Studying a simple TPF-C

Details Studying a simple TPF-C Studying a simple TPF-C

Jul 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spie.6265e.111k&link_type=abstract

Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter. Edited by Mather, John C.; MacEwen, Howard A.; de Gr

Mathematics

Scientific paper

The NASA Terrestrial Planet Finder Coronagraph (TPF-C) mission envisions using a space telescope with an approximately 8 m by 3 m diameter primary mirror to image and spectroscopically characterize at visible wavelengths Earth-like planets orbiting nearby stars. Such terrestrial planets have intensities of 10-10 relative to their stars at separations of a fraction of an arcsecond, requiring extremely high-contrast imaging capabilities. A simple optical system with a minimal number of surfaces will likely have the best chance to image a very faint source near a bright star. A proposed version of a TPF-C integrated starlight suppression system and camera called SpeckleCam encompasses such a design. It incorporates two high-density deformable mirrors to control phase and amplitude wavefront errors, a coronagraph to suppress the stellar diffraction pattern, and simultaneous imaging in three passbands. We use the SpeckleCam concept to examine the utility of the PROPER modeling package, a set of IDL routines that simulate wavefront propagation in an optical system.

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