Published July 1, 2020 | Version v1
Journal article

A Geologically Robust Procedure for Observing Rocky Exoplanets to Ensure that Detection of Atmospheric Oxygen Is a Modern Earth-like Biosignature

  • 1. Applied Physics Laboratory, Johns Hopkins University, 11100 Johns Hopkins Rd., Laurel, MD 20723 (United States)
  • 2. School of Earth and Space Exploration, Arizona State University, P.O. Box 871404, Tempe, AZ 85287-1404 (United States)
  • 3. Department of Earth and Planetary Sciences, University of California, Riverside, 900 University Ave., Riverside, CA 92521 (United States)
  • 4. Southwest Research Institute, San Antonio, TX 28510 (United States)
  • 5. Jet Propulsion Laboratory, 4800 Oak Grove Dr., MS 321-100, Pasadena, CA 91109-8099 (United States)

Description

In the next decades, the astrobiological community will debate whether the first observations of oxygen in an exoplanet's atmosphere signify life, so it is critical to establish procedures now for collection and interpretation of such data. We present a step-by-step observational strategy for using oxygen as a robust biosignature to prioritize exoplanet targets and design future observations. It is premised on avoiding planets lacking subaerial weathering of continents, which would imply geochemical cycles drastically different from modern Earth's, precluding use of oxygen as a biosignature. The strategy starts with the most readily obtained data: orbital semimajor axis and stellar luminosity to ensure residence in the habitable zone and stellar X-ray/ultraviolet flux to ensure an exoplanet can retain a secondary (outgassed) atmosphere. Next, high-precision mass and radius information should be combined with high-precision stellar abundance data to constrain the exoplanet's water content; those incompatible with <0.1 wt% H2O can be deprioritized. Then, reflectance photometry or low-resolution transmission spectroscopy should confirm an optically thin atmosphere. Subsequent long-duration, high-resolution transmission spectroscopy should search for oxygen and ensure that water vapor and CO2 are present only at low (∼102–104 ppm levels). Assuming oxygen is found, attribution to life requires the most difficult step, acquisition of a detailed, multispectral light curve of the exoplanet, to ensure both surface land and water. Exoplanets failing some of these steps might be habitable, even have observable biogenic oxygen, but should be deprioritized because oxygen could not be attributed unambiguously to life, and life therefore would not be detectable on such planets. Finally, we show how to use this scheme for the solar system, the 55 Cnc system, and the TRAPPIST-1 system, in which only the Earth and TRAPPIST-1e successfully pass through our procedure.

Availability note (English)

Available from http://dx.doi.org/10.3847/2041-8213/ab9b91

Additional details

Identifiers

Publishing Information

Journal Title
Astrophysical Journal Letters
Journal Volume
898
Journal Issue
1
Journal Page Range
[9 p.]
ISSN
2041-8205