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Exploring exoplanetary systems beyond 1AU with WFIRST

Published online by Cambridge University Press:  06 January 2014

Matthew T. Penny
Affiliation:
Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH, USA43210 email: penny@astronomy.ohio-state.edu, gaudi@astronomy.ohio-state.edu
B. Scott Gaudi
Affiliation:
Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH, USA43210 email: penny@astronomy.ohio-state.edu, gaudi@astronomy.ohio-state.edu
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Abstract

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The Wide Field InfraRed Survey Telescope (WFIRST) was the top ranked large space mission of the New Worlds, New Horizons Decadal Survey, and is currently under active study by NASA. Its primary instrument will be a large-format high-resolution near-infrared imager and slitless spectrometer. A primary goal of WFIRST will be to perform a high-cadence microlensing survey of the Galactic bulge to search for low-mass exoplanets beyond the ice line. We highlight some of the expected results of the WFIRST exoplanet survey. For example, the survey will probe the abundance of Earth-mass planets from less than 1 AU outwards, including free-floating planets. In its peak sensitivity range of ~2–5 AU, WFIRST will be sensitive to planets with masses lower than Mercury, and even down to the mass of Ganymede. Overall, WFIRST is expected to detect several thousand bound planets, in addition to several thousand free-floating planets. WFIRST will complete the exoplanet census begun by Kepler, enabling an unprecedented understanding of planetary systems and their formation.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2013 

References

Green, J., et al. 2012, arXiv 1208.4012Google Scholar
Spergel, D., et al. 2013, arXiv 1305.5422Google Scholar
Penny, M. T., et al. 2013, MNRAS, 434, 2CrossRefGoogle Scholar
Cassan, A., et al. 2012, Nature 481, 167Google Scholar