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Exoplanet Transmission Spectroscopy/Evidence
Method evidence record

Exoplanet Transmission Spectroscopy

Transmission spectroscopy is a technique for studying the atmospheres of exoplanets by analyzing the light passing through the planetary atmosphere during transit. Pioneered by David Charbonneau in 2002 with the detection of sodium in HD 209458b's atmosphere, this method has become the primary tool for characterizing exoplanet atmospheres and searching for biosignatures.

Sources recorded, not reviewed

Source record

Citations copied verbatim from the method’s source record. No claim-level verification is inferred from them.

Transmission Spectroscopy for Exoplanet Atmosphere Characterization
Taxonomic method record · process-pipeline / astronomy
  • Charbonneau, D., Brown, T. M., Noyes, R. W., & Gilliland, R. L. (2002). Detection of an atmospheric trace constituent in the transmission spectrum of a distant extrasolar planet. Astrophysical Journal, 568(1), 377-384. · DOI 10.1086/338770
  • Kreidberg, L., et al. (2014). A precise water abundance measurement for the hot Jupiter WASP-43b. Astrophysical Journal Letters, 793(2), L15. · DOI 10.1088/2041-8205/793/2/l27
  • Sing, D. K., et al. (2016). The atmospheric circulation of hot Jupiters. Nature, 529(7584), 59-62. · URL
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Curated claims

Claims persisted in the evidence ledger, each with its own assessment.

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Related methods

Generated from the method graph and shown as machine-suggested relations — no evidence claim is inferred.

Same method familyRadiative Transfermachine-suggested · Relational suggestion, not evidence.Same method familySED Fittingmachine-suggested · Relational suggestion, not evidence.Same method familyTransit Photometrymachine-suggested · Relational suggestion, not evidence.

Evidence status

Sources recorded, not reviewed

Bibliographic sources are present. Claim-level evidence review has not been performed.

Sources

3 recorded citations, copied from the method source record.

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