Pith. sign in

REVIEW 4 major objections 4 minor 2 cited by

Combined analysis of the 12.8 and 15 $\mu m$ JWST/MIRI eclipse observations of TRAPPIST-1 b

T0 review · 4 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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

Pith's one-line read Ten JWST eclipses of TRAPPIST-1 b yield two brightness temperatures that fit both a bare ultramafic rock and a hazy CO2 atmosphere, with a phase curve predicted to break the tie.

desk verdict A robust new eclipse-depth measurement for TRAPPIST-1 b, with an interpretation that is more fragile than the paper's two-scenario framing suggests. read the letter →

arxiv 2412.11627 v1 pith:3VY2YNKH submitted 2024-12-16 astro-ph.EP

Elsa Ducrot , Pierre-Olivier Lagage , Michiel Min , Michael Gillon , Taylor J. Bell , Pascal Tremblin , Thomas Greene , Achrene Dyrek
show 31 more authors
Jeroen Bouwman Rens Waters Manuel Gudel Thomas Henning Bart Vandenbussche Olivier Absil David Barrado Anthony Boccaletti Alain Coulais Leen Decin Billy Edwards Rene Gastaud Alistair Glasse Sarah Kendrew Goran Olofsson Polychronis Patapis John Pye Daniel Rouan Niall Whiteford Ioannis Argyriou Christophe Cossou Adrian M. Glauser Oliver Krause Fred Lahuis Pierre Royer Silvia Scheithauer Luis Colina Ewine F. van Dishoeck Goran Ostlin Tom P. Ray Gillian Wright
This is my paper · ORCID
classification astro-ph.EP
keywords secondaryeclipsephotometryTRAPPIST-1bJWSTMIRIthermalemissionbarerockyexoplanetCO2atmospherephotochemicalhazeinversion
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

TRAPPIST-1 b, an Earth-sized rocky planet around an ultra-cool dwarf, was observed in ten secondary eclipses with JWST/MIRI: five in a 12.8 µm filter and five in a 15 µm filter. Combining all ten, the paper measures planet-to-star flux ratios of 452 ± 86 ppm at 12.8 µm and 775 ± 90 ppm at 15 µm, corresponding to brightness temperatures of 424 ± 28 K and 478 ± 27 K. The two bands were chosen to straddle the CO2 absorption feature, but the data do not select a single story: they are consistent either with an airless planet whose surface is fresh, unweathered ultramafic rock, or with a thick, pure-CO2 atmosphere containing photochemical hazes that create an upper-atmosphere temperature inversion and make CO2 emit rather than absorb. The paper shows that two very different worlds can produce the same two broadband measurements, and argues that a forthcoming phase curve should distinguish them.

What carries the argument

The argument runs on the spectral contrast between the two MIRI filters, F1280W (11.6–14.2 µm) and F1500W (13.5–16.6 µm), centered inside and outside the 15 µm CO2 band. On one side, a grid of radiative-convective surface models (basaltic, ultramafic, feldspathic, metal-rich, Fe-oxidized, granitoid) predicts band-integrated eclipse depths; the ultramafic composition (60% olivine, 40% enstatite) matches the observed ratio, while space-weathering expectations make a young surface plausible. On the other, a 1D radiative-transfer retrieval that mixes hydrocarbon haze particles (50 nm particles with optEC(s) optical properties) into a pure-CO2 atmosphere produces a temperature inversion that flips the CO2 feature from absorption to emission, and the same haze abundance also fits the NIRISS transmission spectrum. The proposed discriminator is heat redistribution: the airless model has essentially no nightside flux, whereas the hazy atmosphere redistributes a large fraction of absorbed stellar energy, so the predicted 15 µm phase curve differs sharply between the two cases.

What would settle it

A single 15 µm phase curve (the planned GO 3077 observations) would settle the matter: the airless ultramafic model predicts an almost vanishing nightside flux and a symmetric eclipse (night-to-day flux near zero), whereas the 10-bar hazy CO2 model predicts a night-to-day ratio of 0.85 and a phase-curve offset; if the measured nightside flux is near zero, the hazy-atmosphere scenario is ruled out.

Watch

Extended reading notes

Core claim

The central claim is that the 12.8 µm and 15 µm eclipse depths of TRAPPIST-1 b, analyzed together for the first time, are each individually consistent with more than one physical picture. The authors establish that the brightness temperature at 12.8 µm (424 ± 28 K) is 2.1σ lower than expected for a dark bare rock, implying a Bond albedo of 0.19 ± 0.08. They then show that a bare, geologically fresh ultramafic surface fits the two eclipse depths, and that a hazy CO2-dominated atmosphere with a thermal inversion also fits, producing CO2 in emission at 15 µm. The paper's conclusion is that this two-scenario degeneracy cannot be resolved with only two broadband points, and that the heat-redistribution signal expected from phase-curve observations will tell an airless world apart from a hazy, heat-redistributing atmosphere.

Load-bearing premise

The hazy CO2 scenario depends on photochemical hazes forming and surviving in a hot, CO2-dominated atmosphere via roughly 1% H2S from volcanism, and the paper admits it is unclear whether such H2S abundances can be maintained, so if hazes cannot form the two-scenario conclusion reduces to a bare-surface interpretation.

Editorial extensions

If this is right

  • A single pair of broadband eclipse depths cannot by itself determine whether TRAPPIST-1 b is airless or has a thick atmosphere; the paper predicts that the upcoming 15 µm phase curve (program GO 3077) will separate the two.
  • If the airless interpretation is correct, the surface must be relatively reflective (Bond albedo 0.19 ± 0.08) and geologically fresh ultramafic rock, implying recent volcanic or tectonic resurfacing on a tidally and induction-heated world.
  • If the hazy atmosphere interpretation is correct, hazes produce a strong thermal inversion that makes the 15 µm CO2 band appear in emission, and the needed haze formation pathway depends on volcanic H2S at roughly the 1% level.
  • The 12.8 µm brightness temperature is 2.1σ lower than the null-albedo bare-rock prediction, so neither a dark blackbody nor a simple greenhouse atmosphere matches; both scenarios require a departure from the simplest expectations.
  • The joint fit of all ten eclipses confirms the earlier 15 µm detection at the 1σ level while tightening the eclipse depth, and statistical tests find no significant eclipse-depth variability at 12.8 µm.

Reading between the lines

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

  • The authors stop short of saying so, but the same degeneracy should affect other emission-photometry surveys of rocky M-dwarf planets: any two broadband points can be matched by some surface composition or some haze-affected atmosphere, so phase curves or resolved spectra will be needed before claiming an airless or atmospheric detection.
  • If the fresh ultramafic surface is the right answer, TRAPPIST-1 b would join Io as a volcanically resurfaced world; a testable corollary is that eclipse depth at 12.8 µm could vary on resurfacing timescales, which is exactly the currently insignificant variability hinted at in the five individual eclipses.
  • The haze path could be checked before more telescope time is spent: laboratory or photochemical-model experiments scanning H2S abundance, CO2/O2 ratio, and TRAPPIST-1-like XUV flux would show whether the required 1% H2S and the resulting haze column are realistic, putting a prior on which of the two scenarios to prefer.
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

4 major / 4 minor

Summary. The paper presents five new JWST/MIRI secondary-eclipse observations of TRAPPIST-1 b at 12.8 µm, combined with a re-analysis of five previously observed eclipses at 15 µm. A global fit of all ten eclipses yields eclipse depths of 452 ± 86 ppm at 12.8 µm and 775 ± 90 ppm at 15 µm, corresponding to brightness temperatures of 424 ± 28 K and 478 ± 27 K. The authors then explore two model interpretations: an airless ultramafic surface with a fitted Bond albedo of 0.19 ± 0.08, and a thick, pure-CO2 atmosphere with photochemical hazes producing a thermal inversion. They argue that both scenarios fit the data and that future phase-curve observations can distinguish them.

Significance. The central measurement is a genuine advance: four independent reductions and four distinct analysis methods give mutually consistent eclipse depths, and the data and source products are archived. The 12.8 µm measurement in particular provides a key constraint inside the CO2 band and reveals a possible tension with the previously favored null-albedo bare-rock interpretation. If the two-scenario conclusion holds, the paper will be an important benchmark for broadband emission studies of rocky exoplanets. However, the interpretation stage is less secure: both the Bond-albedo fit and the hazy-CO2 retrieval use the NIRISS/SOSS transmission spectrum as a joint constraint, even though the paper itself argues that this spectrum is strongly contaminated by the transit light source effect. The citation for the haze optical properties is also incorrect. The measurement should stand, but the interpretive claims need strengthening before publication.

major comments (4)
  1. [Methods, '1D atmosphere with full heat redistribution'; Section 1.1] The hazy-CO2 retrieval (fhaze = 4.5×10−4, Eg, Rp) uses the NIRISS/SOSS transmission spectrum of ref. 51 as a constraint, even though Section 1.1 argues that this spectrum is strongly contaminated by the transit light source effect. Because the transmission spectrum is used to fit the same model parameters that then produce the claimed good fit to the eclipse depths, the atmospheric scenario is not an independent MIRI-only result. Please re-run the retrieval using only the two MIRI eclipse depths (or a TLS-marginalized treatment of the NIRISS data) and report whether the hazy-CO2 solution survives; if it does not, the 'two main scenarios' conclusion must be revised to a single preferred scenario.
  2. [Methods, 'Bare surfaces'] The quoted Bond albedo Ab = 0.19 ± 0.08 is derived from a joint fit to both the MIRI eclipse depths and the NIRISS transmission spectrum. This is circular with respect to the claim that the airless model fits the MIRI data well: the albedo is adjusted to match the eclipse depths rather than predicted from them. The only MIRI-only model comparison in the paper is the reduced-χ² table for the fixed surface-composition models (Supplementary Table 1), which does not constrain Ab. Please separate the MIRI-only albedo constraint from the joint-fit value and quantify how the TLS-contaminated transmission spectrum affects Ab.
  3. [Methods, 'Atmospheric models'] Reference 53 is Jones et al. (2013), 'An advanced scattered moonlight model for Cerro Paranal,' which does not contain the optEC(s) hydrocarbon haze optical properties used for the haze opacity. The correct source for these optical constants must be identified and cited, or the constants provided as supplementary data; without this, the thermal inversion calculation is not reproducible.
  4. [Discussion, third paragraph] The statement that the hazy-CO2 model 'can fit the measurements very well' is not supported by a quantitative goodness-of-fit or model-comparison statistic for the atmospheric model. Please provide a chi-squared, Bayesian evidence, or equivalent for the atmospheric scenario against the MIRI data, alongside the existing bare-surface χ²_r values.
minor comments (4)
  1. [Methods, 'Bare surfaces', Eq. (1)] Equation (1) integrates cosθ cosφ dθ dφ with θ defined as longitude and φ as latitude; this appears to contain an extra geometric factor or a missing area element. Please check the projection and area element and correct the equation or the coordinate definitions, as it affects the computed blackbody flux.
  2. [Figure 2 caption] The caption says the measurements are 'compared to realistic emission models for bare surface models,' but the right-hand panel of the figure contains atmospheric models; please make the caption consistent with the two panels.
  3. [Methods, 'Data Reduction: POL'] The text contains broken variable names such as 'Nf rames' and 'aper-ima'; these should be formatted correctly for readability.
  4. [Methods, 'Data Reduction: ED'] There are several typographical errors, e.g., 'fist and last groups' and 'four the four others'; please proofread the Methods section.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the eclipse depths are independent measurements and the model agreements are presented as fits, not as predictions.

full rationale

The eclipse depths are derived from four independent reductions and multiple light-curve fitting methods (Eureka!, trafit, Eureka!/dynesty, POL), and the final values 452 ± 86 ppm and 775 ± 90 ppm are measurements, not outputs of the surface or atmospheric models. The Bond-albedo value AB = 0.19 ± 0.08 is obtained by an explicitly described Bayesian fit of the blackbody-sum model to the MIRI eclipse depths and the NIRISS/SOSS transmission spectrum, and the paper presents it as a best-fit parameter, not as a prediction from first principles. Likewise, the hazy-CO2 retrieval has three free parameters (Rp, fhaze, Eg) fitted to the MIRI eclipses plus the NIRISS spectrum; the sentence 'our model can fit the measurements very well' is a report of that fit, not an out-of-sample prediction, so no fitted parameter is renamed as a prediction. The only forward-looking statement is the phase-curve prediction for GO 3077, which is genuinely independent of the eclipse data used to condition the models. Self-citations (Greene et al. 2023, Eureka!, ARCiS, trafit, Ducrot et al. 2020) are code, method, or prior-measurement citations and are not used as load-bearing uniqueness arguments. Concerns about using the stellar-contaminated NIRISS/SOSS spectrum as a retrieval constraint, and the erroneous citation of ref. 53 for haze optical properties, are data-quality and correctness issues and do not make the derivation circular by construction. Hence no circular step meeting the required evidentiary bar is present.

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

The central measurements are empirical, but the interpretation relies on several fitted parameters and domain assumptions. The Bond albedo and the haze retrieval parameters are fit to the same data they are used to explain, and the models assume specific surface and atmospheric physics. No new physical entities are introduced.

free parameters (4)
  • Bond albedo AB (bare rock model) = 0.19 ± 0.08
    Fit to the two MIRI eclipse depths and NIRISS transmission spectrum in the sum-of-blackbodies airless model.
  • Haze mass fraction fhaze = 4.5e-4 (median)
    Free parameter in the hazy CO2 atmospheric retrieval, constrained by MIRI eclipses and NIRISS transmission spectrum.
  • Hydrocarbon band gap Eg = posterior median, not quoted in text
    Free parameter in the optEC(s) haze model retrieval.
  • Planet radius Rp = 1.12 Rearth (median from corner plot)
    Free parameter in the atmospheric retrieval, though constrained by transits.
assumptions (4)
  • domain assumption SPHINX stellar spectrum with a ~7% correction represents TRAPPIST-1's SED for flux calibration.
    Used to convert eclipse depths to brightness temperatures and to set model bandpass fluxes; the correction is derived from matching the model to measured stellar fluxes, so it is partly empirical.
  • domain assumption The NIRISS/SOSS transmission spectrum (ref 51) can be used as a retrieval constraint despite stellar contamination reported for the same dataset (ref 19).
    The retrieval fits the transmission spectrum; if the contamination is significant, the retrieved haze parameters could be biased. This assumption is not flagged in the atmospheric modeling section.
  • domain assumption Zero heat redistribution on the dayside for the bare rock model.
    The blackbody sum model sets nightside to 45 K and assumes no heat transport; the alternative hazy model assumes a redistribution factor of 0.25.
  • domain assumption Haze particles are 50 nm spheres, uniformly mixed through the atmosphere, and follow the optEC(s) optical properties.
    The 50 nm size is based on laboratory haze from CO2; uniform mixing is a simplification. The paper acknowledges that more realistic layered haze models are needed.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Combined analysis of the 12.8 and 15 $\mu m$ JWST/MIRI eclipse observations of TRAPPIST-1 b." pith.science (2026). https://pith.science/paper/3VY2YNKH

@misc{pith2026241211627,
  author       = {Pith},
  title        = {Pith review of: Combined analysis of the 12.8 and 15 $\mu m$ JWST/MIRI eclipse observations of TRAPPIST-1 b},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/3VY2YNKH}},
  note         = {Machine review of arXiv:2412.11627}
}
abstract

The first JWST/MIRI photometric observations of TRAPPIST-1 b allowed for the detection of the thermal emission of the planet at 15 $\mu m$, suggesting that the planet could be a bare rock with a zero albedo and no redistribution of heat. These observations at 15 $\mu m$ were acquired as part of GTO time that included a twin program at 12.8 $\mu m$ in order to have a measurement in and outside the CO$_2$ absorption band. Here we present five new occultations of TRAPPIST-1 b observed with MIRI in an additional photometric band at 12.8 $\mu m$. We perform a global fit of the 10 eclipses and derive a planet-to-star flux ratio and 1-$\sigma$ error of 452 $\pm$ 86 ppm and 775 $\pm$ 90 ppm at 12.8 $\mu m$ and 15 $\mu m$, respectively. We find that two main scenarios emerge. An airless planet model with an unweathered (fresh) ultramafic surface, that could be indicative of relatively recent geological processes fits well the data. Alternatively, a thick, pure-CO2 atmosphere with photochemical hazes that create a temperature inversion and result in the CO2 feature being seen in emission also works, although with some caveats. Our results highlight the challenges in accurately determining a planet's atmospheric or surface nature solely from broadband filter measurements of its emission, but also point towards two very interesting scenarios that will be further investigated with the forthcoming phase curve of TRAPPIST-1 b.

Figures

Figures reproduced from arXiv: 2412.11627 by the authors.

Figure 1
Figure 1. Phase folded JWST/MIRI observations of TRAPPIST-1 b. a. Phase-folded light curve of the secondary eclipse of TRAPPIST-1 b at 12.8 µm, derived from the observations of 5 eclipses as part of GTO 1279 observations. b. Phase-folded light curve of the secondary eclipse of TRAPPIST-1 b at 15 µm, derived from re-analyses of the observations of 5 eclipses as part of GTO 1177. These figures are derived from the “fiducial ana… view at source ↗
Figure 2
Figure 2. TRAPPIST-1 b’s emission spectrum compared to bare-surface models. O2-rich atmosphere 100 bar Measurements of the eclipse depth of TRAPPIST-1 b in the 12.8 µm and 15 µm bands resulting from 5 visits in each band with their 1σ uncertainties from our “fiducial” joint analysis (MCMC analysis detailed in the Methods section), compared to realistic emission models for bare surface models from ref. 25 . The measurements ar… view at source ↗
Figure 3
Figure 3. Best fit atmosphere model: an hazy-CO2-rich atmosphere. Eclipse spectrum (a.) and temperature structure (b.) for the haze atmosphere models. Model calculations are shown for haze mass fractions (fhaze = 4.5E-4, fhaze =4.5E-5, fhaze =4.5E-7) as well as for our best-fit solution (blue line) and its 1σ uncertainty interval (blue contour). On panel a., the MIRI observations, re￾sulting from 5 visits in each bands, are s… view at source ↗

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 2 Pith papers

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

  1. Interior redox state effects on the stability of secondary atmospheres and observational manifestations: LP 791-18 d as a case study for outgassing rocky exoplanets

    astro-ph.EP 2025-06 conditional novelty 6.0 of 10

    LP 791-18d's outgassed atmosphere is stable only for highly oxidized interiors (fO2-IW greater than about 2); reduced interiors lose their volatiles to hydrodynamic escape within the planet's lifetime.

  2. Stellar Contamination Correction Using Back-to-Back Transits of TRAPPIST-1 b and c

    astro-ph.EP 2024-12 conditional novelty 6.0 of 10

    Back-to-back transits of TRAPPIST-1 b and c allow an observed, model-free correction of stellar contamination in planet c's spectrum, reducing structured noise 2.5x below 2 micrometers.

Reference graph

Works this paper leans on

70 extracted references · 44 canonical work pages · cited by 2 Pith papers

  1. [1]

    D., Beichman, C

    Kirkpatrick, J. D., Beichman, C. A. & Skrutskie, M. F. The Coolest Isolated M Dwarf and Other 2MASS Discoveries. Astrophys. J. 476, 311–318 (1997). URL http://adsabs. harvard.edu/abs/1997ApJ...476..311K

    work page 1997

  2. [2]

    Anglada-Escud ´e, G. et al. A terrestrial planet candidate in a temperate orbit around Proxima Centauri. Nature 536, 437–440 (2016). URL https://www.nature.com/ articles/nature19106. Number: 7617 Publisher: Nature Publishing Group

    work page 2016

  3. [3]

    Zechmeister, M. et al. The CARMENES search for exoplanets around M dwarfs: Two temperate Earth-mass planet candidates around Teegarden’s Star. ˚a 627, A49 (2019). URL https://www.aanda.org/10.1051/0004-6361/201935460

    doi:10.1051/0004-6361/201935460 2019

  4. [4]

    Gillon, M. et al. Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1. Nature 542, 456–460 (2017). URL https://www.nature.com/ articles/nature21360. Number: 7642 Publisher: Nature Publishing Group

    work page 2017

  5. [5]

    Ment, K. et al. A Second Terrestrial Planet Orbiting the Nearby M Dwarf LHS 1140. Astron. J. 157, 32 (2019). URL https://iopscience.iop.org/article/10. 3847/1538-3881/aaf1b1

    work page 2019

  6. [6]

    Dreizler, S. et al. RedDots: a temperate 1.5 Earth-mass planet candidate in a compact multiterrestrial planet system around GJ 1061. Monthly Notices of the Royal Astronomi- cal Society 493, 536–550 (2020). URL https://ui.adsabs.harvard.edu/abs/ 2020MNRAS.493..536D. ADS Bibcode: 2020MNRAS.493..536D

    work page 2020

  7. [7]

    Peterson, M. S. et al. A temperate Earth-sized planet with tidal heating transiting an M6 star. Nature 617, 701–705 (2023). URL https://www.nature.com/articles/ s41586-023-05934-8 . Number: 7962 Publisher: Nature Publishing Group

    work page 2023

  8. [8]

    Vanderspek, R. et al. TESS Discovery of an Ultra-short-period Planet around the Nearby M Dwarf LHS 3844. Astrophys. J. 871, L24 (2019). URL https://ui.adsabs. harvard.edu/abs/2019ApJ...871L..24V. ADS Bibcode: 2019ApJ...871L..24V

    work page 2019

Show all 70 references
  1. [9]

    Agol, E. et al. Refining the Transit-timing and Photometric Analysis of TRAPPIST- 1: Masses, Radii, Densities, Dynamics, and Ephemerides. The Planetary Science Jour- nal 2, 1 (2021). URL https://iopscience.iop.org/article/10.3847/PSJ/ abd022/meta. Publisher: IOP Publishing

    2021 doi

  2. [10]

    Gillon, M. et al. The TRAPPIST-1 JWST Community Initiative. arXiv:2002.04798 [astro- ph] (2020). URL http://arxiv.org/abs/2002.04798. ArXiv: 2002.04798

    2020 arXiv

  3. [11]

    V ., Kreidberg, L., Rustamkulov, Z., Robinson, T

    Morley, C. V ., Kreidberg, L., Rustamkulov, Z., Robinson, T. & Fortney, J. J. Observing the Atmospheres of Known Temperate Earth-sized Planets with JWST. Astrophys. J. 850, 121 (2017). URL http://arxiv.org/abs/1708.04239. ArXiv: 1708.04239. 32

    2017 arXiv

  4. [12]

    Greene, T. P. et al. Thermal emission from the Earth-sized exoplanet TRAPPIST-1 b us- ing JWST (2023). URL http://arxiv.org/abs/2303.14849. ArXiv:2303.14849 [astro-ph]

    2023 arXiv

  5. [13]

    Zieba, S. et al. No thick carbon dioxide atmosphere on the rocky exoplanet TRAPPIST-1 c. Nature 1–4 (2023). URL https://www.nature.com/articles/ s41586-023-06232-z. Publisher: Nature Publishing Group

    2023

  6. [14]

    Mansfield, M. et al. Identifying Atmospheres on Rocky Exoplanets Through Inferred High Albedo. Astrophys. J. 886, 141 (2019). URL http://arxiv.org/abs/1907.13150. ArXiv:1907.13150 [astro-ph]

    2019 arXiv

  7. [15]

    Koll, D. D. B. et al. Identifying Candidate Atmospheres on Rocky M Dwarf Planets via Eclipse Photometry. Astrophys. J. 886, 140 (2019). URL https://ui.adsabs. harvard.edu/abs/2019ApJ...886..140K. ADS Bibcode: 2019ApJ...886..140K

    2019

  8. [16]

    Crossfield, I. J. M. et al. GJ 1252b: A Hot Terrestrial Super-Earth with No Atmo- sphere. Astrophys. J., Letters937, L17 (2022). URLhttps://dx.doi.org/10.3847/ 2041-8213/ac886b. Publisher: The American Astronomical Society

    2022

  9. [17]

    V ., Apai, D

    Rackham, B. V ., Apai, D. & Giampapa, M. S. The Transit Light Source Effect: False Spectral Features and Incorrect Densities for M-dwarf Transiting Planets. Astrophys. J. 853, 122 (2018). URL http://arxiv.org/abs/1711.05691. ArXiv: 1711.05691

    2018 arXiv

  10. [18]

    Howard, W. S. et al. Characterizing the Near-infrared Spectra of Flares from TRAPPIST- 1 During JWST Transit Spectroscopy Observations (2023). URL http://arxiv.org/ abs/2310.03792. ArXiv:2310.03792 [astro-ph]

    2023 arXiv

  11. [19]

    Lim, O. et al. Atmospheric Reconnaissance of TRAPPIST-1 b with JWST/NIRISS: Evi- dence for Strong Stellar Contamination in the Transmission Spectra (2023). URL http: //arxiv.org/abs/2309.07047. ArXiv:2309.07047 [astro-ph]

    2023 arXiv

  12. [20]

    & Agol, E

    Luger, R., Lustig-Yaeger, J. & Agol, E. Planet-Planet Occultations in TRAPPIST-1 and Other Exoplanet Systems. Astrophys. J. 851, 94 (2017). URL http://arxiv.org/ abs/1711.05739. ArXiv: 1711.05739

    2017 arXiv

  13. [21]

    Bell, T. J. et al. Eureka!: An End-to-End Pipeline for JWST Time-Series Observations (2022). URL http://arxiv.org/abs/2207.03585. ArXiv:2207.03585 [astro-ph]

    2022 arXiv

  14. [22]

    Lyu, X. et al. Super-Earth LHS3844b is tidally locked (2023). URL https://ui. adsabs.harvard.edu/abs/2023arXiv231001725L. Publication Title: arXiv e- prints ADS Bibcode: 2023arXiv231001725L

    2023

  15. [23]

    & Kaltenegger, L

    Madden, J. & Kaltenegger, L. A Catalog of Spectra, Albedos, and Colors of Solar System Bodies for Exoplanet Comparison. Astrobiology 18, 1559–1573 (2018). URL https: //www.liebertpub.com/doi/10.1089/ast.2017.1763. Publisher: Mary Ann Liebert, Inc., publishers. 33

    2018

  16. [24]

    & Takahashi, S

    Takahashi, J., Itoh, Y . & Takahashi, S. Mid-Infrared Spectroscopy of 11 Main-Belt Asteroids. Publications of the Astronomical Society of Japan 63, 499 (2011). URL https://ui.adsabs.harvard.edu/abs/2011PASJ...63..499T. ADS Bib- code: 2011PASJ...63..499T

    2011

  17. [25]

    M.-R., Whittaker, E

    Ih, J., Kempton, E. M.-R., Whittaker, E. A. & Lessard, M. Constraining the Thick- ness of TRAPPIST-1 b’s Atmosphere from Its JWST Secondary Eclipse Observation at 15 µm. Astrophys. J., Letters 952, L4 (2023). URL https://dx.doi.org/10.3847/ 2041-8213/ace03b. Publisher: The Ame...

    2023

  18. [26]

    Hu, R., Ehlmann, B. L. & Seager, S. THEORETICAL SPECTRA OF TERRESTRIAL EXOPLANET SURFACES. Astrophys. J. 752, 7 (2012). URL https://dx.doi.org/ 10.1088/0004-637X/752/1/7. Publisher: The American Astronomical Society

    2012 doi

  19. [27]

    Turbet, M. et al. Modeling climate diversity, tidal dynamics and the fate of volatiles on TRAPPIST-1 planets. ˚a 612, A86 (2018). URL https://www.aanda.org/ articles/aa/abs/2018/04/aa31620-17/aa31620-17.html. Publisher: EDP Sciences

    2018

  20. [28]

    Kislyakova, K. G. et al. Magma oceans and enhanced volcanism on TRAPPIST-1 plan- ets due to induction heating. Nature Astronomy 1, 878–885 (2017). URL https: //www.nature.com/articles/s41550-017-0284-0. Publisher: Nature Pub- lishing Group

    2017

  21. [29]

    Robinson, T. D. & Catling, D. C. Common 0.1 bar tropopause in thick atmospheres set by pressure-dependent infrared transparency. Nature Geoscience 7, 12–15 (2014). URL https://www.nature.com/articles/ngeo2020

    2014

  22. [30]

    Bourrier, V . et al. Temporal Evolution of the High-energy Irradiation and Water Content of TRAPPIST-1 Exoplanets. Astron. J. 154, 121 (2017). URL https://iopscience. iop.org/article/10.3847/1538-3881/aa859c

    2017 doi

  23. [31]

    L., Hauschildt, P

    Peacock, S., Barman, T., Shkolnik, E. L., Hauschildt, P. H. & Baron, E. Predicting the Extreme Ultraviolet Radiation Environment of Exoplanets Around Low-Mass Stars: the TRAPPIST-1 System. Astrophys. J. 871, 235 (2019). URL http://arxiv.org/abs/ 1812.06159. ArXiv: 1812.06159

    2019 arXiv

  24. [32]

    Wilson, D. J. et al. The Mega-MUSCLES Spectral Energy Distribution Of TRAPPIST-1. arXiv:2102.11415 [astro-ph] (2021). URL http://arxiv.org/abs/2102.11415. ArXiv: 2102.11415

    2021 arXiv

  25. [33]

    A., Krissansen-Totton, J., Wogan, N., Telus, M

    Thompson, M. A., Krissansen-Totton, J., Wogan, N., Telus, M. & Fortney, J. J. The case and context for atmospheric methane as an exoplanet biosignature. Proceedings of the National Academy of Sciences 119, e2117933119 (2022). URL https://www.pnas.org/doi/ abs/10.1073/pnas.2117...

    2022 doi

  26. [34]

    & Catling, D

    Wogan, N., Krissansen-Totton, J. & Catling, D. C. Abundant Atmospheric Methane from V olcanism on Terrestrial Planets Is Unlikely and Strengthens the Case for Methane as a Biosignature. The Planetary Science Journal1, 58 (2020). URL https://iopscience. iop.org/article/10.3847/...

    2020 doi

  27. [35]

    He, C. et al. Sulfur-driven haze formation in warm CO2-rich exoplanet atmospheres. Na- ture Astronomy 4, 986–993 (2020). URL https://www.nature.com/articles/ s41550-020-1072-9. Publisher: Nature Publishing Group

    2020

  28. [36]

    Redfield, S. et al. Report of the Working Group on Strategic Exoplanet Initiatives with HST and JWST (2024). URL http://arxiv.org/abs/2404.02932. ArXiv:2404.02932 [astro-ph]

    2024 arXiv

  29. [37]

    Stetson, P. B. DAOPHOT - A computer program for crowded-field stellar photometry. Publications of the Astronomical Society of the Pacific 99, 191 (1987). URL http: //iopscience.iop.org/article/10.1086/131977

    1987 doi

  30. [38]

    Greene, T. P. et al. Thermal Emission from the Earth-sized Exoplanet TRAPPIST-1 b using JWST. Nature 1–2 (2023). URL https://www.nature.com/articles/ s41586-023-05951-7. Publisher: Nature Publishing Group

    2023

  31. [39]

    Bushouse, H. et al. JWST Calibration Pipeline (2023). URL https://zenodo.org/ record/7577320

    2023

  32. [40]

    CRDS: Calibration Reference Data System for HST and JWST (2022)

    developers, C. CRDS: Calibration Reference Data System for HST and JWST (2022). URL https://github.com/spacetelescope/crds. Original-date: 2016-02- 18T23:15:38Z

    2022

  33. [41]

    Gillon, M. et al. Improved precision on the radius of the nearby super-Earth 55 Cnc e.˚a 539, A28 (2012). URL http://arxiv.org/abs/1110.4783. ArXiv: 1110.4783

    2012 arXiv

  34. [42]

    Gillon, M. et al. Search for a habitable terrestrial planet transiting the nearby red dwarf GJ

  35. [43]

    & Agol, E

    Mandel, K. & Agol, E. Analytic Light Curves for Planetary Transit Searches. Astrophys. J. 580, L171–L175 (2002). URL https://iopscience.iop.org/article/10. 1086/345520

    2002

  36. [44]

    Ducrot, E. et al. TRAPPIST-1: Global results of the Spitzer Exploration Science Program Red Worlds. ˚a 640, A112 (2020). URL https://www.aanda.org/articles/aa/ abs/2020/08/aa37392-19/aa37392-19.html. Publisher: EDP Sciences

    2020

  37. [45]

    & Angus, R

    Foreman-Mackey, D., Agol, E., Ambikasaran, S. & Angus, R. Fast and scalable Gaussian process modeling with applications to astronomical time series. Astron. J. 154, 220 (2017). URL http://arxiv.org/abs/1703.09710. ArXiv: 1703.09710. 35

    2017 arXiv

  38. [46]

    Nested sampling for general Bayesian computation

    Skilling, J. Nested sampling for general Bayesian computation. Bayesian Analysis 1, 833–859 (2006). URL https://projecteuclid.org/euclid.ba/1340370944. Publisher: International Society for Bayesian Analysis

    2006

  39. [47]

    Speagle, J. S. DYNESTY: a dynamic nested sampling package for estimating Bayesian posteriors and evidences. Monthly Notices of the Royal Astronomical Society 493, 3132– 3158 (2020). URL https://ui.adsabs.harvard.edu/abs/2020MNRAS.493. 3132S. ADS Bibcode: 2020MNRAS.493.3132S

    2020

  40. [48]

    R., Line, M

    Iyer, A. R., Line, M. R., Muirhead, P. S., Fortney, J. J. & Gharib-Nezhad, E. The SPHINX M-dwarf Spectral Grid. I. Benchmarking New Model Atmospheres to Derive Fundamental M-Dwarf Properties. Astrophys. J. 944, 41 (2023). URL http://arxiv.org/abs/ 2206.12010. ArXiv:2206.12010 ...

    2023 arXiv

  41. [49]

    Malik, M. et al. Analyzing Atmospheric Temperature Profiles and Spectra of M Dwarf Rocky Planets. Astrophys. J. 886, 142 (2019). URL https://ui.adsabs.harvard.edu/ abs/2019ApJ...886..142M. ADS Bibcode: 2019ApJ...886..142M

    2019

  42. [50]

    Whittaker, E. A. et al. The Detectability of Rocky Planet Surface and Atmosphere Com- position with JWST: The Case of LHS 3844b. Astron. J. 164, 258 (2022). URL http: //arxiv.org/abs/2207.08889. ArXiv:2207.08889 [astro-ph]

    2022 arXiv

  43. [51]

    Lim, O. et al. JWST Reconnaissance Transmission Spectroscopy of the Earth-sized Exo- planet TRAPPIST-1 b. Bulletin of the AAS 55 (2023). URL https://baas.aas.org/ pub/2023n2i125p06/release/1

    2023

  44. [52]

    Domingue, D. L. et al. Mercury’s Weather-Beaten Surface: Understanding Mercury in the Context of Lunar and Asteroidal Space Weathering Studies. Space Science Reviews 181, 121–214 (2014). URL https://doi.org/10.1007/s11214-014-0039-5

    2014 doi

  45. [53]

    & Kimeswenger, S

    Jones, A., Noll, S., Kausch, W., Szyszka, C. & Kimeswenger, S. An advanced scattered moonlight model for Cerro Paranal. ˚a 560, A91 (2013). URL https://www.aanda. org/articles/aa/abs/2013/12/aa22433-13/aa22433-13.html. Pub- lisher: EDP Sciences

    2013

  46. [54]

    He, C. et al. Laboratory Simulations of Haze Formation in the Atmospheres of Super-Earths and Mini-Neptunes: Particle Color and Size Distribution. Astrophys. J., Letters 856, L3 (2018). URL https://dx.doi.org/10.3847/2041-8213/aab42b. Publisher: The American Astronomical Society

    2018 doi

  47. [55]

    W., Chubb, K., Helling, C

    Min, M., Ormel, C. W., Chubb, K., Helling, C. & Kawashima, Y . The ARCiS framework for Exoplanet Atmospheres: Modelling Philosophy and Retrieval. ˚a 642, A28 (2020). URL http://arxiv.org/abs/2006.12821. ArXiv:2006.12821 [astro-ph]

    2020 arXiv

  48. [56]

    Chubb, K. L. & Min, M. Exoplanet atmosphere retrievals in 3D using phase curve data with ARCiS: application to W ASP-43b. ˚a 665, A2 (2022). URL http://arxiv.org/abs/ 2206.09738. ArXiv:2206.09738 [astro-ph]. 36

    2022 arXiv

  49. [57]

    Tremblin, P. et al. FINGERING CONVECTION AND CLOUDLESS MODELS FOR COOL BROWN DW ARF ATMOSPHERES.Astrophys. J. 804, L17 (2015). URL https: //iopscience.iop.org/article/10.1088/2041-8205/804/1/L17

    2015 doi

  50. [58]

    Drummond, B. et al. The effects of consistent chemical kinetics calculations on the pressure-temperature profiles and emission spectra of hot Jupiters. ˚a 594, A69 (2016). URL https://www.aanda.org/articles/aa/abs/2016/10/aa28799-16/ aa28799-16.html. Publisher: EDP Sciences

    2016

  51. [59]

    & Ikoma, M

    Kawashima, Y . & Ikoma, M. Theoretical Transmission Spectra of Exoplanet Atmospheres with Hydrocarbon Haze: Effect of Creation, Growth, and Settling of Haze Particles. I. Model Description and First Results. Astrophys. J. 853, 7 (2018). URL https://ui.adsabs. harvard.edu/abs/2...

    2018

  52. [60]

    & Barnes, R

    Luger, R. & Barnes, R. Extreme Water Loss and Abiotic O$ 2$ Buildup On Planets Throughout the Habitable Zones of M Dwarfs. Astrobiology 15, 119–143 (2015). URL http://arxiv.org/abs/1411.7412. ArXiv: 1411.7412

    2015 arXiv

  53. [61]

    & Wolf, E

    Hu, R., Peterson, L. & Wolf, E. T. O2- and CO-rich Atmospheres for Potentially Hab- itable Environments on TRAPPIST-1 Planets. Astrophys. J. 888, 122 (2020). URL https://dx.doi.org/10.3847/1538-4357/ab5f07. Publisher: The American Astronomical Society

    2020 doi

  54. [62]

    Arney, G. N. et al. Pale Orange Dots: The Impact of Organic Haze on the Habitability and Detectability of Earthlike Exoplanets. Astrophys. J.836, 49 (2017). URL http://arxiv. org/abs/1702.02994. ArXiv: 1702.02994

    2017 arXiv

  55. [63]

    Luger, R. et al. starry: Analytic Occultation Light Curves. Astron. J. 157, 64 (2019). URL https://ui.adsabs.harvard.edu/abs/2019AJ....157...64L. ADS Bib- code: 2019AJ....157...64L

    2019

  56. [64]

    Foreman-Mackey, D. et al. exoplanet: Gradient-based probabilistic inference for exoplanet data & other astronomical time series.Journal of Open Source Software6, 3285 (2021). URL http://arxiv.org/abs/2105.01994. Number: 62 arXiv:2105.01994 [astro-ph]

    2021 arXiv

  57. [65]

    Salvatier, J., Wiecki, T. V . & Fonnesbeck, C. Probabilistic programming in Python us- ing PyMC3. PeerJ Computer Science 2, e55 (2016). URL https://peerj.com/ articles/cs-55. Publisher: PeerJ Inc

    2016

  58. [66]

    W., Lang, D

    Foreman-Mackey, D., Hogg, D. W., Lang, D. & Goodman, J. emcee: The MCMC Hammer. arXiv:1202.3665 [astro-ph, physics:physics, stat] (2013). URL http://arxiv.org/ abs/1202.3665. ArXiv: 1202.3665

    2013 arXiv

  59. [67]

    Harris, C. R. et al. Array programming with NumPy. Nature 585, 357–362 (2020). URL https://www.nature.com/articles/s41586-020-2649-2. Number: 7825 Publisher: Nature Publishing Group. 37

    2020

  60. [68]

    Robitaille, T. P. et al. Astropy: A community Python package for astronomy. ˚a 558, A33 (2013). URL https://www.aanda.org/articles/aa/abs/2013/10/ aa22068-13/aa22068-13.html. Publisher: EDP Sciences

    2013

  61. [69]

    fiducial

    Hunter, J. D. Matplotlib: A 2D Graphics Environment. Computing in Science & Engineering 9, 90–95 (2007). Conference Name: Computing in Science & Engineering. 38 Supplementary Figures GTO 1279 Visit 1 GTO 1279 Visit 2 Supplementary Fig. 1: STScI pipeline-corrected (Stage 2) ima...

    2007

  62. [1214]

    URL http://www.aanda.org/10.1051/0004-6361/ 201322362

    ˚a 563, A21 (2014). URL http://www.aanda.org/10.1051/0004-6361/ 201322362

    2014 doi

Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.