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Готові списки джерел за темами / Lyot coronagraph

Добірка наукової літератури з теми "Lyot coronagraph"

Автор: Grafiati

Опубліковано: 7 липня 2024

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Статті в журналах з теми "Lyot coronagraph":

1

Leboulleux, Lucie, Alexis Carlotti, and Mamadou N’Diaye. "Redundant apodization for direct imaging of exoplanets." Astronomy & Astrophysics 659 (March 2022): A143. http://dx.doi.org/10.1051/0004-6361/202142410.

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Context. Direct imaging and spectroscopy of Earth-like planets and young Jupiters require contrast values up to 106−1010 at angular separations of a few dozen milliarcseconds. To achieve this goal, one of the most promising approaches consists of using large segmented primary mirror telescopes with coronagraphic instruments. While they are able to reach high contrast at small angular separations, coronagraphs are highly sensitive to wavefront errors, however. The segmentation itself is responsible for phasing errors and segment-level vibrations that have to be controlled at a subnanometric accuracy. Aims. We propose an innovative method for a coronagraph design that allows a consequent relaxation of the segment phasing and stability constraints for low segment-count mirrors and generates an instrument that is more robust to segment-level wavefront errors. Methods. This method is based on an optimization of the coronagraph design that includes a segment-level apodization. This is repeated over the pupil to match the segmentation redundancy and improves the contrast stability beyond the minimum separation set by the single-segment diffraction limit. Results. We validate this method on a Giant Magellan Telescope (GMT)-like pupil (seven circular segments) for two coronagraph types: apodized pupil Lyot coronagraphs, and apodizing phase plate coronagraphs. For the apodized pupil Lyot coronagraphs, redundant apodization enables releasing the piston phasing constraints by a factor of 5-20 compared to classical designs. For the apodizing phase plate coronagraphs, the contrast remains almost constant up to 1 radian RMS of the phasing errors. We also show that redundant apodizations increase the robustness of the coronagraph to segment tip-tilt errors, as well as to missing segment errors. Conclusions. Redundant apodization enables reducing or even removing any constraints on the primary mirror segment phasing at the price of larger angular separations and lower throughputs. This method cannot be applied to higher-segment count mirrors such as the ELT or the TMT, but it is particularly suitable for low segment-count mirrors (fewer than ~20 segments) such as the GMT aperture. These mirrors aim for high-contrast imaging of debris disks or exoplanets down to 100 mas.

2

Kim, I. S., and O. I. Bugaenko. "On magnetic measurements in prominences." Proceedings of the International Astronomical Union 8, S300 (June 2013): 426–27. http://dx.doi.org/10.1017/s1743921313011393.

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AbstractThe successes of magnetic measurements in faint objects located near very bright ones are strongly depending on the stray light in the telescope. We propose a mask with a variable transmission placed on the primary optics of a telescope. Our computations of the stray light in such a telescope indicate that the calculated coronagraphic factor of improvement, K, would increase at least by 2 orders of magnitude compared to the Lyot-type coronagraph.

3

Anche, Ramya M., Ewan Douglas, Kian Milani, Jaren Ashcraft, Maxwell A. Millar-Blanchaer, John H. Debes, Julien Milli, and Justin Hom. "Simulation of High-contrast Polarimetric Observations of Debris Disks with the Roman Coronagraph Instrument." Publications of the Astronomical Society of the Pacific 135, no. 1054 (December 1, 2023): 125001. http://dx.doi.org/10.1088/1538-3873/ad0a72.

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Abstract The Nancy Grace Roman Space Telescope Coronagraph Instrument will enable the polarimetric imaging of debris disks and inner dust belts in the optical and near-infrared wavelengths, in addition to the high-contrast polarimetric imaging and spectroscopy of exoplanets. The Coronagraph uses two Wollaston prisms to produce four orthogonally polarized images and is expected to measure the polarization fraction with measurement errors <3% per spatial resolution element. To simulate the polarization observations through the Hybrid Lyot Coronagraph (HLC) and Shaped Pupil Coronagraph (SPC), we model disk scattering, the coronagraphic point-response function, detector noise, speckles, jitter, and instrumental polarization and calculate the Stokes parameters. To illustrate the potential for discovery and a better understanding of known systems with both the HLC and SPC modes, we model the debris disks around Epsilon Eridani and HR 4796A, respectively. For Epsilon Eridani, using astrosilicates with 0.37 ± 0.01 as the peak input polarization fraction in one resolution element, we recover the peak disk polarization fraction of 0.33 ± 0.01. Similarly, for HR 4796A, for a peak input polarization fraction of 0.92 ± 0.01, we obtain the peak output polarization fraction as 0.80 ± 0.03. The Coronagraph design meets the required precision, and forward modeling is needed to accurately estimate the polarization fraction.

4

Carbillet, Marcel, Philippe Bendjoya, Lyu Abe, Géraldine Guerri, Anthony Boccaletti, Jean-Baptiste Daban, Kjetil Dohlen, et al. "Apodized Lyot coronagraph for SPHERE/VLT." Experimental Astronomy 30, no. 1 (March 24, 2011): 39–58. http://dx.doi.org/10.1007/s10686-011-9219-4.

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5

Rougeot, R., R. Flamary, D. Mary, and C. Aime. "Influence of surface roughness on diffraction in the externally occulted Lyot solar coronagraph." Astronomy & Astrophysics 626 (June 2019): A1. http://dx.doi.org/10.1051/0004-6361/201834634.

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Context. The solar coronagraph ASPIICS will fly on the future ESA formation flying mission Proba-3. The instrument combines an external occulter of diameter 1.42 m and a Lyot solar coronagraph of 5 cm diameter, located downstream at a distance of 144 m. Aims. The theoretical performance of the externally occulted Lyot coronagraph has been computed by assuming perfect optics. In this paper, we improve related modelling by introducing roughness scattering effects from the telescope. We have computed the diffraction at the detector, that we compare to the ideal case without perturbation to estimate the performance degradation. We have also investigated the influence of sizing the internal occulter and the Lyot stop, and we performed a sensitivity analysis on the roughness. Methods. We have built on a recently published numerical model of diffraction propagation. The micro-structures of the telescope are built by filtering a white noise with a power spectral density following an isotropic ABC function, suggested by Harvey scatter theory. The parameters were tuned to fit experimental data measured on ASPIICS lenses. The computed wave front error was included in the Fresnel wave propagation of the coronagraph. A circular integration over the solar disk was performed to reconstruct the complete diffraction intensity. Results. The level of micro-roughness is 1.92 nm root-mean-square. Compared to the ideal case, in the plane of the internal occulter, the diffraction peak intensity is reduced by ≃0.001%. However, the intensity outside the peak increases by 12% on average, up to 20% at 3 R⊙, where the mask does not filter out the diffraction. At detector level, the diffraction peak remains ≃10−6 at 1.1 R⊙, similar to the ideal case, but the diffraction tail at large solar radius is much higher, up to one order of magnitude. Sizing the internal occulter and the Lyot stop does not improve the rejection, as opposed to the ideal case. Conclusions. Besides these results, this paper provides a methodology to implement roughness scattering in the wave propagation model for the solar coronagraph.

6

Leboulleux, Lucie, Jean-François Sauvage, Rémi Soummer, Thierry Fusco, Laurent Pueyo, Laurent M. Mugnier, Christopher Moriarty, Peter Petrone, and Keira Brooks. "Experimental validation of coronagraphic focal-plane wavefront sensing for future segmented space telescopes." Astronomy & Astrophysics 639 (July 2020): A70. http://dx.doi.org/10.1051/0004-6361/202037658.

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Context. Direct imaging of Earth-like planets from space requires dedicated observatories, combining large segmented apertures with instruments and techniques such as coronagraphs, wavefront sensors, and wavefront control in order to reach the high contrast of 1010 that is required. The complexity of these systems would be increased by the segmentation of the primary mirror, which allows for the larger diameters necessary to image Earth-like planets but also introduces specific patterns in the image due to the pupil shape and segmentation and making high-contrast imaging more challenging. Among these defects, the phasing errors of the primary mirror are a strong limitation to the performance. Aims. In this paper, we focus on the wavefront sensing of segment phasing errors for a high-contrast system, using the COronagraphic Focal plane wave-Front Estimation for Exoplanet detection (COFFEE) technique. Methods. We implemented and tested COFFEE on the High-contrast imaging for Complex Aperture Telescopes (HiCAT) testbed, in a configuration without any coronagraph and with a classical Lyot coronagraph, to reconstruct errors applied on a 37 segment mirror. We analysed the quality and limitations of the reconstructions. Results. We demonstrate that COFFEE is able to estimate correctly the phasing errors of a segmented telescope for piston, tip, and tilt aberrations of typically 100 nm RMS. We also identified the limitations of COFFEE for the reconstruction of low-order wavefront modes, which are highly filtered by the coronagraph. This is illustrated using two focal plane mask sizes on HiCAT. We discuss possible solutions, both in the hardware system and in the COFFEE optimizer, to mitigate these issues.

7

Trauger, John, Dwight Moody, John Krist, and Brian Gordon. "Hybrid Lyot coronagraph for WFIRST-AFTA: coronagraph design and performance metrics." Journal of Astronomical Telescopes, Instruments, and Systems 2, no. 1 (January 14, 2016): 011013. http://dx.doi.org/10.1117/1.jatis.2.1.011013.

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8

Soummer, R., L. Pueyo, A. Sivaramakrishnan, and R. J. Vanderbei. "Fast computation of Lyot-style coronagraph propagation." Optics Express 15, no. 24 (2007): 15935. http://dx.doi.org/10.1364/oe.15.015935.

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9

Loutsenko, Igor, and Oksana Yermolayeva. "Quasi-Band-Limited Coronagraph for Extended Sources." Journal of Astronomical Instrumentation 10, no. 01 (February 10, 2021): 2150002. http://dx.doi.org/10.1142/s2251171721500021.

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We propose a class of graded coronagraphic “amplitude” image masks for a high throughput Lyot-type coronagraph that transmits light from an annular region around an extended source and suppresses light, with extremely high ratio, from elsewhere. The interior radius of the region is comparable with its exterior radius. The masks are designed using an idea inspired by approach due M. J. Kuchner and W. A. Traub (“band-limited” masks) and approach to optimal apodization by D. Slepian. One potential application of our masks is direct high-resolution imaging of exo-planets with the help of the Solar Gravitational Lens, where apparent radius of the “Einstein ring” image of a planet is of the order of an arc-second and is comparable with the apparent radius of the sun and solar corona.

10

Xin, Yinzi, Laurent Pueyo, Romain Laugier, Leonid Pogorelyuk, Ewan S. Douglas, Benjamin J. S. Pope, and Kerri L. Cahoy. "Coronagraphic Data Post-processing Using Projections on Instrumental Modes." Astrophysical Journal 963, no. 2 (March 1, 2024): 96. http://dx.doi.org/10.3847/1538-4357/ad1879.

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Abstract Directly observing exoplanets with coronagraphs is impeded by the presence of speckles from aberrations in the optical path, which can be mitigated in hardware with wave front control, as well as in post-processing. This work explores using an instrument model in post-processing to separate astrophysical signals from residual aberrations in coronagraphic data. The effect of wave front error (WFE) on the coronagraphic intensity consists of a linear contribution and a quadratic contribution. When either of the terms is much larger than the other, the instrument response can be approximated by a transfer matrix mapping WFE to detector plane intensity. From this transfer matrix, a useful projection onto instrumental modes that removes the dominant error modes can be derived. We apply this approach to synthetically generated Roman Space Telescope hybrid Lyot coronagraph data to extract “robust observables,” which can be used instead of raw data for applications such as detection testing. The projection improves planet flux ratio detection limits by about 28% in the linear regime and by over a factor of 2 in the quadratic regime, illustrating that robust observables can increase sensitivity to astrophysical signals and improve the scientific yield from coronagraphic data. While this approach does not require additional information such as observations of reference stars or modulations of a deformable mirror, it can and should be combined with these other techniques, acting as a model-informed prior in an overall post-processing strategy.

Більше джерел

Дисертації з теми "Lyot coronagraph":

1

Alagao, Mary Angelie. "Characterization and optimization of the Evanescent Wave Coronagraph." Electronic Thesis or Diss., Saint-Etienne, 2023. http://www.theses.fr/2023STET0060.

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L’imagerie directe des exoplanètes reste difficile en raison du contraste élevé et de la faible séparation angulaire entre l'étoile et la planète. Cela nécessite de supprimer l'éblouissement dû à l'étoile et de s'assurer que la lumière faible de la planète n'est pas noyée au milieu de divers bruits. La détection dépend de la maturité des techniques et des algorithmes utilisés, tout en tenant compte des compromis importants sur le contraste brut, la résolution angulaire et la transmission. L'une de ses composantes clés est l'utilisation de coronagraphes - des instruments ayant pour seul but de bloquer/réduire la lumière provenant de l'étoile. Ce travail présente un nouveau type de coronographe de Lyot, inventé par le Dr Yves Rabbia, qui repose sur le principe de la réflexion interne totale frustrée (FTIR) pour supprimer la lumière de l'étoile. Ce coronographe est appelé Evanescent Wave Coronagraph (EvWaCo) en raison de sa nature : son masque au plan focal, comprenant une lentille et un prisme, réfléchit la source hors axe (planète) et transmet la source sur l'axe (étoile) à l’aide des ondes évanescentes. Cette thèse vise à fournir au lecteur les bases qui mettent en évidence les trois principaux avantages d'EvWaCo : i) le masque est intrinsèquement achromatique, ii) la taille du masque est ajustable en modifiant la pression entre la lentille et le prisme, et iii) à la fois la lumière stellaire et la lumière planétaire peuvent être collectées simultanément pour une détection de front d'onde de bas ordre et un centrage approprié de l’étoile. Les performances d'EvWaCo sont évaluées à travers des expériences en laboratoire, puis comparées à des simulations numériques. Les résultats expérimentaux montrent un contraste brut égal à quelques 10-4 à 3 ��/�� sur toute la bande I (��c = 800 nm, ∆��/�� ≈ 20%) et à 4 ��/�� sur toute la bande R (��c = 650 nm, ∆��/�� ≈ 23%). Les simulations confirment la capacité de rejet achromatique d'EvWaCo, montrant un contraste brut de 10-4 à la même distance radiale sur les deux bandes spectrales. Cette thèse se conclut sur un bilan de l’état du banc développé et les perspectives futures
Direct imaging of exoplanets remains challenging due to the high contrast and the small angular separation between the star and the planet. It requires suppressing the blinding glare from the star and ensuring that the planet's faint light is not buried deep in various noises. Successful detection depends on the technological readiness and maturity of techniques and algorithms employed while considering the significant trade-offs on raw contrast, inner working angle, and throughput. One of its key components is the use of coronagraphs – instruments with the sole purpose of blocking/reducing the light from the star. This work presents a new type of Lyot coronagraph, invented by Dr. Yves Rabbia, that relies on the frustrated total internal reflection (FTIR) principle to suppress the starlight. This coronagraph is aptly called the Evanescent Wave Coronagraph (EvWaCo) owing to its nature that its focal plane mask, comprising a lens and a prism, reflects the off-axis source (planet) and transmits the on-axis source (star) by capturing the evanescent waves. This thesis aims to provide the reader with the groundwork that highlights EvWaCo's three main advantages: i) the mask is inherently achromatic, ii) the size of the mask is adjustable by changing the pressure between the lens and the prism, and iii) both the stellar light and the planet light can be collected simultaneously for low-order wavefront sensing, and proper stellar light centering. The performance of EvWaCo is assessed through experiments in a laboratory and then compared to numerical simulations. The experimental results show a raw contrast equal to a few 10-4 at 3 ��/�� over the full I-band (��c = 800 nm, ∆��/�� ≈ 20%) and at 4 ��/�� over the full R-band (��c = 650 nm, ∆��/�� ≈ 23%). The simulations confirm the achromatic rejection capability of EvWaCo as it showed a raw contrast of 10-4 at the same radial distance over both bandpasses. This thesis concludes with the status of its testbed and future perspectives

2

Venet, Melanie. "Coronographes spatiaux : Solar Orbiter / Metis, Smese / Lyot, Proba-3 / Aspiics." Thesis, Aix-Marseille 1, 2011. http://www.theses.fr/2011AIX10011.

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La couronne solaire est la partie de l'atmosphère du Soleil qui s'étend de la photosphère (surface solaire d'où sont émis les photons) jusque dans le milieu interplanétaire. Sa compréhension relève d'un enjeu majeur car elle est à l'origine de phénomènes qui peuvent perturber les télécommunications, les êtres vivants et même le climat. L'instrument privilégié pour l'observer est le coronographe, système optique occultant le disque solaire au profit de la couronne, un million de fois moins intense. Ma thèse porte sur son étude, en particulier à travers les projets spatiaux :- SOLAR ORBITER, qui doit s'approcher du Soleil à 0.2 unité astronomique (distance Terre-Soleil), permettant ainsi une très haute résolution spatiale ;- SMESE, en coopération avec la Chine, qui étudiera la couronne dans l'infrarouge lointain ;- et ASPIICS, dont l'occulteur externe sera placé à 150 m de l'instrument imageur, permettant d'observer la couronne dans des conditions proches d'une éclipse solaire naturelle.Le premier aspect abordé est la réjection de la lumière parasite instrumentale, dont l'optimisation est une des problématiques majeures en coronographie. Le second concerne les modes d'observation par imagerie en lumière blanche, imagerie monochromatique, et interférométrie, en particulier le Fabry Perot. Le développement et l'amélioration de ces techniques permettra des avancées considérables en terme de résolution et l'accès à la couronne toujours plus proche de la surface du Soleil, lieu encore mal connu où l'activité solaire prend naissance
The solar corona is the part of the Sun's atmosphere that extends from the photosphere (solar surface where the photons are emitted) into the interplanetary medium. Its understanding is a major issue because it is the source of phenomena that can disrupt telecommunications, living beings and even climate. The most appropriate tool to observe it is the coronagraph, an optical system obscuring the solar disk in favor of the corona, a million times fainter. My thesis deals with its review, particularly through the spaceprojects :- Solar Orbiter, which will approach the Sun at 0.2 astronomical unit (distance between Earth and Sun), allowing a very high spatial resolution ;- SMESE, in cooperation with China, which should study the corona in the Lymanalpha (and far infrared) ;- and ASPIICS, which will observe the corona in conditions close to a natural solar eclipse, with its occulting disk located at 150 m from the imaging instrument.The first point tackled is the rejection of instrumental stray light, whose optimization is one of the major problems in coronagraphy. The second concerns the methods of observation and imaging in white light, monochromatic imaging, and interferometry, in particular the Fabry Perot. The development and improvement of these techniques will allow considerable progress in terms of resolution and access to the corona ever closer to the Sun's surface, the location yet little known where the solar activity originates

Частини книг з теми "Lyot coronagraph":

1

Boccaletti, Anthony, Jean-Charles Augereau, Gaël Chauvin, Pierre Riaud, Jacques Baudrand, François Lacombe, Daniel Rouan, Anne-Marie Lagrange, and Pierre Baudoz. "Lyot Coronagraphy at the Palomar and Phase-Mask Coronagraphy at the VLT." In Science with Adaptive Optics, 25–30. Berlin, Heidelberg: Springer Berlin Heidelberg, 2005. http://dx.doi.org/10.1007/10828557_4.

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Тези доповідей конференцій з теми "Lyot coronagraph":

1

Watson, Steven M., and James P. Mills. "Incorporating coronographs with segmented telescopic systems for extrasolar planetary imaging." In OSA Annual Meeting. Washington, D.C.: Optica Publishing Group, 1989. http://dx.doi.org/10.1364/oam.1989.wv2.

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Detection of nonsolar planets is a challenging problem. Due to the planets' faintness relative to the star, it is necessary to suppress the stellar diffracted energy to very low levels. In addition, the planets' proximity to the star requires large diameter optics. This research examines various multiaperture and segmented telescopic systems incorporating Lyot coronagraphs to suppress the stellar diffracted energy and provide the required resolution so that the extrasolar planets can be directly imaged. Because of the phasing tolerances and required contrast ratios, the IR band of 10.5-13.5 µm was examined over a field of view of 0.2-2 arcsec. Various telescopic objectives with the Lyot coronagraph were examined for their ability to suppress the stellar diffracted energy levels. The designs examined were comprised of segmented circular, hexagonal, apodized hexagonal, and rectangular systems. The Lyot coronagraph consists of a Gaussian apodizer at the focal plane of the objective and a Lyot stop at the image plane of the objective.

2

Ftaclas, Christ, Edward T. Siebert, and Richard J. Terrile. "A High Efficiency Coronagraph for Astronomical Applications." In Space Optics for Astrophysics and Earth and Planetary Remote Sensing. Washington, D.C.: Optica Publishing Group, 1988. http://dx.doi.org/10.1364/soa.1988.wa5.

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Direct detection of extra-solar planetary systems is one of a class of astronomical problems requiring a significant reduction of diffracted light within a few arcseconds of a bright point source. Traditional approaches to diffraction reduction control have included pupil plane apodization, which extracts enormous penalties in effective collecting area to obtain small angle performance, and coronagraphs, in which high efficiency requires extensive occultation of the central source giving up a valuable portion of the field of view. We have developed a hybrid, high efficiency, coronagraph which is optimized for diffraction reduction within a few Airy radii of a bright unresolved source. The coronagraph utilizes a graded, or apodized transmission mask to occult the central source. Theoretical models have shown that the mask renders the Lyot stop more efficient while allowing some transmission very close to the parent star. For targets near the parent star we have found that the coronagraphic efficiency remains virtually independent of radius even when transmission losses through the mask are taken into account. Instead of being used to reduce the wings of a focal plane diffraction pattern, apodization is used in this design to reduce the diffraction wings of the pupil plane image. With a more compact pupil plane image, the application of a Lyot stop becomes much more efficient resulting in greatly improved performance without the loss of a valuable portion of the field of view. Theoretical results will be presented as well as data from a breadboard experiment.

3

Smartt, Raymond N., Serge Koutchmy, and Eugene W. Cross. "Prototype reflecting coronagraph." In OSA Annual Meeting. Washington, D.C.: Optica Publishing Group, 1989. http://dx.doi.org/10.1364/oam.1989.wv1.

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A miniature 1-m focal length coronagraph has been constructed at NSO/SP, based on a 5-cm diam superpolished silicon mirror from Zeiss, F.R.G. The optical configuration is simply off-axis reflection from the objective to an occulting disk, Lyot stop, and secondary optics. The coronagraph has been designed to be used either with photographic recording or a video CCD camera, both in combination with a VARO image tube. Details of the design and preliminary results are presented. It is shown that a mirror-objective-based coronagraph has many advantages and few disadvantages compared with the traditional singlet-objective-lens Lyot coronagraph. This reflecting coronagraph design is shown to be appropriate for larger systems, using other types of mirror substrate, with the prospect of very small net instrumental polarization, of crucial importance for certain coronal studies, with excellent aberration correction over modest fields.

4

Trauger, John, Brian Gordon, John Krist, and Dwight Moody. "Hybrid Lyot coronagraph for WFIRST-AFTA: coronagraph design and performance metrics." In SPIE Optical Engineering + Applications, edited by Stuart Shaklan. SPIE, 2015. http://dx.doi.org/10.1117/12.2190625.

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5

Socker, Dennis G., Guenter E. Brueckner, Clarence M. Korendyke, D. N. Lilley, James H. Steenson, Preston M. Kohn, Gail M. Lyons, et al. "LASCO spectrometric Lyot coronagraph tunable passband filter." In SPIE's 1996 International Symposium on Optical Science, Engineering, and Instrumentation, edited by David M. Rust. SPIE, 1996. http://dx.doi.org/10.1117/12.259711.

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6

Vigan, A., M. N'Diaye, and K. Dohlen. "Stop-less Lyot coronagraph for exoplanet characterization." In SPIE Astronomical Telescopes + Instrumentation, edited by Ian S. McLean, Suzanne K. Ramsay, and Hideki Takami. SPIE, 2012. http://dx.doi.org/10.1117/12.925294.

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7

Vial, Jean-Claude, Xueyan Song, Philippe Lemaire, Alan H. Gabriel, Jean-Pierre Delaboudiniere, Karine Bocchialini, Serge L. Koutchmy, et al. "The solar high-resolution imager - coronagraph LYOT mission." In Astronomical Telescopes and Instrumentation, edited by Stephen L. Keil and Sergey V. Avakyan. SPIE, 2003. http://dx.doi.org/10.1117/12.460291.

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8

Lucas, Miles, Michael Bottom, Olivier Guyon, Julien Lozi, Barnaby Norris, Vincent Deo, Sébastien Vievard, Kyohoon Ahn, Nour Skaf, and Peter Tuthill. "A visible-light Lyot coronagraph for SCExAO/VAMPIRES." In Ground-based and Airborne Instrumentation for Astronomy IX, edited by Christopher J. Evans, Julia J. Bryant, and Kentaro Motohara. SPIE, 2022. http://dx.doi.org/10.1117/12.2632269.

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9

Breckinridge, J. B., and R. A. Chipman. "Telescope polarization and image quality: Lyot coronagraph performance." In SPIE Astronomical Telescopes + Instrumentation, edited by Howard A. MacEwen, Giovanni G. Fazio, Makenzie Lystrup, Natalie Batalha, Nicholas Siegler, and Edward C. Tong. SPIE, 2016. http://dx.doi.org/10.1117/12.2231242.

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Zimmerman, Neil T., A. J. Eldorado Riggs, N. Jeremy Kasdin, Alexis Carlotti, and Robert J. Vanderbei. "Shaped pupil Lyot coronagraph designs for WFIRST/AFTA." In SPIE Optical Engineering + Applications, edited by Stuart Shaklan. SPIE, 2015. http://dx.doi.org/10.1117/12.2187141.

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