6 September 2017 Challenges in coronagraph optical design
Author Affiliations +
Abstract
The point spread function (PSF) for astronomical telescopes and instruments depends not only on geometric aberrations and scalar wave diffraction, but also on the apodization and wavefront errors introduced by coatings on reflecting and transmitting surfaces within the optical system. Geometrical ray tracing provides incomplete image simulations for exoplanet coronagraphs with the goal of resolving planets with a brightness less than 10^-9 of their star located within 3 Airy disk radii. The Polaris-M polarization analysis program calculates uncorrected coating polarization aberrations couple around 10^-5 light into crossed polarized diffraction patterns about twice Airy disk size. These wavefronts not corrected by the deformable optics systems. Polarization aberrations expansions have shown how image defects scale with mirror coatings, fold mirror angles, and numerical aperture.
Conference Presentation
© (2017) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Russell A. Chipman, Russell A. Chipman, } "Challenges in coronagraph optical design", Proc. SPIE 10374, Optical Modeling and Performance Predictions IX, 1037403 (6 September 2017); doi: 10.1117/12.2274055; https://doi.org/10.1117/12.2274055
PROCEEDINGS
12 PAGES + PRESENTATION

SHARE
RELATED CONTENT

The Polaris-M ray tracing program
Proceedings of SPIE (August 31 2015)
Form birefringent microstructures: modeling and design
Proceedings of SPIE (April 19 1995)
Hughes Danbury technology transfer program
Proceedings of SPIE (October 12 1995)

Back to Top