Image formation in coronagraphs due to mirror polarization aberrations
| dc.contributor.author | Chipman, Russell A. | |
| dc.date.accessioned | 2018-04-02T16:00:12Z | |
| dc.date.available | 2018-04-02T16:00:12Z | |
| dc.date.issued | 2017-11-27 | |
| dc.identifier.citation | Russell A. Chipman, "Image formation in coronagraphs due to mirror polarization aberrations", Proc. SPIE 10590, International Optical Design Conference 2017, 105901V (27 November 2017); doi: 10.1117/12.2291913; https://doi.org/10.1117/12.2291913 | en |
| dc.identifier.issn | 0277-786X | |
| dc.identifier.doi | 10.1117/12.2291913 | |
| dc.identifier.uri | http://hdl.handle.net/10150/627180 | |
| dc.description.abstract | The PSF for astronomical telescopes and instruments depends not only on geometric wavefront aberrations, but also on those polarization aberrations from the polarization properties of reflecting and transmitting surfaces. The image plane irradiance distribution is the linear superposition of four PSF images: one for each of the two orthogonal polarizations and one for each of two cross-coupled polarization terms. | |
| dc.language.iso | en | en |
| dc.publisher | SPIE-INT SOC OPTICAL ENGINEERING | en |
| dc.relation.url | https://www.spiedigitallibrary.org/conference-proceedings-of-spie/10590/2291913/Image-formation-in-coronagraphs-due-to-mirror-polarization-aberrations/10.1117/12.2291913.full | en |
| dc.rights | © 2017 SPIE. | en |
| dc.rights.uri | http://rightsstatements.org/vocab/InC/1.0/ | |
| dc.subject | Polarization aberration | en |
| dc.title | Image formation in coronagraphs due to mirror polarization aberrations | en |
| dc.type | Article | en |
| dc.identifier.eissn | 1996-756X | |
| dc.contributor.department | Univ Arizona, Coll Opt Sci | en |
| dc.identifier.journal | INTERNATIONAL OPTICAL DESIGN CONFERENCE 2017 | en |
| dc.description.collectioninformation | This 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.version | Final published version | en |
| refterms.dateFOA | 2018-09-12T07:10:16Z | |
| html.description.abstract | The PSF for astronomical telescopes and instruments depends not only on geometric wavefront aberrations, but also on those polarization aberrations from the polarization properties of reflecting and transmitting surfaces. The image plane irradiance distribution is the linear superposition of four PSF images: one for each of the two orthogonal polarizations and one for each of two cross-coupled polarization terms. |
