Caujolle O. Carri\'on-Gonzalez G. Chauvin S. Cuevas O. Gabella M. Houll\'e S. Lagarde P. Martinez E. Pinna B. Rajpoot J. Seidel C. Selmi A. Vigan P. Di Marcantonio
This is my paper
classification astro-ph.IM astro-ph.EP
keywords ExoplanetELTHigh-Contrast Imaging and SpectroscopyAdaptive opticsCoronagraphyLyot coronagraphANDESmolecular mapping
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.

ANDES is the ELT’s planned high-resolution spectrograph. This paper shows that adding a simple classical Lyot coronagraph after its single-conjugate adaptive-optics system can suppress starlight enough to hit the instrument’s 10^{-3} contrast goal at only 20 milliarcseconds across the near-infrared YJH bands. End-to-end simulations with the APU tool then demonstrate that combining that raw contrast with high-dispersion molecular mapping yields 5-sigma detection limits near 10^{-7} for L-type gas giants in a two-hour observation. The work therefore establishes that high-contrast imaging plus R=100,000 spectroscopy on the ELT is within reach with a compact, moderate-gain coronagraph, opening a path to atmospheric characterization of close-in exoplanets in emitted light and, later, reflected light.

Core claim

With a classical Lyot coronagraph sized at FPM diameter 3.9 λ_ref/D (33.4 mas), Lyot outer diameter 0.89 D and inner diameter 0.35 D, the SCAO+CORO combination delivers raw contrast ≤10^{-3} at 20±3.5 mas over 1.0–1.7 µm under median seeing; subsequent molecular-mapping post-processing on APU data cubes reaches ~10^{-7} 5σ contrast for 1600 K gas giants in two hours.

What carries the argument

The optimized classical Lyot coronagraph (opaque focal-plane mask plus annular Lyot stop matched to the ELT pupil) acting on SCAO residual phase screens; its parameter-space design jointly minimizes residual starlight and maximizes planet SNR at 20 mas, after which the APU end-to-end simulator folds in high-dispersion cross-correlation.

Load-bearing premise

The simulated SCAO residual wavefronts plus a first-order error budget (pointing, defocus, chromatic dispersion, Lyot-stop alignment, NCPA) are assumed sufficient to guarantee the on-sky 10^{-3} raw contrast that later multiplies into the 10^{-7} detection claim.

What would settle it

Once the CORO module is built and integrated with SCAO, measure the on-sky raw contrast at 20 mas in median seeing with an I≤8 star; if it exceeds a few times 10^{-3} after the stated tip/tilt and NCPA corrections, the central performance claim fails.

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

If this is right

  • ANDES can target temperate giant planets around nearby stars at separations previously inaccessible to high-resolution spectroscopy.
  • The same CORO+IFU mode supplies the contrast floor needed to attempt reflected-light detection of the ANDES golden-sample rocky planets.
  • A compact classical Lyot design meets the requirement without added system complexity, allowing the module to remain insertable.
  • Preliminary error-budget numbers (2 mas tip/tilt, 30 nm RMS NCPA, 5 mas/µm ADC residual) become the engineering specifications for the opto-mechanical build.

Where Pith is reading between the lines

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

  • If the raw-contrast floor holds, molecular-mapping gain may allow ANDES to reach the 10^{-8} regime quoted in the introduction for the most favorable nearby systems.
  • The large FPM diameter that confers tip/tilt robustness also sets a relatively wide inner working angle (~18 mas), so science cases inside that radius will still rely on non-coronagraphic SCAO-IFU modes.
  • Absence of a full Fresnel model for Lyot-stop longitudinal error implies that deeper contrasts (beyond 10^{-3}) will require a second design iteration once HCIpy-style propagation is 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 / 7 minor

Summary. The manuscript presents the design and simulated performance of the insertable classical Lyot coronagraph (CORO) module for the ANDES SCAO-IFU mode at the ELT. The authors optimize the focal-plane mask diameter and Lyot stop inner/outer diameters by grid search on a joint contrast/SNR metric over 1.0–1.7 µm, arriving at d = 3.9 λ_ref/D (33.4 mas), OD = 0.89D, ID = 0.35D, with a 17.7 mas IWA and 75% planet throughput. Using SPECULA/PASSATA SCAO residual phase screens (median JQM conditions, Strehl ~83% in H), they show raw contrast ≤10⁻³ at 20 mas across YJH, meeting the stated goal. Section 4 injects individual error sources (pointing, defocus, ADC residual, Lyot stop clocking/lateral offset, NCPA) one at a time to derive a preliminary tolerance budget that feeds the companion opto-mechanical design paper. Section 5 previews APU end-to-end simulations indicating ~10⁻⁷ 5σ detection limits for 1600 K L-type giants in 2 h via molecular mapping.

Significance. If the results hold, this is a useful and timely design study: it delivers a concrete, optimized coronagraph point design for an ELT instrument with quantified planet throughput and IWA, and it translates contrast-stability analysis into physical opto-mechanical tolerances (µm-level FPM defocus, Lyot stop positioning) that directly feed hardware design ahead of the 2026 PDR. The APU detection limits are forward predictions under stated assumptions, not fitted to a claimed yield, and a public code release is promised. The work is honest about its preliminary status. Its limitations — separately budgeted errors, a missing Fresnel model for Lyot stop longitudinal placement, and thin detail on the APU post-processing — are acknowledged but do bound how strongly the 10⁻³ on-sky floor and the 10⁻⁷ detection claim can be taken as guaranteed.

major comments (3)
  1. [§4.1–4.7 (error budget)] All error sources are injected individually, and each tolerance is then tightened by an ad-hoc margin 'to account for further source errors' (e.g., 2 mas pointing vs. 3 mas robustness; 30 nm RMS NCPA vs. 70 nm RMS tolerance). Since the §4.7 values flow directly into the opto-mechanical design (ref. 7), the manuscript should demonstrate — or at least estimate — that the simultaneous combination of all errors at their specified values still yields ≤10⁻³ at 20 mas. A single joint simulation at the spec values, or a quadrature-sum argument based on the individual contrast contributions, would substantially strengthen the central claim that the budget 'ensures a stable 10⁻³ contrast'.
  2. [§4.5 (Lyot stop longitudinal position)] The ±0.5 mm longitudinal tolerance for the Lyot stop is adopted by analogy with SPHERE, with the assertion that 'the depth of focus at the pupil plane is quite large.' No quantitative support is given, and the authors themselves note that Fresnel propagation effects 'can alter the coronagraph performance for deep contrasts' but that no Fresnel model was available. Given that this is the one tolerance in §4.7 not derived from simulation, a scaling estimate (e.g., Fresnel number at the relayed pupil given the 10.15 mm beam and F/34.75) showing the effect is sub-dominant at 10⁻³ would close this gap; alternatively the text should state explicitly that this value is unvalidated and carries design risk.
  3. [§5 and Fig. 14 (APU detection limits)] The headline ~10⁻⁷ 5σ detection limit is under-specified in this manuscript: the host-star magnitude, the separation at which 10⁻⁷ is reached, the number of spectral channels entering the cross-correlation, and the relative treatment of photon noise versus quasi-static speckle noise are not stated, and the molecular-mapping implementation is deferred entirely to Simonnin et al. (in prep). Since Fig. 14 is presented as a result of this paper, the key assumptions needed to assess it should be summarized here; otherwise the 10⁻⁷ figure should be explicitly scoped as an illustrative external result rather than a finding of this work.
minor comments (7)
  1. [§2.1, §2.3, §3] The contrast metric is defined three ways: a radial profile averaged in 3.5 mas bins (§2.1), a 7 mas-diameter photometric aperture (§2.3), and a 7 mas-wide annulus centered at 20 mas (§3). Please harmonize or clarify which definition applies to the quoted 10⁻³ performance.
  2. [Figs. 7–13] The curve envelopes 'represent the results for different realizations of AO residuals,' but the number of realizations is never stated. Please give N and clarify whether envelopes show min–max or a percentile range.
  3. [§2.3] The broadband optimization averages residual intensity over 1.0–1.7 µm, but the spectral weighting (flat, stellar spectrum, or photon-weighted) is not specified; this affects the selected optimum.
  4. [§4.3] The ADC residual is modeled as linear in wavelength with perfect correction at λ_ref = 1.6 µm. Real ADC residuals are chromatic in a more complex way; a sentence noting this idealization and its likely impact on the 5 mas/µm requirement would be helpful.
  5. [Figs. 4–6] Curves at 950 and 1850 nm are shown although the requirement band is 1.0–1.7 µm; please state whether these are illustrative extrapolations outside the CORO operating range.
  6. [§2.1] The parenthetical '(initially 77% at 500 Hz) 83% at 1 kHz' is confusing — please clarify which Strehl/loop-speed assumption is used in the simulations presented here.
  7. [Throughout] Typographical: 'carbon-to-monoxide ratio' (§5) should presumably be 'carbon-to-oxygen (C/O) ratio'; 'magnitude larger than 8' (§2.1) should read 'brighter than I=8'; 'have showed' → 'have shown' (§4.5, §5); heading artifacts 'IMP ACT' and 'OBSER V A TIONS'.

Circularity Check

0 steps flagged

No significant circularity: forward engineering simulations against external AO residuals and standard coronagraph metrics.

full rationale

The paper’s load-bearing chain is ordinary instrument design and end-to-end simulation, not a closed logical loop. Contrast requirements (3×10⁻³ baseline / 10⁻³ goal at 20 mas over YJH) are stated as instrument specs; CLC parameters (FPM d=3.9 λ_ref/D, Lyot OD=0.89D, ID=0.35D) are chosen by a grid search that maximizes residual-star intensity and SNR⁻¹ in aberration-free broadband light, then re-evaluated under SPECULA/PASSATA SCAO residual phase screens (external AO library) plus a first-order error budget. Achieved raw contrast ≤10⁻³ is therefore a computed output of wave-optics propagation under stated inputs, not a quantity fitted to the target or defined in terms of itself. APU 5σ detection limits (~10⁻⁷ for L-type giants) are likewise forward predictions under listed assumptions (2 h, BT-Settl/ATMO/petitRADTRANS spectra, tellurics, ETC noise, molecular mapping), not tautological restatements of fitted constants. Self-citations (Berio et al. companion optomechanics; Simonnin et al. APU in prep; Pinna/Agapito SCAO) supply subsystem context and residual screens but do not import a uniqueness theorem or force the contrast result by definition. No self-definitional step, fitted-input-as-prediction, or renamed empirical law is present.

Axiom & Free-Parameter Ledger

4 free parameters · 6 axioms · 2 invented entities

Central contrast and yield claims rest on external AO simulation libraries, median-atmosphere assumptions, a classical Lyot forward model without full Fresnel propagation, and APU post-processing assumptions (planet atmosphere grids, tellurics, noise model). No new physical entities; free parameters are design choices and tolerance cutoffs selected to meet the 10⁻³ requirement.

free parameters (4)
  • FPM diameter d = 3.9 λ_ref/D (33.4 mas at 1.6 µm)
    Chosen by grid search (3.0–4.5 λ_ref/D) to optimize joint contrast/SNR metric; final 3.9 λ_ref/D is a design free parameter, not derived from first principles.
  • Lyot stop OD, ID = OD=0.89 D, ID=0.35 D
    Grid-searched (OD 0.82–0.96 D, ID 0.30–0.45 D); selected 0.89 D / 0.35 D as joint-metric optimum.
  • Pointing / defocus / NCPA / ADC / Lyot alignment tolerances = 2 mas; 30 nm RMS; 5 mas/µm; 1°; 1% D; ±0.5 mm
    Cutoffs (2 mas, 30 nm RMS, 5 mas/µm, 1°, 1% D_ELT, ±0.5 mm) chosen so contrast stays ≤10⁻³ with margin; not uniquely determined by data.
  • APU observation time and planet T_eff = 2 h; T_eff=1600 K
    2 h integration and 1600 K L-type case are scenario choices that set the quoted 10⁻⁷ limit.
axioms (6)
  • domain assumption SPECULA/PASSATA SCAO residuals under median 0.67" seeing deliver ~83% Strehl in H and ~1.2×10⁻² raw contrast at 20 mas before the coronagraph.
    §2.1 and §3.1; all coronagraph gains are measured relative to these screens.
  • domain assumption A classical Lyot coronagraph (opaque FPM + undersized Lyot stop) is an adequate starlight-suppression architecture for the 10⁻³ requirement over YJH; vortex or other masks deferred.
    §2.1 design choice justified by residual WFE level and bandwidth.
  • domain assumption Contrast is the azimuthally averaged, peak-normalized intensity in a 7 mas (1 spaxel) radial bin; planet throughput uses infinite and 7 mas photometric apertures.
    §2.1–2.3 metric definitions that set the optimization target.
  • domain assumption Molecular-mapping / cross-correlation on R=100,000 IFU cubes supplies the additional orders-of-magnitude contrast gain from ~10⁻³ raw to ~10⁻⁷ detection limit.
    §1 and §5; relies on Snellen et al. 2015 / Hoeijmakers et al. 2018 scaling under APU noise model.
  • ad hoc to paper Individual error sources may be budgeted separately; joint simultaneous injection and Fresnel propagation of Lyot longitudinal error are second-order for this contrast floor.
    §4 structure and explicit note that Fresnel model ‘was not available at the time of writing’.
  • domain assumption BT-Settl / ATMO / petitRADTRANS planet and star spectra, TelFit tellurics, SkyCalc emission, and ANDES ETC noise are adequate for first-order yield.
    §5 APU assumptions.
invented entities (2)
  • ANDES CORO module (insertable classical Lyot unit in SCAO-IFU path) no independent evidence
    purpose: Provide the starlight suppression hardware that turns SCAO+IFU into a high-contrast spectro-imager.
    Instrument subsystem officially baselined April 2025; design parameters and tolerances are the paper’s main product. Not a new physical particle/force—hardware entity with independent future lab/on-sky tests planned.
  • APU (ANDES Performance Unfolded) end-to-end simulator no independent evidence
    purpose: Propagate SCAO residuals through coronagraph+IFU and post-process to exoplanet detection limits and yields.
    Cited as Simonnin et al. in prep; first public release expected 2026. Results in Fig. 14 depend on it.

pith-pipeline@v1.2.0-grok45-kimik3 · 22888 in / 4242 out tokens · 77300 ms · 2026-07-30T19:11:37.783600+00:00 · methodology

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read the original abstract

We present the simulated performance of the coronagraph (CORO) module for ANDES, the Extremely Large Telescope (ELT) high-resolution spectrograph. ANDES aims to address a broad range of science cases, including the characterization of the atmosphere of exoplanets. With a first light envisioned by 2035, the instrument baseline features a modular fiber-fed echelle spectrograph with visible and near-infrared ultra-stable spectral arms to provide a simultaneous spectral range of 0.4-1.8\,$\mu$m with a spectral resolving power up to 100,000. ANDES also includes an Integral Field Unit (IFU) mode-fed by a single-conjugate adaptive optics (SCAO) module and an insertable CORO module, enabling the combination of high-contrast imaging and high-dispersion spectroscopy (R=100,000) for the study of exoplanet properties. In this contribution, the ANDES CORO design, its main features and its simulated performance are detailed in the presence of SCAO residual errors to probe exoplanet atmospheres with the spectro-imager mode at high-spatial resolution and with unprecedented angular resolution. We show the preliminary simulation results on the predicted contrast and the expected detection performance with ANDES performance unfolded (APU), the simulation tool to determine the yield of exoplanets that will be detected in emitted and possibly reflected light. The characterization operation of the instrument will be discussed to assess the ANDES ability to detect atomic and molecular signatures connected to the exoplanet atmosphere characteristics.

Figures

Figures reproduced from arXiv: 2607.23555 by A. Chiavassa, A. Simonnin, A. Spang, A. Vigan, B. Rajpoot, C. Bailet, C. Selmi, E. Pinna, G. Agapito, G. Carl\`a, G. Chauvin, J. Seidel, M. Houll\'e, M. N'Diaye, O. Carri\'on-Gonzalez, O. Gabella, P. Berio, P. Di Marcantonio, P. Martinez, S. Cuevas, S. Lagarde, Y. Caujolle.

Figure 1
Figure 1. Figure 1: Optical layout of the CLC with four planes: the entrance pupil plane A, the downstream focal plane B in which [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Display of pupils for the CLC. Left: ELT pupil. Right: Example of Lyot stop (final version for the coronagraph). [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Residual intensity Is in log scale in broadband light (optimization in YJH band) (left), the SNR−1 (middle), and the joint metric (right), inside the coronagraphic image within the search area, i.e., 20.0±3.5 mas from the star, as a function of the Lyot stop OD and ID for a FPM diameter d=3.9 λref /D (left). The white cross-mark denotes the selected solution that is recalled in [PITH_FULL_IMAGE:figures/fu… view at source ↗
Figure 4
Figure 4. Figure 4: Normalized planet throughput as a function of the angular separation from an observed star at different [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Simulated images of an on-axis point source in median observing conditions after SCAO correction. The top [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Azimuthally averaged intensity profiles of the images in median observing conditions (JQM) after SCAO correc [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Azimuthally averaged contrast level of the coronagraphic images over an annulus of 7 mas centered at 20 mas [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Azimuthally averaged contrast level of the coronagraphic images over an annulus of 7mas width centered at [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Azimuthally averaged contrast level of the coronagraphic images over an annulus of 7 mas width centered at [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Azimuthally averaged contrast level of the coronagraphic images over an annulus of 7 mas width centered [PITH_FULL_IMAGE:figures/full_fig_p010_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Azimuthally averaged contrast level of the coronagraphic images over an annulus of 7 mas width centered at [PITH_FULL_IMAGE:figures/full_fig_p011_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Azimuthally averaged contrast level of the coronagraphic images over an annulus of 7mas width centered at [PITH_FULL_IMAGE:figures/full_fig_p012_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Azimuthally averaged contrast level of the coronagraphic images over an annulus of 7 mas-width centered at [PITH_FULL_IMAGE:figures/full_fig_p013_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: 5σ detection limits with ANDES using APU for L-type gas giant planets as a function of the angular separation. The top and bottom curves represent the spectrally averaged raw contrast curves and the contrast curves after post￾processing using molecular mapping techniques. The red and blue curves represent the curves of the images without and with coronagraph. The envelope of the top curves represents the … view at source ↗

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