[ { "id": "authors:b0a4s-1w889", "collection": "authors", "collection_id": "b0a4s-1w889", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201109-112630553", "type": "book_section", "title": "Topological pupil segmentation and point spread function analysis for large aperture imaging systems", "book_title": "AOPC 2020: Optics Ultra Precision Manufacturing and Testing", "author": [ { "family_name": "Feng", "given_name": "Yi-Ting", "clpid": "Feng-Yi-Ting" }, { "family_name": "Ashcraft", "given_name": "Jaren Nicholas", "clpid": "Ashcraft-Jaren-N" }, { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Harvey", "given_name": "James E.", "clpid": "Harvey-J-E" }, { "family_name": "Douglas", "given_name": "Ewan S.", "clpid": "Douglas-E-S" }, { "family_name": "Choi", "given_name": "Heejoo", "clpid": "Choi-Hejoo" }, { "family_name": "Lillie", "given_name": "Charles", "clpid": "Lillie-C-F" }, { "family_name": "Hull", "given_name": "Tony", "clpid": "Hull-T" }, { "family_name": "Kim", "given_name": "Dae Wook", "clpid": "Kim-Dae-Wook" } ], "contributor": [ { "family_name": "Kong", "given_name": "Lingbao", "clpid": "Kong-Lingbao" }, { "family_name": "Zhang", "given_name": "Dawei", "clpid": "Zhang-Dawei" }, { "family_name": "Luo", "given_name": "Xichun", "clpid": "Luo-Xichun" } ], "abstract": "Future large aperture telescopes and high contrast imaging systems will often include segment gaps, structural obscurations, along with outer edges which produce diffraction effects that are disadvantageous to high contrast imaging (e.g., for exoplanet detection) or continuous wavefront control across the optical aperture. We present an optimization strategy for several pupil segment topologies for next-generation telescope concepts. Wave propagation results based on diffraction-limited point spread function analyses using Fraunhofer diffraction theory are presented using the Python-based POPPY simulation tool.", "doi": "10.1117/12.2575809", "isbn": "9781510639577", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2020-11-05", "pages": "Art. No. 115680I" }, { "id": "authors:2rg0z-8x231", "collection": "authors", "collection_id": "2rg0z-8x231", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200826-131025019", "type": "book_section", "title": "Physical optics analysis of image formation in science instruments", "book_title": "Roland V. Shack Memorial Session: A Celebration of One of the Great Teachers of Optical Aberration Theory", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Lehan", "given_name": "John P.", "clpid": "Lehan-J-P" } ], "abstract": "Several factors affect image quality in scientific measurement systems. These factors were subjects researched and taught by Professor Roland Shack during his career. We examine image formation in science instruments within the frame-work of our current understanding of physical optics. Our motivation is to increase instrument scientific yield and minimize cost. We consider the collective effects of polarization aberrations, partial coherence, optical materials, diffraction, optical surface count, scattered light (bulk and surface) and 1st order optical system mechanical lay-out.", "doi": "10.1117/12.2567356", "isbn": "9781510637641", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "publication_date": "2020-08-24", "pages": "Art. No. 1147904" }, { "id": "authors:jd307-18d93", "collection": "authors", "collection_id": "jd307-18d93", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190913-081328146", "type": "book_section", "title": "ExoPlanet Optics: conceptual design processes for stealth telescopes", "book_title": "UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts IX", "author": [ { "family_name": "Breckinridge", "given_name": "J. B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Harvey", "given_name": "J. E.", "clpid": "Harvey-J-E" }, { "family_name": "Irvin", "given_name": "R.", "clpid": "Irvin-R-G" }, { "family_name": "Chipman", "given_name": "R.", "clpid": "Chipman-R-A" }, { "family_name": "Kupinski", "given_name": "M.", "clpid": "Kupinski-M" }, { "family_name": "Davis", "given_name": "J.", "clpid": "Davis-Jeffrey" }, { "family_name": "Kim", "given_name": "D. W.", "clpid": "Kim-Dae-Wook" }, { "family_name": "Ewan", "given_name": "D.", "clpid": "Ewan-D-S" }, { "family_name": "Lillie", "given_name": "C. F.", "clpid": "Lillie-C-F" }, { "family_name": "Hull", "given_name": "T.", "clpid": "Hull-T-B" } ], "contributor": [ { "family_name": "Barto", "given_name": "Allison A.", "clpid": "Barto-A-A" }, { "family_name": "Breckinridge", "given_name": "James B.", "clpid": "Breckinridge-J-B" }, { "family_name": "Stahl", "given_name": "H. Philip", "clpid": "Stahl-H-P" } ], "abstract": "In this paper we examine several contrast-degrading static signature sources present in current terrestrial exoplanet Lyot Coronagraph/Telescope optical systems. These are: - Unnecessary optical surfaces, which increase cost, absorption, scatter, wavefront control and alignment issues. A suggested solution is to make every effort to investigate innovative solutions to reduce the number of optical surfaces during the early design phase. Consider free-form optics. - Diffraction from secondary support systems and classical hexagon segmented apertures, which masks the low IWA terrestrial exoplanets. A suggested mitigation is to investigate curved secondary support systems and a pinwheel architecture for the deployable primary aperture. - Polarization Fresnel and form birefringence aberrations, which distort the system PSF, introduce absorption, scatter and wavefront control issues. Mitigation is to reduce all ray-angles of incidence to a minimum, investigate zero-loss polarization compensation wavefront technology, and investigate metal thin film deposition processes required to minimize form birefringence in large-area high-reflectivity coatings. - Small-angle specular or resolved angle scattered light, which places a narrow halo of incoherent light around the base of the PSF. There is no requirement on mirror smooth-surface scatter. Investigate the physical source of the small angle scatter and develop mirror polishing and thin film deposition processes to minimize scatter.", "doi": "10.1117/12.2528825", "isbn": "9781510629233", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2019-09-09", "pages": "Art. No. 111150H" }, { "id": "authors:q3gh5-tcx19", "collection": "authors", "collection_id": "q3gh5-tcx19", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190913-072409336", "type": "book_section", "title": "Numerical modeling of the Habex coronagraph", "book_title": "Techniques and Instrumentation for Detection of Exoplanets IX", "author": [ { "family_name": "Krist", "given_name": "John", "clpid": "Krist-John-E" }, { "family_name": "Martin", "given_name": "Stefan", "clpid": "Martin-S-R" }, { "family_name": "Kuan", "given_name": "Gary", "clpid": "Kuan-Gary" }, { "family_name": "Mennesson", "given_name": "Bertrand", "orcid": "0000-0003-4205-4800", "clpid": "Mennesson-B" }, { "family_name": "Ruane", "given_name": "Garreth", "orcid": "0000-0003-4769-1665", "clpid": "Ruane-G-J" }, { "family_name": "Saini", "given_name": "Navtej", "clpid": "Saini-N-S" }, { "family_name": "Trauger", "given_name": "John", "clpid": "Trauger-J-T" }, { "family_name": "Breckinridge", "given_name": "James", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Mawet", "given_name": "Dimitri", "orcid": "0000-0002-8895-4735", "clpid": "Mawet-D" }, { "family_name": "Stahl", "given_name": "Philip", "clpid": "Stahl-P" }, { "family_name": "Davis", "given_name": "Jeffrey", "clpid": "Davis-J" } ], "contributor": [ { "family_name": "Shaklan", "given_name": "Stuart B.", "clpid": "Shaklan-S-B" } ], "abstract": "The Habex study, commissioned by NASA in preparation for the 2020 Decadal Survey, is evaluating a 4 meter space telescope for high contrast imaging and spectral characterization of extrasolar terrestrial planets. Its off-axis configuration, active structural metrology, and low-disturbance pointing control provide an optimal system for coronagraphs. We present predictions of the Habex performance using a charge 6 vortex coronagraph that have been obtained using numerical modeling techniques developed for the WFIRST coronagraph. The models include realistic optical surface and polarization-induced aberrations, pointing jitter, and thermally-induced wavefront variations. Wavefront control using dual deformable mirrors is simulated to create a dark, high-contrast hole around the star. The results show that current technologies can closely approach the Habex performance goals, and with some additional development in key areas (e.g., deformable mirror surface quality, low-polarization coatings, etc.) over the next few years they should reliably meet them.", "doi": "10.1117/12.2530462", "isbn": "9781510629271", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2019-09-09", "pages": "Art. No. 1111705" }, { "id": "authors:ysyz4-3ms44", "collection": "authors", "collection_id": "ysyz4-3ms44", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181220-092841023", "type": "book_section", "title": "Novel designs for minimizing diffraction effects of large segmented mirror telescopes", "book_title": "Current Developments in Lens Design and Optical Engineering XIX", "author": [ { "family_name": "Harvey", "given_name": "James E.", "clpid": "Harvey-J-E" }, { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Irvin", "given_name": "Ryan G.", "clpid": "Irvin-R-G" }, { "family_name": "Pfisterer", "given_name": "Richard N.", "clpid": "Pfisterer-R-N" } ], "contributor": [ { "family_name": "Johnson", "given_name": "R. Barry", "clpid": "Johnson-R-B" }, { "family_name": "Mahajan", "given_name": "Virendra N.", "clpid": "Mahajan-V-N" }, { "family_name": "Thibault", "given_name": "Simon", "clpid": "Thibault-S" } ], "abstract": "Diffraction effects of large segmented mirror gaps and secondary mirror support struts produce diffraction peaks or flares that are a detriment to exoplanet detection. In this paper we present a detailed diffraction analysis of innovative segmented mirror concepts utilizing curved segment gaps and secondary support struts that eliminate these diffraction spikes that can obscure the faint exoplanet image. The resulting diffraction performance will be quantitatively compared to that of both monolithic circular pupils and classical hexagonally segmented mirrors. We will utilize performance-based merit functions consisting of both radial and azimuthal profiles of the resulting telescope point spread function.", "doi": "10.1117/12.2326923", "isbn": "9781510620612", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2018-09-17", "pages": "Art. No. 107450L" }, { "id": "authors:x0c3j-0m319", "collection": "authors", "collection_id": "x0c3j-0m319", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190823-134014912", "type": "book_section", "title": "HabEx polarization ray trace and aberration analysis", "book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Davis", "given_name": "Jeffrey", "clpid": "Davis-Jeffrey" }, { "family_name": "Kupinski", "given_name": "Meredith K.", "clpid": "Kupinski-M-K" }, { "family_name": "Chipman", "given_name": "Russell A.", "clpid": "Chipman-R-A" }, { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Lystrup", "given_name": "Mackenzie", "clpid": "Lystrup-M" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Fazio", "given_name": "Giovanni G.", "clpid": "Fazio-G-G" }, { "family_name": "Batalha", "given_name": "Natalie", "clpid": "Batalha-N-M" }, { "family_name": "Siegler", "given_name": "Nicholas", "clpid": "Siegler-N" }, { "family_name": "Tong", "given_name": "Edward C.", "clpid": "Tong-E-C" } ], "abstract": "The flux difference between a terrestrial exoplanet and a much brighter nearby star creates an enormous optical design challenge for space-based imaging systems. Coronagraphs are designed to block the star's flux and obtain a high-dynamic-range image of the exoplanet. The contrast of an optical system is calculated using the point spread function (PSF). Contrast quantifies starlight suppression of an imaging system at a given separation of the two objects. Contrast requirements can be as small as 10^(\u221210) for earth-like planets. This work reports an analysis of the September 2017 Habitable Exoplanet Imaging Mission (HabEx) end-to-end optical system prescription for geometric and polarization aberrations across the 450 to 550 nm channel. The Lyot coronagraph was modeled with a vector vortex charge 6 mask but without adaptive optics (AO) to correct the phase of the Jones pupil. The detector plane irradiance was calculated for three states of the telescope/coronagraph system: (1) free of geometric and polarization aberrations; (2) isotropic mirror coatings throughout the end-toend system; and (3) isotropic mirrors with form birefringence on the primary mirror. For each of these three states the system response both with and without a coronagraph mask was calculated. Two merit functions were defined to quantify the system's ability to attenuate starlight: (1) normalized polychromatic irradiance (NPI), and (2) starlight suppression factor (SSF). Both of these are dimensionless and their values are functions of position across the focal plane. The NPI is defined as the irradiance point-by-point across the detector plane with a coronagraph mask divided by the value of the on-axis irradiance without a coronagraph mask. The SSF is the irradiance point-by-point across the detector plane with a coronagraph mask divided by the pointby-point value of the irradiance across the detector plane without a coronagraph mask. Both the NPI and the SSF provide insights into coronagraph performance. Deviations from the aberration-free case are calculated and summarized in table 2. The conclusions are: (1) the HabEx optical system is well-balanced for both geometric and polarization aberrations; (2) the spatially dependent polarization reflectivity for the HabEx primary mirror should be specified to ensure the coating is isotropic; (3) AO to correct the two orthogonal polarization-dependent wavefront errors is essential.", "doi": "10.1117/12.2313670", "isbn": "9781510619494", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2018-07-16", "pages": "Art. No. 106983H" }, { "id": "authors:jnf4j-c8s17", "collection": "authors", "collection_id": "jnf4j-c8s17", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180718-154034697", "type": "book_section", "title": "Terrestrial exoplanet coronagraph image quality polarization aberrations in Habex", "book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Breckinridge", "given_name": "J. B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Kupinski", "given_name": "M.", "clpid": "Kupinski-M" }, { "family_name": "Davis", "given_name": "J.", "clpid": "Davis-J" }, { "family_name": "Daugherty", "given_name": "B.", "clpid": "Daugherty-B" }, { "family_name": "Chipman", "given_name": "R. A.", "clpid": "Chipman-R-A" } ], "contributor": [ { "family_name": "Lystrup", "given_name": "Makenzie", "clpid": "Lyastrup-M" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Fazio", "given_name": "Giovanni G.", "clpid": "Fazio-G-G" }, { "family_name": "Batalha", "given_name": "Natalie", "clpid": "Batalha-N-M" }, { "family_name": "Siegler", "given_name": "Nicholas", "clpid": "Siegler-N" }, { "family_name": "Tong", "given_name": "Edward C.", "clpid": "Tong-Edward-C" } ], "abstract": "Direct imaging and spectroscopy of terrestrial exoplanets requires the control of vector electromagnetic fields to approximately one part in ten to the fifth over a few milliarc second FOV to achieve the necessary 10-10 intensity contrast levels. Observations using space telescopes are necessary to achieve these levels of diffracted and scattered light control. The highly reflecting metal mirrors and their coatings needed to image these very faint exoplanets introduce polarization into the wavefront, which, in turn affects image quality and reduces exoplanet yield unless corrected. To identify and create the technologies and the electro-optical/mechanical-spacecraft systems models that will achieve these levels, NASA is currently developing two mission concepts, each with their own hardware vision. These are: The Habex, a habitable planet explorer and the LUVOIR, a Large Ultra-Violet Optical-Infrared space telescope system. This paper reports the results of polarization ray-tracing the HabEx detailed optical prescription provided by the project to the authors in the fall of 2017. Diattenuation and retardance across both the exit pupil associated with the occulting mask and the exit pupil associated with the coronagraph image plane are given as well as the corresponding Jones pupil matrices. These are calculated assuming isotropic coatings on all mirrors. Analysis and physical measurements indicates that the specification of the primary mirror for exoplanet coronagraphs will need to include a constraint on spatially varying polarization reflectivity (anisotropic coatings). The Jones exit-pupil phase terms, phi XX and phi YY just before the occulting mask differ in shape and are displaced one from the other by about 10 milli-waves. This shows that A/O, which corrects for geometric path differences, cannot completely correct for wavefront errors introduced by polarization for this particular prescription for HabEx. We suggest that these differences may be corrected by adjusting the opto-mechanical design to change angles of incidence on mirrors and corrected by adjusting the design of the dielectric coatings on the highly-reflecting mirror surfaces. Super-posing the phase of XX onto the phase of YY and then correcting using A/O will assure maximum power transmittance through the system and best contrast. These aspects require further investigation.", "doi": "10.1117/12.2311880", "isbn": "9781510619494", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2018-07-06", "pages": "Art. No. 106981D" }, { "id": "authors:4q5b0-vr031", "collection": "authors", "collection_id": "4q5b0-vr031", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180718-152258159", "type": "book_section", "title": "The role of narrow-angle forward surface scatter and particulate scatter in exoplanet exploration", "book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Pfisterer", "given_name": "Richard N.", "clpid": "Pfisterer-R-N" }, { "family_name": "Harvey", "given_name": "James E.", "clpid": "Harvey-J-E" }, { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Lystrup", "given_name": "Makenzie", "clpid": "Lystrup-M" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Fazio", "given_name": "Giovanni G.", "clpid": "Fazio-G-G" }, { "family_name": "Batalha", "given_name": "Natalie", "clpid": "Batalha-N-M" }, { "family_name": "Siegler", "given_name": "Nicholas", "clpid": "Siegler-N" }, { "family_name": "Tong", "given_name": "Edward C.", "clpid": "Tong-Edward-C" } ], "abstract": "It is often thought that because of the very small solid angle subtended by the field-of-view of the coronagraph, scattered light from optical surfaces will have no effect on images recorded for terrestrial exoplanet spectroscopy. In this paper, we examine mirror surface scatter and particulate contamination scatter as sources of background light or noise signal in large aperture terrestrial exoplanet telescope/coronagraph systems. Scattered light control to one part in 10^(+10) or better is required for exoplanet exploration. We will discuss the optical fabrication tolerances necessary to minimize narrowangle forward scatter and their relative effects upon direct imaging coronagraph instruments used to characterize terrestrial exoplanets.", "doi": "10.1117/12.2314229", "isbn": "9781510619494", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2018-07-06", "pages": "Art. No. 106985F" }, { "id": "authors:cgckk-hpy45", "collection": "authors", "collection_id": "cgckk-hpy45", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180718-152857173", "type": "book_section", "title": "Diffraction analysis of large segmented mirror concepts for exoplanet exploration", "book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Harvey", "given_name": "James E.", "clpid": "Harvey-J-E" }, { "family_name": "Irvin", "given_name": "Ryan G.", "clpid": "Irvin-R-G" }, { "family_name": "Crabtree", "given_name": "Karlton", "clpid": "Crabtree-K" }, { "family_name": "Pfisterer", "given_name": "Richard N.", "clpid": "Pfisterer-R-N" }, { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Lystrup", "given_name": "Makenzie", "clpid": "Lystrup-M" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Fazio", "given_name": "Giovanni G.", "clpid": "Fazio-G-G" }, { "family_name": "Batalha", "given_name": "Natalie", "clpid": "Batalha-N-M" }, { "family_name": "Siegler", "given_name": "Nicholas", "clpid": "Siegler-N" }, { "family_name": "Tong", "given_name": "Edward C.", "clpid": "Tong-Edward-C" } ], "abstract": "Diffraction effects of large segmented mirror gaps and secondary mirror support struts produce diffraction peaks or flares that are a detriment to exoplanet detection. In this paper we present detailed parametric diffraction analyses of an innovative \"Pinwheel Pupil\" segmented mirror concept utilizing curved segment gaps and secondary support struts that can potentially eliminate these diffraction flares that can obscure a faint exoplanet image. The resulting numerical diffraction performance predictions are quantitatively compared to that of both ideal monolithic circular pupils and classical annular pupils with straight secondary mirror struts. We utilize performance \u2013 based merit functions consisting of both radial and azimuthal profiles of the resulting telescope point spread function.", "doi": "10.1117/12.2313999", "isbn": "9781510619494", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2018-07-06", "pages": "Art. No. 106981Q" }, { "id": "authors:zkbtw-4ds28", "collection": "authors", "collection_id": "zkbtw-4ds28", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180718-153413745", "type": "book_section", "title": "Exoplanet telescope diffracted light minimized: the pinwheel-pupil solution", "book_title": "Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Harvey", "given_name": "James E.", "clpid": "Harvey-J-E" }, { "family_name": "Crabtree", "given_name": "Karlton", "clpid": "Crabtree-K" }, { "family_name": "Hull", "given_name": "Tony", "clpid": "Hull-T" } ], "contributor": [ { "family_name": "Lystrup", "given_name": "Makenzie", "clpid": "Lystrup-M" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Fazio", "given_name": "Giovanni G.", "clpid": "Fazio-G-G" }, { "family_name": "Batalha", "given_name": "Natalie", "clpid": "Batalha-N-M" }, { "family_name": "Siegler", "given_name": "Nicholas", "clpid": "Siegler-N" }, { "family_name": "Tong", "given_name": "Edward C.", "clpid": "Tong-Edward-C" } ], "abstract": "Terrestrial exoplanets shine in light reflected from a parent star. Optical spectra are required to provide evidence of a life-supporting environment. Exoplanets are very faint and their optical spectra are contaminated by the spectrum of the parent star. High angular resolution provided by large apertures is needed to distinguish between the spectrum of the exoplanet and its star. Today, large aperture telescopes use segmented primary mirrors that employ close-packed hexagonal segments. The telescope primary mirror is periodically discontinuous with straight lines. These discontinuities scatter unwanted radiation from the much brighter parent star across the field of view to obscure the light from the very faint terrestrial exoplanet. These discontinuities, which mimic a diffraction grating, result in a non-uniform distribution of background light across the image plane. This non-uniformity masks or hides exoplanets from view, to reduce the number of exoplanets that can be observed with a large aperture telescope or to reduce the quality of spectra and thus lead to misinterpretation of data. Here we introduce the concept of the pinwheel pupil whose unique diffraction pattern significantly reduces the non-uniform distribution of background radiation. Diffraction patterns from pinwheel pupils are compared to the monolithic filled aperture, the classical Cassegrain, the 60-degree symmetry of the hexagonal segments (JWST, E-ELT, etc.). Diffraction \"spikes\" are reduced by at least 105. We discuss the \"pinwheel pupil\" advantages to spectroscopy, image processing, and observatory operations. We show that, segment fabrication of curved-sided mirrors is not more difficult than fabrication of hexagonal mirror segments. . This is the report of quantitative study of Fraunhofer (far field) diffraction patterns produced by three different topologies or architectures of mirror segmentation, when illuminated by a plane wave of monochromatic white-light. A plot, in angular units of the intensity as a function of azimuth, Phi_f , within annular rings at different FOVs, centered on the system axis of the diffraction pattern will be presented. The advantages of the segmented pinwheel pupil is discussed.", "doi": "10.1117/12.2311811", "isbn": "9781510619494", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2018-07-06", "pages": "Art. No. 106981P" }, { "id": "authors:0a5rn-vrd10", "collection": "authors", "collection_id": "0a5rn-vrd10", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180718-154558929", "type": "book_section", "title": "A 4-m evolvable space telescope configured for NASA's HabEx Mission: the initial stage of LUVOIR", "book_title": "UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VIII", "author": [ { "family_name": "Lillie", "given_name": "Charles F.", "clpid": "Lillie-C-F" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Polidan", "given_name": "Ronald S.", "clpid": "Polidan-R-S" }, { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "MacEwen", "given_name": "Harold A.", "clpid": "MacEwen-H-A" }, { "family_name": "Breckinridge", "given_name": "James B.", "clpid": "Breckinridge-J-B" } ], "abstract": "Previous papers have described our concept for a large telescope that would be assembled in space in several stages (in different configurations) over a period of fifteen to 20 years. Spreading the telescope development, launch and operations cost over 20 years would minimize the impact on NASA's annual budget and drastically shorten the time between program start and \"first light\" for this space observatory. The first Stage of this Evolvable Space Telescope (EST) would consist of an instrument module located at the prime focus of three 4-meter hexagonal mirrors arranged in a semi-circle to form one-half of a 12-m segmented mirror. After several years three additional 4-m mirrors would be added to create a 12-m filled aperture. Later, twelve more 4-m mirrors will be added to this Stage 2 telescope to create a 20-m filled aperture space telescope. At each stage the telescope would have an unparalleled capability for UVOIR observations, and the results of these observations will guide the evolution of the telescope and its instruments. In this paper we describe our design concept for an initial configuration of our Evolvable Space Telescope that can meet the requirements of the 4-m version of the HabEx spacecraft currently under consideration by NASA's Habitable Exoplanet Science and Technology Definition Team. This \"Stage Zero\" configuration will have only one 4-m mirror segment with the same 30-m focal length and a prime focus coronagraph with normal incidence optics to minimize polarization effects. After assembly and checkout in cis-lunar space, the telescope would transfer to a Sun-Earth L2 halo orbit and obtain high sensitivity, high resolution, high contrast UVOIR observations that address the scientific objectives of the Habitable-Exoplanet Imaging Missions.", "doi": "10.1117/12.2274623", "isbn": "9781510612532", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2017-09-05", "pages": "Art. no. 103980R" }, { "id": "authors:14nee-ex260", "collection": "authors", "collection_id": "14nee-ex260", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161116-070011797", "type": "book_section", "title": "Prime focus architectures for large space telescopes: reduce surfaces to save cost", "book_title": "Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Breckinridge", "given_name": "J. B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Lillie", "given_name": "C. F.", "clpid": "Lillie-C-F" } ], "contributor": [ { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Fazio", "given_name": "Giovanni G.", "clpid": "Fazio-G-G" }, { "family_name": "Lystrup", "given_name": "Makenzie", "clpid": "Lystrup-M" }, { "family_name": "Batalha", "given_name": "Natalie", "clpid": "Batalha-N-M" }, { "family_name": "Siegler", "given_name": "Nicholas", "clpid": "Siegler-N" }, { "family_name": "Tong", "given_name": "Edward C.", "clpid": "Tong-Edward-C" } ], "abstract": "Conceptual architectures are now being developed to identify future directions for post JWST large space telescope systems to operate in the UV Optical and near IR regions of the spectrum. Here we show that the cost of optical surfaces within large aperture telescope/instrument systems can exceed $100M/reflection when expressed in terms of the aperture increase needed to over come internal absorption loss. We recommend a program in innovative optical design to minimize the number of surfaces by considering multiple functions for mirrors. An example is given using the Rowland circle imaging spectrometer systems for UV space science. With few exceptions, current space telescope architectures are based on systems optimized for ground-based astronomy. Both HST and JWST are classical \"Cassegrain\" telescopes derived from the ground-based tradition to co-locate the massive primary mirror and the instruments at the same end of the metrology structure. This requirement derives from the dual need to minimize observatory dome size and cost in the presence of the Earth's 1-g gravitational field. Space telescopes, however function in the zero gravity of space and the 1- g constraint is relieved to the advantage of astronomers. Here we suggest that a prime focus large aperture telescope system in space may have potentially have higher transmittance, better pointing, improved thermal and structural control, less internal polarization and broader wavelength coverage than Cassegrain telescopes. An example is given showing how UV astronomy telescopes use single optical elements for multiple functions and therefore have a minimum number of reflections.", "doi": "10.1117/12.2232144", "isbn": "978-1-5106-0187-1", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2016-08-01", "pages": "Art. No. 99044K" }, { "id": "authors:qvtc4-sh515", "collection": "authors", "collection_id": "qvtc4-sh515", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161114-155237636", "type": "book_section", "title": "Telescope polarization and image quality: Lyot coronagraph performance", "book_title": "Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave", "author": [ { "family_name": "Breckinridge", "given_name": "J. B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Chipman", "given_name": "R. A.", "clpid": "Chipman-R-A" } ], "contributor": [ { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Fazio", "given_name": "Giovanni G.", "clpid": "Fazio-G-G" }, { "family_name": "Lystrup", "given_name": "Makenzie", "clpid": "Lystrup-M" } ], "abstract": "In this paper we apply a vector representation of physical optics, sometimes called polarization aberration theory to study image formation in astronomical telescopes and instruments. We describe image formation in-terms of interferometry and use the Fresnel polarization equations to show how light, upon propagation through an optical system become partially polarized. We make the observation that orthogonally polarized light does not interfere to form an intensity image. We show how the two polarization aberrations (diattenuation and and retardance) distort the system PSF, decrease transmittance, and increase unwanted background above that predicted using the nonphysical scalar models. We apply the polarization aberration theory (PolAbT) described earlier (Breckinridge, Lam and Chipman, 2015, PASP 127, 445-468) to the fore-optics of the system designed for AFTA-WFIRST\u2013 CGI to obtain a performance estimate. Analysis of the open-literature design using PolAbT leads us to estimate that the WFIRST-CGI contrast will be in the 10^(-5) regime at the occulting mask. Much above the levels predicted by others (Krist, Nemati and Mennesson, 2016, JATIS 2, 011003). Remind the reader: 1. Polarizers are operators, not filters in the same sense as colored filters, 2. Adaptive optics does not correct polarization aberrations, 3. Calculations of both diattenuation and retardance are needed to model real-world telescope/coronagraph systems.", "doi": "10.1117/12.2231242", "isbn": "978-1-5106-0187-1", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_publication": "Bellingham, WA", "publication_date": "2016-07-29", "pages": "Art. No. 99041C" }, { "id": "authors:txx6y-12678", "collection": "authors", "collection_id": "txx6y-12678", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180718-155617229", "type": "book_section", "title": "An evolvable space telescope for future astronomical missions 2015 update", "book_title": "UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts VII", "author": [ { "family_name": "Polidan", "given_name": "Ronald S.", "clpid": "Polidan-R-S" }, { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Lillie", "given_name": "Charles F.", "clpid": "Lillie-C-F" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Flannery", "given_name": "Martin R.", "clpid": "Flannery-M-R" }, { "family_name": "Dailey", "given_name": "Dean R.", "clpid": "Dailey-D-R" }, { "family_name": "Baldauf", "given_name": "Brian", "clpid": "Baldauf-B" }, { "family_name": "Makowski", "given_name": "David", "clpid": "Makowski-D" }, { "family_name": "Rafanelli", "given_name": "Gerard L.", "clpid": "Rafanelli-G-L" } ], "contributor": [ { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Breckinridge", "given_name": "James B.", "clpid": "Breckinridge-J-B" } ], "abstract": "In 2014 we presented a concept for an Evolvable Space Telescope (EST) that was assembled on orbit in 3 stages, growing from a 4x12 meter telescope in Stage 1, to a 12-meter filled aperture in Stage 2, and then to a 20-meter filled aperture in Stage 3. Stage 1 is launched as a fully functional telescope and begins gathering science data immediately after checkout on orbit. This observatory is then periodically augmented in space with additional mirror segments, structures, and newer instruments to evolve the telescope over the years to a 20-meter space telescope. In this 2015 update of EST we focus upon three items: 1) a restructured Stage 1 EST with three mirror segments forming an off-axis telescope (half a 12-meter filled aperture); 2) more details on the value and architecture of the prime focus instrument accommodation; and 3) a more in depth discussion of the essential in-space infrastructure, early ground testing and a concept for an International Space Station testbed called MoDEST. In addition to the EST discussions we introduce a different alternative telescope architecture: a Rotating Synthetic Aperture (RSA). This is a rectangular primary mirror that can be rotated to fill the UV-plane. The original concept was developed by Raytheon Space and Airborne Systems for non-astronomical applications. In collaboration with Raytheon we have begun to explore the RSA approach as an astronomical space telescope and have initiated studies of science and cost performance.", "doi": "10.1117/12.2189105", "isbn": "9781628417685", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2015-09-22", "pages": "Art. No. 960207" }, { "id": "authors:rj58z-g1502", "collection": "authors", "collection_id": "rj58z-g1502", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160108-124749706", "type": "book_section", "title": "Polarization Aberration in Astronomical Telescopes", "book_title": "Polarization Science and Remote Sensing VII", "author": [ { "family_name": "Chipman", "given_name": "Russell A.", "clpid": "Chipman-R-A" }, { "family_name": "Lam", "given_name": "Wai Sze Tiffany", "clpid": "Lam-Wai-Sze-Tiffany" }, { "family_name": "Breckinridge", "given_name": "James", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Shaw", "given_name": "Joseph A.", "clpid": "Shaw-J-A" }, { "family_name": "LeMaster", "given_name": "Daniel A.", "clpid": "LeMaster-D-A" } ], "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. The functional form of these aberrations, called polarization aberrations, result from the angles of incidence and the variations of the coatings as a function of angle. These coatings induce small modifications to the PSF, which consists of four separate components, two nearly Airy-disk PSF components, and two faint components, we call ghost PSF components, with a spatial extent about twice the size of the diffraction limited image. As the specifications of optical systems constantly improve, these small effects become increasingly important. It is shown how the magnitude of these ghost PSF components, at ~10^(-5) in the example telescope, can interfere with exoplanet detection with coronagraphs.", "doi": "10.1117/12.2188921", "isbn": "9781628417791", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_publication": "Bellingham, WA", "publication_date": "2015-09-03", "pages": "Art. No. 96130H" }, { "id": "authors:ptr7f-1v980", "collection": "authors", "collection_id": "ptr7f-1v980", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150303-140817829", "type": "book_section", "title": "Bumps in the Road", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Kahan", "given_name": "Mark A.", "clpid": "Kahan-M-A" } ], "abstract": "I have two subjects I want to talk about today \u2013 one is on some historical experiences, and\nthe other is about mistakes made in the development of high-performance optical systems,\ndevelop of functional requirements and flow-downs, identification of design approaches\nfor an instrument, etc. One thing I'm working on relates to polarization and how it affects\nradiometry and the image quality of an optical system and so we'll spend a little bit of time\ntalking about that. Finally, though the HST failure has been widely covered, a few\nadditional comments are probably also worthy of mention.", "doi": "10.1117/12.2066922", "publisher": "Society of Photo-optical Instrumentation Engineers", "publication_date": "2014-12-05" }, { "id": "authors:3x4bk-taf42", "collection": "authors", "collection_id": "3x4bk-taf42", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150311-084101107", "type": "book_section", "title": "Space optics contributions by the College of Optical Sciences over the past 50 years", "book_title": "Fifty Years of Optical Sciences at the Universe of Arizona", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Smith", "given_name": "Peter", "clpid": "Smith-P" } ], "contributor": [ { "family_name": "Barrett", "given_name": "Harrison H.", "clpid": "Barrett-H-H" }, { "family_name": "Greivenkamp", "given_name": "John E.", "clpid": "Greivenkamp-J-E" }, { "family_name": "Dereniak", "given_name": "Eustace L.", "clpid": "Dereniak-E-L" } ], "abstract": "We present a review of the contributions by students, staff, faculty and alumni to the Nation's space program over the past 50 years. The balloon polariscope led the way to future space optics missions. The missions Pioneer Venus (large probe solar flux radiometer), Pioneer 10/11 (imaging photopolarimeter) to Jupiter and Saturn, Hubble Space Telescope (HST), and next generation large aperture space telescopes are discussed.", "doi": "10.1117/12.2064892", "isbn": "978-1-62841-213-0", "publisher": "SPIE", "place_of_publication": "Bellingham, WA", "publication_date": "2014-10-20", "pages": "Art. No. 918606" }, { "id": "authors:dap8c-fs969", "collection": "authors", "collection_id": "dap8c-fs969", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20140210-104351544", "type": "book_section", "title": "Self-induced polarization anisoplanatism", "book_title": "UV/Optical/IR space telescopes and instruments: innovative technologies and concepts VI", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Breckinridge", "given_name": "James B.", "clpid": "Breckinridge-J-B" } ], "abstract": "This paper suggests that the astronomical science data recorded with low F# telescopes for applications requiring a known point spread function shape and those applications requiring instrument polarization calibration may be compromised unless the effects of vector wave propagation are properly modeled and compensated. Exoplanet coronagraphy requires \"matched filter\" masks and explicit designs for the real and imaginary parts for the mask transmittance. Three aberration sources dominate image quality in astronomical optical systems: amplitude, phase and polarization. Classical ray-trace aberration analysis used today by optical engineers is inadequate to model image formation in modern low F# high-performance astronomical telescopes. We show here that a complex (real and imaginary) vector wave model is required for high performance, large aperture, very wide-field, low F# systems. Self-induced polarization anisoplanatism (SIPA) reduces system image quality, decreases contrast and limits the ability of image processing techniques to restore images. This paper provides a unique analysis of the image formation process to identify measurements sensitive to SIPA. Both the real part and the imaginary part of the vector complex wave needs to be traced through the entire optical system, including each mirror surface, optical filter, and all masks. Only at the focal plane is the modulus squared taken to obtain an estimate of the measured intensity. This paper also discusses the concept of the polarization conjugate filter, suggested by the author to correct telescope/instrument corrupted phase and amplitude and thus mitigate6, in part the effects of phase and amplitude errors introduced by reflections of incoherent white-light from metal coatings.", "doi": "10.1117/12.2028479", "isbn": "978-0-8194-9710-9", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_publication": "Bellingham, WA", "publication_date": "2013-09-27", "pages": "Art. No. 886012" }, { "id": "authors:dwvtb-n4659", "collection": "authors", "collection_id": "dwvtb-n4659", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180718-162409515", "type": "book_section", "title": "Large diffractive/refractive apertures for space and airborne telescopes", "book_title": "Sensors and Systems for Space Applications VI", "author": [ { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Pham", "given_name": "Khanh D.", "clpid": "Pham-Khanh-D" }, { "family_name": "Cox", "given_name": "Joseph L.", "clpid": "Cox-J-L" }, { "family_name": "Howard", "given_name": "Richard T.", "clpid": "Howard-R-T" }, { "family_name": "Chen", "given_name": "Genshe", "clpid": "Chen-Genshe" } ], "abstract": "Recent work, specifically the Lawrence Livermore National Laboratory (LLNL) Eyeglass and the DARPA MOIRE programs, have evaluated lightweight, easily packaged and deployed, diffractive/refractive membrane transmissive lenses as entrance apertures for large space and airborne telescopes. This presentation describes a new, innovative approach to the theory of diffractive and refractive effects in lenses used as telescope entrance apertures and the fabrication of the necessary large membrane optics. Analyses are presented to indicate how a broadband, highly transmissive diffractive / refractive membrane lens can be developed and fabricated, and potential applications in defense and astronomy are briefly discussed.", "doi": "10.1117/12.2015457", "isbn": "9780819495303", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2013-05-21", "pages": "Art. No. 873904" }, { "id": "authors:nb5km-cny09", "collection": "authors", "collection_id": "nb5km-cny09", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161028-144850723", "type": "book_section", "title": "Polarization compensation of Fresnel aberrations in telescopes", "book_title": "UV/Optical/IR Space Telescopes and Instruments: Innovative Technologies and Concepts V", "author": [ { "family_name": "Clark", "given_name": "Natalie", "clpid": "Clark-N" }, { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "Breckinridge", "given_name": "James B.", "clpid": "Breckinridge-J-B" } ], "abstract": "Large aperture space telescopes are built with low F#'s to accommodate the mechanical constraints of launch vehicles and to reduce resonance frequencies of the on-orbit system. Inherent with these low F# is Fresnel polarization which effects image quality. We present the design and modeling of a nano-structure consisting of birefringent layers. Analysis shows a device that functions across a 400nm bandwidth tunable from 300nm to 1200nm. This Fresnel compensator device has a cross leakage of less than 0.001 retardance.", "doi": "10.1117/12.896638", "isbn": "978-0-8194-8756-8", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_publication": "Bellingham, WA", "publication_date": "2011-09-14", "pages": "Art. No. 81460O" }, { "id": "authors:24e0s-z6260", "collection": "authors", "collection_id": "24e0s-z6260", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161101-072905392", "type": "book_section", "title": "Fourier Transforms By White-Light Interferometry: Michelson Stellar Interferometer Fringes", "book_title": "Tribute to Joseph W. Goodman", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Caulfield", "given_name": "H. John", "clpid": "Caulfield-H-J" }, { "family_name": "Arsenault", "given_name": "Henri H.", "clpid": "Arsenault-H-H" } ], "abstract": "The white-light compensated rotational shear interferometer (coherence interferometer) was developed in an effort to study the spatial frequency content of passively illuminated white-light scenes in real-time and to image sources of astronomical interest at high spatial frequencies through atmospheric turbulence. This work was inspired by Professor Goodman's studies of the image formation properties of coherent (laser) illuminated transparencies. We discovered that real-time image processing is possible using white-light interferometry. The concept of a quasimonoplanatic approximation is introduced as a parallel to the quasimonochromatic approximation needed to describe the theory of Fourier transform spectrometers. This paper describes the coherence interferometer and reviews its image formation properties under the conditions of quasimonoplanacity and describes its development and its applications to physical optics, optical processing and astrophysics including the search for exoplanets.", "doi": "10.1117/12.890537", "isbn": "978-0-81948-732-2", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2011-09-08", "pages": "Art. No. 812206" }, { "id": "authors:1pkct-w6157", "collection": "authors", "collection_id": "1pkct-w6157", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110321-085232350", "type": "book_section", "title": "Shape correction of thin mirrors in a reconfigurable modular space telescope", "book_title": "Space telescopes and instrumentation 2010 : optical, infrared, and millimeter wave", "author": [ { "family_name": "Patterson", "given_name": "Keith", "clpid": "Patterson-K" }, { "family_name": "Pellegrino", "given_name": "Sergio", "orcid": "0000-0001-9373-3278", "clpid": "Pellegrino-S" }, { "family_name": "Breckinridge", "given_name": "James", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Oschmann", "given_name": "Jacobus M.", "clpid": "Oschmann-J-M" }, { "family_name": "Clampin", "given_name": "Mark C.", "clpid": "Clampin-M-C" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" } ], "abstract": "In order to facilitate the construction of future large space telescopes, the development of low cost, low mass\nmirrors is necessary. However, such mirrors suffer from a lack of structural stability, stiffness, and shape accuracy.\nActive materials and actuators can be used to alleviate this deficiency. For observations in the visible wavelengths,\nthe mirror surface must be controlled to an accuracy on the order of tens of nanometers. This paper presents\nan exploration of several mirror design concepts and compares their effectiveness at providing accurate shape\ncontrol. The comparison test is the adjustment of a generic mirror from its manufactured spherical shape to the\nshape required by various off-axis mirrors in a segmented primary mirror array. A study of thermal effects is\nalso presented and, from these results, a recommended design is chosen.", "doi": "10.1117/12.861442", "isbn": "978-0-81948-221-1", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2010-08-10", "pages": "Art. No. 773121" }, { "id": "authors:9z87k-85x97", "collection": "authors", "collection_id": "9z87k-85x97", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180718-162952782", "type": "book_section", "title": "Innovative pupil topographies for sparse aperture telescopes and SNR", "book_title": "Optical and Infrared Interferometry", "author": [ { "family_name": "Breckinridge", "given_name": "James", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" }, { "family_name": "Bryant", "given_name": "Nevin", "clpid": "Bryant-N" }, { "family_name": "Lorre", "given_name": "John", "clpid": "Lorre-J" } ], "contributor": [ { "family_name": "Sch\u00f6ller", "given_name": "Markus", "clpid": "Sch\u00f6ller-M" }, { "family_name": "Danchi", "given_name": "William C.", "clpid": "Danchi-W-C" }, { "family_name": "Delplancke", "given_name": "Fran\u00e7oise", "clpid": "Delplancke-" } ], "abstract": "Since the first application of the telescope to astronomy in 1610, most new astronomical discoveries require larger and larger radiation collecting areas. Today, the twin 10-meter Keck telescopes are operational and several 30-meter-aperture class telescopes are being planned. Optical interferometers and sparse aperture ground telescopes for astronomy have been proposed and built. Fienup showed the dependence between exposure time and the dilution factor of the aperture needed to maintain image quality.1 Carpenter suggests a sparse aperture telescope system for the purpose of imaging across the surfaces of stars.2 This paper demonstrates that the ability to reconstruct images from white-light extended sources with different contrast levels also depends on the specific pupil topography that is applied to the telescope system. Signal-to-noise ratios for recorded images are calculated for scene contrast, pupil shape, detector full-well, detected photons, and exposure times.", "doi": "10.1117/12.787011", "isbn": "9780819472236", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2008-07-28", "pages": "Art. No. 70133E" }, { "id": "authors:sz4j8-5jp38", "collection": "authors", "collection_id": "sz4j8-5jp38", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190318-142119417", "type": "book_section", "title": "The effects of instrumental elliptical polarization on stellar point spread function fine structure", "book_title": "Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter", "author": [ { "family_name": "Carson", "given_name": "Joseph C.", "clpid": "Carson-J-C" }, { "family_name": "Kern", "given_name": "Brian D.", "clpid": "Kern-B-D" }, { "family_name": "Trauger", "given_name": "John T.", "clpid": "Trauger-J-T" }, { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Mather", "given_name": "John C.", "clpid": "Mather-J-C" }, { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" }, { "family_name": "de Graauw", "given_name": "Mattheus W. M.", "clpid": "de-Graauw-M-W-M" } ], "abstract": "We present a status report on a study on the effects of instrumental polarization on the fine structure of the stellar point spread function (PSF). These effects are important to understand because the the aberration caused by instrumental polarization on an otherwise diffraction-limited PSF will likely have have severe consequences for extreme high contrast imaging systems such as NASA's proposed Terrestrial Planet Finder (TPF) mission and the proposed NASA Eclipse mission. The report here, describing our efforts to examine these effects, includes two parts: 1) a numerical analysis of the effect of metallic reflection, with some polarization-specific retardation, on a spherical wavefront; 2) an experimental approach for observing this effect, along with a status report on preliminary laboratory results. The numerical analysis indicates that the inclusion of polarization-specific phase effects (retardation) results in a point spread function (PSF) aberration more severe than the amplitude (reflectivity) effects previously recorded in the literature. Preliminary in-lab results are consistent with our numerical predictions.", "doi": "10.1117/12.672518", "isbn": "9780819463302", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2006-07-07", "pages": "Art. No. 62653M" }, { "id": "authors:xc4rr-y2650", "collection": "authors", "collection_id": "xc4rr-y2650", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181217-151248029", "type": "book_section", "title": "Challenges to optimizing a telescope system to detect and characterize exo-solar planetary systems", "book_title": "Novel Optical Systems Design and Optimization VIII", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Sasi\u00e1n", "given_name": "Jos\u00e9 M.", "clpid": "Sasi\u00e1n-J-M" }, { "family_name": "Koshel", "given_name": "R. John", "clpid": "Koshel-R-J" }, { "family_name": "Juergens", "given_name": "Richard C.", "clpid": "Juergens-R-C" } ], "abstract": "Novel optical design and engineering ideas are needed to build the large space telescopes for the direct detection and characterization of exo-solar system planets. For example, the Terrestrial Planet Finder Coronagraph requires a primary mirror 4 x 8 meters in size that is >10 x smoother than the 2.8 meter HST mirror and have a uniform reflectivity across the mirror to within 0.1%. The telescope system will need to control scattered light to within a part in 10 billion. The Terrestrial Planet Finder Interferometer will be a white-light, broadband infrared interferometer with a baseline in excess of 50 meters. In addition to direct imaging, planets masses and orbits can be derived from very precise measurements of the position of a star as it moves across the background. Interferometers provide the highest accuracy measurements of relative positions We will show that the optical design and the mechanical layout & configuration for these new telescopes need to be optimized for polarization as well as scattered light. Material science and coating technology plays an important role in the optimization of these systems. Stress across the surface of a mirror and stress within the optical thin film introduces polarization dependent scattered light. A new method to measure the anisotropy of the polarization-reflectivity of thin metal films on large astronomical mirrors is described.", "doi": "10.1117/12.619697", "isbn": "9780819458803", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_publication": "Bellingham, WA", "publication_date": "2005-08-29", "pages": "Art. No. 587508" }, { "id": "authors:g7zqx-4xh19", "collection": "authors", "collection_id": "g7zqx-4xh19", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180725-081118035", "type": "book_section", "title": "Space optics: challenge and opportunity", "book_title": "Novel Optical Systems Design and Optimization VII", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Sasian", "given_name": "Jose M.", "clpid": "Sasian-J-M" }, { "family_name": "Koshel", "given_name": "R. John", "clpid": "Koshel-R-J" }, { "family_name": "Manhart", "given_name": "Paul K.", "clpid": "Manhart-P-K" }, { "family_name": "Juergens", "given_name": "Richard C.", "clpid": "Juergens-R-C" } ], "abstract": "Innovative optical designs are needed to create the space sensor systems of the future. The NASA mission development process has created several very challenging design and engineering problems. Three of these are discussed: The SAFIR is a 15 to 25 meter clear aperture telescope cooled to 4 degrees Kelvin, with spectrographs and imaging systems cooled to 1 degree Kelvin. The Terrestrial Planet Finder (TPF) will detect and characterize planets in orbit about other stars, The Stellar Interferometer (SI) will image across the surfaces of distant stars. Issues related to optical design & engineering and image quality will be discussed. This paper reviews the optical systems and engineering needs for next generation astrophysics missions.", "doi": "10.1117/12.560474", "isbn": "9780819454621", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2004-10-22", "pages": "9-13" }, { "id": "authors:v7yga-twd94", "collection": "authors", "collection_id": "v7yga-twd94", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181112-113117698", "type": "book_section", "title": "Image formation in high-contrast optical systems: the role of polarization", "book_title": "Optical, Infrared, and Millimeter Space Telescopes", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Mather", "given_name": "John C.", "clpid": "Mather-J-C" } ], "abstract": "To find evidence of life in the Universe outside our solar system is one of the most compelling and visionary adventures of the 21st century. The technologies to create the telescopes and instruments that will enable this discovery are now within the grasp of mankind. Direct imaging of a very faint planet around a neighboring bright star requires high contrast or a hypercontrast optical imaging system capable of controlling unwanted radiation within the system to one part in ten to the 11th. This paper identifies several physical phenomena that affect image quality in high contrast imaging systems. Polarization induced at curved metallic surfaces and by anisotropy in the deposition process (Smith-Purcell effect) along with beam shifts introduced by the Goos-Hachen effect are discussed. A typical configuration is analyzed, and technical risk mitigation concepts are discussed.", "doi": "10.1117/12.548932", "isbn": "9780819454195", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2004-10-12", "pages": "1337-1345" }, { "id": "authors:1k5hc-r6j21", "collection": "authors", "collection_id": "1k5hc-r6j21", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180725-074440132", "type": "book_section", "title": "Astronomical search for origins: Are we alone?", "book_title": "UV/Optical/IR Space Telescopes: Innovative Technologies and Concepts", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "MacEwen", "given_name": "Howard A.", "clpid": "MacEwen-H-A" } ], "abstract": "Recent advances in astronomical research have led to a much-improved understanding of the evolution of the physical Universe. Recent advances in biology and genetics have led to a much-improved understanding of our biological Universe. Scientists now believe that we have the research tools to begin to answer one of man's two most compelling research questions: Are we alone? and How did we get here? This paper reviews the requirements and challenges we face to engineer and build the large space-based systems of interferometers and innovative single-aperture telescopes to detect and characterize in detail earth type planets around stars other than our sun.", "doi": "10.1117/12.507763", "isbn": "0819450391", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2004-01-30", "pages": "8-12" }, { "id": "authors:sc58s-rxw35", "collection": "authors", "collection_id": "sc58s-rxw35", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180724-145755957", "type": "book_section", "title": "Telescope revolution", "book_title": "Imaging Technology and Telescopes", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Bilbro", "given_name": "James W.", "clpid": "Bilbro-J-W" }, { "family_name": "Breckinridge", "given_name": "James B.", "clpid": "Breckinridge-J-B" }, { "family_name": "Carreras", "given_name": "Richard A.", "clpid": "Carreras-R-A" }, { "family_name": "Czyzak", "given_name": "Stanley R.", "clpid": "Czyzak-S-R" }, { "family_name": "Eckart", "given_name": "Mark J.", "clpid": "Eckart-M-J" }, { "family_name": "Fiete", "given_name": "Robert D.", "clpid": "Fiete-R-D" }, { "family_name": "Idell", "given_name": "Paul S.", "clpid": "Idell-P-S" } ], "abstract": "The scientific and technical challenges facing the astronomical community during the next decade are discussed within the framework of new technology and technical management issues. The astronomical telescope and instrument communities of industry, academia and government need to be prepared to meet the challenges of 21st century Astronomy. Emphasis is given to ground-based optical and infrared astronomy.", "doi": "10.1117/12.405765", "isbn": "0819437360", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2000-10-31", "pages": "1-5" }, { "id": "authors:t4g4q-76d77", "collection": "authors", "collection_id": "t4g4q-76d77", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180725-160851946", "type": "book_section", "title": "Evolution of imaging spectrometry: past, present, and future", "book_title": "Imaging Spectrometry II", "author": [ { "family_name": "Breckinridge", "given_name": "James B.", "orcid": "0000-0002-9488-098X", "clpid": "Breckinridge-J-B" } ], "contributor": [ { "family_name": "Descour", "given_name": "Michael R.", "clpid": "Descour-M-R" }, { "family_name": "Mooney", "given_name": "Jonathan Martin", "clpid": "Mooney-J-M" } ], "abstract": "An overview of the physical principals of imaging spectrometry for detailed characterization of remote objects and of gas vapors is given. The terms multi-spectral, hyperspectral, and ultra-spectral are defined within the framework of applications and instrument system design approaches. History of the development of imaging spectrometers is reviewed. We are at the threshold of major commercial efforts for these instrument systems.", "doi": "10.1117/12.258055", "isbn": "9780819422071", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "1996-11-13", "pages": "2-6" } ]