Pith. sign in

REVIEW 3 major objections 5 minor 193 references

Instrumentation prospects for rocky exoplanet atmospheres studies with high resolution spectroscopy

T0 review · 3 major / 5 minor · reviewed 2026-08-16 · deepseek-v4-flash

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

Pith's one-line read This paper argues that pushing ground-based spectrographs from R=100,000 to R=300,000 would allow astronomers to detect molecular oxygen in rocky exoplanet atmospheres with up to four times shorter exposure time in hazy, cloudy scenarios.

desk verdict New ETC numbers for O2 at R=300k/500k under haze extend prior work, but the headline 4x gain rests on a crude clipping model and should not be used as a precise design driver. read the letter →

arxiv 2505.01102 v1 pith:OFA4D65H submitted 2025-05-02 astro-ph.EP astro-ph.IM

Surangkhana Rukdee This is my paper · ORCID
classification astro-ph.EPastro-ph.IM
keywords high-resolutionspectroscopyexoplanetatmospheresmolecularoxygendetectiontransmissionbiosignaturesexposuretimecalculatorhazeandcloudsinstrumentation
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

This paper reviews current and upcoming high-resolution spectrograph designs for studying rocky exoplanet atmospheres and then makes a concrete quantitative case about spectral resolution. Using detailed exposure time calculations for the O2 A-band, it argues that increasing resolution from R=100,000 to R=300,000 yields higher detection significance at the same exposure time. In the realistic case where haze clips half the signal, the required exposure drops by about one third; in the pessimistic case of haze plus a cloud deck clipping 90% of the signal, the exposure time and number of transits drop by a factor of four. This matters because O2 is a proposed biosignature, and current instruments would need decades to detect it around Earth analogs, so a factor-of-four reduction could make such searches feasible.

What carries the argument

The central mechanism is an exposure time calculator for the O2 A-band that simulates signal-to-noise per resolution element, comparing an oxygen-bearing atmospheric model against a no-oxygen model via repeated Monte Carlo realizations and a chi-square difference between the two templates. The calculator adopts three haze and cloud scenarios in which the O2 transmission profile is partially clipped to a constant, following earlier work on hazy sub-Neptunes. This machinery converts spectral resolution into a predicted exposure time and transit count, and it is what supports the factor-of-four reduction in the most obscured scenario.

What would settle it

Model a realistic hazy or cloudy terrestrial atmosphere with full radiative transfer, generate synthetic transit spectra at R=100,000 and R=300,000, and compute the exposure time needed for a fixed O2 detection significance; if the heavy-haze ratio does not approach a factor of four, the paper's central scaling assumption is not correct. A direct on-sky test would compare the same hazy exoplanet at both resolutions with equal exposure and check whether the higher resolution actually delivers the predicted significance gain.

Watch

Extended reading notes

Core claim

The central claim is that spectral resolution is a direct lever on the detectability of O2 in transmission spectra of terrestrial exoplanets. At fixed exposure time, R=300,000 gives a higher chi-square difference between an O2-bearing and a no-oxygen model than R=100,000; equivalently, the exposure time required for a given significance shrinks by about 10% in clear skies, about 30% when haze suppresses half the line signal, and about a factor of four when haze and a cloud deck suppress 90% of the signal. The gain comes from resolving atmospheric line cores, which concentrate the planetary signal into fewer resolution elements and rise above the flattened continuum produced by clouds and hazes. The paper also finds that pushing to R=500,000 gives only modest additional gains over R=300,000, placing the near-optimal range for future instruments at roughly R=300,000 to 400,000.

Load-bearing premise

The factor-of-four gain assumes that real hazes and cloud decks suppress the O2 signal by simply clipping the upper half of each line profile to a constant, and that exposure time scales linearly with the resulting chi-square difference; if actual aerosols erode line cores in a different way, the quoted reduction could change.

Editorial extensions

If this is right

  • At the same exposure time, a spectrograph at R=300,000 reaches higher O2 detection significance than one at R=100,000 across all three modeled haze scenarios.
  • The number of transits needed for a significant O2 detection is reduced by roughly a factor of four when haze and clouds suppress 90% of the signal, by about 30% under 50% haze, and by about 10% in clear skies.
  • Pushing from R=300,000 to R=500,000 adds only small additional gains, so future instrument designs near R=300,000 to 400,000 capture most of the benefit.
  • Interferometric or resolution-booster designs that achieve ultra-high resolution in compact form are viable paths for ELT-era and space-based O2 searches.
  • High-resolution spectroscopy can partially overcome the flat, featureless spectra that clouds and hazes produce, because it reads the upper line cores of atmospheric absorption features.

Reading between the lines

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

  • If real hazes erode the tops and cores of spectral lines more gradually than the simple clipping model assumes, the factor-of-four gain in the worst-case scenario could shrink, though the qualitative advantage of higher resolution should persist because line-core probing is a physical effect, not just a numerical artifact.
  • The same resolution-versus-exposure argument should apply to other narrow molecular features such as CH4 or water lines; rerunning the exposure time calculation for those bands is a direct, testable extension of this paper's method.
  • The near-optimal resolution range around 300,000 to 400,000 gives a concrete design target for future space missions, where avoiding telluric contamination in the O2 A-band could make the resolution gain even cleaner than in ground-based observations.
  • A practical test would be to observe the same hazy exoplanet at both R=100,000 and R=300,000 with equal total exposure and compare the cross-correlation significance, which would directly check whether the predicted gain materializes on sky.
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 reviews ground-based high-resolution spectroscopy techniques for studying rocky exoplanet atmospheres, covering echelle spectrographs, Fourier transform spectrometers, VIPA devices, and Fabry-Perot based resolution boosters. It presents a new exposure time calculator (ETC) for detecting O2 in transmission spectroscopy, comparing spectral resolutions R=100,000, 300,000, and 500,000 under clear, 50% haze, and 90% haze-and-cloud scenarios. The headline quantitative claim is that in the most challenging haze/cloud case, increasing resolution from R=100,000 to R=300,000 reduces the required exposure time by roughly a factor of four (Figure 4 reports 3.68). The paper also provides an empirical comparison of telluric O2 spectra from X-shooter, an FTS, and the FIOS demonstrator.

Significance. If the exposure-time reduction factors are robust, the paper provides a useful quantitative argument for ultra-high-resolution spectrographs on next-generation ELTs and possibly for high-resolution capabilities on space missions such as HWO. The ETC is described with explicit equations and parameters, and the Monte Carlo approach is appropriate. The review portion assembles a useful instrument inventory, and the on-sky FIOS and FTS spectra provide concrete demonstrations of the technological readiness of interferometric spectrographs. However, the central factor-of-four result rests on a simplified haze parameterization and an ETC that omits telluric contamination, so the quantitative claim needs further sensitivity testing before it can serve as a firm design driver.

major comments (3)
  1. [§3, Figure 4; §2 haze parameterization] The factor-of-3.68 exposure-time reduction in the 90% haze/cloud scenario depends on the transmissivity-clipping model adopted from Hood et al. (2020), in which the upper half of the O2 line profile is cut off and set to a constant. This creates a sharp corner at the clip height; at R=300,000 many more independent wavelength bins sample the flat clipped region than at R=100,000, which can inflate the Δχ² gain independently of the physical line-core information. The statement that the exposure time scales linearly with Δχ² does not address this shape dependence. I recommend a sensitivity test that varies the shape of the haze profile (e.g., smoothly rounded shoulders or a wavelength-dependent cloud-top opacity) and the clip level, to demonstrate that the reported ratios are not dominated by the artificial sharp edge.
  2. [§3 text vs. Figure 4 and §4.2] The quoted exposure-time reduction factors are internally inconsistent. Section 3 states that in the 50% haze scenario R=300,000 'reduces the necessary exposure time by about 34%', but Figure 4's ratio of 1.39 implies a 28% reduction (1 − 1/1.39). Section 4.2 summarizes the reductions as '1.1, 2x and 4x' for the three scenarios, whereas Figure 4 gives 1.10, 1.39, and 3.68. The abstract's 'factor of 4' should also be matched to the computed 3.68 or the calculations should be adjusted. These numbers must be reconciled before publication.
  3. [§2, ETC description] The ETC explicitly does not include telluric contamination, yet the paper's motivation is ground-based ELT observations in the O2 A-band, which is strongly affected by telluric O2 lines. The statement that the results should 'generalize approximately proportionally' to the full band and that telluric effects were handled in a previous study (ref. 46) does not ensure that the resolution-dependent exposure-time ratios are unchanged, because telluric absorption adds a strong, wavelength-dependent foreground that interacts differently with the line-spread function at R=100,000 versus R=300,000. The authors should either include telluric lines in the ETC or explicitly restrict the headline claims to space-based or telluric-free observations.
minor comments (5)
  1. [Table 1] Table 1 contains factual errors in the telescope column: HARPS is at the ESO 3.6m telescope, not Keck II; HARPS-N is at the TNG 3.58m; and GIANO is also at the TNG 3.58m, not 10m. These should be corrected for a review paper.
  2. [Equation (2)] Equation (2) has an unbalanced parenthesis: the second sum has an extra closing parenthesis. Please fix the mathematical notation.
  3. [Abstract and title] The title contains a grammatical error ('rocky exoplanet atmospheres studies' should be 'rocky exoplanet atmosphere studies' or 'studies of rocky exoplanet atmospheres'); the abstract would also benefit from a careful grammar check.
  4. [Data availability] The ETC code is not released, and the data availability statement only offers data 'on reasonable request.' Given that the exposure-time calculation is the paper's main new quantitative contribution, providing the ETC code or a documented input/output table would substantially improve reproducibility.
  5. [Section 2, haze model description] The description of the haze clipping is brief and somewhat ambiguous ('the upper half is cut off and set to a constant'). A sentence or a small schematic clarifying exactly how the transmissivity profile is modified for the 50% and 90% scenarios would make the method easier to interpret.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the factor-of-four exposure-time gain is a conditional ETC result from an externally cited haze scenario, not a fitted or self-referential prediction.

full rationale

The central claim (R=300,000 reaches higher significance than R=100,000 and reduces needed exposure time by up to about 4x in the 90% haze/cloud scenario) is produced by the exposure time calculator described in Section 2, using Equation 2 as a chi-square comparison of O2 and no-O2 models generated with ESO SkyCalc. No parameter is fitted to the claimed factor; the haze/cloud scenarios are explicitly taken from Hood et al. (2020), an external assumption whose realism is a robustness question, not circularity. The resolution scaling of line depth is imported from independent prior simulations, and the author's FIOS on-sky data are empirical demonstrations, not inputs to the ETC. No load-bearing step in the derivation reduces to the conclusion by construction, and the self-citations are engineering or observational rather than argumentative. The sharp-edged clipping model could affect the magnitude of the gain, but that is a model-dependence concern, not a circular-reasoning defect.

Assumptions & free parameters 6 free parameters · 5 assumptions · 0 invented entities

The central simulation rests on several domain assumptions about haze behavior, line depth scaling, and the linearity of chi-square with exposure time. No new physical entities are introduced. The chosen haze fractions and instrument parameters are free parameters in the sense that they are selected by hand and directly influence the headline exposure reduction factors.

free parameters (6)
  • haze and cloud transmissivity fraction = 50% and 90% clipping
    The three observing scenarios (clear, 50% haze, 90% haze+cloud) are chosen by hand to represent optimistic, realistic, and pessimistic cases. The factor-4 exposure reduction depends directly on the 90% clipping assumption.
  • transit depth = 1%
    Assumed planet transit depth for the simulations; real targets vary.
  • telescope diameter = 8 m
    Assumed aperture; results may scale with collecting area.
  • detector read noise = 1 electron
    Assumed modern CMOS detector parameter.
  • detector dark current = 0.1 electrons/s
    Assumed cooled detector parameter.
  • exposure time for Figure 4 = 600 s
    The reported ratios are shown for 10-minute exposures; the paper states other exposures give similar results because of the linear scaling.
assumptions (5)
  • domain assumption O2 A-band model spectra from ESO SkyCalc are accurate for exoplanet transmission spectra
    Section 2, the ETC uses ESO SkyCalc models for signal and noise.
  • domain assumption Increasing spectral resolution from R=100,000 to R=300,000 roughly doubles average line depth
    Taken from ref 46 and used as the basis for the expected gain; not independently derived in this paper.
  • domain assumption The relation between exposure time and delta chi-square significance is linear
    Section 3, used to convert delta chi-square improvements into exposure time reduction factors.
  • domain assumption The haze clipping model from Hood et al. 2020 applies to O2 A-band observations
    Section 2, the 50% and 90% transmissivity clipping scenarios follow ref 77.
  • standard math Gaussian noise and standard chi-square statistics are valid for the Monte Carlo comparison
    Equation 2 and the Monte Carlo procedure assume normally distributed noise.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Instrumentation prospects for rocky exoplanet atmospheres studies with high resolution spectroscopy." pith.science (2026). https://pith.science/paper/OFA4D65H

@misc{pith2026250501102,
  author       = {Pith},
  title        = {Pith review of: Instrumentation prospects for rocky exoplanet atmospheres studies with high resolution spectroscopy},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/OFA4D65H}},
  note         = {Machine review of arXiv:2505.01102}
}
read the original abstract

Studying the atmospheres of exoplanets is one of the most promising ways to learn about distant worlds beyond our solar system. The composition of an exoplanet's atmosphere can provide critical insights into its geology and potential habitability. For instance, the presence of certain molecules such as water vapor, oxygen, or methane have been proposed to indicate the possibility of life. From an observation point of view, over the past fifteen years, significant progress has been made in characterizing exoplanetary atmospheres. This work reviews recent developments in ground-based high-resolution spectroscopic instruments that make it possible to analyze distant atmospheres in great detail. High-resolution transmission spectroscopy, one of the most effective methods used, has examined the atmospheres of Jupiter-like and is pushing towards the smaller, sub-Neptunian exoplanets. Numerous molecules have been detected using this technique, including CO,H2O,TiO,HCN,CH4,NH3,C2H2,OH. We explore the intriguing possibilities that lie ahead for future ground-based instrumentation, particularly in the context of detecting biologically relevant molecules within Earth-analog exoplanetary atmospheres including molecular oxygen (O2). With detailed exposure time calculations for detecting O2 we find that at the same exposure time spectral resolution of 300,000 reaches higher significance compared to 100,000. The exposure time and therefore the needed number of transits is reduced by a factor of 4 in challenging haze and cloud scenarios.

Figures

Figures reproduced from arXiv: 2505.01102 by the authors.

Figure 1
Figure 1. The confirmed exoplanets discovered with high-contrast imaging (purple) are compared to those found with transits (green) as of September 2024 from the NASA Exoplanet Archive. The marker size corresponds to the relative radius. Molecule detection can be enhanced by high-resolution spectroscopy. Two decades ago, high dispersion spectroscopy (HDS) was suggested22, 23 as a way to boost detection capabilities by relying… view at source ↗
Figure 2
Figure 2. Comparison of (telluric) molecular oxygen spectrum observed using low-medium resolution spectrograph and interferometer-based instruments. The top panel shows the observed telluric spectrum from archival X-Shooter spectra with spectral resolution ranging from R=1500 to R=18000 in different colors. The lower panel shows the spectrum from FTS126 (red) with R=700,000 and FIOS-demo133 (purple) with R=250,000 overlaid wi… view at source ↗
Figure 3
Figure 3. Comparison of transit depth observed at different spectral resolutions: R=100,000 (top left panel, blue line in the right panels), R=300,000 (middle left panel, orange line in the right panels), and R=500,000 (bottom left panel, green line in the right panels), assuming 1% of the star’s light passes through the exoplanet’s atmosphere. Left panels: simulated model comparison of transit spectral features for different… view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: Exposure time reduction factors. Columns indicate the considered scenarios: clear atmosphere (optimistic case), 50% haze (realistic case), and 90% haze (pessimistic case) at different instrument spectral resolutions (R=100,000, R=300,000, R=500,000) with a 10-minute ex…
Figure 5
Figure 5. Figure 5: Detection of molecules prominently involved in biological processes on Earth using current instrumentation: H2O 142–150, CH4 151, CO2 144, 150, 152, HCN153, O2, O3 and featureless of Earth- to Neptune-size planets using ground-based (black square) and space-based (blue…
Figure 6
Figure 6. Figure 6: The photon efficiency of high-resolution spectrographs, most of which are grating-based, can reach 50% when using VIPA132. The light shaded area below R=200,000 indicates where the signal may be clipped due to hazes, while the dark grey shaded area below R=150,000 sugg…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

193 extracted references · 29 canonical work pages

  1. [1]

    & Meyer, M

    Pepe, F., Ehrenreich, D. & Meyer, M. R. Instrumentation for the detection and characterization of exoplanets. Nature 513, 358–366, DOI: 10.1038/nature13784 (2014). 1409.5266

    arXiv 2014

  2. [2]

    Birkby, J. L. Exoplanet Atmospheres at High Spectral Resolution. arXiv e-prints arXiv:1806.04617, DOI: 10.48550/arXiv.1806.04617 (2018). 1806.04617

    arXiv doi:10.48550/arxiv.1806.04617 2018

  3. [3]

    Follette, K. B. An introduction to high contrast differential imaging of exoplanets and disks. Publ. Astron. Soc. Pac. 135, 093001, DOI: 10.1088/1538-3873/aceb31 (2023)

    doi:10.1088/1538-3873/aceb31 2023

  4. [4]

    Fischer, D. A. et al. Exoplanet Detection Techniques. In Beuther, H., Klessen, R. S., Dullemond, C. P. & Henning, T. (eds.) Protostars and Planets VI, 715–737, DOI: 10.2458/azu_uapress_9780816531240-ch031 (2014). 1505.06869

    arXiv 2014

  5. [5]

    Macintosh, B. et al. Discovery and spectroscopy of the young jovian planet 51 eri b with the gemini planet imager. Science 350, 64–67, DOI: 10.1126/science.aac5891 (2015)

    doi:10.1126/science.aac5891 2015

  6. [6]

    Franson, K. et al. Astrometric accelerations as dynamical beacons: A giant planet imaged inside the debris disk of the young star af lep. The Astrophys. J. Lett. 950, L19, DOI: 10.3847/2041-8213/acd6f6 (2023)

    doi:10.3847/2041-8213/acd6f6 2023

  7. [7]

    Extreme Adaptive Optics

    Guyon, O. Extreme Adaptive Optics. ARAA 56, 315–355, DOI: 10.1146/annurev-astro-081817-052000 (2018)

    doi:10.1146/annurev-astro-081817-052000 2018

  8. [8]

    Fusco, T. et al. High-order adaptive optics requirements for direct detection of extrasolar planets: Application to the SPHERE instrument. Opt. Express 14, 7515, DOI: 10.1364/OE.14.007515 (2006)

    doi:10.1364/oe.14.007515 2006

Show all 193 references
  1. [9]

    Graham, J. R. et al. Ground-based direct detection of exoplanets with the gemini planet imager (gpi) (2007). 0704.1454. 13/21

    2007 arXiv

  2. [10]

    Macintosh, B. et al. First light of the gemini planet imager. proceedings Natl. Acad. Sci. 111, 12661–12666 (2014)

    2014

  3. [11]

    Currie, T. et al. Scexao: First results and on-sky performance. Proc. Int. Astron. Union 8, 34–35, DOI: 10.1017/S1743921313007746 (2013)

    2013 doi

  4. [12]

    Beuzit, J.-L. et al. Sphere: the exoplanet imager for the very large telescope. Astron. & Astrophys. 631, A155, DOI: 10.1051/ 0004-6361/201935251 (2019)

    2019

  5. [13]

    The Study of the Solar Corona and Prominences without Eclipses (George Darwin Lecture, delivered by M

    Lyot, B. The Study of the Solar Corona and Prominences without Eclipses (George Darwin Lecture, delivered by M. Bernard Lyot, Assoc.R.A.S., on 1939 May 12). Mon. Notices Royal Astron. Soc. 99, 580–594, DOI: 10.1093/mnras/99.8.580 (1939). https: //academic.oup.com/mnras/article...

    1939 doi

  6. [14]

    J., Vanderbei, R

    Kasdin, N. J., Vanderbei, R. J., Spergel, D. N. & Littman, M. G. Extrasolar planet finding via optimal apodized-pupil and shaped-pupil coronagraphs. The Astrophys. J. 582, 1147, DOI: 10.1086/344751 (2003)

    2003 doi

  7. [15]

    & Kostinski, A

    Yang, W. & Kostinski, A. B. One-sided achromatic phase apodization for imaging of extrasolar planets. The Astrophys. J. 605, 892 – 901 (2004)

    2004

  8. [16]

    Phase-induced amplitude apodization of telescope pupils for extrasolar terrestrial planet imaging

    Guyon, O. Phase-induced amplitude apodization of telescope pupils for extrasolar terrestrial planet imaging. Astron. & Astrophys. 404, 379–387, DOI: 10.1051/0004-6361:20030457 (2003)

    2003 doi

  9. [17]

    Pizza: a phase-induced zonal zernike apodization designed for stellar coronagraphy

    Martinache, F. Pizza: a phase-induced zonal zernike apodization designed for stellar coronagraphy. J. Opt. A: Pure Appl. Opt. 6, 809 – 814 (2004)

    2004

  10. [18]

    Ruffio, J.-B. et al. Radial velocity measurements of hr 8799 b and c with medium resolution spectroscopy. The Astron. J. 158, 200 (2019)

    2019

  11. [19]

    Dekany, R. et al. Palm-3000: Exoplanet adaptive optics for the 5 m hale telescope. The Astrophys. J. 776, 130, DOI: 10.1088/ 0004-637X/776/2/130 (2013)

    2013

  12. [20]

    A pathfinder for imaging exo-earths

    Currie, T. A pathfinder for imaging exo-earths. Nat. Astron. 3, 463–463 (2019)

    2019

  13. [21]

    Chauvin, G. et al. Discovery of a warm, dusty giant planet around hip 65426. Astron. & Astrophys. 605, L9, DOI: 10.1051/ 0004-6361/201731152 (2017)

    2017

  14. [22]

    Sparks, W. B. & Ford, H. C. Imaging spectroscopy for extrasolar planet detection.The Astrophys. J. 578, 543–564, DOI: 10.1086/342401 (2002)

    2002 doi

  15. [23]

    & Jean, S

    Riaud, P. & Jean, S. Improving earth-like planets’ detection with an elt: The differential radial velocity experiment.Astron. & Astrophys. - ASTRON ASTROPHYS 469, 355–361, DOI: 10.1051/0004-6361:20077085 (2007)

    2007 doi

  16. [24]

    Snellen, I. et al. Combining high-dispersion spectroscopy with high contrast imaging: Probing rocky planets around our nearest neighbors. Astronomy and Astrophysics 576, A59, DOI: 10.1051/0004-6361/201425018 (2015). 1503.01136

    2015 arXiv

  17. [25]

    & Benneke, B

    Wang, J., Mawet, D., Ruane, G., Hu, R. & Benneke, B. Observing Exoplanets with High Dispersion Coronagraphy. I. The Scientific Potential of Current and Next-generation Large Ground and Space Telescopes. AJ 153, 183, DOI: 10.3847/1538-3881/aa6474 (2017). 1703.00582

    2017 arXiv

  18. [26]

    Vigan, A. et al. First light of vlt/hirise: High-resolution spectroscopy of young giant exoplanets. A@AND@A 682, A16, DOI: 10.1051/0004-6361/202348019 (2024)

    2024 doi

  19. [27]

    Kotani, T. et al. Extremely high-contrast, high spectral resolution spectrometer REACH for the Subaru Telescope. In Schreiber, L., Schmidt, D. & Vernet, E. (eds.) Adaptive Optics Systems VII , vol. 11448 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference S...

    2020 doi

  20. [28]

    Delorme, J.-R. et al. Keck Planet Imager and Characterizer: a dedicated single-mode fiber injection unit for high-resolution exoplanet spectroscopy. J. Astron. Telesc. Instruments, Syst. 7, 035006, DOI: 10.1117/1.JATIS.7.3.035006 (2021). 2107.12556

    2021 arXiv

  21. [29]

    Finnerty, L. et al. Characterizing Hot Jupiter Atmospheres at high resolution with Keck/KPIC. Bull. AAS 55 (2023). Https://baas.aas.org/pub/2023n2i324p08

    2023

  22. [30]

    Lovis, C. et al. Atmospheric characterization of proxima b by coupling the sphere high-contrast imager to the espresso spectrograph. Astron. & Astrophys. 599, A16, DOI: 10.1051/0004-6361/201629682 (2017)

    2017 doi

  23. [31]

    Chazelas, B. et al. RISTRETTO: seven spaxel single mode spectrograph design. In Evans, C. J., Bryant, J. J. & Motohara, K. (eds.) Ground-based and Airborne Instrumentation for Astronomy IX , vol. 12184 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Ser...

    2022 arXiv

  24. [32]

    Eisenhauer, F. et al. GRA VITY: Observing the Universe in Motion.The Messenger 143, 16–24 (2011)

    2011

  25. [33]

    Eisenhauer, F. et al. GRA VITY+: Towards Faint Science, All Sky, High Contrast, Milli-Arcsecond Optical Interferometric Imaging. White Paper based on the GRA VITY+ proposal to ESO (2020)

    2020

  26. [34]

    Wagner, K. et al. Imaging low-mass planets within the habitable zone of α Centauri. Nat. Commun. 12, 922, DOI: 10.1038/ s41467-021-21176-6 (2021). 2102.05159. 14/21

    2021 arXiv

  27. [35]

    Thatte, N. et al. Harmoni: the elt’s first-light near-infrared and visible integral field spectrograph. Publ. The Messenger vol. 182 pp. 7-12, March 2021., DOI: 10.18727/0722-6691/5215 (2021)

    2021 doi

  28. [36]

    & Carlotti, A

    Bidot, A., Mouillet, D. & Carlotti, A. Exoplanet detection limits using spectral cross-correlation with spectro-imaging. Analytical model applied to the case of ELT/HARMONI. Astronomy and Astrophysics 682, A10, DOI: 10.1051/0004-6361/202346185 (2024). 2311.13275

    2024 arXiv

  29. [37]

    Vaughan, S. R. et al. Behind the mask: can HARMONI@ELT detect biosignatures in the reflected light of Proxima b? MNRAS 528, 3509–3522, DOI: 10.1093/mnras/stae242 (2024). 2401.09589

    2024

  30. [38]

    Brandl, B. et al. Metis: The mid-infrared elt imager and spectrograph. Publ. The Messenger vol. 182 pp. 22-26, March 2021., DOI: 10.18727/0722-6691/5218 (2021)

    2021 doi

  31. [39]

    Marconi, A. et al. ANDES, the high resolution spectrograph for the ELT: science case, baseline design and path to construction. In Evans, C. J., Bryant, J. J. & Motohara, K. (eds.) Ground-based and Airborne Instrumentation for Astronomy IX , vol. 12184 of Society of Photo-Opti...

    2022 doi

  32. [40]

    Palle, E. et al. Ground-breaking exoplanet science with the andes spectrograph at the elt (2023). 2311.17075

    2023 arXiv

  33. [41]

    Stevens, D. J. & Gaudi, B. S. A Posteriori Transit Probabilities. PASP 125, 933, DOI: 10.1086/672572 (2013). 1305.1298

    2013 arXiv

  34. [42]

    L., Zimmerman, N

    Saxena, P., Villanueva, G. L., Zimmerman, N. T., Mandell, A. M. & Smith, A. J. R. W. Simulating reflected light exoplanet spectra of the promising direct imaging target, andromedae d, with a new, fast sampling method using the planetary spectrum generator. The Astron. J. 162, ...

    2021 doi

  35. [43]

    & Sasselov, D

    Seager, S. & Sasselov, D. D. Theoretical Transmission Spectra during Extrasolar Giant Planet Transits. ApJ 537, 916–921, DOI: 10.1086/309088 (2000). astro-ph/9912241

    2000 arXiv

  36. [44]

    M., Noyes, R

    Charbonneau, D., Brown, T. M., Noyes, R. W. & Gilliland, R. L. Detection of an Extrasolar Planet Atmosphere. ApJ 568, 377–384, DOI: 10.1086/338770 (2002). astro-ph/0111544

    2002 arXiv

  37. [45]

    Boldt-Christmas, L. et al. Optimising spectroscopic observations of transiting exoplanets. Astronomy and Astrophysics 683, A244, DOI: 10.1051/0004-6361/202347398 (2024). 2312.08320

    2024 arXiv

  38. [46]

    H., Meadows, V

    Currie, M. H., Meadows, V . S. & Rasmussen, K. C. There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets. PSJ 4, 83, DOI: 10.3847/PSJ/accf86 (2023). 2304.10683

    2023 arXiv

  39. [47]

    Lopez-Morales, M. et al. Detecting earth-like biosignatures on rocky exoplanets around nearby stars with ground-based extremely large telescopes. Bull. AAS 51 (2019). Https://baas.aas.org/pub/2020n3i162

    2019

  40. [48]

    Ben-Ami, S., López-Morales, M., Garcia-Mejia, J., Abad, G. G. & Szentgyorgyi, A. High-resolution spectroscopy using fabry–perot interferometer arrays: An application to searches for o2 in exoplanetary atmospheres, DOI: 10.3847/1538-4357/aac835 (2018)

    2018 doi

  41. [49]

    Szentgyorgyi, A. et al. The GMT-Consortium Large Earth Finder (G-CLEF): an optical Echelle spectrograph for the Giant Magellan Telescope (GMT). In Ground-based and Airborne Instrumentation for Astronomy VI , vol. 9908 of Proc. SPIE , 990822, DOI: 10.1117/12.2233506 (2016)

    2016 doi

  42. [50]

    Rukdee, S. et al. Characterization of a multi-etalon array for ultra-high resolution spectroscopy. In Evans, C. J., Bryant, J. J. & Motohara, K. (eds.) Ground-based and Airborne Instrumentation for Astronomy VIII , vol. 11447, 337 – 350, DOI: 10.1117/12.2561046. International ...

    doi

  43. [51]

    Brogi, M. et al. Rotation and Winds of Exoplanet HD 189733 b Measured with High-dispersion Transmission Spectroscopy. ApJ 817, 106, DOI: 10.3847/0004-637X/817/2/106 (2016). 1512.05175

    2016 arXiv

  44. [52]

    Snellen, I. A. G., de Kok, R. J., de Mooij, E. J. W. & Albrecht, S. The orbital motion, absolute mass and high-altitude winds of exoplanet HD209458b. Nature 465, 1049–1051, DOI: 10.1038/nature09111 (2010). 1006.4364

    2010 arXiv

  45. [53]

    Nugroho, S. K. et al. High-resolution Spectroscopic Detection of TiO and a Stratosphere in the Day-side of W ASP-33b.AJ 154, 221, DOI: 10.3847/1538-3881/aa9433 (2017). 1710.05276

    2017 arXiv

  46. [54]

    & Henning, T

    Yan, F. & Henning, T. An extended hydrogen envelope of the extremely hot giant exoplanet KELT-9b.Nat. Astron. 2, 714–718, DOI: 10.1038/s41550-018-0503-3 (2018). 1807.00869

    2018 arXiv

  47. [55]

    Brogi, M. et al. The signature of orbital motion from the dayside of the planet τ Boötis b. Nature 486, 502–504, DOI: 10.1038/ nature11161 (2012). 1206.6109

    2012 arXiv

  48. [56]

    High-dispersion spectroscopy of extrasolar planets: from co in hot jupiters to o<sub>2</sub> in exo-earths

    Snellen, I. High-dispersion spectroscopy of extrasolar planets: from co in hot jupiters to o<sub>2</sub> in exo-earths. Philos. Transactions Royal Soc. A: Math. Phys. Eng. Sci. 372, 20130075, DOI: 10.1098/rsta.2013.0075 (2014). https://royalsocietypublishing. org/doi/pdf/10.10...

    2014

  49. [57]

    Giacobbe, P. et al. Five carbon- and nitrogen-bearing species in a hot giant planet’s atmosphere. Nature 592, 205–208, DOI: 10.1038/s41586-021-03381-x (2021). 2104.03352

    2021 arXiv

  50. [58]

    Merritt, S. R. et al. An inventory of atomic species in the atmosphere of WASP-121b using UVES high-resolution spectroscopy. MNRAS 506, 3853–3871, DOI: 10.1093/mnras/stab1878 (2021). 2106.15394. 15/21

    2021 arXiv

  51. [59]

    Exoplanet atmospheres at high resolution through a modest-size telescope - fein mascara-2b and kelt-9b with fies on the nordic optical telescope

    Bello-Arufe, Aaron et al. Exoplanet atmospheres at high resolution through a modest-size telescope - fein mascara-2b and kelt-9b with fies on the nordic optical telescope. A@AND@A 662, A51, DOI: 10.1051/0004-6361/202142787 (2022)

    2022 doi

  52. [60]

    & Snellen, I

    Mollière, P. & Snellen, I. A. G. Detecting isotopologues in exoplanet atmospheres using ground-based high-dispersion spectroscopy. Astron. &amp; Astrophys. 622, A139, DOI: 10.1051/0004-6361/201834169 (2019)

    2019 doi

  53. [61]

    Line, M. R. et al. A solar C/O and sub-solar metallicity in a hot Jupiter atmosphere. Nature 598, 580–584, DOI: 10.1038/ s41586-021-03912-6 (2021). 2110.14821

    2021 arXiv

  54. [62]

    M., Barman, T

    Konopacky, Q. M., Barman, T. S., Macintosh, B. A. & Marois, C. Detection of carbon monoxide and water absorption lines in an exoplanet atmosphere. Science 339, 1398–1401, DOI: 10.1126/science.1232003 (2013)

    2013 doi

  55. [63]

    Meadows, V . S.et al. Exoplanet Biosignatures: Understanding Oxygen as a Biosignature in the Context of Its Environment.Astrobiology 18, 630–662, DOI: 10.1089/ast.2017.1727 (2018). 1705.07560

    2018

  56. [64]

    Brogi, M. et al. Detection of Molecular Absorption in the Dayside of Exoplanet 51 Pegasi b? ApJ 767, 27, DOI: 10.1088/0004-637X/ 767/1/27 (2013). 1302.6242

    2013 arXiv

  57. [65]

    J., Birkby, J

    Brogi, M., de Kok, R. J., Birkby, J. L., Schwarz, H. & Snellen, I. A. G. Carbon monoxide and water vapor in the atmosphere of the non-transiting exoplanet HD 179949 b. Astronomy and Astrophysics 565, A124, DOI: 10.1051/0004-6361/201423537 (2014). 1404.3769

    2014 arXiv

  58. [66]

    Cabot, S. H. C., Madhusudhan, N., Hawker, G. A. & Gandhi, S. On the robustness of analysis techniques for molecular detections using high-resolution exoplanet spectroscopy. MNRAS 482, 4422–4436, DOI: 10.1093/mnras/sty2994 (2019). 1811.05978

    2019 arXiv

  59. [67]

    de Kok, R. J. et al. Detection of carbon monoxide in the high-resolution day-side spectrum of the exoplanet HD 189733b. Astronomy and Astrophysics 554, A82, DOI: 10.1051/0004-6361/201321381 (2013). 1304.4014

    2013 arXiv

  60. [68]

    & Barnes, J

    Rodler, F., Kürster, M. & Barnes, J. R. Detection of CO absorption in the atmosphere of the hot Jupiter HD 189733b. MNRAS 432, 1980–1988, DOI: 10.1093/mnras/stt462 (2013)

    2013 doi

  61. [69]

    Alonso-Floriano, F. J. et al. Multiple water band detections in the CARMENES near-infrared transmission spectrum of HD 189733 b. Astronomy and Astrophysics 621, A74, DOI: 10.1051/0004-6361/201834339 (2019). 1811.08901

    2019 arXiv

  62. [70]

    Birkby, J. L. et al. Detection of water absorption in the day side atmosphere of HD 189733 b using ground-based high-resolution spectroscopy at 3.2µm. MNRAS 436, L35–L39, DOI: 10.1093/mnrasl/slt107 (2013). 1307.1133

    2013 arXiv

  63. [71]

    Guilluy, G. et al. Exoplanet atmospheres with GIANO. II. Detection of molecular absorption in the dayside spectrum of HD 102195b. Astronomy and Astrophysics 625, A107, DOI: 10.1051/0004-6361/201834615 (2019). 1904.04170

    2019 arXiv

  64. [72]

    A., Madhusudhan, N., Cabot, S

    Hawker, G. A., Madhusudhan, N., Cabot, S. H. C. & Gandhi, S. Evidence for Multiple Molecular Species in the Hot Jupiter HD 209458b. ApJL 863, L11, DOI: 10.3847/2041-8213/aac49d (2018). 1808.03645

    2018 arXiv

  65. [73]

    Lockwood, A. C. et al. Near-IR Direct Detection of Water Vapor in Tau Boötis b.ApJL 783, L29, DOI: 10.1088/2041-8205/783/2/L29 (2014). 1402.0846

    2014 arXiv

  66. [74]

    Hoeijmakers, H. J. et al. A search for tio in the optical high-resolution transmission spectrum of hd 209458b: Hindrance due to inaccuracies in the line database. Astron. & Astrophys. 575, A20, DOI: 10.1051/0004-6361/201424794 (2015)

    2015 doi

  67. [75]

    Xue, Q. et al. JWST Transmission Spectroscopy of HD 209458b: A Supersolar Metallicity, a Very Low C/O, and No Evidence of CH4, HCN, or C2H2. ApJL 963, L5, DOI: 10.3847/2041-8213/ad2682 (2024). 2310.03245

    2024 arXiv

  68. [76]

    Kreidberg, L. et al. Clouds in the atmosphere of the super-Earth exoplanet GJ1214b. Nature 505, 69–72, DOI: 10.1038/nature12888 (2014). 1401.0022

    2014 arXiv

  69. [77]

    Hood, C. E. et al. Prospects for Characterizing the Haziest Sub-Neptune Exoplanets with High-resolution Spectroscopy. AJ 160, 198, DOI: 10.3847/1538-3881/abb46b (2020). 2008.11299

    2020 arXiv

  70. [78]

    Exoplanet clouds

    Helling, C. Exoplanet clouds. Annu. Rev. Earth Planet. Sci. 47, 583–606, DOI: 10.1146/annurev-earth-053018-060401 (2019)

    2019 doi

  71. [79]

    Helling, C. et al. Exoplanet weather and climate regimes with clouds and thermal ionospheres. A model grid study in support of large-scale observational campaigns. Astronomy and Astrophysics 671, A122, DOI: 10.1051/0004-6361/202243956 (2023). 2208.05562

    2023 arXiv

  72. [80]

    & Webb, R

    Gandhi, S., Brogi, M. & Webb, R. K. Seeing above the clouds with high-resolution spectroscopy. MNRAS 498, 194–204, DOI: 10.1093/mnras/staa2424 (2020). 2008.11464

    2020 arXiv

  73. [81]

    Xuan, J. W. et al. A clear view of a cloudy brown dwarf companion from high-resolution spectroscopy. The Astrophys. J. 937, 54, DOI: 10.3847/1538-4357/ac8673 (2022)

    2022 doi

  74. [82]

    Keles, E. et al. The PEPSI exoplanet transit survey (PETS) I: investigating the presence of a silicate atmosphere on the super-earth 55 Cnc e. MNRAS 513, 1544–1556, DOI: 10.1093/mnras/stac810 (2022). 2203.16856

    2022 arXiv

  75. [83]

    Crossfield, I. J. M., Barman, T. & Hansen, B. M. S. High-resolution, Differential, Near-infrared Transmission Spectroscopy of GJ 1214b. ApJ 736, 132, DOI: 10.1088/0004-637X/736/2/132 (2011). 1104.1173

    2011 arXiv

  76. [84]

    J., de Mooij, E

    Esteves, L. J., de Mooij, E. J. W., Jayawardhana, R., Watson, C. & de Kok, R. A Search for Water in a Super-Earth Atmosphere: High-resolution Optical Spectroscopy of 55Cancri e. AJ 153, 268, DOI: 10.3847/1538-3881/aa7133 (2017). 1705.03022. 16/21

    2017 arXiv

  77. [85]

    Goldsmith, P. F.et al. O2 in Interstellar Molecular Clouds. ApJL 539, L123–L127, DOI: 10.1086/312854 (2000)

    2000 doi

  78. [86]

    Liseau, R. et al. Multi-line detection of O2 toward ρ Ophuichi A. Astronomy and Astrophysics 541, A73, DOI: 10.1051/0004-6361/ 201118575 (2012). 1202.5637

    2012 arXiv

  79. [87]

    Goldsmith, P. F.et al. Herschel Measurements of Molecular Oxygen in Orion. ApJ 737, 96, DOI: 10.1088/0004-637X/737/2/96 (2011). 1108.0441

    2011 arXiv

  80. [88]

    Wang, J. et al. Molecular oxygen in the nearest qso mrk 231. The Astrophys. J. 889, 129, DOI: 10.3847/1538-4357/ab612d (2020)

    2020 doi

  81. [89]

    & Marceau, F

    Leger, A., Pirre, M. & Marceau, F. J. Search for primitive life on a distant planet: relevance of 02 and 03 detections. Astronomy and Astrophysics 277, 309 (1993)

    1993

  82. [90]

    Des Marais, D. J. et al. Remote Sensing of Planetary Properties and Biosignatures on Extrasolar Terrestrial Planets. Astrobiology 2, 153–181, DOI: 10.1089/15311070260192246 (2002)

    2002 doi

  83. [91]

    Segura, A. et al. Ozone Concentrations and Ultraviolet Fluxes on Earth-Like Planets Around Other Stars. Astrobiology 3, 689–708, DOI: 10.1089/153110703322736024 (2003)

    2003 doi

  84. [92]

    Kozakis, T., Mendonça, J. M. & Buchhave, L. A. Is ozone a reliable proxy for molecular oxygen?. I. The O 2-O3 relationship for Earth-like atmospheres. Astronomy and Astrophysics 665, A156, DOI: 10.1051/0004-6361/202244164 (2022). 2208.09415

    2022 arXiv

  85. [93]

    K., Apai, D., Bergsten, G

    Hardegree-Ullman, K. K., Apai, D., Bergsten, G. J., Pascucci, I. & López-Morales, M. Bioverse: A Comprehensive Assessment of the Capabilities of Extremely Large Telescopes to Probe Earth-like O2 Levels in Nearby Transiting Habitable-zone Exoplanets. AJ 165, 267, DOI: 10.3847/1...

    2023 arXiv

  86. [94]

    Future nasa scope would find life on alien worlds

    Clery, D. Future nasa scope would find life on alien worlds. (2023)

    2023

  87. [95]

    of Sciences Engineering, N. A. & Medicine. Exoplanet Science Strategy (The National Academies Press, Washington, DC, 2018)

    2018

  88. [96]

    McLean, I. S. et al. Design and development of NIRSPEC: a near-infrared echelle spectrograph for the Keck II telescope. In Fowler, A. M. (ed.) Infrared Astronomical Instrumentation, vol. 3354 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 566–5...

    1998 doi

  89. [97]

    & Kotzlowski, H

    Dekker, H., D’Odorico, S., Kaufer, A., Delabre, B. & Kotzlowski, H. Design, construction, and performance of UVES, the echelle spectrograph for the UT2 Kueyen Telescope at the ESO Paranal Observatory. In Iye, M. & Moorwood, A. F. (eds.) Optical and IR Telescope Instrumentation...

    2000 doi

  90. [98]

    Noguchi, K. et al. High Dispersion Spectrograph (HDS) for the Subaru Telescope. PASJ 54, 855–864, DOI: 10.1093/pasj/54.6.855 (2002)

    2002 doi

  91. [99]

    Kotani, T. et al. The infrared Doppler (IRD) instrument for the Subaru telescope: instrument description and commissioning results. In Evans, C. J., Simard, L. & Takami, H. (eds.) Ground-based and Airborne Instrumentation for Astronomy VII , vol. 10702 of Society of Photo-Opti...

    2018 doi

  92. [100]

    Moutou, C. et al. SPIRou: a spectropolarimeter for the CFHT. In SF2A-2015: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, 205–212, DOI: 10.48550/arXiv.1510.01368 (2015). 1510.01368

    2015 doi arXiv

  93. [101]

    Kaeufl, H.-U. et al. CRIRES: a high-resolution infrared spectrograph for ESO’s VLT. In Moorwood, A. F. M. & Iye, M. (eds.) Ground-based Instrumentation for Astronomy, vol. 5492 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 1218–1227, DOI: 10.1...

    2004 doi

  94. [102]

    Dorn, R. J. et al. CRIRES+ on sky at the ESO Very Large Telescope. Observing the Universe at infrared wavelengths and high spectral resolution. Astronomy and Astrophysics 671, A24, DOI: 10.1051/0004-6361/202245217 (2023)

    2023 doi

  95. [103]

    Oliva, E. et al. GIANO, the high resolution IR spectrograph of the TNG: geometry of the echellogram and strategies for the 2D reduction of the spectra. In Evans, C. J., Simard, L. & Takami, H. (eds.) Ground-based and Airborne Instrumentation for Astronomy VII, vol. 10702 of So...

    2018 doi

  96. [104]

    Quirrenbach, A. et al. CARMENES instrument overview. In Ground-based and Airborne Instrumentation for Astronomy V , vol. 9147 of Proc. SPIE, 91471F, DOI: 10.1117/12.2056453 (2014)

    2014 doi

  97. [105]

    Park, C. et al. Design and early performance of IGRINS (Immersion Grating Infrared Spectrometer). In Ramsay, S. K., McLean, I. S. & Takami, H. (eds.) Ground-based and Airborne Instrumentation for Astronomy V , vol. 9147 of Society of Photo-Optical Instrumentation Engineers (SP...

    2014 doi

  98. [106]

    Mayor, M. et al. Setting New Standards with HARPS. The Messenger 114, 20–24 (2003)

    2003

  99. [107]

    Cosentino, R. et al. Harps-N: the new planet hunter at TNG. In McLean, I. S., Ramsay, S. K. & Takami, H. (eds.) Ground-based and Airborne Instrumentation for Astronomy IV , vol. 8446 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series , 84461V , DOI:...

    2012 doi

  100. [108]

    Cale, B. L. et al. Commissioning observations of HD 189733 with the PAlomar Radial Velocity Instrument. J. Astron. Telesc. Instruments, Syst. 9, 038006, DOI: 10.1117/1.JATIS.9.3.038006 (2023). 17/21

    2023 doi

  101. [109]

    Blackman, R. T.et al. Performance Verification of the EXtreme PREcision Spectrograph.AJ 159, 238, DOI: 10.3847/1538-3881/ab811d (2020). 2003.08852

    2020 arXiv

  102. [110]

    Wildi, F. et al. First light of NIRPS, the near-infrared adaptive-optics assisted high resolution spectrograph for the ESO 3.6m. In Evans, C. J., Bryant, J. J. & Motohara, K. (eds.) Ground-based and Airborne Instrumentation for Astronomy IX , vol. 12184 of Society of Photo-Opt...

    2022 doi

  103. [111]

    Crass, J. et al. The final design of the iLocater spectrograph: an optimized architecture for diffraction-limited EPRV instruments. In Evans, C. J., Bryant, J. J. & Motohara, K. (eds.) Ground-based and Airborne Instrumentation for Astronomy IX , vol. 12184 of Society of Photo-...

    2022 arXiv

  104. [112]

    J., Bechter, E

    Bechter, A. J., Bechter, E. B., Crepp, J. R., King, D. & Crass, J. A radial velocity error budget for single-mode Doppler spectrographs. In Evans, C. J., Simard, L. & Takami, H. (eds.) Ground-based and Airborne Instrumentation for Astronomy VII , vol. 10702 of Society of Photo...

    2018 arXiv

  105. [113]

    Pepe, F. et al. ESPRESSO at VLT. On-sky performance and first results. Astronomy and Astrophysics 645, A96, DOI: 10.1051/ 0004-6361/202038306 (2021). 2010.00316

    2021 arXiv

  106. [114]

    Strassmeier, K. G. et al. PEPSI: The high-resolution échelle spectrograph and polarimeter for the Large Binocular Telescope. Astron. Nachrichten 336, 324, DOI: 10.1002/asna.201512172 (2015). 1505.06492

    2015 arXiv

  107. [115]

    Kuo Tiong, B. C. et al. IRANTI: a compact flexible configuration infrared échelle spectrograph integrating emerging technologies for precise radial velocity measurements. In Evans, C. J., Bryant, J. J. & Motohara, K. (eds.) Ground-based and Airborne Instrumentation for Astrono...

    2020 doi

  108. [116]

    Schroeder, D. J. Astronomical Optics (Elsevier, 2000)

    2000

  109. [117]

    Crepp, J. R. Improving planet-finding spectrometers. Science 346, 809–810, DOI: 10.1126/science.1262071 (2014). 1412.2992

    2014 arXiv

  110. [118]

    Jovanovic, N. et al. Efficiently feeding single-mode fiber photonic spectrographs with an extreme adaptive optics system: on- sky characterization and preliminary spectroscopy. In Evans, C. J., Simard, L. & Takami, H. (eds.) Ground-based and Airborne Instrumentation for Astron...

    2016 doi

  111. [119]

    El Morsy, M. et al. Validation of strategies for coupling exoplanet psfs into single-mode fibres for high-dispersion coronagraphy.Astron. &amp; Astrophys. 667, A171, DOI: 10.1051/0004-6361/202243408 (2022)

    2022 doi

  112. [120]

    & Roddier, F

    Shaklan, S. & Roddier, F. Coupling starlight into single-mode fiber optics. Appl. Opt. 27, 2334–2338, DOI: 10.1364/AO.27.002334 (1988)

    1988 doi

  113. [121]

    Jovanovic, N. et al. Efficient injection from large telescopes into single-mode fibres: Enabling the era of ultra-precision astronomy. Astronomy and Astrophysics 604, A122, DOI: 10.1051/0004-6361/201630351 (2017). 1706.08821

    2017 arXiv

  114. [122]

    Otten, G. P. P. L.et al. Direct characterization of young giant exoplanets at high spectral resolution by coupling SPHERE and CRIRES+. Astronomy and Astrophysics 646, A150, DOI: 10.1051/0004-6361/202038517 (2021). 2009.01841

    2021 arXiv

  115. [123]

    P., Abrams, M

    Davis, S. P., Abrams, M. C. & Brault, J. W. F ourier transform spectrometry(Elsevier, 2001)

    2001

  116. [124]

    Hall, D. N. B., Ridgway, S., Bell, E. A. & Yarborough, J. M. A 1.4 Meter Fourier Transform Spectrometer for Astronomical Observations. In Crawford, D. L. (ed.) Instrumentation in Astronomy III, vol. 172 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Se...

    1979 doi

  117. [125]

    Behr, B. B. et al. Stellar Astrophysics with a Dispersed Fourier Transform Spectrograph. I. Instrument Description and Orbits of Single-lined Spectroscopic Binaries. ApJ 705, 543–553, DOI: 10.1088/0004-637X/705/1/543 (2009). 0909.3241

    2009 arXiv

  118. [126]

    H., Livingston, W

    Wallace, L., Hinkle, K. H., Livingston, W. C. & Davis, S. P. An Optical and Near-infrared (2958-9250 Å) Solar Flux Atlas. ApJS 195, 6, DOI: 10.1088/0067-0049/195/1/6 (2011)

    2011 doi

  119. [127]

    & Reinsch, K

    Reiners, A., Mrotzek, N., Lemke, U., Hinrichs, J. & Reinsch, K. The IAG solar flux atlas: Accurate wavelengths and absolute convective blueshift in standard solar spectra. Astronomy and Astrophysics 587, A65, DOI: 10.1051/0004-6361/201527530 (2016). 1511.03014

    2016 arXiv

  120. [128]

    Virtually imaged phased array

    Shirasaki, M. Virtually imaged phased array. Fujitsu Sci. & Tech. J. 35, 113–125 (1999)

    1999

  121. [129]

    Zhu, X., Lin, D., Hao, Z., Wang, L. & He, J. A VIPA spectrograph with ultra-high resolution and wavelength calibration for astronomical applications. The Astron. J. 160, 135, DOI: 10.3847/1538-3881/aba836 (2020)

    2020 doi

  122. [130]

    Bourdarot, G. et al. Nanovipa: a miniaturized high-resolution echelle spectrometer, for the monitoring of young stars from a 6u cubesat. CEAS Space J. 9, 411–419 (2017)

    2017

  123. [131]

    Zhu, X., Lin, D., Zhang, Z., Xie, X. & He, J. Dispersion Characteristics of the Multi-mode Fiber-fed VIPA Spectrograph. AJ 165, 228, DOI: 10.3847/1538-3881/accc30 (2023)

    2023 doi

  124. [132]

    Carlotti, A. et al. On-sky demonstration at Palomar Observatory of the near-IR, high-resolution VIPA spectrometer. In Evans, C. J., Bryant, J. J. & Motohara, K. (eds.) Ground-based and Airborne Instrumentation for Astronomy IX , vol. 12184 of Society of Photo-Optical Instrumen...

    2022 arXiv

  125. [133]

    Rukdee, S. et al. First on-sky results of a Fabry-Perot Instrument for Oxygen Searches (FIOS) prototype. Astronomy and Astrophysics 678, A114, DOI: 10.1051/0004-6361/202346619 (2023). 2307.14947

    2023 arXiv

  126. [134]

    Fowler, J. et al. Visible extreme adaptive optics on extremely large telescopes: Towards detecting oxygen in Proxima Centauri b and analogs. arXiv e-prints arXiv:2309.00725, DOI: 10.48550/arXiv.2309.00725 (2023). 2309.00725

    2023 doi arXiv

  127. [135]

    Le, H. A. N. et al. Exposure time calculator for Immersion Grating Infrared Spectrograph: IGRINS. Adv. Space Res. 55, 2509–2518, DOI: 10.1016/j.asr.2015.03.007 (2015). 1501.03249

    2015 arXiv

  128. [136]

    Rukdee, S. et al. Tardys: Design and prototype of an exoplanet hunter for tao using a r6 echelle grating. Exp. Astron. 48, 145–169, DOI: 10.1007/s10686-019-09642-y (2019)

    2019 doi

  129. [137]

    Vanzi, L. et al. Precision stellar radial velocity measurements with FIDEOS at the ESO 1-m telescope of La Silla. MNRAS 477, 5041–5051, DOI: 10.1093/mnras/sty936 (2018). 1804.07441

    2018 arXiv

  130. [138]

    Noll, S. et al. An atmospheric radiation model for Cerro Paranal. I. The optical spectral range. Astronomy and Astrophysics 543, A92, DOI: 10.1051/0004-6361/201219040 (2012). 1205.2003

    2012 arXiv

  131. [139]

    & Kimeswenger, S

    Jones, A., Noll, S., Kausch, W., Szyszka, C. & Kimeswenger, S. An advanced scattered moonlight model for Cerro Paranal. Astronomy and Astrophysics 560, A91, DOI: 10.1051/0004-6361/201322433 (2013). 1310.7030

    2013 arXiv

  132. [140]

    Moehler, S. et al. Flux calibration of medium-resolution spectra from 300 nm to 2500 nm: Model reference spectra and telluric correction. Astronomy and Astrophysics 568, A9, DOI: 10.1051/0004-6361/201423790 (2014). 1408.1797

    2014 arXiv

  133. [141]

    Vernet, J. et al. X-shooter, the new wide band intermediate resolution spectrograph at the eso very large telescope. Astron. &amp; Astrophys. 536, A105, DOI: 10.1051/0004-6361/201117752 (2011)

    2011 doi

  134. [142]

    Tsiaras, A. et al. A Population Study of Gaseous Exoplanets. AJ 155, 156, DOI: 10.3847/1538-3881/aaaf75 (2018). 1704.05413

    2018 arXiv

  135. [143]

    P., Tinetti, G., Tennyson, J

    Tsiaras, A., Waldmann, I. P., Tinetti, G., Tennyson, J. & Yurchenko, S. N. Water vapour in the atmosphere of the habitable-zone eight-Earth-mass planet K2-18 b. Nat. Astron. 3, 1086–1091, DOI: 10.1038/s41550-019-0878-9 (2019). 1909.05218

    2019 arXiv

  136. [144]

    Edwards, B. et al. Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3. AJ 166, 158, DOI: 10.3847/1538-3881/acea77 (2023). 2306.13645

    2023 arXiv

  137. [145]

    Kreidberg, L. et al. Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c.AJ 164, 124, DOI: 10.3847/1538-3881/ac85be (2022). 2006.07444

    2022 arXiv

  138. [146]

    Mikal-Evans, T. et al. Hubble Space Telescope Transmission Spectroscopy for the Temperate Sub-Neptune TOI-270 d: A Possible Hydrogen-rich Atmosphere Containing Water Vapor. AJ 165, 84, DOI: 10.3847/1538-3881/aca90b (2023). 2211.15576

    2023 arXiv

  139. [147]

    Roy, P.-A. et al. Water Absorption in the Transmission Spectrum of the Water World Candidate GJ 9827 d. ApJL 954, L52, DOI: 10.3847/2041-8213/acebf0 (2023). 2309.10845

    2023 arXiv

  140. [148]

    Edwards, B. et al. Hubble WFC3 Spectroscopy of the Habitable-zone Super-Earth LHS 1140 b. AJ 161, 44, DOI: 10.3847/1538-3881/ abc6a5 (2021). 2011.08815

    2021 arXiv

  141. [149]

    Brande, J. et al. A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b. AJ 164, 197, DOI: 10.3847/1538-3881/ac8b7e (2022). 2201.04197

    2022 arXiv

  142. [150]

    Bean, J. L. et al. High atmospheric metal enrichment for a Saturn-mass planet. Nature 618, 43–46, DOI: 10.1038/s41586-023-05984-y (2023). 2303.14206

    2023 arXiv

  143. [151]

    Swain, M. R. et al. Detection of an Atmosphere on a Rocky Exoplanet. AJ 161, 213, DOI: 10.3847/1538-3881/abe879 (2021). 2103.05657

    2021 arXiv

  144. [152]

    Madhusudhan, N. et al. Carbon-bearing Molecules in a Possible Hycean Atmosphere. ApJL 956, L13, DOI: 10.3847/2041-8213/acf577 (2023). 2309.05566

    2023 arXiv

  145. [153]

    Tsiaras, A. et al. Detection of an Atmosphere Around the Super-Earth 55 Cancri e. ApJ 820, 99, DOI: 10.3847/0004-637X/820/2/99 (2016). 1511.08901

    2016 arXiv

  146. [154]

    & Schwarz, H

    Brogi, M., Line, M., Bean, J., Désert, J.-M. & Schwarz, H. A framework to combine low- and high-resolution spectroscopy for the atmospheres of transiting exoplanets. The Astrophys. J. 839, L2, DOI: 10.3847/2041-8213/aa6933 (2017)

    2017 doi

  147. [155]

    Pino, L. et al. Combining low- to high-resolution transit spectroscopy of HD 189733b. Linking the troposphere and the thermosphere of a hot gas giant. Astronomy and Astrophysics 612, A53, DOI: 10.1051/0004-6361/201731244 (2018). 1709.09678

    2018 arXiv

  148. [156]

    & Marinelli, M

    Dressel, L. & Marinelli, M. Wide field camera 3 instrument handbook, version 15. Balt. STScI (2023)

    2023

  149. [157]

    Fleming, B. T. et al. Colorado Ultraviolet Transit Experiment: a dedicated CubeSat mission to study exoplanetary mass loss and magnetic fields. J. Astron. Telesc. Instruments, Syst. 4, 014004, DOI: 10.1117/1.JATIS.4.1.014004 (2018). 1801.02673

    2018 arXiv

  150. [158]

    Tinetti, G. et al. The science of ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey). In MacEwen, H. A. et al. (eds.) Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave , vol. 9904 of Society of Photo-Optical Instrumentation Engin...

    2016 doi

  151. [159]

    Stotesbury, I. et al. Twinkle: a small satellite spectroscopy mission for the next phase of exoplanet science. In Coyle, L. E., Matsuura, S. & Perrin, M. D. (eds.) Space Telescopes and Instrumentation 2022: Optical, Infrared, and Millimeter Wave , vol. 12180 of Society of Phot...

    2022 arXiv

  152. [160]

    Ricker, G. R. et al. Transiting Exoplanet Survey Satellite. J. Astron. Telesc. Instruments, Syst. 1, 1 – 10, DOI: 10.1117/1.JATIS.1.1. 014003 (2014)

    2014 doi

  153. [161]

    Rando, N. et al. CHEOPS, the ESA mission for exo-planets characterization: early operations and commissioning results. In Lystrup, M., Perrin, M. D., Batalha, N., Siegler, N. & Tong, E. C. (eds.)Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave,...

    2020 doi

  154. [162]

    A-thano, N. et al. Revisiting the Transit Timing and Atmosphere Characterization of the Neptune-mass Planet HAT-P-26 b.AJ 166, 223, DOI: 10.3847/1538-3881/acfeea (2023). 2303.03610

    2023 arXiv

  155. [163]

    Basilicata, M. et al. The GAPS Programme at TNG LV . Multiple molecular species in the atmosphere of HAT-P-11 b and review of the HAT-P-11 planetary system. arXiv e-prints arXiv:2403.01527, DOI: 10.48550/arXiv.2403.01527 (2024). 2403.01527

    2024 doi arXiv

  156. [164]

    Radica, M. et al. Muted Features in the JWST NIRISS Transmission Spectrum of Hot Neptune LTT 9779b. ApJL 962, L20, DOI: 10.3847/2041-8213/ad20e4 (2024). 2401.15548

    2024 arXiv

  157. [165]

    Benneke, B. et al. JWST Reveals CH4, CO2, and H2O in a Metal-rich Miscible Atmosphere on a Two-Earth-Radius Exoplanet. arXiv e-prints arXiv:2403.03325, DOI: 10.48550/arXiv.2403.03325 (2024). 2403.03325

    2024 doi arXiv

  158. [166]

    & Madhusudhan, N

    Holmberg, M. & Madhusudhan, N. Possible Hycean conditions in the sub-Neptune TOI-270 d. Astronomy and Astrophysics 683, L2, DOI: 10.1051/0004-6361/202348238 (2024). 2403.03244

    2024 arXiv

  159. [167]

    Benneke, B. et al. Water Vapor and Clouds on the Habitable-zone Sub-Neptune Exoplanet K2-18b. ApJL 887, L14, DOI: 10.3847/ 2041-8213/ab59dc (2019). 1909.04642

    2019 arXiv

  160. [168]

    Damiano, M., Bello-Arufe, A., Yang, J. & Hu, R. LHS 1140 b is a potentially habitable water world. arXiv e-prints arXiv:2403.13265, DOI: 10.48550/arXiv.2403.13265 (2024). 2403.13265

    2024 doi arXiv

  161. [169]

    Greene, T. P. et al. Thermal emission from the Earth-sized exoplanet TRAPPIST-1 b using JWST. Nature 618, 39–42, DOI: 10.1038/s41586-023-05951-7 (2023). 2303.14849

    2023 arXiv

  162. [170]

    Lim, O. et al. Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evidence for Strong Stellar Contamination in the Transmission Spectra. ApJL 955, L22, DOI: 10.3847/2041-8213/acf7c4 (2023). 2309.07047

    2023 arXiv

  163. [171]

    & Blain, D

    Bézard, B., Charnay, B. & Blain, D. Methane as a dominant absorber in the habitable-zone sub-Neptune K2-18 b. arXiv e-prints arXiv:2011.10424, DOI: 10.48550/arXiv.2011.10424 (2020). 2011.10424

    2020 doi arXiv

  164. [172]

    Deibert, E. K. et al. A Near-infrared Chemical Inventory of the Atmosphere of 55 Cancri e. AJ 161, 209, DOI: 10.3847/1538-3881/ abe768 (2021). 2102.08965

    2021 arXiv

  165. [173]

    May, E. M. et al. Double Trouble: Two Transits of the Super-Earth GJ 1132 b Observed with JWST NIRSpec G395H. ApJL 959, L9, DOI: 10.3847/2041-8213/ad054f (2023). 2310.10711

    2023 arXiv

  166. [174]

    V .et al

    Mugnai, L. V .et al. ARES. V . No Evidence For Molecular Absorption in the HST WFC3 Spectrum of GJ 1132 b.AJ 161, 284, DOI: 10.3847/1538-3881/abf3c3 (2021). 2104.01873

    2021 arXiv

  167. [175]

    Beatty, T. G. et al. Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b. ApJL 970, L10, DOI: 10.3847/2041-8213/ad55e9 (2024). 2406.04450

    2024 arXiv

  168. [176]

    Grasser, N., Snellen, I. A. G., Landman, R., Picos, D. G. & Gandhi, S. Peering above the clouds of the warm Neptune GJ 436 b with CRIRES+. Astronomy and Astrophysics 688, A191, DOI: 10.1051/0004-6361/202449932 (2024). 2407.06707

    2024 arXiv

  169. [177]

    Barclay, T. et al. The transmission spectrum of the potentially rocky planet L 98-59 c. arXiv e-prints arXiv:2301.10866, DOI: 10.48550/arXiv.2301.10866 (2023). 2301.10866

    2023 doi arXiv

  170. [178]

    Damiano, M. et al. A Transmission Spectrum of the Sub-Earth Planet L98-59 b in 1.1-1.7 µm. AJ 164, 225, DOI: 10.3847/1538-3881/ ac9472 (2022). 2210.10008

    2022 arXiv

  171. [179]

    & Zhu, Y

    Zhou, L., Ma, B., Wang, Y . & Zhu, Y . Hubble WFC3 Spectroscopy of the Rocky Planet L 98-59 b: No Evidence for a Cloud-free Primordial Atmosphere. AJ 164, 203, DOI: 10.3847/1538-3881/ac8fe9 (2022). 2210.10699

    2022 arXiv

  172. [180]

    Ridden-Harper, A. et al. High-resolution Transmission Spectroscopy of the Terrestrial Exoplanet GJ 486b. AJ 165, 170, DOI: 10.3847/1538-3881/acbd39 (2023). 2212.11816

    2023 arXiv

  173. [181]

    Bouwman, J. et al. Spectroscopic Time Series Performance of the Mid-infrared Instrument on the JWST. PASP 135, 038002, DOI: 10.1088/1538-3873/acbc49 (2023). 2211.16123

    2023 arXiv

  174. [182]

    Zhang, M. et al. GJ 367b Is a Dark, Hot, Airless Sub-Earth. ApJL 961, L44, DOI: 10.3847/2041-8213/ad1a07 (2024). 2401.01400

    2024 arXiv

  175. [183]

    M., Charbonneau, D

    Diamond-Lowe, H., Mendonça, J. M., Charbonneau, D. & Buchhave, L. A. Ground-based Optical Transmission Spectroscopy of the Nearby Terrestrial Exoplanet LTT 1445Ab. AJ 165, 169, DOI: 10.3847/1538-3881/acbf39 (2023). 2210.11809. 20/21

    2023 arXiv

  176. [184]

    Garcia, L. J. et al. HST/WFC3 transmission spectroscopy of the cold rocky planet TRAPPIST-1h. Astronomy and Astrophysics 665, A19, DOI: 10.1051/0004-6361/202142603 (2022). 2203.13698

    2022 arXiv

  177. [185]

    Moran, S. E. et al. High Tide or Riptide on the Cosmic Shoreline? A Water-rich Atmosphere or Stellar Contamination for the Warm Super-Earth GJ 486b from JWST Observations. ApJL 948, L11, DOI: 10.3847/2041-8213/accb9c (2023). 2305.00868

    2023

  178. [186]

    López-Morales, M. et al. Optimizing Ground-based Observations of O2 in Earth Analogs. AJ 158, 24, DOI: 10.3847/1538-3881/ab21d7 (2019). 1905.05862

    2019 arXiv

  179. [187]

    Team, T. L. The luvoir mission concept study final report (2019). 1912.06219

    2019 arXiv

  180. [188]

    Gaudi, B. S. et al. The habitable exoplanet observatory (habex) mission concept study final report (2020). 2001.06683

    2020 arXiv

  181. [189]

    Tacconi, L. et al. V oyage 2050 - Final recommendations from the V oyage 2050 Senior Committee.Eur. Space Agency (2021)

    2021

  182. [190]

    Plavchan, P. et al. EarthFinder Probe Mission Concept Study: Characterizing nearby stellar exoplanet systems with Earth-mass analogs for future direct imaging. arXiv e-prints arXiv:2006.13428, DOI: 10.48550/arXiv.2006.13428 (2020). 2006.13428

    2020 doi arXiv

  183. [191]

    Bourdarot, G. et al. Experimental test of a 40 cm-long R=100 000 spectrometer for exoplanet characterisation. In Evans, C. J., Simard, L. & Takami, H. (eds.) Ground-based and Airborne Instrumentation for Astronomy VII , vol. 10702 of Society of Photo-Optical Instrumentation En...

    2018 arXiv

  184. [192]

    & Serabyn, E

    Zhang, J., Bottom, M. & Serabyn, E. Direct detection and characterization of exoplanets using imaging Fourier transform spectroscopy. arXiv e-prints arXiv:2310.15231, DOI: 10.48550/arXiv.2310.15231 (2023). 2310.15231

    2023 doi arXiv

  185. [193]

    Atkins, C. et al. Lightweighting design optimisation for additively manufactured mirrors. In Hull, T. B., Kim, D. W. & Hallibert, P. (eds.) Astronomical Optics: Design, Manufacture, and Test of Space and Ground Systems II , vol. 11116 of Society of Photo-Optical Instrumentatio...

    2019 doi

Pith tools

Reviewed August 16, 2026 · model on record in the stance chip above.