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dc.contributor.authorChipman, Russell A.
dc.date.accessioned2018-04-02T18:29:45Z
dc.date.available2018-04-02T18:29:45Z
dc.date.issued2017-09-06
dc.identifier.citationRussell 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/10.1117/12.2274055en
dc.identifier.issn0277-786X
dc.identifier.issn1996-756X
dc.identifier.doi10.1117/12.2274055
dc.identifier.urihttp://hdl.handle.net/10150/627190
dc.description.abstractThe 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.
dc.language.isoenen
dc.publisherSPIE-INT SOC OPTICAL ENGINEERINGen
dc.relation.urlhttps://www.spiedigitallibrary.org/conference-proceedings-of-spie/10374/2274055/Challenges-in-coronagraph-optical-design/10.1117/12.2274055.fullen
dc.rights© (2017) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE).en
dc.subjectPolarizationen
dc.subjectcoronagraphen
dc.subjectimagingen
dc.subjectpolarization aberrationen
dc.subjectpolarization ray tracingen
dc.titleChallenges in coronagraph optical designen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Coll Opt Scien
dc.identifier.journalOPTICAL MODELING AND PERFORMANCE PREDICTIONS IXen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-09-12T07:10:45Z
html.description.abstractThe 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.


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