Pith. sign in

REVIEW 2 major objections 5 minor 47 references

An empirical optical methane linelist extracted from Titan enables the first high-resolution cross-correlation detections of CH4 in visible planetary spectra.

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 →

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

T0 review · grok-4.5

2026-07-14 13:11 UTC pith:CJZHLIAH

load-bearing objection Usable empirical optical CH4 linelist plus first optical HRCCS detections on Titan and Jupiter; the independent Jupiter Doppler match is the real validation. the 2 major comments →

arxiv 2607.10250 v1 pith:CJZHLIAH submitted 2026-07-11 astro-ph.EP astro-ph.IMphysics.ao-phphysics.chem-ph

High Resolution Optical Methane Linelist from observations of Titan for Cross-Correlation studies

Rafael Rian\c{c}o-Silva , Pedro Machado , Clara Sousa Silva , Sergey Yurchenko , Giovanna Tinetti This is my paper
classification astro-ph.EP astro-ph.IMphysics.ao-phphysics.chem-ph
keywords exoplanet atmospheresmethaneoptical spectroscopyhigh-resolution cross-correlationTitanspectral linelistsVLT-ESPRESSOplanetary atmospheres
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.

High-resolution optical spectroscopy of exoplanets has been blocked for methane because neither theory nor laboratory work has delivered usable linelists across most of the visible range. The authors treat Titan as a natural cold cell: its atmosphere is dominated by CH4 absorption, so a high-resolution VLT-ESPRESSO spectrum of Titan can be cleaned of solar and telluric lines to yield an empirical list of thousands of CH4 features. That list, called RRS-2026, is turned into a cross-correlation template and recovers strong, velocity-consistent detections of methane in both Titan and Jupiter optical spectra—the first such detections ever made with a visible CH4 template. The result supplies the missing tool for searching for methane around cooler, smaller exoplanets with present and future optical spectrographs.

Core claim

By isolating absorption lines that appear only in Titan after solar and telluric masking, the authors construct an empirical low-temperature optical CH4 linelist (RRS-2026) containing thousands of previously unidentified features at R ~ 190 000. The same linelist, used as a cross-correlation template, produces the first high-resolution cross-correlation spectroscopy detections of methane in optical spectra of planetary atmospheres, recovering clear signals on both Titan and Jupiter whose Doppler centroids match the known radial-velocity and rotational shifts.

What carries the argument

The RRS-2026 linelist: a conservative, observation-based catalogue of CH4 line positions and relative depths extracted from VLT-ESPRESSO Titan spectra after successive rejection of solar and telluric contaminants, then converted into a binary spectral mask for high-resolution cross-correlation.

Load-bearing premise

That virtually every residual absorption feature left in Titan after solar and telluric lines are removed is pure methane, and that the cold relative intensities measured there remain useful for cross-correlation on warmer or chemically different atmospheres.

What would settle it

A high-resolution optical spectrum of a CH4-free atmosphere (or a laboratory CH4 spectrum at comparable temperature and resolution) that still produces a strong cross-correlation peak with the RRS-2026 template, or a clear mismatch between the template and an independent high-resolution CH4 measurement in the same wavelength window.

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

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

2 major / 5 minor

Summary. The paper extracts an empirical high-resolution (R ≈ 190 000) optical CH4 linelist (RRS-2026) from VLT-ESPRESSO UHR spectra of Titan by detecting lines above a 5σ depth threshold and rejecting solar and telluric contaminants via FWHM matching against a Kurucz solar atlas and a contemporaneous A0V telluric calibrator star, with a dual-epoch cross-check against a 2021 Titan dataset. Two versions are produced (5806 lines after 2-step rejection; 4997 after the more conservative 3-step path). These are converted into the first optical HRCCS templates for CH4 and applied to the Titan 2024 spectrum (recovering 32–34σ peaks at ~0 km s−1) and, independently, to a 2019 Jupiter ESPRESSO spectrum (recovering 25–27σ peaks at −1.4 ± 1.0 km s−1, consistent with the expected orbital-plus-rotational Doppler shift of −1.75 km s−1). Band envelopes match Karkoschka & Tomasko (2010) low-resolution cross-sections; partial line matches exist with Campargue et al. (2023); and a comparison with the SS-2025 Titan feature list is presented. The work claims the first optical HRCCS detections of CH4 in planetary atmospheres and supplies the linelist for future exoplanet searches.

Significance. The result fills a long-standing spectroscopic gap: no high-resolution optical CH4 linelist suitable for HRCCS previously existed, limiting optical searches with ESPRESSO, RISTRETTO and ELT-ANDES. The independent Jupiter validation at the predicted non-zero velocity is a strong, falsifiable test that residual solar/telluric contamination cannot explain the CCF signal and that the empirical relative intensities transfer to a chemically and thermally distinct (H2/He-broadened) atmosphere. Public release of the full linelist plus intermediate line lists supports reproducibility. The contribution is practical and timely for cold exoplanet and Solar-System atmospheric characterization.

major comments (2)
  1. §3.1 (final paragraphs) and §4.3: the central claim that residual Titan features after solar/telluric FWHM masking are overwhelmingly CH4 rests on the absence of other known optical absorbers and on abundance arguments (C2H6 ≲ 20 ppm). While the independent Jupiter CCF at the correct Doppler shift (Fig. 4b) already rules out solar/telluric residuals as the signal source, the manuscript should add a short quantitative bound (even an order-of-magnitude estimate) on possible residual contamination by unlisted minor hydrocarbons/nitriles, or state explicitly that such a bound cannot yet be placed because those species also lack optical linelists. This is the only load-bearing purity assumption that is not fully closed by the Jupiter test.
  2. §3.2 and Fig. 4 caption: reported CCF significances for the Titan 2-step template differ between the main text (32.6σ) and the figure caption (32.2σ). The same section quotes HWHM velocity uncertainties that should be cross-checked for consistency with the plotted peaks. These numbers underpin the “first optical HRCCS detection” claim and must be reconciled before publication.
minor comments (5)
  1. §3.1 Path descriptions and Table 1: the machine-readable supplementary linelist is promised but the exact column definitions (especially the “In RRS-2026 (3-steps)?” flag) should be stated once in the main text for users who download only the table.
  2. Fig. 5 and Fig. 7: the dual y-axes (relative line depth vs. absorption coefficient) are useful but the scaling between the two panels is not stated; a brief note on how the empirical depths were normalized for visual comparison would help.
  3. §4.2: the comparison with Campargue et al. (2023) is limited to two red-end bands; a short statement of the fraction of strong lines that coincide within the ESPRESSO FWHM would strengthen the external validation.
  4. Throughout: a few typographical inconsistencies appear (e.g., “RRS-2025” vs. “RRS-2026” in one figure legend label, “32.2σ” vs. “32.6σ”, occasional missing spaces around units). A final proof-read pass is warranted.
  5. §5: the recommendation to use RRS-2026 (2-step) for T < 200 K exoplanets is clear; adding one sentence on the expected degradation of CCF SNR if the template is applied to warmer atmospheres (without re-deriving intensities) would help non-specialist users.

Circularity Check

0 steps flagged

No significant circularity: empirical linelist extracted by solar/telluric masking is validated on independent Jupiter data at the expected non-zero Doppler velocity.

full rationale

The paper constructs RRS-2026 by detecting absorption lines on Titan 2024 (cross-checked against Titan 2021), then discarding any whose wavelengths fall inside the measured FWHM of Kurucz solar lines or Star 2024 telluric lines (§3.1 Paths 1–2). The resulting positions and relative depths form a mask that is cross-correlated with the same Titan spectrum (sanity check, peak at ~0 km s⁻¹) and, crucially, with an entirely independent Jupiter 2019 ESPRESSO spectrum. The Jupiter CCF peaks at (−1.39 ± 0.98) km s⁻¹, matching the known barycentric + rotational Doppler shift (−1.75 km s⁻¹) of the fibre placement. Because the validation target, its chemistry (H₂/He vs N₂), temperature regime, and systemic velocity all differ from the extraction data, the detection cannot be a self-correlation artefact. Minor self-citations (Rianço-Silva et al. 2024 method, 2026 observations) supply procedural context but are not load-bearing for the linelist or the first-optical-HRCCS claim. No fitted parameter is renamed a prediction, no uniqueness theorem is imported, and no ansatz is smuggled via citation. The residual risk that minor hydrocarbons contribute a few lines is an empirical assumption, not a circular reduction.

Axiom & Free-Parameter Ledger

1 free parameters · 3 axioms · 0 invented entities

The central claim rests on standard observational astronomy practices plus two domain assumptions about Titan chemistry and the transferability of a low-T empirical list. No free parameters are fitted to produce the claimed detections; the only tunable threshold is the conventional 5σ line-depth cut. No new physical entities are invented.

free parameters (1)
  • line-depth detection threshold = 5σ
    Lines retained only if depth exceeds 5 times the local spectral flux error; conventional but still a discrete choice that controls the final line count (5806 vs fewer).
axioms (3)
  • domain assumption CH4 is the sole molecular species in Titan’s atmosphere that produces significant absorption bands between ~500–800 nm at the observed abundances.
    Stated in §3.1 and used to assign all residual Titan features to CH4; supported by low-resolution literature but not proven at R=190000 for every weak line.
  • domain assumption Relative line depths measured under Titan’s temperature and N2-broadening conditions remain sufficiently similar for cross-correlation on Jupiter (H2/He, different T/P).
    Implicit in the successful Jupiter CCF; authors caution that the list is low-T and empirical, yet still claim applicability.
  • domain assumption Solar and telluric lines are adequately removed by FWHM coincidence with the Kurucz atlas and the Star 2024 calibrator.
    Core of the two- and three-step filtering paths in §3.1; residual contamination would produce spurious CCF power.

pith-pipeline@v1.1.0-grok45 · 24853 in / 2768 out tokens · 33409 ms · 2026-07-14T13:11:05.512612+00:00 · methodology

0 comments
read the original abstract

Exoplanet atmosphere characterization heavily relies on molecular spectroscopic data. Despite efforts to obtain comprehensive spectral libraries for the chemical characterization of exoplanet atmospheres, large gaps remain, particularly for larger molecules and higher frequencies at high spectral resolution. One key example is the methane (CH4) optical spectrum. CH4, the simplest hydrocarbon, is a crucial species for exoplanet atmosphere characterization and a possible biosignature. However, until now, high-resolution linelists at optical wavelengths for CH4 have been very challenging to obtain either experimentally or computationally, leaving the high resolution spectrum of CH4 uncharacterised across most of the visible spectrum. This restricts exploration of CH4 absorption in the optical regime, as upcoming instruments such as ELT-ANDES and VLT-RISTRETTO will start probing the atmospheres of ever smaller exoplanets in optical wavelengths. To address this spectroscopic data limitation, we observed Titan's optical spectrum, dominated by CH4 absorption, at the highest spectral resolution to date with VLT-ESPRESSO. From it, we produced an empirical, low-temperature high-resolution (R ~ 190000) linelist of CH4 in optical wavelengths which we present here, with thousands of previously unidentified lines. We employ this CH4 linelist (RRS-2026) to build a template suitable for high resolution cross-correlation spectroscopy (HRCCS) studies, a first for CH4 in optical wavelengths. With this new linelist, we performed the first HRCCS detection of CH4 in the atmospheres of Titan and Jupiter using optical high resolution spectra. This work sets the stage for the search for CH4 in exoplanet atmospheres through HRCCS with current and future ground-based high-resolution optical spectrographs, showcasing how Solar System observations provide useful products for exoplanet research.

Figures

Figures reproduced from arXiv: 2607.10250 by Clara Sousa Silva, Giovanna Tinetti, Pedro Machado, Rafael Rian\c{c}o-Silva, Sergey Yurchenko.

Figure 1
Figure 1. Figure 1: Line detections above 5σ of spectral noise for the spectra: a) Titan 2024, b) Titan 2021, c) Star 2024 (corresponding to the telluric calibrator observation of star HD 218639) and d) Kurucz Solar [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Two examples of the spectral line characterization, comparing Titan 2024 (black), Titan 2021 (green), Solar (red), and Stellar telluric calibration (blue) spectra, and showcasing spectral line categorization as “Titan”, “Solar” or “Telluric” in origin. Titan lines are split between the ones which are identified in both Titan 2021 and Titan 2024 spectra (green circles) and the ones which are only identified… view at source ↗
Figure 3
Figure 3. Figure 3: Line detections across the distinct stages of the line characterization method: a) “Non Solar Titan 2024 lines”, resulting from step 1; b) “RRS-2026 (2 steps)” resulting from step 2 of Path 1; c) “Non Solar Titan 2024 & 2021”, resulting from step 2 of Path 2 and d) “RRS-2026 (3 steps)” resulting from step 3 of Path 2. The two sets of RRS-2026 linelists shown in plots b) and d) are also shown, combined, in … view at source ↗
Figure 4
Figure 4. Figure 4: Cross-Correlation Functions (CCFs) of VLT-ESPRESSO UHR Spectra of Titan (a) and Jupiter (b), using the CCF templates obtained with the CH4 visible RRS-2026 linelists retrieved in this work. These CCFs yielded detection strengths of CH4 for the Titan VLT-ESPRESSO spectrum of 32.2σ for the RRS-2026 (2 steps) linelist and 34.1σ for the RRS-2026 (3 steps) linelist. Titan CCFs peak at radial velocities of (0.28… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison between this work’s RRS-2026 visible CH4 linelists: the more complete RRS-2026 (2 steps), also shown in figure 3b (here in black), which contains the entirety of the more conservative RRS-2026 (3 steps), also shown in figure 3d (here in green), and E. Karkoschka & M. Tomasko (2010) visible CH4 absorption cross-section, in blue, with CH4 band assignment following L.P.Giver (1978). Up to now, the … view at source ↗
Figure 6
Figure 6. Figure 6: Comparison between the RRS-2026 CH4 (2-step) linelist and the CH4 linelists described in A. Campargue et al. (2023), overlapping only in 2 CH4 visible absorption bands above 715 nm, shown in figues a) and b). Figure c) shows a zoom into the central, densest region of the 727nm CH4 band, allowing a comparison between the finer structure of both linelists. method to weaker features in these probed spectral r… view at source ↗
Figure 7
Figure 7. Figure 7: Comparison between this work’s CH4 visible high resolution linelist, RRS-2026 (2-steps, in black, and RRS-2026 (3-steps), in green, with S. Sithajan et al. (2025) Titan spectral features, associated to CH4 absorption features (SS-2025). In blue we identify the SS-2025 features that match in wavelength spectral lines in RRS-2026 (2 step, the most comprehensive line set), whereas in red are shown the spectra… view at source ↗
Figure 8
Figure 8. Figure 8: Cross-Correlation Functions (CCFs) of VLT-ESPRESSO UHR Spectra of Titan (a) and Jupiter (b), using the CCF templates obtained with the CH4 visible SS-2025 linelists retrieved in S. Sithajan et al. (2025) (complete or masked for contaminating sources). These CCFs yielded detection strengths of CH4 for the Titan VLT-ESPRESSO spectrum of 54.1σ for the SS-2025 (complete) linelist and 27.3σ for the SS-2025 (mas… view at source ↗
Figure 9
Figure 9. Figure 9: “Non Solar Titan 2021 lines”, resulting from step 1, equivalent to Figure 3a for Titan 2021 lines. Hayden-Smith, W., Conner, C., & Baines, K. 1990, Icarus, 85, 58, doi: doi:10.1016/0019-1035(90)90103-G Hayes, A., Lorenz, R., & Lunine, J. 2018, Nature Geoscience, 11, 306–313, doi: https://doi.org/10.1038/s41561-018-0103-y Horizons, J. P. L. C. S. D. 2025 Available online: https://ssd.jpl.nasa.gov/horizons/ … view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

47 extracted references · 15 canonical work pages · 1 internal anchor

  1. [1]

    2026, JQSRT, 349, doi: https://doi.org/10.1016/j.jqsrt.2025.109736

    Bertin, T., Gordon, I., Hargreaves, R., et al. 2026, JQSRT, 349, doi: https://doi.org/10.1016/j.jqsrt.2025.109736

    doi:10.1016/j.jqsrt.2025.109736 2026

  2. [2]

    2018, doi: https://doi.org/10.48550/arXiv.1806.04617

    Birkby, J. 2018, doi: https://doi.org/10.48550/arXiv.1806.04617

    Pith/arXiv arXiv doi:10.48550/arxiv.1806.04617 2018

  3. [3]

    2019, AJ, 157, 114, doi: 10.3847/1538-3881/aaffd3

    Brogi, M., & Line, M. 2019, AJ, 157, 114, doi: 10.3847/1538-3881/aaffd3

    doi:10.3847/1538-3881/aaffd3 2019

  4. [4]

    2023, Physical Chemistry Chemical Physics, 25, 32778, doi: https://doi.org/10.1039/D3CP02385K

    Campargue, A., Karlovets, E., Vasilchenko, S., & Turbet, M. 2023, Physical Chemistry Chemical Physics, 25, 32778, doi: https://doi.org/10.1039/D3CP02385K

    work page doi:10.1039/d3cp02385k 2023

  5. [5]

    2024, RAS Techniques and Instruments, 3, 636–690, doi: https://doi.org/10.1093/rasti/rzae039

    Chubb, K., Robert, S., Sousa-Silva, C., et al. 2024, RAS Techniques and Instruments, 3, 636–690, doi: https://doi.org/10.1093/rasti/rzae039

    work page doi:10.1093/rasti/rzae039 2024

  6. [6]

    2003, Icarus, 161, doi: doi:10.1016/S0019-1035(02)00028-3

    Coustenis, A., Salama, A., Schulz, B., et al. 2003, Icarus, 161, doi: doi:10.1016/S0019-1035(02)00028-3

    doi:10.1016/s0019-1035(02)00028-3 2003

  7. [7]

    2015, C.R

    Encrenaz, T. 2015, C.R. Geoscience, 347, 3, doi: 10.1016/j.crte.2015.02.002/

    work page doi:10.1016/j.crte.2015.02.002/ 2015

  8. [8]

    Esparza-Borges, E., L´ opez-Morales, M., Redai, J. I. A., et al. 2023, ApJL, 955, L19, doi: 10.3847/2041-8213/acf27b

    doi:10.3847/2041-8213/acf27b 2023

  9. [9]

    2020, The Astronomical Journal, 160, 288, doi: 10.3847/1538-3881/abc5bd

    Fortney, J., Visscher, C., Marley, M., et al. 2020, The Astronomical Journal, 160, 288, doi: 10.3847/1538-3881/abc5bd

    doi:10.3847/1538-3881/abc5bd 2020

  10. [10]

    2020, MNRAS, 495, 224–237, doi: doi:10.1093/mnras/staa981

    Gandhi, S., Brogi, M., Yurchenko, S., et al. 2020, MNRAS, 495, 224–237, doi: doi:10.1093/mnras/staa981

    doi:10.1093/mnras/staa981 2020

  11. [11]

    2021, Nature, 592, 205–208, doi: https://doi.org/10.1038/s41586-021-03381-x

    Giacobbe, P., Brogi, M., Gandhi, S., & et al. 2021, Nature, 592, 205–208, doi: https://doi.org/10.1038/s41586-021-03381-x

    doi:10.1038/s41586-021-03381-x 2021

  12. [12]

    2026a, Journal of Quantitative Spectroscopy and Radiative Transfer, 109807, doi: https://doi.org/10.1016/j.jqsrt.2026.109807

    Gordon, I., Rothman, L., Hargreaves, R., et al. 2026a, Journal of Quantitative Spectroscopy and Radiative Transfer, 109807, doi: https://doi.org/10.1016/j.jqsrt.2026.109807

    doi:10.1016/j.jqsrt.2026.109807 2026

  13. [13]

    2020, The Astrophysical Journal Supplement Series, 247, doi: https://doi.org/10.3847/1538-4365/ab7a1a 18 5000 5500 6000 6500 7000 7500 8000

    Hargreaves, R., Gordon, I., Rey, M., et al. 2020, The Astrophysical Journal Supplement Series, 247, doi: https://doi.org/10.3847/1538-4365/ab7a1a 18 5000 5500 6000 6500 7000 7500 8000

    doi:10.3847/1538-4365/ab7a1a 2020

  14. [14]

    Non Solar Titan 2021 lines

    Wavelength, Angstrom 10 2 10 1 100 Line Depth Non Solar Titan 2021: 6092 lines Figure 9.“Non Solar Titan 2021 lines”, resulting from step 1, equivalent to Figure 3a for Titan 2021 lines

    2021

  15. [15]

    1990, Icarus, 85, 58, doi: doi:10.1016/0019-1035(90)90103-G

    Hayden-Smith, W., Conner, C., & Baines, K. 1990, Icarus, 85, 58, doi: doi:10.1016/0019-1035(90)90103-G

    work page doi:10.1016/0019-1035(90)90103-g 1990

  16. [16]

    2018, Nature Geoscience, 11, 306–313, doi: https://doi.org/10.1038/s41561-018-0103-y

    Hayes, A., Lorenz, R., & Lunine, J. 2018, Nature Geoscience, 11, 306–313, doi: https://doi.org/10.1038/s41561-018-0103-y

    work page doi:10.1038/s41561-018-0103-y 2018

  17. [17]

    Horizons, J. P. L. C. S. D. 2025 Available online: https://ssd.jpl.nasa.gov/horizons/ (accessed on 16 July 2025)

    2025

  18. [18]

    2019, Icarus, 321, 572–582, doi: https://doi.org/10.1016/j.icarus.2018.12.008

    Irwin, P., Bowles, N., Braude, A., et al. 2019, Icarus, 321, 572–582, doi: https://doi.org/10.1016/j.icarus.2018.12.008

    doi:10.1016/j.icarus.2018.12.008 2019

  19. [19]

    1994, Icarus, 111, 174, doi: https://doi.org/10.1006/icar.1994.1139

    Karkoschka, E. 1994, Icarus, 111, 174, doi: https://doi.org/10.1006/icar.1994.1139

    doi:10.1006/icar.1994.1139 1994

  20. [20]

    1998, Icarus, 133, 134–146, doi: https://doi.org/10.1006/icar.1998.5913

    Karkoschka, E. 1998, Icarus, 133, 134–146, doi: https://doi.org/10.1006/icar.1998.5913

    doi:10.1006/icar.1998.5913 1998

  21. [21]

    2010, Icarus, 205, 674–694, doi: doi:10.1016/j.icarus.2009.07.044

    Karkoschka, E., & Tomasko, M. 2010, Icarus, 205, 674–694, doi: doi:10.1016/j.icarus.2009.07.044

    work page doi:10.1016/j.icarus.2009.07.044 2010

  22. [22]

    2024, JQSRT, 316, 108897, doi: https://doi.org/10.1016/j.jqsrt.2024.108897

    Kefala, K., Boudon, V., Yurchenko, S., & Tennyson, J. 2024, JQSRT, 316, 108897, doi: https://doi.org/10.1016/j.jqsrt.2024.108897

    work page doi:10.1016/j.jqsrt.2024.108897 2024

  23. [23]

    2023, AA, 669, A113, doi: https://doi.org/10.1051/0004-6361/202142969

    Kitzmann, D., Hoeijmakers, H., Grimm, S., et al. 2023, AA, 669, A113, doi: https://doi.org/10.1051/0004-6361/202142969

    doi:10.1051/0004-6361/202142969 2023

  24. [24]

    High Resolution Irradiance Spectrum from 300 to 1000 nm

    Kurucz, R. 2006, published in ArXiv, 0, 3, doi: https://doi.org/10.48550/arXiv.astro-ph/0605029

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0605029 2006

  25. [25]

    1999, Icarus, 142, 391–401, doi: https://doi.org/10.1006/icar.1999.6225

    Lorenz, R., Lemmon, M., Smith, P., & Lockwood, G. 1999, Icarus, 142, 391–401, doi: https://doi.org/10.1006/icar.1999.6225

    work page doi:10.1006/icar.1999.6225 1999

  26. [26]

    2022, Proceedings of the SPIE, 12184, doi: 10.1117/12.2627923 L.P.Giver

    Lovis, C., Blind, N., Chazelas, B., et al. 2022, Proceedings of the SPIE, 12184, doi: 10.1117/12.2627923 L.P.Giver. 1978, Journal of Quantitative Spectroscopy and Radiative Transfer, 19, 311, doi: https://doi.org/10.1016/0022-4073(78)90064-X

    doi:10.1117/12.2627923 2022

  27. [27]

    2008, Nature Geoscience, 1, 159–164, doi: https://doi.org/10.1038/ngeo125

    Lunine, J., & Atreya, S. 2008, Nature Geoscience, 1, 159–164, doi: https://doi.org/10.1038/ngeo125

    work page doi:10.1038/ngeo125 2008

  28. [28]

    2023, Universe, 9, 491, doi: https://doi.org/10.3390/universe9120491

    Machado, P., Silva, J., Brasil, F., et al. 2023, Universe, 9, 491, doi: https://doi.org/10.3390/universe9120491

    doi:10.3390/universe9120491 2023

  29. [29]

    2025, PNAS, 122, 39, doi: https://doi.org/10.1073/pnas.2416194122

    Cooke, G. 2025, PNAS, 122, 39, doi: https://doi.org/10.1073/pnas.2416194122

    doi:10.1073/pnas.2416194122 2025

  30. [30]

    2016, Orig Life Evol Biosph, 46, 487–498, doi: https://doi.org/10.1007/s11084-016-9493-2

    Martins, J., Santos, N., Figueira, P., & Melo, C. 2016, Orig Life Evol Biosph, 46, 487–498, doi: https://doi.org/10.1007/s11084-016-9493-2

    work page doi:10.1007/s11084-016-9493-2 2016

  31. [31]

    2001, Planetary and Space Science, 49, 79, doi: https://doi.org/10.1016/S0032-0633(00)00051-9

    McKay, C., Coustenis, A., Samuelson, R., et al. 2001, Planetary and Space Science, 49, 79, doi: https://doi.org/10.1016/S0032-0633(00)00051-9

    work page doi:10.1016/s0032-0633(00)00051-9 2001

  32. [32]

    1996, Astrophysical Journal v

    Neale, L., Miller, S., & Tennyson, J. 1996, Astrophysical Journal v. 464, p. 516, 464, 516

    1996

  33. [33]

    2025, Experimental Astronomy, 59, 29, doi: https://doi.org/10.1007/s10686-025-10000-4 19

    Palle, E., Biazzo, K., Bolmont, E., et al. 2025, Experimental Astronomy, 59, 29, doi: https://doi.org/10.1007/s10686-025-10000-4 19

    doi:10.1007/s10686-025-10000-4 2025

  34. [34]

    2014, Astron

    Pepe, F., Molaro, P., Cristiani, S., et al. 2014, Astron. Nachr, 335, 10, doi: https://doi.org/10.1002/asna.201312004

    doi:10.1002/asna.201312004 2014

  35. [35]

    2021, AA, 645, A96, doi: https://doi.org/10.1051/0004-6361/202038306 Rian¸ co-Silva, R., Machado, P., Martins, Z., et al

    Pepe, F., Cristiani, S., Rebolo, R., et al. 2021, AA, 645, A96, doi: https://doi.org/10.1051/0004-6361/202038306 Rian¸ co-Silva, R., Machado, P., Martins, Z., et al. 2024, Planet. Space Sci., 240, p. 105836, doi: https://doi.org/10.1016/j.pss.2023.105836 Rian¸ co-Silva, R., Machado, P., Rannou, P., et al. 2026, MNRAS, stag447, doi: https://doi.org/10.1093...

    doi:10.1051/0004-6361/202038306 2021

  36. [36]

    Rothman, L., Gordon, I., Barber, R., et al. 2010, J. Quant. Spectrosc. Radiat. Transfer, 111, 2139, doi: https://doi.org/10.1016/j.jqsrt.2010.05.001

    doi:10.1016/j.jqsrt.2010.05.001 2010

  37. [37]

    2016, AA, 585, A113, doi: https://doi.org/10.1051/0004-6361/201322749

    Rudolf, N., G¨ unther, H., Schneider, P., & Schmitt, J. 2016, AA, 585, A113, doi: https://doi.org/10.1051/0004-6361/201322749

    work page doi:10.1051/0004-6361/201322749 2016

  38. [38]

    1964, Analytical Chemistry, 36, 8, doi: https://doi.org/10.1021/ac60214a047

    Savitzky, A., & Golay, M. 1964, Analytical Chemistry, 36, 8, doi: https://doi.org/10.1021/ac60214a047

    doi:10.1021/ac60214a047 1964

  39. [39]

    2025, The Astronomical Journal, 170, 315, doi: 10.3847/1538-3881/ae0e1f

    Meethong, S. 2025, The Astronomical Journal, 170, 315, doi: 10.3847/1538-3881/ae0e1f

    work page doi:10.3847/1538-3881/ae0e1f 2025

  40. [40]

    2025, ARAA, 63, 83, doi: https: //doi.org/10.1146/annurev-astro-052622-031342

    Snellen, I. 2025, ARAA, 63, 83, doi: https: //doi.org/10.1146/annurev-astro-052622-031342

    doi:10.1146/annurev-astro-052622-031342 2025

  41. [41]

    2010, Nature, 465, 1049–1051, doi: https://doi.org/10.1038/nature09111

    Snellen, I., de Kok, R., de Mooij, E., & Albrecht, S. 2010, Nature, 465, 1049–1051, doi: https://doi.org/10.1038/nature09111

    doi:10.1038/nature09111 2010

  42. [42]

    Yurchenko, S. N. 2015, Monthly Notices of the Royal Astronomical Society, 446, 2337

    2015

  43. [43]

    2012, MNRAS, 425, 21, doi: https://doi.org/10.1111/j.1365-2966.2012.21440.x

    Tennyson, J., & Yurchenko, S. 2012, MNRAS, 425, 21, doi: https://doi.org/10.1111/j.1365-2966.2012.21440.x

    doi:10.1111/j.1365-2966.2012.21440.x 2012

  44. [44]

    N., Al-Refaie, A

    Tennyson, J., Yurchenko, S. N., Al-Refaie, A. F., et al. 2016, Journal of Molecular Spectroscopy, 327, 73

    2016

  45. [45]

    2022, PNAS, 119, 14, doi: https://doi.org/10.1073/pnas.21179331191 V.Boudon, Champion, J., Gabard, T., et al

    Thompson, M., Krissansen-Totton, J., Wogan, N., Telus, M., & Fortney, J. 2022, PNAS, 119, 14, doi: https://doi.org/10.1073/pnas.21179331191 V.Boudon, Champion, J., Gabard, T., et al. 2009, EPN, 40, 17, doi: DOI:10.1051/epn/2009601

    work page doi:10.1073/pnas.21179331191 2022

  46. [46]

    2024, MNRAS, 528, 3719–3729, doi: https://doi.org/10.1093/mnras/stae148

    Yurchenko, S., Owens, A., Kefala, K., & Tennyson, J. 2024, MNRAS, 528, 3719–3729, doi: https://doi.org/10.1093/mnras/stae148

    doi:10.1093/mnras/stae148 2024

  47. [47]

    2025, Nature Reviews Physics, 7, 645–659, doi: 10.1038/s42254-025-00839-z

    Yurchenko, S., Tennyson, J., & Brogi, M. 2025, Nature Reviews Physics, 7, 645–659, doi: 10.1038/s42254-025-00839-z

    doi:10.1038/s42254-025-00839-z 2025