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REVIEW 3 major objections 5 minor 78 references

A Precise Metallicity and Carbon-to-Oxygen Ratio for a Warm Giant Exoplanet from its Panchromatic JWST Emission Spectrum

T0 review · 3 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read JWST eclipse spectrum of WASP-80 b pins down super-solar metallicity and near-solar C/O, pointing to a hot-giant formation path around a low-mass star.

desk verdict The molecule detections and the panchromatic spectrum are the real advance; the [M/H] and C/O values are probably right, but the quoted precision is not yet credible because the model is rejected and the MIRI band is poorly fit. read the letter →

arxiv 2506.01800 v1 pith:AHOYOLPT submitted 2025-06-02 astro-ph.EP

Lindsey S. Wiser , Taylor J. Bell , Michael R. Line , Everett Schlawin , Thomas G. Beatty , Luis Welbanks , Thomas P. Greene , Vivien Parmentier
show 6 more authors
Matthew M. Murphy Jonathan J. Fortney Kenny Arnold Nishil Mehta Kazumasa Ohno Sagnick Mukherjee
This is my paper · ORCID
classification astro-ph.EP
keywords exoplanetatmospheresJWSTsecondaryeclipsespectroscopyWASP-80batmosphericmetallicitycarbon-to-oxygenratioradiative-convective-photochemicalequilibriumdisequilibriumchemistry
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 reports the first panchromatic 2.4–12 µm JWST emission spectrum of a gas giant around a late K/early M dwarf, the warm sub-Jovian WASP-80 b. By combining NIRCam F322W2, F444W, and MIRI LRS secondary eclipse observations, it achieves confident detections of water, methane, carbon monoxide, and carbon dioxide, plus a tentative ammonia detection. From these, the authors derive a super-solar atmospheric metallicity of $[M/H] = 0.55^{+0.12}_{-0.10}$ and a near-solar carbon-to-oxygen ratio of $\mathrm{C/O} = 0.48^{+0.06}_{-0.07}$. The composition matches other hot gas giants, leading the paper to conclude that WASP-80 b's formation pathway may not differ fundamentally from giants around higher-mass stars, despite its rare host-star environment.

What carries the argument

The argument is carried by a grid of one-dimensional radiative-convective-photochemical-equilibrium (1D-RCPE) atmosphere models computed with the self-consistent ScCHIMERA framework coupled to the VULCAN photochemistry code, spanning dayside temperature, internal temperature, metallicity, carbon-to-oxygen ratio, and vertical eddy diffusion. The grid is interpolated within a nested-sampling retrieval that also fits a vertically uniform grey cloud opacity and a dilution factor $A$ multiplying the model flux; $A = 1.14 \pm 0.03$ is interpreted as accounting for dayside temperature inhomogeneities. A parallel free retrieval with 14 free parameters, using the CHIMERA framework with parameterized temperature structure and constant-with-altitude molecular abundances, serves as a cross-check that the grid-based assumptions are not driving the abundance results.

What would settle it

Re-fit the published 2.4–12 µm eclipse depth spectrum with a two-dimensional or cloud-free model that does not require a dilution factor above unity; if the best-fit $[M/H]$ and $\mathrm{C/O}$ move outside the quoted $1\sigma$ uncertainties, the 1D-equilibrium assumption is the limiting step. Alternatively, an independent measurement of the dayside temperature map (e.g., from phase-resolved eclipse mapping) that rules out the brightness distribution implied by $A = 1.14$ would falsify the dilution interpretation.

Watch

Extended reading notes

Core claim

The central claim is that a warm (≈820 K) sub-Jovian planet around a low-mass star has an atmospheric composition indistinguishable from hot gas giants around sunlike stars: metallicities about 3–5 times solar and a carbon-to-oxygen ratio consistent with solar. The claim rests on the panchromatic spectrum, which provides simultaneous coverage of multiple carbon- and oxygen-bearing molecules and thereby breaks degeneracies that plague narrower wavelength coverage. The paper demonstrates that the four major molecules are detected at high significance (H2O at 13.0σ, CH4 at 15.1σ, CO2 at 10.0σ, CO at 7.5σ) and that the inferred $[M/H]$ and $\mathrm{C/O}$ are robust to the choice of retrieval approach, as both the grid-based radiative-convective-photochemical-equilibrium retrieval and a more flexible free retrieval give consistent answers.

Load-bearing premise

The retrieved metallicity and C/O assume the dayside of WASP-80 b is accurately represented by a one-dimensional radiative-convective-photochemical-equilibrium model with a vertically uniform grey cloud and a dilution factor of 1.14 that lets the model emit about 14 percent more flux than observed; if that missing flux is actually missing opacity or thermal structure rather than genuine dayside inhomogeneity, the abundances would shift.

Editorial extensions

If this is right

  • WASP-80 b becomes a benchmark for warm giant atmospheres: the first late-K/early-M-dwarf host with a complete 2.4–12 µm emission spectrum, providing a reference for interpreting the rarer giant planets around low-mass stars.
  • The confident detections of CH4, CO, CO2, and H2O in a single planet demonstrate that panchromatic JWST coverage can simultaneously measure the carbon and oxygen reservoirs needed to estimate $[M/H]$ and $\mathrm{C/O}$ in temperate giants.
  • The super-solar metallicity and near-solar C/O imply that WASP-80 b likely accreted a mix of oxygen-rich ices and carbon-poor solids during migration, consistent with a core-accretion-plus-migration history similar to hot Jupiters.
  • The 7.3σ preference for a high internal temperature ($T_{\rm int} = 381^{+38}_{-39}$ K) and strong vertical mixing ($\log_{10} K_{zz} = 9.13^{+1.06}_{-0.74}$) indicates that disequilibrium quenching of CH4 is required to explain the spectrum, a mechanism previously invoked for WASP-107 b.
  • The grid-based retrieval is statistically rejected by the global fit ($\chi^2/{\rm NDOF} = 1.38$, $p = 4\times10^{-4}$), with the MIRI LRS subset having $\chi^2/{\rm NDOF} = 5.38$, so the precision of the quoted abundances depends on the adequacy of the 1D-equilibrium model plus dilution factor.

Reading between the lines

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

  • If the composition match with hot giants holds across more low-stellar-mass Jovians, the rarity of these planets would be a disk-mass and migration-efficiency effect, not a composition effect, which would sharpen predictions for population synthesis models.
  • The tentative NH3 detection at 2.8σ, if confirmed with deeper MIRI observations, would make WASP-80 b a rare testbed for nitrogen chemistry at ~820 K, where ammonia and nitrogen gas can coexist.
  • The large fitted dilution factor (A > 1) is a red flag that the 1D model underproduces the observed flux by ~14%; a two-dimensional or cloud-free model that removes the need for A>1 could shift the retrieved $[M/H]$ and $\mathrm{C/O}$ beyond the quoted uncertainties, a testable check with the published eclipse depths.
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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 presents a panchromatic JWST secondary-eclipse spectrum of the warm sub-Jovian exoplanet WASP-80 b, combining NIRCam F322W2, F444W, and MIRI LRS to cover 2.4–12 μm. The authors report confident detections of H2O, CH4, CO, and CO2 (all >7.5σ) and a tentative NH3 detection. Using a grid of 1D radiative-convective-photochemical-equilibrium models and a complementary free retrieval, they estimate a super-solar metallicity [M/H] = 0.55 (+0.12/−0.10) and near-solar C/O = 0.48 (+0.06/−0.07) for the dayside atmosphere, and they argue that this composition is consistent with other hot gas giants, implying a similar formation pathway despite the rarity of giant planets around low-mass stars.

Significance. If the compositional constraints are robust, this is a valuable dataset: it is the first complete JWST emission spectrum of a gas giant around a late-K/early-M dwarf and the coolest such planet observed across 2.4–12 μm. The paper's strengths include three independent data reductions that agree to within ~0.4σ, cross-validation between grid-based and free retrievals, a NIRCam-only retrieval that reproduces the headline values, and transparent reporting of fit statistics, model grids, and reduction products. The molecular detections appear secure. However, the quantitative [M/H] and C/O claims—and hence the formation interpretation—are conditional on the treatment of a fitted dilution factor and on the model's ability to reproduce the MIRI LRS data, which is formally rejected by the χ² statistic. The paper honestly discloses these tensions, but they are load-bearing for the 'precise' claim in the title.

major comments (3)
  1. [Results; SI Table S2] The fiducial grid-based and free retrievals are formally rejected by the χ² test (p = 4×10⁻⁴ and p = 8×10⁻⁴, respectively), and the MIRI LRS subset alone gives χ²/NDOF = 5.38 while NIRCam alone gives 0.95. The K-S test indicates Gaussian residuals, but the χ² rejection means the model does not reproduce the data within the reported uncertainties. Since the central claim is a 'precise' [M/H] and C/O, the authors should quantify how much the retrieved values shift under a more conservative treatment of the poor MIRI fit—for example, by inflating MIRI uncertainties to force χ²/NDOF ≈ 1, by fitting the two instruments separately, or by excluding the worst-fitting MIRI channels. Without such a test, the stated precision appears to be internal retrieval precision rather than accuracy anchored to the physical model.
  2. [Grid-Based Retrieval; Table 3] The dilution factor A = 1.14 ± 0.03 (grid) and 1.09 ± 0.04 (free) is greater than unity, meaning the adopted physical model underproduces the observed dayside flux by roughly 14% at face value. The authors interpret A as a proxy for dayside temperature inhomogeneity, but the eclipse-mapping test only rules out simple non-uniform brightness patterns at the broadband level; it does not validate a uniform 14% scale offset. Because A is a wavelength-independent multiplier, it cannot absorb the wavelength-dependent residuals seen in the MIRI LRS band; those residuals must instead be absorbed by abundance or thermal parameters. If the MIRI discrepancy is actually missing continuum opacity, cloud scattering, or a thermal-structure effect, then [M/H] and C/O are coupled to that missing physics. I recommend that the authors test the sensitivity of [M/H] and C/O to the treatment of A—e.g., fix A = 1, or allow a wavelength-dependent correction—and discuss whether the 14% flux shortfall could alternatively be explained by missing opacity sources or by a different thermal profile.
  3. [Results; Discussion] The high internal temperature (Tint = 381 K) and vertical mixing (Kzz) are invoked to quench CH4, and the paper shows that fixing Tint = 150 K and log10(Kzz) = 9.0 leads to a low C/O and a 7.3σ worse fit. However, this test is performed within the same RCPE grid that also carries the dilution factor and the poor MIRI fit. The conclusion that the free Tint and Kzz are required is therefore entangled with the ability of A and the cloud parameters to absorb other model deficits. The authors should demonstrate that the 7.3σ preference is not driven by the MIRI channels that are poorly fit in the fiducial model, for instance by repeating the fixed-Tint test on the NIRCam-only data.
minor comments (5)
  1. [Discussion] The Discussion states that WASP-80 b is 'the coolest planet for which JWST has obtained a complete emission spectrum 2.4–10 μm,' but the abstract and the rest of the paper consistently state 2.4–12 μm; the 10 μm appears to be a typo.
  2. [Discussion] The Discussion refers to 'NIRCam F332W2,' which should be 'F322W2' to match the filter name used elsewhere.
  3. [Table 3; Results] The text following Table 3 quotes 'Tday = 895.25(+3.16/−3.19) K,' but Table 3 lists the grid-based retrieval value as 'Tday = 859.87(+7.08/−9.10) K.' This apparent inconsistency should be resolved and a single value quoted.
  4. [Results] For the grid-based detection significances, the paper notes that models with a molecule 'turned off' are no longer in RCPE. It would be helpful to state explicitly whether those models were re-equilibrated or merely post-processed with the molecule's opacity removed, since that affects the interpretation of the quoted grid-based significance values.
  5. [Methods] The eclipse-mapping test is described only briefly; the text would benefit from a sentence noting that the test uses broadband light curves and therefore cannot place strong constraints on wavelength-dependent brightness maps, which is directly relevant to the interpretation of A.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the paper's [M/H] and C/O values are fitted retrieval outputs from the observed spectrum, cross-checked by an independent free retrieval, not derived from the claimed conclusion by construction.

full rationale

The paper's central quantities ([M/H], C/O, Tint, Kzz, cloud opacity, dilution factor A, and molecular abundances) are all parameters estimated by fitting model spectra to the JWST eclipse-depth data using nested sampling. The text explicitly frames them as estimates from a grid-based RCPE retrieval and a complementary free retrieval, and it does not present them as first-principles predictions. There is no equation in which a headline result is defined in terms of the data quantity it claims to predict, nor any fitted subset that is then renamed as a prediction. The molecular detections are supported by Bayesian evidence comparisons of free retrievals with and without each molecule, a procedure that does not presuppose the detection. The grid-based and free retrievals agree, and the NIRCam-only retrieval reproduces the same [M/H] and C/O within uncertainties, indicating that the abundance constraints are driven by the data rather than by the RCPE grid's construction. The self-citations to CHIMERA, ScCHIMERA, VULCAN, and the earlier WASP-80 b paper are methodological reuse or prior-data context, not load-bearing uniqueness claims or ansatz smuggling that forces the central result. The poor chi-squared statistics (chi2/NDOF = 1.38, p = 4e-4 for the grid fit; MIRI LRS chi2/NDOF = 5.38) and the dilution factor A > 1 are genuine model-data discrepancy concerns that affect the physical interpretation of the retrieved abundances, but they are correctness or robustness risks, not circularity: A is a fitted scaling parameter, and the paper does not use A as both input and output to define [M/H] or C/O. No specific reduction of the claimed derivation to its own inputs can be exhibited, so the appropriate finding is no significant circularity.

Assumptions & free parameters 9 free parameters · 8 assumptions · 2 invented entities

The headline numbers are retrieval outputs, so every claimed quantity is fitted. The RCPE model grid injects the only upstream physics (thermochemical equilibrium, VULCAN kinetics, GJ676A UV proxy, 1D structure), all of which are assumed inputs rather than derived results. The grey cloud and dilution factor are empirical constructs whose presence is not independently confirmed.

free parameters (9)
  • [M/H] metallicity = 0.55 (+0.12/-0.10)
    Headline result; fitted by nested sampling over the ScCHIMERA grid with prior (0.375, 1.375).
  • C/O ratio = 0.48 (+0.06/-0.07)
    Headline result; fitted with prior (0.3, 0.7).
  • Dayside temperature Tday = 859.87 K (+7.08/-9.10)
    Scaled incident flux grid parameter (825 to 900 K), fitted.
  • Internal temperature Tint = 381.08 K (+37.70/-38.98)
    Fitted; the high value quenches CH4; prior (150 to 450 K).
  • log10 Kzz eddy diffusion = 9.13 (+1.06/-0.74)
    Fitted vertical mixing strength; 2-sigma upper limit at 11.07; prior (8.0 to 11.5).
  • Grey cloud opacity log10 kappa_cld = -29.50 (+0.06/-0.05)
    Fitted in the grid retrieval; the free retrieval gives only a 2-sigma upper limit at -30.22, so clouds are inconclusive.
  • Dilution factor A = 1.14 (+/-0.03)
    Fitted flux multiplier; exceeds unity, indicating the model underproduces the observed emission by about 14 percent.
  • Free retrieval: 6 molecular mixing ratios = log10 XH2O = -2.33, XCO = -2.49, XCO2 = -5.14, XCH4 = -3.86, XNH3 = -5.65, XSO2 = -9.47
    Fitted without RCPE assumptions; consistent with the grid abundances.
  • Free retrieval: 6 T-P profile parameters = T1uBar = 667.79 K, alpha1 = 1.07, alpha2 = 0.40, log10 P1 = -1.75, log10 P2 = -3.89, log10 P3 = 0.95
    Parametric Madhusudhan-Seager profile, fitted.
assumptions (8)
  • standard math Bayesian nested sampling (PyMultiNest) yields unbiased posterior estimates and reliable evidence differences.
    Relied on for all parameter estimates and detection significances (Modeling Approach).
  • domain assumption A 1D hydrostatic atmosphere spanning 1e-6 to 1e1.2 bar represents the dayside emission.
    Used in both grid and free retrievals (Modeling Approach, free retrieval).
  • domain assumption Thermochemical equilibrium (CEA2) plus VULCAN photochemistry with the H-C-O-N-S network gives correct abundances along the T-P profile.
    The grid-based retrieval maps abundances to [M/H] and C/O through this chemistry (Modeling Approach, Grid-Based Retrieval).
  • domain assumption The GJ676A M0V UV spectrum (attributed to Mega-MUSCLES, ref. 54) is a valid proxy for WASP-80's UV irradiation.
    Feeds VULCAN photochemistry; the cited ref. 54 is the TRAPPIST-1 SED paper, so the provenance of the GJ676A spectrum is unclear (Modeling Approach).
  • domain assumption The PHOENIX stellar model (Tstar = 4143 K, log g = 4.663), the adopted system parameters, and zero eccentricity are correct.
    Sets the incident flux and eclipse geometry; e = 0 is supported by the SI timing fit (Table S1), and the stellar and orbital parameters come from ref. (16).
  • domain assumption A uniform-brightness dayside is adequate (Delta BIC ~ 18 versus non-uniform models).
    Justifies the starry uniform eclipse model (Methods, eclipse mapping test).
  • domain assumption Dayside temperature heterogeneities are fully absorbed by the dilution factor A.
    A is fitted to 1.14 +/- 0.03, so the assumption is that A is not masking other model errors (Modeling Approach; Results).
  • ad hoc to paper The unusually high internal temperature (Tint = 381 K) and vertical mixing are responsible for CH4 quenching.
    The grid retrieval needs Tint about 381 K and Kzz to match the CH4 abundance; fixing Tint = 150 K with Kzz = 9 forces C/O down and fails the 4.3 micron CO2 feature (preferred by 7.3 sigma). This is the paper's main modeling lever, introduced to make the model fit (Results; Discussion).
invented entities (2)
  • Vertically uniform grey cloud opacity (kappa_cld)
    purpose: Absorbs unresolved aerosol opacity in the grid models
    Standard retrieval nuisance parameter, not a new physical entity; grid and free retrievals disagree on its presence, so it is an empirical construct.
  • Dilution factor A
    purpose: Scales model planetary flux to mimic unresolved dayside temperature inhomogeneity
    Fitted normalization fudge at 1.14 +/- 0.03; can mask model errors such as missing opacity or wrong thermal structure.

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Cite this review

Pith. "Pith review of A Precise Metallicity and Carbon-to-Oxygen Ratio for a Warm Giant Exoplanet from its Panchromatic JWST Emission Spectrum." pith.science (2026). https://pith.science/paper/AHOYOLPT

@misc{pith2026250601800,
  author       = {Pith},
  title        = {Pith review of: A Precise Metallicity and Carbon-to-Oxygen Ratio for a Warm Giant Exoplanet from its Panchromatic JWST Emission Spectrum},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/AHOYOLPT}},
  note         = {Machine review of arXiv:2506.01800}
}
abstract

WASP-80 b, a warm sub-Jovian (equilibrium temperature ~820 K, 0.5 Jupiter masses), presents an opportunity to characterize a rare gas giant exoplanet around a low-mass star. In addition, its moderate temperature enables its atmosphere to host a range of carbon and oxygen species (H$_2$O, CH$_4$, CO, CO$_2$, NH$_3$). In this paper, we present a panchromatic emission spectrum of WASP-80 b, the first gas giant around a late K/early M-dwarf star and the coolest planet for which the James Webb Space Telescope has obtained a complete emission spectrum spanning 2.4-12 $\mu$m, including NIRCam F322W2 (2.4-4 $\mu$m) and F444W (4-5 $\mu$m), and MIRI LRS (5-12 $\mu$m). We report confident detections of H$_2$O, CH$_4$, CO, and CO$_2$, and a tentative detection of NH$_3$. We estimate WASP-80 b's atmospheric metallicity and carbon-to-oxygen ratio and compare them with estimates for other gas giants. Despite the relative rarity of giant planets around low-mass stars, we find that WASP-80 b's composition is consistent with other hot gas giants, suggesting that the formation pathway of WASP-80 b may not be dissimilar from hot gas giants around higher-mass stars.

Figures

Figures reproduced from arXiv: 2506.01800 by the authors.

Figure 1
Figure 1. An artist’s rendering of the warm exoplanet WASP-80 b and an overview of its planet-system parameters. Planet image credit: NASA/Ames Research Center. giant atmospheres. We seek precise constraints on WASP￾80 b’s atmospheric metallicity ([M/H], in which M includes all non-H/He elements and [] denotes log10 relative to solar abundances) and carbon-to-oxygen ratio (C/O). [M/H] and C/O are commonly estimated metrics hy… view at source ↗
Figure 4
Figure 4. [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 6
Figure 6. Metallicity and C/O estimates for WASP-80 b and other gas giant planets and brown dwarfs. Planets shown in grey are close-in transiting gas giants. Composition inferences shown with circular points are drawn from JWST observations, while square points indicate ground-based high-resolution observations. Blue points are cool gas giants and brown dwarfs (∼10-30 MJupiter) with wide orbits (62). Dotted lines denote appro… view at source ↗

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Works this paper leans on

78 extracted references · 77 canonical work pages

  1. [1]

    The Astrophysical Journal 923, 242 (2021)

    JM Goyal , NK Lewis , HR Wakeford , RJ MacDonald , NJ Mayne , Why is it So Hot in Here? Exploring Population Trends in Spitzer Thermal Emission Observations of Hot Jupiters Using Planet-specific, Self-consistent Atmospheric Models . The Astrophysical Journal 923, 242 (2021)

    work page 2021

  2. [2]

    The Astrophysical Journal Supplement Series 260, 3 (2022)

    Q Changeat , et al., Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse . The Astrophysical Journal Supplement Series 260, 3 (2022)

    work page 2022

  3. [3]

    The Astrophysical Journal 971, 33 (2024)

    LS Wiser , et al., Lessons from Hubble and Spitzer: 1D Self-consistent Model Grids for 19 Hot Jupiter Emission Spectra . The Astrophysical Journal 971, 33 (2024)

    work page 2024

  4. [4]

    Monthly Notices of the Royal Astronomical Society 524, 817--834 (2023)

    J Taylor , et al., Awesome SOSS: atmospheric characterization of WASP-96 b using the JWST early release observations . Monthly Notices of the Royal Astronomical Society 524, 817--834 (2023)

    work page 2023

  5. [5]

    The Astrophysical Journal Letters 956, L32 (2023)

    D Grant , et al., JWST-TST DREAMS: Quartz Clouds in the Atmosphere of WASP-17b . The Astrophysical Journal Letters 956, L32 (2023)

    work page 2023

  6. [6]

    Nature 623, 709--712 (2023)

    TJ Bell , et al., Methane throughout the atmosphere of the warm exoplanet WASP-80b . Nature 623, 709--712 (2023)

    work page 2023

  7. [7]

    Nature 618, 43--46 (2023)

    JL Bean , et al., High atmospheric metal enrichment for a Saturn-mass planet . Nature 618, 43--46 (2023)

    work page 2023

  8. [8]

    Nature 630, 836--840 (2024)

    L Welbanks , et al., A high internal heat flux and large core in a warm Neptune exoplanet . Nature 630, 836--840 (2024)

    work page 2024

Show all 78 references
  1. [9]

    Nature Astronomy 8, 1562--1574 (2024)

    MM Murphy , et al., Evidence for morning-to-evening limb asymmetry on the cool low-density exoplanet WASP-107 b . Nature Astronomy 8, 1562--1574 (2024)

    2024

  2. [10]

    Nature Astronomy 8, 879--898 (2024)

    TJ Bell , et al., Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b . Nature Astronomy 8, 879--898 (2024)

    2024

  3. [11]

    The Astrophysical Journal Letters 970, L28 (2024)

    MC Nixon , et al., New Insights into the Internal Structure of GJ 1214 b Informed by JWST . The Astrophysical Journal Letters 970, L28 (2024)

    2024

  4. [12]

    The Astronomical Journal 168, 104 (2024)

    E Schlawin , et al., Multiple Clues for Dayside Aerosols and Temperature Gradients in WASP-69 b from a Panchromatic JWST Emission Spectrum . The Astronomical Journal 168, 104 (2024)

    2024

  5. [13]

    The Astrophysical Journal Letters 970, L10 (2024)

    TG Beatty , et al., Sulfur Dioxide and Other Molecular Species in the Atmosphere of the Sub-Neptune GJ 3470 b . The Astrophysical Journal Letters 970, L10 (2024)

    2024

  6. [14]

    S Ida , DNC Lin , Toward a Deterministic Model of Planetary Formation. I. A Desert in the Mass and Semimajor Axis Distributions of Extrasolar Planets . The Astrophysical Journal 604, 388--413 (2004)

    2004

  7. [15]

    Journal of Geophysical Research (Planets) 126, e06629 (2021)

    JJ Fortney , RI Dawson , TD Komacek , Hot Jupiters: Origins, Structure, Atmospheres . Journal of Geophysical Research (Planets) 126, e06629 (2021)

    2021

  8. [16]

    Monthly Notices of the Royal Astronomical Society 450, 2279--2290 (2015)

    AHMJ Triaud , et al., WASP-80b has a dayside within the T-dwarf range . Monthly Notices of the Royal Astronomical Society 450, 2279--2290 (2015)

    2015

  9. [17]

    The Astrophysical Journal 737, 15 (2011)

    JI Moses , et al., Disequilibrium Carbon, Oxygen, and Nitrogen Chemistry in the Atmospheres of HD 189733b and HD 209458b . The Astrophysical Journal 737, 15 (2011)

    2011

  10. [18]

    SM Tsai , et al., VULCAN: Chemical Kinetics For Exoplanetary Atmospheres (Astrophysics Source Code Library, record ascl:1704.011) (2017)

    2017

  11. [19]

    The Astrophysical Journal 790, 108 (2014)

    A Fukui , et al., Multi-band, Multi-epoch Observations of the Transiting Warm Jupiter WASP-80b . The Astrophysical Journal 790, 108 (2014)

    2014

  12. [20]

    The Astronomical Journal 164, 30 (2022)

    I Wong , et al., The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b . The Astronomical Journal 164, 30 (2022)

    2022

  13. [21]

    Astronomische Nachrichten 326, 913--919 (2005)

    FC Adams , P Bodenheimer , G Laughlin , M dwarfs: planet formation and long term evolution . Astronomische Nachrichten 326, 913--919 (2005)

    2005

  14. [22]

    Icarus 124, 62--85 (1996)

    JB Pollack , et al., Formation of the Giant Planets by Concurrent Accretion of Solids and Gas . Icarus 124, 62--85 (1996)

    1996

  15. [23]

    H Beuther , RS Klessen , CP Dullemond , T Henning

    G Chabrier , A Johansen , M Janson , R Rafikov , Giant Planet and Brown Dwarf Formation in Protostars and Planets VI , eds. H Beuther , RS Klessen , CP Dullemond , T Henning . pp. 619--642 (2014)

    2014

  16. [24]

    R Burn , et al., The New Generation Planetary Population Synthesis (NGPPS). IV. Planetary systems around low-mass stars . Astronomy & Astrophysics 656, A72 (2021)

    2021

  17. [25]

    The Astrophysical Journal Letters 743, L16 (2011)

    KI \"O berg , R Murray-Clay , EA Bergin , The Effects of Snowlines on C/O in Planetary Atmospheres . The Astrophysical Journal Letters 743, L16 (2011)

    2011

  18. [26]

    The Astrophysical Journal 832, 41 (2016)

    C Mordasini , R van Boekel , P Molli \`e re , T Henning , B Benneke , The Imprint of Exoplanet Formation History on Observable Present-day Spectra of Hot Jupiters . The Astrophysical Journal 832, 41 (2016)

    2016

  19. [27]

    The Astrophysical Journal 829, 114 (2016)

    K Batygin , PH Bodenheimer , GP Laughlin , In Situ Formation and Dynamical Evolution of Hot Jupiter Systems . The Astrophysical Journal 829, 114 (2016)

    2016

  20. [28]

    Monthly Notices of the Royal Astronomical Society 469, 4102--4115 (2017)

    N Madhusudhan , B Bitsch , A Johansen , L Eriksson , Atmospheric signatures of giant exoplanet formation by pebble accretion . Monthly Notices of the Royal Astronomical Society 469, 4102--4115 (2017)

    2017

  21. [29]

    Monthly Notices of the Royal Astronomical Society 469, 3994--4011 (2017)

    RA Booth , CJ Clarke , N Madhusudhan , JD Ilee , Chemical enrichment of giant planets and discs due to pebble drift . Monthly Notices of the Royal Astronomical Society 469, 3994--4011 (2017)

    2017

  22. [30]

    The Astronomical Journal 163, 159 (2022)

    H Reggiani , KC Schlaufman , BF Healy , JD Lothringer , DK Sing , Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line . The Astronomical Journal 163, 159 (2022)

    2022

  23. [31]

    The Astrophysical Journal 943, 112 (2023)

    Y Chachan , HA Knutson , J Lothringer , GA Blake , Breaking Degeneracies in Formation Histories by Measuring Refractory Content in Gas Giants . The Astrophysical Journal 943, 112 (2023)

    2023

  24. [32]

    Astronomy & Astrophysics 562, A126 (2014)

    L Mancini , et al., Physical properties and transmission spectrum of the WASP-80 planetary system from multi-colour photometry . Astronomy & Astrophysics 562, A126 (2014)

    2014

  25. [33]

    Astronomy & Astrophysics 551, A80 (2013)

    AHMJ Triaud , et al., WASP-80b: a gas giant transiting a cool dwarf . Astronomy & Astrophysics 551, A80 (2013)

    2013

  26. [34]

    The Journal of Open Source Software 7, 4503 (2022)

    T Bell , et al., Eureka!: An End-to-End Pipeline for JWST Time-Series Observations . The Journal of Open Source Software 7, 4503 (2022)

    2022

  27. [35]

    Nature Astronomy (2024)

    TJ Bell , et al., Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b . Nature Astronomy (2024)

    2024

  28. [36]

    Publications of the Astronomical Society of the Pacific 98, 609--617 (1986)

    K Horne , An optimal extraction algorithm for CCD spectroscopy. Publications of the Astronomical Society of the Pacific 98, 609--617 (1986)

    1986

  29. [37]

    The Astronomical Journal 157, 64 (2019)

    R Luger , et al., starry: Analytic Occultation Light Curves . The Astronomical Journal 157, 64 (2019)

    2019

  30. [38]

    The Astrophysical Journal 649, 1020 (2006)

    PK Williams, D Charbonneau, CS Cooper, AP Showman, JJ Fortney, Resolving the surfaces of extrasolar planets with secondary eclipse light curves. The Astrophysical Journal 649, 1020 (2006)

    2006

  31. [39]

    The Astrophysical Journal 664, 1199--1209 (2007)

    E Rauscher , et al., Toward Eclipse Mapping of Hot Jupiters . The Astrophysical Journal 664, 1199--1209 (2007)

    2007

  32. [40]

    The Astronomical Journal 168, 4 (2024)

    M Hammond , et al., Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS . The Astronomical Journal 168, 4 (2024)

    2024

  33. [41]

    Nature 620, 292--298 (2023)

    LP Coulombe , et al., A broadband thermal emission spectrum of the ultra-hot Jupiter WASP-18b . Nature 620, 292--298 (2023)

    2023

  34. [42]

    Annals of Statistics 6, 461--464 (1978)

    G Schwarz , Estimating the Dimension of a Model . Annals of Statistics 6, 461--464 (1978)

    1978

  35. [43]

    The Astronomical Journal 154, 220 (2017)

    D Foreman-Mackey , E Agol , S Ambikasaran , R Angus , Fast and Scalable Gaussian Process Modeling with Applications to Astronomical Time Series . The Astronomical Journal 154, 220 (2017)

    2017

  36. [44]

    Research Notes of the American Astronomical Society 2, 31 (2018)

    D Foreman-Mackey , Scalable Backpropagation for Gaussian Processes using Celerite . Research Notes of the American Astronomical Society 2, 31 (2018)

    2018

  37. [45]

    J Salvatier , TV Wiecki \^a , C Fonnesbeck , PyMC3: Python probabilistic programming framework (Astrophysics Source Code Library, record ascl:1610.016) (2016)

    2016

  38. [46]

    Statistical Science 7, 457--472 (1992)

    A Gelman , DB Rubin , Inference from Iterative Simulation Using Multiple Sequences . Statistical Science 7, 457--472 (1992)

    1992

  39. [47]

    Publications of the Astronomical Society of the Pacific 127, 1161 (2015)

    L Kreidberg , batman: BAsic Transit Model cAlculatioN in Python . Publications of the Astronomical Society of the Pacific 127, 1161 (2015)

    2015

  40. [48]

    Publications of the Astronomical Society of the Pacific 125, 306--312 (2013)

    D Foreman-Mackey , DW Hogg , D Lang , J Goodman , emcee: The MCMC Hammer . Publications of the Astronomical Society of the Pacific 125, 306--312 (2013)

    2013

  41. [49]

    MR Line , et al., A Systematic Retrieval Analysis of Secondary Eclipse Spectra. I. A Comparison of Atmospheric Retrieval Techniques . The Astrophysical Journal 775, 137 (2013)

    2013

  42. [50]

    AR Iyer , MR Line , PS Muirhead , JJ Fortney , E Gharib-Nezhad , The SPHINX M-dwarf Spectral Grid. I. Benchmarking New Model Atmospheres to Derive Fundamental M-dwarf Properties . The Astrophysical Journal 944, 41 (2023)

    2023

  43. [51]

    Astronomy & Astrophysics 553, A6 (2013)

    TO Husser , et al., A new extensive library of PHOENIX stellar atmospheres and synthetic spectra . Astronomy & Astrophysics 553, A6 (2013)

    2013

  44. [52]

    part 1: Analysis, (NASA Lewis Research Center), Technical Report 19950013764 (1994)

    S Gordon, BJ Mcbride, Computer program for calculation of complex chemical equilibrium compositions and applications. part 1: Analysis, (NASA Lewis Research Center), Technical Report 19950013764 (1994)

    1994

  45. [53]

    Nature 617, 483--487 (2023)

    SM Tsai , et al., Photochemically produced SO _ 2 in the atmosphere of WASP-39b . Nature 617, 483--487 (2023)

    2023

  46. [54]

    The Astrophysical Journal 911, 18 (2021)

    DJ Wilson , et al., The Mega-MUSCLES Spectral Energy Distribution of TRAPPIST-1 . The Astrophysical Journal 911, 18 (2021)

    2021

  47. [55]

    Astronomy & Astrophysics 564, A125 (2014)

    J Buchner , et al., X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue . Astronomy & Astrophysics 564, A125 (2014)

    2014

  48. [56]

    Monthly Notices of the Royal Astronomical Society 493, 4342--4354 (2020)

    J Taylor , et al., Understanding and mitigating biases when studying inhomogeneous emission spectra with JWST . Monthly Notices of the Royal Astronomical Society 493, 4342--4354 (2020)

    2020

  49. [57]

    The Astrophysical Journal 707, 24--39 (2009)

    N Madhusudhan , S Seager , A Temperature and Abundance Retrieval Method for Exoplanet Atmospheres . The Astrophysical Journal 707, 24--39 (2009)

    2009

  50. [58]

    SM Tsai , EKH Lee , R Pierrehumbert , A mini-chemical scheme with net reactions for 3D general circulation models. I. Thermochemical kinetics . Astronomy & Astrophysics 664, A82 (2022)

    2022

  51. [59]

    Journal of Geophysical Research (Planets) 126, e06655 (2021)

    P Gao , HR Wakeford , SE Moran , V Parmentier , Aerosols in Exoplanet Atmospheres . Journal of Geophysical Research (Planets) 126, e06655 (2021)

    2021

  52. [60]

    Nature 630, 831--835 (2024)

    DK Sing , et al., A warm Neptune's methane reveals core mass and vigorous atmospheric mixing . Nature 630, 831--835 (2024)

    2024

  53. [61]

    The Astrophysical Journal 881, 152 (2019)

    TD Komacek , AP Showman , V Parmentier , Vertical Tracer Mixing in Hot Jupiter Atmospheres . The Astrophysical Journal 881, 152 (2019)

    2019

  54. [62]

    The Astrophysical Journal 970, 71 (2024)

    JW Xuan , et al., Are These Planets or Brown Dwarfs? Broadly Solar Compositions from High-resolution Atmospheric Retrievals of 10 30 M _ Jup Companions . The Astrophysical Journal 970, 71 (2024)

    2024

  55. [63]

    Nature 632, 752--756 (2024)

    G Fu , et al., Hydrogen sulfide and metal-enriched atmosphere for a Jupiter-mass exoplanet . Nature 632, 752--756 (2024)

    2024

  56. [64]

    The Astrophysical Journal Letters 963, L5 (2024)

    Q Xue , et al., JWST Transmission Spectroscopy of HD 209458b: A Supersolar Metallicity, a Very Low C/O, and No Evidence of CH _ 4 , HCN, or C _ 2 H _ 2 . The Astrophysical Journal Letters 963, L5 (2024)

    2024

  57. [65]

    The Astronomical Journal 165, 91 (2023)

    M Brogi , et al., The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b . The Astronomical Journal 165, 91 (2023)

    2023

  58. [66]

    The Astrophysical Journal Letters 953, L24 (2023)

    PC August , et al., Confirmation of Subsolar Metallicity for WASP-77Ab from JWST Thermal Emission Spectroscopy . The Astrophysical Journal Letters 953, L24 (2023)

    2023

  59. [67]

    The Astronomical Journal 168, 14 (2024)

    M Weiner Mansfield , et al., The Metallicity and Carbon-to-oxygen Ratio of the Ultrahot Jupiter WASP-76b from Gemini-S/IGRINS . The Astronomical Journal 168, 14 (2024)

    2024

  60. [68]

    The Astron

    A Gressier , et al., JWST-TST DREAMS: A Supersolar Metallicity in WASP-17 b's Dayside Atmosphere from NIRISS SOSS Eclipse Spectroscopy . The Astron. J. 169, 57 (2025)

    2025

  61. [69]

    PCB Smith , et al., The Roasting Marshmallows Program with IGRINS on Gemini South. II. WASP-121 b has Superstellar C/O and Refractory-to-volatile Ratios . The Astronomical Journal 168, 293 (2024)

    2024

  62. [70]

    Science 276, 1836--1839 (1997)

    AP Boss , Giant planet formation by gravitational instability. Science 276, 1836--1839 (1997)

    1997

  63. [71]

    B Reipurth , D Jewitt , K Keil

    RH Durisen , et al., Gravitational Instabilities in Gaseous Protoplanetary Disks and Implications for Giant Planet Formation in Protostars and Planets V , eds. B Reipurth , D Jewitt , K Keil . p. 607 (2007)

    2007

  64. [72]

    arXiv e-prints p

    J Wang , Early Accretion of Large Amount of Solids for Directly-Imaged Exoplanets . arXiv e-prints p. arXiv:2310.00088 (2023)

    2023 arXiv

  65. [73]

    The Astrophysical Journal Letters 887, L20 (2019)

    L Welbanks , et al., Mass-Metallicity Trends in Transiting Exoplanets from Atmospheric Abundances of H _ 2 O, Na, and K . The Astrophysical Journal Letters 887, L20 (2019)

    2019

  66. [74]

    Astronomy & Astrophysics 434, 343--353 (2005)

    Y Alibert , C Mordasini , W Benz , C Winisdoerffer , Models of giant planet formation with migration and disc evolution . Astronomy & Astrophysics 434, 343--353 (2005)

    2005

  67. [75]

    C Mordasini , Y Alibert , W Benz , Extrasolar planet population synthesis. I. Method, formation tracks, and mass-distance distribution . Astronomy & Astrophysics 501, 1139--1160 (2009)

    2009

  68. [76]

    S Savvidou , B Bitsch , There is no disk mass budget problem of planet formation . Astron. & Astrophys. 693, A302 (2025)

    2025

  69. [77]

    Astronomy & Astrophysics 679, A42 (2023)

    S Savvidou , B Bitsch , How to make giant planets via pebble accretion . Astronomy & Astrophysics 679, A42 (2023)

    2023

  70. [78]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry add.period write newline FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION o...

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.