Pith. sign in

REVIEW 3 major objections 5 minor 25 references

ANDES, the high-resolution spectrograph for the ELT: design and performance analysis of the YJH spectrograph

T0 review · 3 major / 5 minor · reviewed 2026-08-01 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read The V36 design of the ANDES YJH spectrograph attains an average 2-pixel sampling, and with a 15% degradation margin the modelled resolving power stays between 100,000 and 123,000 across the Y, J and H bands.

desk verdict A credible, workmanlike design status paper for ANDES V36; the headline R≥100,000 rests on an honest but unverified 15% degradation margin, and the LSF simulation doesn't match the baseline mosaic, but these are typical growing pains for a preliminary design. read the letter →

arxiv 2607.22388 v1 pith:ZSXER4FF submitted 2026-07-24 astro-ph.IM

Vinooja Thurairethinam (1) , David Lee (1) , James Stevenson (1) , Étienne Artigau (2) , Frédérique Baron (2) , Ciarán Breen (1) , Bella Boyd (1) , Denis Brousseau (3)
show 29 more authors
David Buscher (4) Neil J. Cook (2) René Doyon (2) Martin Fisher (4) Bradley Frank (1) Vincent Geers (1) Rory Gillespie (1) Oscar Gonzalez (1) Éamonn J. Harvey (1) Wei Li (4) Lison Malo (2) Roberto Maiolino (4) David Montgomery (1) Alan O'Brien (1) Ernesto Oliva (5) Jonathan St-Antoine (2) Jay Stephan (1) Simon Thibault (3) Philippe Vallée (2) Chris Waring (1) Sandi Wilson (1) Junyi Zhou (1) Paolo Di Marcantonio (6) ((1) UK Astronomy Technology Centre (2) Université de Montréal (3) Université Laval (4) Cavendish Laboratory University of Cambridge (5) INAF - Osservatorio Astrofisico di Arcetri (6) INAF - Osservatorio Astronomico di Trieste)
This is my paper · ORCID
classification astro-ph.IM
keywords ANDESYJHspectrographELTinstrumentationechellegratingmosaiccryogenicfibre-fedspectralresolutionnear-infraredspectroscopy
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 reports the current design and performance analysis of the YJH infrared spectrograph module for the ELT's ANDES instrument, covering 0.95–1.8 µm at a target spectral resolution of about 100,000. The central claim is that the redesigned V36 optical train achieves an average sampling of exactly 2 pixels across the fibre spread function, and that even after applying a 15% degradation margin to represent manufacturing and alignment errors, the resolving power at the detector remains between 100,000 and 123,000 in all three bands. This matters because the YJH module must combine ultra-stable wavelength calibration with high resolution on the largest telescope, to study exoplanet atmospheres, the intergalactic medium, and fundamental constants. The riskiest element is the primary disperser: a cryogenic R4 echelle grating mosaic over a metre long, which no existing instrument has built.

What carries the argument

The load-bearing component is the cryogenic R4 echelle grating mosaic: a roughly 1.3 metre long, 16 lines-per-mm grating on an Invar substrate, assembled from four segments because no single grating of that size can be manufactured, and mounted with same-material kinematics to keep alignment from room temperature to 100 K. Around it, the optical system uses a 75-fibre reformatted slit with microlenses, an anamorphic slit module, a non-Littrow off-axis collimator, dichroic splitters into Y/J/H channels, and three five-lens cameras each feeding an H4RG-15 detector. The performance claim is carried by the end-to-end model and the PyEchelle simulator that convert the fibre spread function FWHM i

What would settle it

A concrete check: once the V36 spectrograph is built, measure the collapsed fibre spread function FWHM at a grid of positions in the Y, J and H detectors and compute the resolving power from the delivered line profile; if any order falls below R=100,000, the paper's central claim is falsified. Before build, a full tolerance analysis that varies the 4x1 Invar mosaic segment piston, tip and tilt at 0.95–1.8 µm and propagates the resulting wavefront error through the end-to-end model would also settle whether the 15% margin is adequate.

Watch

Extended reading notes

Core claim

On the paper's own terms, the discovery is a design validation rather than a new astrophysical result: the V36 YJH spectrograph layout, after moving the anamorphic slit module and rebalancing the three cameras, produces a collapsed fibre spread function with a FWHM averaging 2.0 pixels across the Y, J and H orders. When the end-to-end model applies an estimated 15% FWHM degradation as a stand-in for as-built tolerances, the FWHM falls between 2.0 and 3.0 pixels, the inter-order gaps exceed 6 pixels, and the resolving power stays between 100,000 and 123,000 at every wavelength. The paper stresses that these are preliminary numbers to be confirmed by a matured optical model, a full tolerance a

Load-bearing premise

The central claim rests on the assumption, stated in Section 4.2, that a single uniform 15% FWHM degradation margin chosen from prior experience with cryogenic instruments represents the combined manufacturing and alignment errors of this as-built spectrograph; if the real degradation is larger or nonuniform, the R≥100,000 result may not hold.

Editorial extensions

If this is right

  • If the V36 performance holds in the as-built instrument, a single fibre-fed cryogenic spectrograph can cover the full 0.95–1.8 µm range at R≥100,000 without being oversampled, meeting the baseline ANDES resolution requirement.
  • The greater-than-10^14 suppression of thermal background from the cold slit selector at 1.8 µm means the H band, the hardest for warm background, is usable for high-resolution science.
  • Because the 4x1 Invar mosaic keeps the line spread function between 2.0 and 3.0 pixels, the detector sampling stays in the regime needed for precise radial-velocity work, supporting the 1 m/s stability goal over 24 hours.
  • The grating mosaic's gaps and segment misalignments produce LSF wing distortion at infrared wavelengths but, at the simulated levels, do not push resolving power below 100,000; this defines how much grating segment alignment error the science can tolerate.

Reading between the lines

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

  • The paper leaves implicit that the 15% degradation margin is a placeholder rather than a measured budget; a full tolerance analysis could show the real FWHM growth varies across the field, which would make the R≥100,000 claim wavelength-dependent.
  • The misalignment simulation in the paper uses a 3x1 Zerodur mosaic at 0.5 µm, while the baseline is a 4x1 Invar mosaic operating at 0.95–1.8 µm; repeating the piston-shift study at the baseline configuration would test whether the H-band LSF distortion seen in the simulation actually matters for the science cases.
  • The tight link between the R4 mosaic's supply and the resolution requirement suggests that if the supplier cannot deliver the 16 lines-per-mm R4 grating with the assumed efficiency, the whole 100,000-resolving-power case would need to be reworked.
  • The interchangeable seeing-limited and diffraction-limited modes place different illumination patterns on the same slit and detector; the paper's FWHM metric is based on a particular fibre format, so the IFU mode may need its own verification of sampling and LSF.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

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 reports the current V36 design of the YJH (YS) cryogenic echelle spectrograph for the ANDES instrument on the ELT, covering 0.95–1.8 μm at a target resolving power R ≈ 100,000. It describes the optical layout, the dual seeing-limited/IFU slit concept, the cold slit selector, the cryogenic/mechanical architecture, and the main technological risk: a metre-scale R4 echelle grating mosaic. The performance section presents end-to-end simulations (Zemax, PCGrate, PyEchelle) of throughput, spot diagrams, sampling, and resolving power. The central claim is that, after applying an estimated uniform 15% FWHM degradation to represent manufacturing and alignment tolerances, the as-built spectrometer will deliver FWHM between 2.0 and 3.0 pixels and resolving power between 100,000 and 123,000 across all three Y, J, H bands (§4.2, §5).

Significance. If the performance claim holds, the YS design demonstrates a feasible path to a large cryogenic high-resolution NIR spectrograph for the ELT, including a technology-critical 4×1 Invar echelle mosaic. The paper is valuable as a design-study status report, and the use of end-to-end simulations with PCGrate and PyEchelle is a strength. However, the headline result—R ≥ 100,000 after tolerances—rests on a single hand-assigned 15% FWHM degradation margin that is not derived from a tolerance analysis, and the only supporting misalignment simulation uses a different mosaic configuration and a wavelength outside the YS band. The claim is therefore not yet substantiated at the level required for a definitive performance guarantee, though the design itself appears plausible.

major comments (3)
  1. [§4.2 and §5] The central claim that the as-built instrument will maintain R between 100,000 and 123,000 is based entirely on 'an estimated 15% degradation margin' applied uniformly in the end-to-end model, justified only by 'prior experience with other cryogenic instruments.' No tolerance analysis, sensitivity study, or error budget is presented. The conclusion itself cautions that 'full tolerance analysis' will be needed in later phases. This makes the R ≥ 100,000 guarantee load-bearing but unsupported. Please provide either a tolerance propagation, a realistic bound on the degradation, or a sensitivity curve showing how R and FWHM vary with the degradation percentage (e.g., 10%, 15%, 20%, 25%) and with non-uniform degradation across field, band, and order.
  2. [§3.2.1 and §3.3] The only quantitative misalignment simulation used to inform the degradation margin is for a 3×1 Zerodur grating mosaic, evaluated at 0.5 μm and 1.8 μm. The V36 baseline, however, is a 4×1 Invar IC-DX mosaic (§3.3), and the YS operating band is 0.95–1.8 μm. The 0.5 μm case is explicitly outside the YS band, and the 3×1 versus 4×1 geometry, substrate, and gap spacing (4 mm vs 10 mm) affect both the number of phase steps and the width of the pupil distribution. Moreover, the simulation reports qualitative LSF distortion but does not convert that distortion into a FWHM or resolving-power change. Thus this simulation does not directly support the 15% margin applied to the baseline design. Please either rerun the misalignment study for the 4×1 Invar geometry over the full YS band, or clearly state that the existing simulation is only illustrative and provide an alternative quantitative basis
  3. [§3.2.1] The text states: 'At the shortest, visible wavelength of 0.5 μm of the YS...'. The YS band begins at 0.95 μm; 0.5 μm is not a wavelength of the YS. This is not merely a typo: it reveals that the simulation was designed for a different spectral range (likely the full ANDES visible arm) and was then applied to the NIR instrument. Please correct the wavelength attribution and ensure the simulation is relevant to the YS operating band.
minor comments (5)
  1. [§4.2] The term 'sampling' is used interchangeably for 'FWHM of the collapsed FSF in pixels' and 'average sampling.' Define both formally at first use, and report the range of sampling across orders/bands, not only the average.
  2. [Figure 10] The LSF plots would benefit from quantitative axes (intensity vs. pixel or angular scale) and from a statement of the piston offset magnitude (in nm or waves) used in the simulation. Without these, the reader cannot judge whether the applied offsets are representative of the as-built alignment tolerances.
  3. [§1 and abstract] The paper alternates between '0.4–1.8 μm' and '0.35–1.8 μm' for the full ANDES coverage; make the numbers consistent.
  4. [References] Reference [8] and [21] are duplicates (same Bouchy et al. paper). Also check author list formatting for Ref. [17]; 'for the for the' appears in the title.
  5. [§5] Minor grammatical issue: 'which would result in the degrading and blurring the image' should be 'degrading and blurring the image'.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the R/FWHM values are model outputs under a disclosed 15% degradation assumption, not fitted inputs or self-referential predictions.

full rationale

The central performance claim (V36 sampling ≈2 pixels and R = 100,000–123,000 after degradation) is produced by the end-to-end model with a stated 15% FWHM degradation margin applied in Section 4.2. This margin is an input assumption, not a parameter fitted to the required resolving power, and the paper explicitly labels it as 'an estimated 15 % degradation margin... based primarily on prior experience with other cryogenic instruments.' The resulting FWHM and R values are therefore a model prediction conditional on that assumption, not a restatement of the assumption itself. The paper does not derive the 15% from the target R, nor does it rename a measured output as a prediction. The only quantitative tolerance simulation (Section 3.2.1) is presented as preliminary, uses a 3×1 Zerodur mosaic at 0.5 and 1.8 µm rather than the V36 baseline 4×1 Invar mosaic, and the paper explicitly leaves open whether the LSF distortion is significant for science ('whether this distortion of the LSF is sufficiently large to cause a significant effect on the current science cases remains yet to be determined'). It is therefore not used to force the headline result. Self-citations (e.g., Ref. 9 for prior camera design; Refs. 6–8 for heritage material experience) are normal engineering heritage references and are not load-bearing for the R≥100,000 claim. The paper's own caveat that 'preliminary results will be confirmed in the next phases... with a further matured optical model, full tolerance analysis, and MAIT measurements' is a limitation on validation, not circularity. No step in the derivation reduces to its own input by construction.

Assumptions & free parameters 3 free parameters · 4 assumptions · 0 invented entities

No new physical entities are introduced; the free parameters are margins and model assumptions used in the preliminary performance estimate. The main load-bearing assumption is the 15% degradation factor, which lacks a tolerance-analysis basis.

free parameters (3)
  • FWHM degradation margin = 15%
    Hand-applied margin to convert ideal optical performance to as-built estimate for manufacturing/alignment tolerances, based on prior cryogenic instrument experience (§4.2). This margin directly determines whether R≥100,000 is claimed.
  • Throughput contingency margin = 5%
    Uniform contingency applied to all optical throughput components to cover non-compliant optics (§4.1).
  • Grating groove facet angle = 90°
    Assumed blaze facet angle in PCGrate model for nominal efficiency simulation (§4.1).
assumptions (4)
  • domain assumption Zemax, PCGrate and PyEchelle simulations correctly model diffraction and imaging for the described design.
    Performance results depend entirely on these commercial/scientific simulation tools (§4).
  • domain assumption Custom optical material catalogue (refractive indices, thermo-optical behavior over 100–293 K) is accurate.
    Used to optimize the camera designs (§2.1); errors would shift focus and image quality.
  • domain assumption Heritage from SCUBA2, MOONS, HARMONI, SPIRou, NIRPS transfers to YS mechanical/thermal design.
    Used to set cryostat architecture, cooling strategy and detector readout performance (§2.3, 3.1).
  • ad hoc to paper The 3×1 Zerodur grating mosaic misalignment study represents the baseline Invar 4×1 mosaic's tolerance behavior.
    The simulation in §3.2.1 uses a different mosaic geometry than the current baseline; the paper does not present an equivalent study for the 4×1 Invar design, yet uses it to argue misalignment effects are limited.

how reviews work

0 comments
Cite this review

Pith. "Pith review of ANDES, the high-resolution spectrograph for the ELT: design and performance analysis of the YJH spectrograph." pith.science (2026). https://pith.science/paper/ZSXER4FF

@misc{pith2026260722388,
  author       = {Pith},
  title        = {Pith review of: ANDES, the high-resolution spectrograph for the ELT: design and performance analysis of the YJH spectrograph},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZSXER4FF}},
  note         = {Machine review of arXiv:2607.22388}
}
abstract

The ArmazoNes high Dispersion Echelle Spectrograph (ANDES) is a powerful second-generation high-resolution spectroscopic instrument for the Extremely Large Telescope (ELT). The UBV, RIZ, and YJH modules comprise fibre-fed spectrographs of the ANDES baseline design and will offer continuous wavelength coverage of 0.35-1.8 $\mu$m, with the addition of a K-band channel providing coverage up to 2.4 $\mu$m. Coupled with a spectral resolution of $\sim$100,000, ANDES must deliver the required wavelength calibration stability of 1 m/s over 24 hours, with a goal of 0.02 m/s across 10 years. These requirements establish the framework for the infrared module of ANDES, the YJH Spectrograph, leading to what will likely be the largest cryogenic, ultra-stable, high-resolution spectrograph ever built, and will offer the unique ability to observe in both seeing- and diffraction-limited modes interchangeably. We present the current design and performance analysis of the ANDES YJH Spectrograph, outlining the engineering challenges encountered alongside the corresponding strategies adopted to navigate them. In particular, we detail the technology development of the primary dispersing element, an echelle grating mosaic that will span over a metre in length.

Figures

Figures reproduced from arXiv: 2607.22388 by the authors.

Figure 1
Figure 1. The parameter space of wavelength coverage versus spectral resolution that is occupied by a number of ELT [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Current location of the YJH Spectrograph, shown in blue, in the ELT Coud´e room, with six electronics cabinets [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Opto-mechanical model of the V36 ANDES YJH spectrograph. The Y-band beam path is indicated in blue, the [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figures from the paper (13 more)
Figure 4
Figure 4. Figure 4: Optical ray-trace diagrams of the Y-, J-, and H-band cameras. The material of each lens is specified and [PITH_FULL_IMAGE:figures/full_fig_p005_4.png]
Figure 5
Figure 5. Figure 5: YJH spectrograph vacuum vessel with its upper segment removed. Fibres and cabling are not shown here. [PITH_FULL_IMAGE:figures/full_fig_p006_5.png]
Figure 6
Figure 6. Figure 6: Example blackbody spectra with and without a cold slit selector. The dashed black line shows an example [PITH_FULL_IMAGE:figures/full_fig_p007_6.png]
Figure 7
Figure 7. Figure 7: Mechanical layout of the slit selector mechanism assembly. [PITH_FULL_IMAGE:figures/full_fig_p008_7.png]
Figure 8
Figure 8. Figure 8: Beam footprint diagram at the echelle grating, for the H-band V36 design. The size of the grating shown is [PITH_FULL_IMAGE:figures/full_fig_p009_8.png]
Figure 9
Figure 9. Figure 9: Illustrations of the different grating mosaic configurations. The direction of the grooves is indicated using [PITH_FULL_IMAGE:figures/full_fig_p010_9.png]
Figure 10
Figure 10. Figure 10: Simulated spectral LSF for a 3 x 1 grating mosaic with random piston offsets assigned to each grating segment [PITH_FULL_IMAGE:figures/full_fig_p011_10.png]
Figure 11
Figure 11. Figure 11: The composition of the grating module and the local coordinate system for two designs currently being [PITH_FULL_IMAGE:figures/full_fig_p012_11.png]
Figure 12
Figure 12. Figure 12: Total YS throughput as a function of wavelength. The different bands of Y, J and H are shown in blue, green [PITH_FULL_IMAGE:figures/full_fig_p012_12.png]
Figure 13
Figure 13. Figure 13: Bubble plot of RMS spot radius in microns versus image position on the detector for the various wavebands [PITH_FULL_IMAGE:figures/full_fig_p013_13.png]
Figure 14
Figure 14. Figure 14: Interpolated maps of Sampling (left) and Resolving Power (right) measured in the E2E final product, for [PITH_FULL_IMAGE:figures/full_fig_p014_14.png]
Figure 15
Figure 15. Figure 15: Interpolated maps of Sampling (left) and Resolving Power (right) measured in the E2E final product, for [PITH_FULL_IMAGE:figures/full_fig_p014_15.png]
Figure 16
Figure 16. Figure 16: Interpolated maps of Sampling (left) and Resolving Power (right) measured in the E2E final product, for [PITH_FULL_IMAGE:figures/full_fig_p015_16.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

25 extracted references

  1. [1]

    Andes, the high resolution spectrograph for the elt: science goals, project overview, and future developments,

    Marconi, A., Abreu, M., Adibekyan, V., Alberti, V., Albrecht, S., Alcaniz, J., Aliverti, M., Prieto, C. A., Alvarado-Gomez, J., Alves, C., et al., “Andes, the high resolution spectrograph for the elt: science goals, project overview, and future developments,” in [Ground-Based and Airborne Instrumentation for Astronomy X],13096, 478–503, SPIE (2024)

    2024

  2. [2]

    Ground-breaking exoplanet science with the andes spectrograph at the elt,

    Palle, E., Biazzo, K., Bolmont, E., Molli` ere, P., Poppenhaeger, K., Birkby, J., Brogi, M., Chauvin, G., Chiavassa, A., Hoeijmakers, J., et al., “Ground-breaking exoplanet science with the andes spectrograph at the elt,”Experimental Astronomy59(3), 29 (2025)

    2025

  3. [3]

    The discovery space of elt-andes. stars and stellar populations,

    Roederer, I. U., Alvarado-G´ omez, J. D., Allende Prieto, C., Adibekyan, V., Aguado, D. S., Amado, P. J., Amazo-G´ omez, E. M., Baratella, M., Barnes, S. A., Bensby, T., et al., “The discovery space of elt-andes. stars and stellar populations,”Experimental Astronomy57(2), 17 (2024)

    2024

  4. [4]

    Galaxy formation and symbiotic evolution with the inter-galactic medium in the age of elt-andes,

    D’Odorico, V., Bolton, J. S., Christensen, L., De Cia, A., Zackrisson, E., Kordt, A., Izzo, L., Li, J., Maiolino, R., Marconi, A., et al., “Galaxy formation and symbiotic evolution with the inter-galactic medium in the age of elt-andes,”Experimental Astronomy58(3), 21 (2024)

    2024

  5. [5]

    Cosmology and fundamental physics with the elt-andes spectrograph,

    Martins, C. J., Cooke, R., Liske, J., Murphy, M., Noterdaeme, P., Schmidt, T., Alcaniz, J., Alves, C., Balashev, S., Cristiani, S., et al., “Cosmology and fundamental physics with the elt-andes spectrograph,” Experimental Astronomy57(1), 5 (2024)

    2024

  6. [6]

    First light of the gemini planet imager,

    Macintosh, B., Graham, J. R., Ingraham, P., Konopacky, Q., Marois, C., Perrin, M., Poyneer, L., Bauman, B., Barman, T., Burrows, A. S., et al., “First light of the gemini planet imager,”proceedings of the National Academy of Sciences111(35), 12661–12666 (2014)

    2014

  7. [9]

    Andes, the high-resolution spectrograph for the elt: opto-mechanical design of the cameras for the yjh spectrograph,

    Vall´ ee, P., Brousseau, D., Thibault, S., Baron, F., Doyon, R., Saint-Antoine, J., Artigau,´E., Cook, N. J., and Zanutta, A., “Andes, the high-resolution spectrograph for the elt: opto-mechanical design of the cameras for the yjh spectrograph,” in [Ground-based and Airborne Instrumentation for Astronomy X],13096, 1627– 1632, SPIE (2024)

    2024

  8. [10]

    The cryo-mechanical design of scuba-2: a wide-field imager for the james clerk maxwell telescope,

    Gostick, D., Montgomery, D., Wall, B., McGregor, H., Cliffe, M., Woodcraft, A., and Gannaway, F., “The cryo-mechanical design of scuba-2: a wide-field imager for the james clerk maxwell telescope,” in [Ground- based Instrumentation for Astronomy],5492, 1743–1754, SPIE (2004)

    2004

Show all 25 references
  1. [11]

    Moons: the multi-object optical and near-infrared spectrograph for the vlt,

    Cirasuolo, M., Afonso, J., Carollo, M., Flores, H., Maiolino, R., Oliva, E., Paltani, S., Vanzi, L., Evans, C., Abreu, M., et al., “Moons: the multi-object optical and near-infrared spectrograph for the vlt,” in [Ground-based and airborne instrumentation for astronomy V],9147,...

    2014

  2. [12]

    Harmoni at elt: the revitalised high-resolution near-infrared ifu for the eso elt,

    Dunlop, J., Neichel, B., Chittick, S., Costille, A., Le Mignant, D., Lithgow, C., de Lorenzo-C´ aceres, A., Swinback, M., Taylor, W., Tecza, M., et al., “Harmoni at elt: the revitalised high-resolution near-infrared ifu for the eso elt,” in [Ground-based and airborne instrumen...

    2026

  3. [13]

    Performance of moons cryostat and control system,

    Waring, C., Strachan, J., and Gonzalez, O., “Performance of moons cryostat and control system,” in [Ground-based and Airborne Instrumentation for Astronomy X],13096, 130962J, SPIE (2024)

    2024

  4. [14]

    Characterisation, performance and oper- ational aspects of the h4rg-15 near infrared detectors for the moons instrument,

    Ives, D., Alvarez, D., Bezawada, N., George, E., and Serra, B., “Characterisation, performance and oper- ational aspects of the h4rg-15 near infrared detectors for the moons instrument,” in [X-Ray, Optical, and Infrared Detectors for Astronomy IX],11454, 299–318, SPIE (2020)

    2020

  5. [15]

    A large mosaic echelle grating for espresso spectrograph,

    Lizon, J. L., Dekker, H., Manescau, A., Megevan, D., Pepe, F. A., and Riva, M., “A large mosaic echelle grating for espresso spectrograph,” in [Optical and Infrared Interferometry and Imaging VI],10701, 766– 775, SPIE (2018)

    2018

  6. [16]

    Harps: Eso’s coming planet searcher. chasing exoplanets with the la silla 3.6-m telescope,

    Pepe, F., Mayor, M., Rupprecht, G., Avila, G., Ballester, P., Beckers, J.-L., Benz, W., Bertaux, J.-L., Bouchy, F., Buzzoni, B., et al., “Harps: Eso’s coming planet searcher. chasing exoplanets with the la silla 3.6-m telescope,”Messenger110, 9–14 (2002)

    2002

  7. [17]

    The habitable-zone planet finder: A status update on the development of a stabilized fiber-fed near-infrared spectrograph for the for the hobby-eberly telescope,

    Mahadevan, S., Ramsey, L. W., Terrien, R., Halverson, S., Roy, A., Hearty, F., Levi, E., Stefansson, G. K., Robertson, P., Bender, C., et al., “The habitable-zone planet finder: A status update on the development of a stabilized fiber-fed near-infrared spectrograph for the for...

    2014

  8. [18]

    Highly sensitive, non-cryogenic nir high-resolution spectrograph, winered,

    Ikeda, Y., Kondo, S., Otsubo, S., Hamano, S., Yasui, C., Matsunaga, N., Sameshima, H., Yoshikawa, T., Fukue, K., Nakanishi, K., et al., “Highly sensitive, non-cryogenic nir high-resolution spectrograph, winered,” Publications of the Astronomical Society of the Pacific134(1031)...

    2022

  9. [19]

    Nirps back-end: design and performance,

    Thibault, S., Brousseau, D., Poulin-Girard, A.-S., Auger, H., Wildi, F., Doyon, R., Reshetov, V., Malo, L., Baron, F., Vall´ ee, P., et al., “Nirps back-end: design and performance,” in [Ground-based and Airborne Instrumentation for Astronomy IX],12184, 1652–1659, SPIE (2022)

    2022

  10. [20]

    Manufacturing of a highly efficient gold coated echelle grating for nir on a thick silicon substrate with small straylight and wavefront error,

    Sadlowski, S., Fl¨ ugel-Paul, T., Wildi, F., Wittig, M., Benkenstein, T., Nathanael, J., Trost, M., Munzert, P., Scheler, M., and Zeitner, U., “Manufacturing of a highly efficient gold coated echelle grating for nir on a thick silicon substrate with small straylight and wavefr...

    2022

  11. [21]

    Nirps joining harps at eso 3.6 m: on-sky performance and science objectives,

    Bouchy, F., Doyon, R., Pepe, F., Melo, C., Artigau, ´E., Malo, L., Wildi, F., Baron, F., Delfosse, X., De Medeiros, J. R., et al., “Nirps joining harps at eso 3.6 m: on-sky performance and science objectives,” Astronomy & Astrophysics700, A10 (2025)

    2025

  12. [22]

    The spectrometer optics of giano- tng,

    Gennari, S., Mochi, I., Donati, S., Oliva, E., Origlia, L., and Sandri, P., “The spectrometer optics of giano- tng,” in [Ground-based and Airborne Instrumentation for Astronomy],6269, 1288–1297, SPIE (2006)

    2006

  13. [23]

    Spirou: Nir velocimetry and spectropolarimetry at the cfht,

    Donati, J., Kouach, D., Moutou, C., Doyon, R., Delfosse, X., Artigau, E., Baratchart, S., Lacombe, M., Barrick, G., H´ ebrard, G., et al., “Spirou: Nir velocimetry and spectropolarimetry at the cfht,”Monthly Notices of the Royal Astronomical Society498(4), 5684–5703 (2020)

    2020

  14. [24]

    Design and development of nirspec: a near-infrared echelle spectrograph for the keck ii telescope,

    McLean, I. S., Becklin, E. E., Bendiksen, O., Brims, G., Canfield, J., Figer, D. F., Graham, J. R., Hare, J., Lacayanga, F., Larkin, J. E., et al., “Design and development of nirspec: a near-infrared echelle spectrograph for the keck ii telescope,” in [Infrared astronomical in...

    1998

  15. [25]

    The advanced super invar alloys with zero thermal expansion for space telescopes,

    Ona, K., Sakaguchi, N., Ohno, H., and Utsunomiya, S., “The advanced super invar alloys with zero thermal expansion for space telescopes,”Transactions of the Japan Society for Aeronautical and Space Sciences, Aerospace Technology Japan18(3), 32–37 (2020)

    2020

  16. [26]

    Sca test report h4rg-21947 roman space telescope,

    Miko, L., “Sca test report h4rg-21947 roman space telescope,” tech. rep., Goddard Space Flight Center (2021)

    2021

  17. [27]

    Echelle++, a fast generic spectrum simulator,

    St¨ urmer, J., Seifahrt, A., Robertson, Z., Schwab, C., and Bean, J. L., “Echelle++, a fast generic spectrum simulator,”Publications of the Astronomical Society of the Pacific131(996), 024502 (2019)

    2019

Pith tools

Reviewed August 1, 2026 · model on record in the stance chip above.