Biology
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21734309e&link_type=abstract
American Astronomical Society, AAS Meeting #217, #343.09; Bulletin of the American Astronomical Society, Vol. 43, 2011
Biology
Scientific paper
Of the 400+ extrasolar planets that have been discovered to date, the vast majority are massive gas giants. This is largely due to the inherent difficulty of detecting terrestrial planets, which are small and faint by comparison. Both NASA and ESA have proposed mission concepts for space-based observatories (Terrestrial Planet Finder [TPF] and Darwin, respectively) capable of detecting these planets by suppressing the light of their host stars, in order to discern the light reflected by the planetary companion. Following a successful detection, TPF/Darwin will then analyze the planet's spectrum to determine its chemical composition, and whether it may be capable of supporting life. Prior to the launch of such missions, we will need to understand the spectral characteristics of the planets we may find, and how detectable these characteristics will be. NASA's Virtual Planetary Laboratory (VPL) has generated synthetic spectra for a variety of possible planets, including the early and modern-day Earth, other planets in our solar system, and model planets around other stars. Using these spectra and a TPF-C simulator (provided by S. Heap and D. Lindler, GSFC), we have calculated the exposure times necessary to obtain the spectral resolution required to identify signs of habitability and life, such as the presence of oxygen and liquid water. By determining the detectability of key spectral characteristics within the limitations of a mission concept such as TPF, we hope to evaluate and quantify what is essential for a successful future planet-characterizing mission. Support for this work was provided by the NASA Astrobiology Institute's Virtual Planetary Laboratory.
Domagal-Goldman Shawn D.
Evans Nicole
Meadows Victoria S.
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