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    "title": "JWST transmission spectroscopy identifies carbon dioxide in WASP-39b",
    "summary": "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.",
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        "title": "Identification of carbon dioxide in an exoplanet atmosphere",
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        "date": "2022-08-24"
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        "title": "Early Release Science of the Exoplanet WASP-39b with JWST NIRSpec G395H",
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        "description": "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.",
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          "citation": "Identification of carbon dioxide in an exoplanet atmosphere",
          "url": "https://arxiv.org/pdf/2208.11692v1"
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      "statement": "# JWST transmission spectroscopy identifies carbon dioxide in WASP-39b\n\nThe 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.\n\n## Scientific scope\n\nThe 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.\n\n## Reading status\n\nThis 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.\n\n## People and systems\n\nEva-Maria Ahrer; Lili Alderson; Natalie M. Batalha\n\nThese 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.\n\n\n\n## Original sources\n\n- [Identification of carbon dioxide in an exoplanet atmosphere](https://arxiv.org/pdf/2208.11692v1)\n- [Early Release Science of the Exoplanet WASP-39b with JWST NIRSpec G395H](https://arxiv.org/pdf/2211.10488v1)\n",
      "summary": "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.",
      "title": "JWST transmission spectroscopy identifies carbon dioxide in WASP-39b"
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    "id": "jwst-ers-wasp39b-carbon-dioxide-transit-spectroscopy-2022",
    "entry_id": "jwst-ers-wasp39b-carbon-dioxide-transit-spectroscopy-2022",
    "revision": 1,
    "title": "JWST transmission spectroscopy identifies carbon dioxide in WASP-39b",
    "context": "Exoplanetary astronomy and spectroscopy",
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    "what_changed": "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.",
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    "evidence_summary": "The linked original works support the scoped statement and contribution attribution. WRS has not independently replayed experiments or reconstructed a full mathematical proof. 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.",
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