TPF-I SWG Report - Exoplanet Exploration Program - NASA

TPF-I F L I G H T B ASELINE D ESIGN
once. Additionally, the completeness per star varies in the new simulation. In general, the closer stars are
more complete than those that are further away. The completeness per star as a function of angular radius
to the mid-HZ and distance to the star is shown in Fig. 5-29.
The completeness calculations for this simulation are lower than previous estimations because there is
now more fidelity in the current model. We compute planet flux as a function of HZ distance in the new
simulations. Because there is a sharp fall-off in the mid-IR flux in the outer HZ, fewer outer HZ planets
are observable. Furthermore, if we map completeness across the HZ, there is a marked fall-off of
completeness as a function of pseudo-planet distance. Future work includes a study of the effect of forced
revisits on completeness.
5.9 References
Lay, O. P., “Imaging properties of rotating nulling interferometers,” Appl. Opt. 44, 5859–5871 (2005).
Martin, S., “The flight instrument design for the Terrestrial Planet Finder Interferometer,” Techniques and
Instrumentation for Detection of Exoplanets II, Proc. SPIE 5905, edited by D. R. Coulter, 21–35
(2005).
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