Phosphine Gas in the Cloud Decks of Venus

Abstract

Measurements of trace-gases in planetary atmospheres help us explore chemical conditions different to those on Earth. Our nearest neighbor, Venus, has cloud decks that are temperate but hyper-acidic. We report the apparent presence of phosphine (PH3) gas in Venusian atmosphere, where any phosphorus should be in oxidized forms. Single-line millimeter-waveband spectral detections (quality up to ~15 sigma) from the JCMT and ALMA telescopes have no other plausible identification. Atmospheric PH3 at ~20 parts-per-billion abundance is inferred. The presence of phosphine is unexplained after exhaustive study of steady-state chemistry and photochemical pathways, with no currently-known abiotic production routes in Venusian atmosphere, clouds, surface and subsurface, or from lightning, volcanic or meteoritic delivery. Phosphine could originate from unknown photochemistry or geochemistry, or, by analogy with biological production of phosphine on Earth, from the presence of life. Other PH3 spectral features should be sought, while in-situ cloud and surface sampling could examine sources of this gas.

References in corpus (6)

• Phosphine as a Biosignature Gas in Exoplanet Atmospheres
• Hydrogen Cyanide in Nitrogen-Rich Atmospheres of Rocky Exoplanets
• The Venusian Lower Atmosphere Haze as a Depot for Desiccated Microbial Life: A Proposed Life Cycle for Persistence of the Venusian Aerial Biosphere
• Toward the analysis of JWST exoplanet spectra: Identifying troublesome model parameters
• Spectroscopic Analysis in the Virtual Observatory Environment with SPLAT-VO
• Tunnelling splitting in the phosphine molecule

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• The statistical reliability of 267 GHz JCMT observations of Venus: No significant evidence for phosphine absorption
• Complications in the ALMA Detection of Phosphine at Venus
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• Phosphine in the Venusian Atmosphere: A Strict Upper Limit from SOFIA GREAT Observations
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• On the Robustness of Phosphine Signatures in Venus' Clouds
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• Large Interferometer For Exoplanets (LIFE): VIII. Where is the phosphine? Observing exoplanetary PH3 with a space based MIR nulling interferometer
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• Dynamics and Clouds in Planetary Atmospheres from Telescopic Observations
• Detecting Biosignatures in the Atmospheres of Gas Dwarf Planets with the James Webb Space Telescope
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