What is recorded here?
The JWST Transiting Exoplanet Community Early Release Science Team observed a transit of the hot gas giant WASP-39b and measured a strong approximately 4.3-micrometre absorption feature, attributed to carbon dioxide from its spectral shape. Four reductions of the same observing dataset yielded similar spectra. A separate G395H transit spectrum showed additional absorption near 4.1 micrometres, interpreted as sulfur dioxide by model comparison.
Source-linked catalogue note. A detailed explanatory guide has not yet been prepared for this entry.
Scientific scope
The 26-sigma feature significance is the authors’ model comparison for this one dataset; the four reductions are not four independent transits. The study analyzes the unsaturated 3.0–5.5 micrometre region. Its approximately ten-times-solar metallicity fit is a model-grid result under one-dimensional radiative, convective and thermochemical equilibrium assumptions, not a fully quantified model-independent abundance. A smaller approximately 4.0-micrometre feature was tentative and unidentified in this v1. Previous water and alkali observations and broad-band hints of carbon dioxide remain distinct prior contributions. The individual contributor list shown here is incomplete. The independent 30–31 July 2022 G395H observation is a single later transit, not the 10 July PRISM observation. Its eleven processing and fitting pipelines analyze the same data, not independent transits; a mid-transit mirror-tilt event required treatment. SO2 identification at 4.8 sigma is the authors’ Bayesian gas-removal model comparison; a Gaussian residual test gives 3.5 sigma and cannot identify the absorber by itself. A 4.56-micrometre feature at 3.3 sigma remained unexplained; CO was not robustly confirmed. Photochemical formation is an interpretation, not a directly measured mechanism. The original and later papers have separate, incompletely listed contributors.
Read the original work
- Identification of carbon dioxide in an exoplanet atmosphere
- Early Release Science of the Exoplanet WASP-39b with JWST NIRSpec G395H
This English explanation is an editorial reading view. It does not replace the complete original work or certify its science.
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People and systems
Eva-Maria Ahrer; Lili Alderson; Natalie M. Batalha
These are the listed authors of the cited contribution sources. Paper authorship does not quantify individual effort. An incomplete list is explicitly marked; same names are not automatically merged. The recorded author list is incomplete.
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English catalogue narrative
JWST transmission spectroscopy identifies carbon dioxide in WASP-39b
The JWST Transiting Exoplanet Community Early Release Science Team observed a transit of the hot gas giant WASP-39b and measured a strong approximately 4.3-micrometre absorption feature, attributed to carbon dioxide from its spectral shape. Four reductions of the same observing dataset yielded similar spectra. A separate G395H transit spectrum showed additional absorption near 4.1 micrometres, interpreted as sulfur dioxide by model comparison.
Scientific scope
The 26-sigma feature significance is the authors’ model comparison for this one dataset; the four reductions are not four independent transits. The study analyzes the unsaturated 3.0–5.5 micrometre region. Its approximately ten-times-solar metallicity fit is a model-grid result under one-dimensional radiative, convective and thermochemical equilibrium assumptions, not a fully quantified model-independent abundance. A smaller approximately 4.0-micrometre feature was tentative and unidentified in this v1. Previous water and alkali observations and broad-band hints of carbon dioxide remain distinct prior contributions. The individual contributor list shown here is incomplete. The independent 30–31 July 2022 G395H observation is a single later transit, not the 10 July PRISM observation. Its eleven processing and fitting pipelines analyze the same data, not independent transits; a mid-transit mirror-tilt event required treatment. SO2 identification at 4.8 sigma is the authors’ Bayesian gas-removal model comparison; a Gaussian residual test gives 3.5 sigma and cannot identify the absorber by itself. A 4.56-micrometre feature at 3.3 sigma remained unexplained; CO was not robustly confirmed. Photochemical formation is an interpretation, not a directly measured mechanism. The original and later papers have separate, incompletely listed contributors.
Reading status
This is a source-linked WRS catalogue note. A full explanatory guide and independent scientific reconstruction have not been completed for this entry. Read the identified original work for its complete narrative and arguments.
People and systems
Eva-Maria Ahrer; Lili Alderson; Natalie M. Batalha
These are the listed authors of the cited contribution sources. Paper authorship does not quantify individual effort. An incomplete list is explicitly marked; same names are not automatically merged.