Pith. sign in

REVIEW 3 major objections 5 minor 1 cited by

Atmospheric characterization of terrestrial exoplanets in the mid-infrared: biosignatures, habitability & diversity

T0 review · 3 major / 5 minor · reviewed 2026-08-14 · deepseek-v4-flash

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

Pith's one-line read A large space-based mid-infrared interferometer is the only approach able to survey dozens of terrestrial exoplanet atmospheres for signs of life and test how common Earth-like conditions are.

desk verdict A well-argued Voyage 2050 white paper for a MIR nulling interferometer: the science case is strong and the retrieval comparison is genuinely useful, but the yield numbers rest on an end-to-end nulling performance that has not been demonstrated. read the letter →

arxiv 1908.01316 v3 pith:IKY76AEI submitted 2019-08-04 astro-ph.EP astro-ph.IMastro-ph.SR

Sascha P. Quanz , Olivier Absil , Daniel Angerhausen , Willy Benz , Xavier Bonfils , Jean-Philippe Berger , Matteo Brogi , Juan Cabrera
show 40 more authors
William C. Danchi Denis Defrère Ewine van Dishoeck David Ehrenreich Steve Ertel Jonathan Fortney Scott Gaudi Julien Girard Adrian Glauser John Lee Grenfell Michael Ireland Markus Janson Jens Kammerer Daniel Kitzmann Stefan Kraus Oliver Krause Lucas Labadie Sylvestre Lacour Tim Lichtenberg Michael Line Hendrik Linz Jérôme Loicq Bertrand Mennesson Michael R. Meyer Yamila Miguel John Monnier Mamadou N'Diaye Enric Pallé Didier Queloz Heike Rauer Ignasi Ribas Sarah Rugheimer Franck Selsis Gene Serabyn Ignas Snellen Alessandro Sozzetti Karl R. Stapelfeldt Amaury Triaud Stéphane Udry Mark Wyatt
This is my paper · ORCID
classification astro-ph.EPastro-ph.IMastro-ph.SR
keywords mid-infraredinterferometryterrestrialexoplanetsatmosphericcharacterizationbiosignatureshabitablezonenullinginterferometerspectralretrievalspacemissionconcept
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 argues that the only way to find out whether any other world harbors signs of life, and how common Earth-like surface conditions are, is a single kind of instrument that has not yet been built: a large space-based mid-infrared interferometer measuring the heat emitted by terrestrial planets around nearby stars. The authors claim that no currently adopted mission or ground facility, including JWST and the coming extremely large ground telescopes, can obtain thermal emission spectra of temperate rocky planets in the numbers needed, namely dozens. Three quantitative results carry the argument: a spectral retrieval showing that a simulated Earth-twin's mid-infrared spectrum pins down atmospheric abundances, surface pressure, surface temperature, and radius; a statistical calculation showing that roughly 30-50 characterized planets suffice for a null result to bound how rare Earth-like conditions are; and Monte Carlo yield simulations predicting more than 400 detectable planets, including about 30 terrestrial planets in the empirical habitable zone, around 320 stars within 20 parsecs. The paper presents this mission concept as the timely next step for a European-led long-term space science program.

What carries the argument

The central object is the mid-infrared thermal emission spectrum of a terrestrial planet, whose absorption bands - ozone near 9.6 μm, methane near 7.7 μm, nitrous oxide near 7.8 μm, water near 6.2 μm, carbon dioxide near 15 μm, and carbon monoxide near 4.67 μm - carry the information about composition, temperature structure, surface pressure, and surface temperature. The instrument proposed to obtain these spectra is a nulling interferometer, a formation of collector telescopes of roughly 2.5 m aperture spaced over baselines up to about 170 m whose beams are combined so the host star's light interferes destructively, reaching the contrast of $10^{-7}$ to $10^{-6}$ needed to see a planet some 0.1 arcseconds from a Sun-like star at 10 parsecs. Around these two anchors sit three supporting mechanisms: an atmospheric retrieval framework that inverts the simulated Earth-twin spectrum into posterior distributions for key parameters; a Poisson-statistics calculation that sizes the sample a null result would need; and a Monte Carlo simulator that converts assumed planet occurrence rates, random orbits, and instrument sensitivities into the predicted 423 detections.

What would settle it

The decisive test is engineering: an integrated cryogenic demonstration in which the nulling system reaches a post-processing starlight suppression near $10^{-7}$ at 10 μm while the collector spacecraft simultaneously maintain millimeter-level formation over ~150 m baselines - if either capability falls short at the required scale, the mission concept and its yield estimates collapse. On the science side, a radial-velocity census of the proposed target stars that found temperate small planets to be much rarer than the Kepler-based occurrence rates assumed in the yield simulations would settle the yield claim directly, by showing that the projected ~30 habitable-zone planets were an overestimate.

Watch

Extended reading notes

Core claim

The central claim, stated on the paper's own terms, is that spatially resolved observations of thermal emission from terrestrial exoplanets in the mid-infrared — a search phase of broad-band imaging near 5.6, 10, and 15 μm followed by low-resolution spectroscopy from roughly 3 to 20 μm — are the most powerful and the only currently viable route to the three driving science goals: detecting atmospheric biosignatures, assessing whether surface conditions allow liquid water, and mapping the diversity of terrestrial-planet atmospheres. The retrieval study shows that a single mid-infrared spectrum of an Earth-twin at spectral resolution $R=100$ and signal-to-noise 20 yields molecular abundances to about 0.5 dex, surface pressure to 0.1 dex, surface temperature to better than 5 K, and radius to a few percent, while recovering the pressure-temperature profile; methane and nitrous oxide are accessible only in the thermal infrared, ozone serves as a proxy for molecular oxygen, and carbon monoxide appears as a contextual anti-biosignature. The yield analysis predicts that a search phase of under one year of on-source time across 320 nearby FGK and M stars detects over 400 planets spanning $0.5$-$6.0\,R_\oplus$ and $0.1$-$1000$ times Earth's insolation, with about 30 small planets in the empirical habitable zone - the minimum sample for a statistically meaningful null result about habitability. The paper concludes that none of the currently adopted projects, from the ground or in space, can deliver this dataset, and that the technology for a mid-infrared nulling interferometer has matured to the point where a large space mission is the logical next step.

Load-bearing premise

The load-bearing premise is an engineering one: a fleet of free-flying telescope spacecraft can hold formation to millimeter precision over baselines of roughly 150 meters while suppressing the host star's light to about one part in a million after post-processing, even though the deep-nulling and the formation-flying capabilities have so far only been demonstrated separately, not as one working system in space.

Editorial extensions

If this is right

  • A single mid-infrared spectrum of an Earth-twin at $R=100$ and $\mathrm{SNR}=20$ lets one retrieve molecular abundances to about 0.5 dex, surface pressure to 0.1 dex, surface temperature to better than 5 K, and radius to a few percent, from the emission spectrum alone.
  • If none of roughly 30-50 characterized habitable-zone planets shows conditions that allow liquid water, that null result rejects the hypothesis that 50% of such planets are habitable at about $5\sigma$ (with 30 planets) and can bound the true fraction down to 10-20% (with 50 planets).
  • A search phase of under three years on 320 stars within 20 pc would detect more than 400 exoplanets across $0.5$-$6\,R_\oplus$ and $0.1$-$1000$ times Earth's insolation, including about 30 terrestrial planets in the empirical habitable zone, enough for the null-result test.
  • Methane, nitrous oxide, and carbon monoxide are only detectable in the thermal infrared, and ozone provides a mid-infrared proxy for oxygen, so reflected-light surveys would miss key biosignature and anti-biosignature gases even for the few planets they can reach.
  • No currently selected mission or planned ground facility can assemble the required sample, so if the paper is right, answering whether Earth is unique requires building this mission.

Reading between the lines

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

  • An implication the authors leave implicit is that the two observation windows are complementary rather than rivals: oxygen is seen only in reflected light while methane and nitrous oxide appear only in the mid-infrared, so the strongest roadmap may be a staged sequence in which a reflected-light survey identifies candidate targets and the mid-infrared mission delivers the definitive biosignature s
  • The claimed retrieval accuracy for an Earth-twin (surface temperature within 5 K, pressure within 0.1 dex) could be validated before any mission flies by running the same retrieval pipeline on Earth itself, observed as a distant point source by a mid-infrared spectrograph.
  • The paper notes that most of its ~320 target stars have unmeasured exozodiacal dust levels and that southern-sky targets are not covered by current surveys; a ground-based survey of the southern stars could test the assumed dust background, since higher dust levels would eat into the predicted ~30 habitable-zone detections.
  • The sample-sizing logic for the null result transfers to any future technique that delivers tens of temperate terrestrial planets, meaning the statistical framework stands even if the specific interferometer architecture is superseded.
Share X Bluesky LinkedIn Reddit HN

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. This white paper argues that a large space-based mid-infrared nulling interferometer is the only currently conceived approach that can detect and spectroscopically characterize dozens of terrestrial exoplanets, addressing three questions: the prevalence of atmospheric biosignatures (Q1), the fraction of planets with conditions suitable for liquid water (Q2), and the diversity of terrestrial exoplanet atmospheres (Q3). It presents a spectral retrieval simulation of an Earth-twin observed at R=100 and SNR=20 over 3-30 micron; a statistical analysis of the power of a null result as a function of the number of characterized habitable-zone planets; an updated Monte Carlo yield simulation based on Kepler occurrence rates and a 320-star sample within 20 pc, predicting about 423 detectable planets and about 30 habitable-zone terrestrial planets; and a review of technology readiness and required developments. The central claim is that the MIR approach surpasses reflected-light alternatives and should be pursued as an ESA L-class mission.

Significance. If the quantitative yields and retrieval performance hold up, the proposed mission would provide the first statistically meaningful sample of terrestrial exoplanet atmospheres, enabling direct searches for biosignature gases (O3, CH4, N2O) and measurements of surface conditions. The paper is timely for the Voyage 2050 planning cycle and provides a useful synthesis of occurrence-rate statistics, retrieval methods, and interferometry technology status. Its strengths include the explicit use of external empirical benchmarks for planet occurrence and exozodi levels, the transparent acknowledgment that several key technologies are not yet space-qualified (Section 4.2), and a quantitative comparison with a reflected-light retrieval study. The principal weakness is the dependence of the central claims on extrapolated nulling performance and simplified statistical and retrieval models, which the paper does not yet subject to sensitivity analysis.

major comments (3)
  1. [Sections 1.2.3, 2.2, and 4.1] The simulated yield of about 423 detected planets and about 30 habitable-zone terrestrial planets (Figure 6) assumes a nulling interferometer with about 170 m baselines and about 2.5 m collectors that achieves a post-processed stellar leakage sufficient to detect an Earth-Sun contrast of about 1e-7 at 10 micron. The cited laboratory demonstrations do not cover this parameter range: Martin et al. (2012) report a null depth of 8e-6 at 10 micron with 10% bandwidth (with 1e-8 total suppression after post-processing), and the Adaptive Nuller reached 1e-5 at 34% bandwidth. Neither demonstrates the required chromatic null stability from 3-20 micron, cryogenic operation, or performance under the metrology and pointing errors of a free-flying multi-spacecraft configuration. The paper itself identifies cryogenic validation as future work (Section 4.2). Consequently the yield numbers, which are central to the paper's argument for a large mission, are extrapolations. To make the claim load-bearing, the authors should add a sensitivity analysis showing how the yield and the number of habitable-zone planets vary with nulling floor (e.g., 1e-6 vs 1e-5), instrument throughput, and exozodi level, or explicitly state that the yield estimates are upper bounds pending technology demonstration.
  2. [Section 1.2.1 and Figures 2-3] The retrieval study used to demonstrate the scientific potential of MIR spectra for Earth-twin characterization is not described in sufficient detail to be reproducible or to substantiate the claimed precision. Neither the atmospheric forward model, the retrieval algorithm, the noise model, nor the prior ranges for the free parameters (including the pressure-temperature profile) are specified. The conclusion that 'all parameters are well constrained' rests on a single simulation at R=100 and SNR=20 per resolution element over 3-30 micron; no tests of robustness to clouds, haze, or model uncertainty are presented. The comparison with the reflected-light retrievals of Feng et al. (2018) is also imperfect because the spectral coverage, resolution, and SNR definitions differ between the two studies. Since this comparison underpins the claim in the Abstract that the MIR approach surpasses other approaches, the retrieval analysis needs either additional methodological detail and robustness checks, or the claim should be softened to reflect the illustrative character of the simulation.
  3. [Section 1.2.2 and Figure 4] The statistical power analysis for a possible null result assumes that the 30 or 50 observed habitable-zone planets are an unbiased, independent sample from the population described by H0 and that the outcome 'provides conditions for liquid water' can be determined unambiguously for each planet. In practice, the detectability of a planet in the search phase depends on its radius, insolation, and distance, and the characterization of surface conditions from a MIR spectrum will carry systematic uncertainties. These selection effects and measurement errors would degrade the statistical power relative to the idealized calculation, so the statement that '30 planets is the minimum number needed' (Section 1.2.3) is an optimistic lower bound. Please add a caveat to that effect and, if possible, a simple simulation that incorporates selection effects.
minor comments (5)
  1. [Section 1.2.1 and Figure 2] The figure caption and text mention a spectral range of 3-30 micron, while the title and abstract emphasize 3-20 micron; please unify the wavelength range or explicitly state why the difference is negligible.
  2. [Figure 6] The left panel's color bar and the numbers inside the bins are not explained in the caption; please add a legend or note that numbers indicate expected detections per bin.
  3. [Section 4.1] The description of PRISMA and PROBA-3 could be clearer: the text states PRISMA demonstrated sub-cm positioning and PROBA-3 will achieve mm-level precision, but it does not explain whether the PROBA-3 requirement is for inter-satellite separation or line-of-sight jitter; this distinction matters for the nulling application.
  4. [References] There are several distinct Defrère et al. (2018) entries in the reference list; please disambiguate them in the text (e.g., Defrère et al. 2018a,b,c) and ensure each citation points to the correct paper.
  5. [Section 4.3] The citation 'Ertel et al. (in prep); Ertel et al., 2018' is unusual for a peer-reviewed paper; perhaps cite only Ertel et al. (2018) and mention that the HOSTS results include a future publication.

Circularity Check

0 steps flagged · score 2.0 of 10

No circular derivation: the MIR mission case rests on external benchmarks, with only non-load-bearing self-citations.

full rationale

The paper's central argument for a large MIR nulling interferometer is an extrapolation from external data and standard simulation tools, not a conclusion forced by its own inputs. The retrieval study (Section 1.2.1) uses a simulated Earth-twin spectrum as input and shows that the retrieved parameters recover the input values; this is a closed-loop self-consistency test of spectral information content, not an independent prediction, and its comparative value comes from the independent reflected-light retrieval of Feng et al. (2018). The yield estimate (Section 1.2.3) is an updated Monte Carlo simulation built on external Kepler/SAG13 occurrence rates, Dressing & Charbonneau (2015) M-star rates, a stellar sample from Crossfield (2013), and JWST/MIRI sensitivity limits with a stated throughput penalty; the roughly 400 total detections and about 30 habitable-zone planets are outputs of these assumptions, not fitted parameters relabeled as predictions. The technology case (Section 4.1) relies on external laboratory demonstrations (Martin et al. 2012; NASA 2009) and the PROBA-3 mission specifications. Self-citations do appear (Kammerer & Quanz 2018; Quanz et al. 2018; Defrere et al. 2018; Ertel et al. 2018; Linz et al. 2019), but the load-bearing inputs in each case are external measurements, standard methods, or mission facts; no uniqueness theorem or substantive conclusion is imported solely from the authors' prior work. Section 4.2 explicitly lists cryogenic nulling, spatial filters, and formation-flying integration as still requiring development, which is a feasibility caveat rather than a circular step. The 'unique scientific potential' conclusion is an argued synthesis from these external comparisons, not an equivalence with its own premises.

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

The quantitative claims in the white paper depend on several user-chosen parameters and on extrapolating Kepler occurrence rates and laboratory nulling performance to a space mission. No new physical entities are introduced.

free parameters (5)
  • Spectral resolution R = 100
    Chosen for the Earth-twin retrieval simulation to match comparable reflected-light studies; not a mission requirement.
  • Signal-to-noise ratio per resolution element = 20
    Assumed in the retrieval simulation; retrieval precision scales with this choice.
  • Nulling interferometer baseline = up to 170 m
    Assumed to achieve angular resolution to resolve an Earth-like planet at 10 pc; from earlier concept studies.
  • Instrument throughput relative to JWST/MIRI = 1/3.5
    Ad hoc degradation factor for interferometer losses in the yield simulation (Kammerer & Quanz 2018).
  • Integration time per target star in search phase = 35000 s
    Uniform observing time per star in the Monte Carlo yield simulation; total search phase under 3 years.
assumptions (5)
  • domain assumption Kepler occurrence statistics (SAG13) apply to the Solar neighborhood within 20 pc.
    The yield simulation assumes the radius and period distributions from NASA's SAG13 working group and Dressing & Charbonneau (2015) for M stars are valid for the 320 target stars.
  • domain assumption Planet fluxes follow black-body emission with randomly drawn Bond albedos.
    Used to estimate detectability in the yield simulation; real thermal phase curves and cloud effects are ignored.
  • domain assumption The Earth-twin model spectrum is representative of a habitable terrestrial exoplanet.
    The retrieval study uses an Earth model (Schwieterman et al. 2018) to benchmark what a mission must detect; real exoplanets may differ substantially.
  • domain assumption The nulling interferometer achieves the assumed sensitivity and null depth.
    Based on laboratory demonstrations (Martin et al. 2012) and expected PROBA-3 formation flying performance; not yet demonstrated at mission scale in space.
  • domain assumption Exozodiacal dust levels follow the HOSTS survey distribution for Sun-like stars.
    High dust levels could increase background noise and lengthen the search phase; median 4.5x solar is assumed for most stars.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Atmospheric characterization of terrestrial exoplanets in the mid-infrared: biosignatures, habitability & diversity." pith.science (2026). https://pith.science/paper/IKY76AEI

@misc{pith2026190801316,
  author       = {Pith},
  title        = {Pith review of: Atmospheric characterization of terrestrial exoplanets in the mid-infrared: biosignatures, habitability & diversity},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/IKY76AEI}},
  note         = {Machine review of arXiv:1908.01316}
}
read the original abstract

Exoplanet science is one of the most thriving fields of modern astrophysics. A major goal is the atmospheric characterization of dozens of small, terrestrial exoplanets in order to search for signatures in their atmospheres that indicate biological activity, assess their ability to provide conditions for life as we know it, and investigate their expected atmospheric diversity. None of the currently adopted projects or missions, from ground or in space, can address these goals. In this White Paper we argue that a large space-based mission designed to detect and investigate thermal emission spectra of terrestrial exoplanets in the MIR wavelength range provides unique scientific potential to address these goals and surpasses the capabilities of other approaches. While NASA might be focusing on large missions that aim to detect terrestrial planets in reflected light, ESA has the opportunity to take leadership and spearhead the development of a large MIR exoplanet mission within the scope of the "Voyage 2050" long-term plan establishing Europe at the forefront of exoplanet science for decades to come. Given the ambitious science goals of such a mission, additional international partners might be interested in participating and contributing to a roadmap that, in the long run, leads to a successful implementation. A new, dedicated development program funded by ESA to help reduce development and implementation cost and further push some of the required key technologies would be a first important step in this direction. Ultimately, a large MIR exoplanet imaging mission will be needed to help answer one of mankind's most fundamental questions: "How unique is our Earth?"

Figures

Figures reproduced from arXiv: 1908.01316 by the authors.

Figure 1
Figure 1. Molecules relevant to terrestrial planet characterization between 3-20 [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Results of a retrieval study of an Earth-twin atmosphere observed over a wavelength range [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Comparing the retrieval results for the simulated thermal emission spectrum shown in Fig [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: The statistical power of a null-result: in case 30 (blue curve) or 50 (red curve) exoplanets [PITH_FULL_IMAGE:figures/full_fig_p009_4.png]
Figure 5
Figure 5. Figure 5: All known GKM main-sequence stars within 15 pc from the Sun as a function of their [PITH_FULL_IMAGE:figures/full_fig_p010_5.png]
Figure 6
Figure 6. Figure 6: Estimated exoplanet yield in a hypothetical 3-year search phase for a space-based MIR [PITH_FULL_IMAGE:figures/full_fig_p011_6.png]
Figure 7
Figure 7. Figure 7: Adopted space missions related to exoplanet science from ESA. Image credit: ESA; [PITH_FULL_IMAGE:figures/full_fig_p016_7.png]
Figure 8
Figure 8. Figure 8: Space missions related to exoplanet science from NASA including potential future mis [PITH_FULL_IMAGE:figures/full_fig_p017_8.png]
Figure 9
Figure 9. Figure 9: Left: 6-hour measurement of the null-depth achieved at 10 [PITH_FULL_IMAGE:figures/full_fig_p018_9.png]
Figure 10
Figure 10. Figure 10: All known exoplanets and two additional yet unpublished candidates from the CARMENES [PITH_FULL_IMAGE:figures/full_fig_p020_10.png]

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Characterizing the oxidation state of rocky exoplanets with the Large Interferometer for Exoplanets (LIFE)

    astro-ph.EP 2026-07 conditional novelty 5.5 of 10

    LIFE baseline mid-IR observations of Earth-sized planets at 10 pc can retrieve CO2, CH4, and NH3 well enough to distinguish mantle redox states from IW-6 to IW+6 under the paper's modeling assumptions.

Reference graph

Works this paper leans on

67 extracted references · 43 canonical work pages · cited by 1 Pith paper

  1. [1]

    P., Abbott, R., Abbott, T

    Abbott, B. P., Abbott, R., Abbott, T. D., et al. 2016, Phys. Rev. Lett., 116, 061102

    2016

  2. [2]

    2006, A&A, 448, 787 Anglada-Escud´ e, G., Amado, P

    Absil, O., den Hartog, R., Gondoin, P., et al. 2006, A&A, 448, 787 Anglada-Escud´ e, G., Amado, P. J., Barnes, J., et al. 2016, Nature, 536, 1

    work page 2006

  3. [3]

    2012, in 35th Annual AAS Guidance and Control Confer- ence Bonfils, X., Delfosse, X., Udry, S., et al

    Bodin, P., Noteborn, R., Larsson, R., et al. 2012, in 35th Annual AAS Guidance and Control Confer- ence Bonfils, X., Delfosse, X., Udry, S., et al. 2013, A&A, 549, A109

    work page 2012

  4. [4]

    J., Christiansen, J

    Burke, C. J., Christiansen, J. L., Mullally, F., et al. 2015, ApJ, 809, 8

    work page 2015

  5. [5]

    P., et al

    Cassan, A., Kubas, D., Beaulieu, J. P., et al. 2012, Nature, 481, 167

    2012

  6. [6]

    C., Krissansen-Totton, J., Kiang, N

    Catling, D. C., Krissansen-Totton, J., Kiang, N. Y., et al. 2018, Astrobiology, 18, 709

    work page 2018

  7. [7]

    2017, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Cessa, V., Beck, T., Benz, W., et al. 2017, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10563, SPIE, 105631L

    work page 2017

  8. [8]

    2017, The Astrophysical Journal, 834, 17

    Chen, J., & Kipping, D. 2017, The Astrophysical Journal, 834, 17

    work page 2017

Show all 67 references
  1. [9]

    S., Herbst, T., L´ eger, A., et al

    Cockell, C. S., Herbst, T., L´ eger, A., et al. 2009, Experimental Astronomy, 23, 435

    2009

  2. [10]

    L., Mullally, F., Thompson, S

    Coughlin, J. L., Mullally, F., Thompson, S. E., et al. 2016, The Astrophysical Journal Supplement Series, 224, 12 Crossfield, I. J. M. 2013, Astronomy & Astrophysics, 551, A99 de Wit, J., Wakeford, H. R., Lewis, N. K., et al. 2018, Nature Astronomy, 2, 214 Defr` ere, D., Absil,...

    2016

  3. [11]

    D., & Charbonneau, D

    Dressing, C. D., & Charbonneau, D. 2015, The Astrophysical Journal, 807, 45

    2015

  4. [12]

    2018, AJ, 155, 194 Event Horizon Telescope Collaboration, Akiyama, K., Alberdi, A., et al

    Ertel, S., Defr` ere, D., Hinz, P., et al. 2018, AJ, 155, 194 Event Horizon Telescope Collaboration, Akiyama, K., Alberdi, A., et al. 2019, ApJ, 875, L1

    2018

  5. [13]

    K., Robinson, T

    Feng, Y. K., Robinson, T. D., Fortney, J. J., et al. 2018, The Astronomical Journal, 155, 200

    2018

  6. [14]

    J., McMurtry, C

    Forrest, W. J., McMurtry, C. W., Dorn, M., Pipher, J., & Cabrera, M. S. 2016, in AAS/Division for Planetary Sciences Meeting Abstracts #48, AAS/Division for Planetary Sciences Meeting Abstracts, 123.59

    2016

  7. [15]

    L., Stock, J

    Gebauer, S., Grenfell, J. L., Stock, J. W., et al. 2017, Astrobiology, 17, 27

    2017

  8. [16]

    Gillon, M., Triaud, A. H. M. J., Demory, B.-O., et al. 2017, Nature, 542, 456

    2017

  9. [17]

    H., Bauwens, E., et al

    Glasse, A., Rieke, G. H., Bauwens, E., et al. 2015, PASP, 127, 686 Gravity Collaboration, Lacour, S., Nowak, M., et al. 2019, A&A, 623, L11

    2015

  10. [18]

    P., Line, M

    Greene, T. P., Line, M. R., Montero, C., et al. 2016, ApJ, 817, 17

    2016

  11. [19]

    Gretzinger, T., Gross, S., Arriola, A., & Withford, M. J. 2019, Opt. Express, 27, 8626

    2019

  12. [20]

    2011, ApJ, 729, 110

    Hanot, C., Mennesson, B., Martin, S., et al. 2011, ApJ, 729, 110

    2011

  13. [21]

    2013, Astronomy & Astrophysics, 553, A9

    Hedelt, P., von Paris, P., Godolt, M., et al. 2013, Astronomy & Astrophysics, 553, A9

    2013

  14. [22]

    C., Ford, E

    Hsu, D. C., Ford, E. B., Ragozzine, D., & Ashby, K. 2019, arXiv e-prints, arXiv:1902.01417

    2019 arXiv

  15. [23]

    2010, MNRAS, 408, 514

    Janson, M. 2010, MNRAS, 408, 514

    2010

  16. [24]

    2017, Annual Review of Astronomy and Astrophysics, 55, 433

    Kaltenegger, L. 2017, Annual Review of Astronomy and Astrophysics, 55, 433

    2017

  17. [25]

    Kammerer, J., & Quanz, S. P. 2018, A&A, 609, A4

    2018

  18. [26]

    Kitzmann, D., Patzer, A. B. C., von Paris, P., Godolt, M., & Rauer, H. 2011, A&A, 531, A62

    2011

  19. [27]

    Kitzmann, D., Patzer, A. B. C., von Paris, P., et al. 2010, A&A, 511, A66

    2010

  20. [28]

    K., Ramirez, R., Kasting, J

    Kopparapu, R. K., Ramirez, R., Kasting, J. F., et al. 2013, ApJ, 765, 131

    2013

  21. [29]

    k., H´ ebrard, E., Belikov, R., et al

    Kopparapu, R. k., H´ ebrard, E., Belikov, R., et al. 2018, The Astrophysical Journal, 856, 122

    2018

  22. [30]

    L., Ireland, M

    Kraus, A. L., Ireland, M. J., Huber, D., Mann, A. W., & Dupuy, T. J. 2016, AJ, 152, 8

    2016

  23. [31]

    2016, ApJ, 832, L12 20 Atmospheric characterization of terrestrial exoplanets in the MIR: biosignatures, habitability & diversity

    Kreidberg, L., & Loeb, A. 2016, ApJ, 832, L12 20 Atmospheric characterization of terrestrial exoplanets in the MIR: biosignatures, habitability & diversity

    2016

  24. [32]

    L., D´ esert, J.-M., et al

    Kreidberg, L., Bean, J. L., D´ esert, J.-M., et al. 2014, Nature, 505, 69

    2014

  25. [33]

    Labadie, L., Minardi, S., Mart´ ın, G., & Thomson, R. R. 2018, Experimental Astronomy, 46, 433

    2018

  26. [34]

    2013, A&A, 554, A69

    Leconte, J., Forget, F., Charnay, B., et al. 2013, A&A, 554, A69

    2013

  27. [35]

    2015, Experimental Astronomy, 40, 449 L´ eger, A., Defr` ere, D., Garcia Munoz, A., et al

    Leconte, J., Forget, F., & Lammer, H. 2015, Experimental Astronomy, 40, 449 L´ eger, A., Defr` ere, D., Garcia Munoz, A., et al. 2019, Astrobiology, 19, 797

    2015

  28. [36]

    2019, arXiv e-prints, arXiv:1907.07989 L´ opez-Morales, M., Ben-Ami, S., Gonzalez-Abad, G., et al

    Linz, H., Bhatia, D., Buinhas, L., et al. 2019, arXiv e-prints, arXiv:1907.07989 L´ opez-Morales, M., Ben-Ami, S., Gonzalez-Abad, G., et al. 2019, AJ, 158, 24

    2019 arXiv

  29. [37]

    2017, A&A, 599, A16

    Lovis, C., Snellen, I., Mouillet, D., et al. 2017, A&A, 599, A16

    2017

  30. [38]

    S., Mendoza, G

    Lustig-Yaeger, J., Meadows, V. S., Mendoza, G. T., et al. 2018, The Astronomical Journal, 156, 301

    2018

  31. [39]

    2018, Handbook of Exoplanets, ISBN 978-3-319-55332-0

    Madhusudhan, N. 2018, Handbook of Exoplanets, ISBN 978-3-319-55332-0. Springer International Publishing AG, part of Springer Nature, 2018, id.104, 104

    2018

  32. [40]

    2012, Appl

    Martin, S., Booth, A., Liewer, K., et al. 2012, Appl. Opt., 51, 3907

    2012

  33. [41]

    1995, Nature, 378, 355

    Mayor, M., & Queloz, D. 1995, Nature, 378, 355

    1995

  34. [42]

    2011, arXiv.org, arXiv:1109.2497

    Mayor, M., Marmier, M., Lovis, C., et al. 2011, arXiv.org, arXiv:1109.2497

    2011 arXiv

  35. [43]

    S., Reinhard, C

    Meadows, V. S., Reinhard, C. T., Arney, G. N., et al. 2018, Astrobiology, 18, 630

    2018

  36. [44]

    V., Kreidberg, L., Rustamkulov, Z., Robinson, T., & Fortney, J

    Morley, C. V., Kreidberg, L., Rustamkulov, Z., Robinson, T., & Fortney, J. J. 2017, ApJ, 850, 121 NASA. 2009, Exoplanet Interferometry Technology Milestone #3 Report Broadband Starlight Sup- pression Demonstration, Tech. rep

    2017

  37. [45]

    L., De Rosa, R

    Nielsen, E. L., De Rosa, R. J., Macintosh, B., et al. 2019, AJ, 158, 13

    2019

  38. [46]

    P., Crossfield, I., Meyer, M

    Quanz, S. P., Crossfield, I., Meyer, M. R., Schmalzl, E., & Held, J. 2015, International Journal of Astrobiology, 14, 279

    2015

  39. [47]

    P., Kammerer, J., Defr` ere, D., et al

    Quanz, S. P., Kammerer, J., Defr` ere, D., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10701, Optical and Infrared Interferometry and Imaging VI, 107011I

    2018

  40. [48]

    2014, Experimental Astronomy, 38, 249

    Rauer, H., Catala, C., Aerts, C., et al. 2014, Experimental Astronomy, 38, 249

    2014

  41. [49]

    Rogers, L. A. 2015, The Astrophysical Journal, 801, 41

    2015

  42. [50]

    M., et al

    Sampaolo, A., Patimisco, P., Kriesel, J. M., et al. 2015, Opt. Express, 23, 195

    2015

  43. [51]

    W., Robinson, T

    Schwieterman, E. W., Robinson, T. D., Meadows, V. S., Misra, A., & Domagal-Goldman, S. 2015, The Astrophysical Journal, 810, 57

    2015

  44. [52]

    W., Kiang, N

    Schwieterman, E. W., Kiang, N. Y., Parenteau, M. N., et al. 2018, Astrobiology, 18, 663

    2018

  45. [53]

    2013, ApJ, 777, 95

    Seager, S., Bains, W., & Hu, R. 2013, ApJ, 777, 95

    2013

  46. [54]

    2010, Annual Review of Astronomy and Astrophysics, 48, 631

    Seager, S., & Deming, D. 2010, Annual Review of Astronomy and Astrophysics, 48, 631

    2010

  47. [55]

    L., Schafer, J., & Ford, E

    Seager, S., Turner, E. L., Schafer, J., & Ford, E. B. 2005, Astrobiology, 5, 372

    2005

  48. [56]

    K., Fortney, J

    Sing, D. K., Fortney, J. J., Nikolov, N., et al. 2016, Nature, 529, 59

    2016

  49. [57]

    L., et al

    Snellen, I., de Kok, R., Birkby, J. L., et al. 2015, A&A, 576, A59

    2015

  50. [58]

    2018, Handbook of Exoplanets, ISBN 978-3-319-55332-0

    Sozzetti, A., & de Bruijne, J. 2018, Handbook of Exoplanets, ISBN 978-3-319-55332-0. Springer In- ternational Publishing AG, part of Springer Nature, 2018, id.81, 81

    2018

  51. [59]

    C., Roberge, A., Mandell, A., & Robinson, T

    Stark, C. C., Roberge, A., Mandell, A., & Robinson, T. D. 2014, ApJ, 795, 122

    2014

  52. [60]

    2017, Appl

    Takahashi, A., Enya, K., Haze, K., et al. 2017, Appl. Opt., 56, 6694

    2017

  53. [61]

    2017, A&A, 602, A66

    Tepper, J., Labadie, L., Diener, R., et al. 2017, A&A, 602, A66

    2017

  54. [62]

    2018, Experimental Astronomy, 46, 135 von Paris, P., Hedelt, P., Selsis, F., Schreier, F., & Trautmann, T

    Tinetti, G., Drossart, P., Eccleston, P., et al. 2018, Experimental Astronomy, 46, 135 von Paris, P., Hedelt, P., Selsis, F., Schreier, F., & Trautmann, T. 2013, Astronomy & Astrophysics, 551, A120

    2018

  55. [63]

    M., Marcy, G

    Weiss, L. M., Marcy, G. W., Petigura, E. A., et al. 2018, AJ, 155, 48

    2018

  56. [64]

    A., & Ford, E

    Wolfgang, A., Rogers, L. A., & Ford, E. B. 2016, The Astrophysical Journal, 825, 19

    2016

  57. [65]

    J., & Knight, J

    Yu, F., Wadsworth, W. J., & Knight, J. C. 2012, Opt. Express, 20, 11153

    2012

  58. [66]

    2017, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Zamkotsian, F., Lanzoni, P., Barette, R., et al. 2017, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10116, SPIE, 101160M

    2017

  59. [67]

    Zsom, A., Seager, S., de Wit, J., & Stamenkovi´ c, V. 2013, ApJ, 778, 109 21 Atmospheric characterization of terrestrial exoplanets in the MIR: biosignatures, habitability & diversity Team of co-authors and supporters (in alphabetic order) Name Affiliation Country Email Olivier ...

    2013

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.