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Journal articles on the topic 'Lyot coronagraph'

Author: Grafiati

Published: 7 July 2024

Last updated: 31 July 2025

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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 acc

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2

Kim, I. S., and O. I. Bugaenko. "On magnetic measurements in prominences." Proceedings of the International Astronomical Union 8, S300 (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.

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3

Anche, Ramya M., Ewan Douglas, Kian Milani, et al. "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 (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),

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4

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 estima

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5

Carbillet, Marcel, Philippe Bendjoya, Lyu Abe, et al. "Apodized Lyot coronagraph for SPHERE/VLT." Experimental Astronomy 30, no. 1 (2011): 39–58. http://dx.doi.org/10.1007/s10686-011-9219-4.

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6

Leboulleux, Lucie, Jean-François Sauvage, Rémi Soummer, et al. "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. Amon

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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 (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 (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

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10

Xin, Yinzi, Laurent Pueyo, Romain Laugier, et al. "Coronagraphic Data Post-processing Using Projections on Instrumental Modes." Astrophysical Journal 963, no. 2 (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 approxima

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11

Aime, C. "Principle of an Achromatic Prolate Apodized Lyot Coronagraph." Publications of the Astronomical Society of the Pacific 117, no. 835 (2005): 1012–19. http://dx.doi.org/10.1086/432687.

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12

Martinez, P., A. Boccaletti, M. Kasper, P. Baudoz, and C. Cavarroc. "Optimization of apodized pupil Lyot coronagraph for ELTs." Astronomy & Astrophysics 474, no. 2 (2007): 671–78. http://dx.doi.org/10.1051/0004-6361:20077708.

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13

Vigan, A., M. N’Diaye, K. Dohlen, et al. "Calibration of quasi-static aberrations in exoplanet direct-imaging instruments with a Zernike phase-mask sensor." Astronomy & Astrophysics 629 (August 26, 2019): A11. http://dx.doi.org/10.1051/0004-6361/201935889.

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Second-generation exoplanet imagers using extreme adaptive optics (ExAO) and coronagraphy have demonstrated their great potential for studying close circumstellar environments and for detecting new companions and helping to understand their physical properties. However, at very small angular separation, their performance in contrast is limited by several factors: diffraction by the complex telescope pupil (central obscuration and spiders) not perfectly canceled by the coronagraph, residual dynamic wavefront errors, chromatic wavefront errors, and wavefront errors resulting from noncommon path

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14

CHI, Jinpeng, Hongxin ZHANG, Xiaodong WANG, et al. "Optical system and stray light suppression of Lyot coronagraph." Optics and Precision Engineering 30, no. 17 (2022): 2050–57. http://dx.doi.org/10.37188/ope.20223017.2050.

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15

Soummer, R., B. R. Oppenheimer, S. Hinkley, et al. "The Lyot project coronagraph: data processing and performance analysis." EAS Publications Series 22 (2006): 199–212. http://dx.doi.org/10.1051/eas:2006133.

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16

Hufbauer, Karl. "Artificial Eclipses: Bernard Lyot and the Coronagraph, 1929-1939." Historical Studies in the Physical and Biological Sciences 24, no. 2 (1994): 337–94. http://dx.doi.org/10.2307/27757726.

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17

Murakami, N., R. Uemura, N. Baba, Y. Sato, J. Nishikawa, and M. Tamura. "Four‐Quadrant Phase Mask Coronagraph with a Jacquinot‐Lyot Stop." Astrophysical Journal 677, no. 2 (2008): 1425–32. http://dx.doi.org/10.1086/527668.

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18

Bu Heyang, 卜和阳, 张红鑫 Zhang Hongxin, 卢振武 Lu Zhenwu, and 张正正 Zhang Zhengzheng. "Analysis on the Parameter of Lyot Stop in Internally Occulting Refractive Coronagraph." Acta Optica Sinica 34, no. 12 (2014): 1212006. http://dx.doi.org/10.3788/aos201434.1212006.

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19

Ferrari, André, Claude Aime, and Rémi Soummer. "ANALYTICAL COMPUTATION OF THE LYOT CORONAGRAPH RESPONSE TO AN EXTENDED SOURCE." Astrophysical Journal 708, no. 1 (2009): 218–23. http://dx.doi.org/10.1088/0004-637x/708/1/218.

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20

Guerri, Géraldine, Jean-Baptiste Daban, Sylvie Robbe-Dubois, et al. "Apodized Lyot coronagraph for SPHERE/VLT: II. Laboratory tests and performance." Experimental Astronomy 30, no. 1 (2011): 59–81. http://dx.doi.org/10.1007/s10686-011-9220-y.

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21

Ge, Rui, Hui Zhao, Jing-Xuan Wei, et al. "Improved two-step optimization procedure used for designing an apodizer and Lyot stop in the Lyot coronagraph." Applied Optics 59, no. 16 (2020): 4939. http://dx.doi.org/10.1364/ao.391959.

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22

Smartt, Raymond N., Serge Koutchmy, and Jacques-Clair NoëNs. "Near-IR Solar Coronal Observations with New-Technology Reflecting Coronographs." Symposium - International Astronomical Union 154 (1994): 603–8. http://dx.doi.org/10.1017/s0074180900124908.

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Emission-line and K-coronal observations in the IR have the significant advantage of reduced sky brightness compared with the visible, while the effects of seeing are also reduced. Moreover, strong lines are available in the near-IR. Examples of the current capabilities of IR coronal observations using conventional Lyot coronagraphs are discussed briefly. Photometric measurements using the two IR lines of Fe XIII (10,747 Å and 10,798 Å), together with the Fe XIII 3,388 Å line, have provided a valuable electron-density diagnostic, but with low-angular-resolution. The 10,747 Å line has high intr

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23

Martinez, P. "Fast-modulation imaging with the self-coherent camera." Astronomy & Astrophysics 629 (September 2019): L10. http://dx.doi.org/10.1051/0004-6361/201936496.

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Context. Direct detection of exoplanets requires imaging in a highly dynamic range and exquisite image quality and stability. Wavefront error (atmospheric errors, manufacturing errors on optics, cophasing residuals, temperature variations, etc.) will limit the efficiency of this endeavor by creating various flavors of speckles that evolve with different timescales. Active wavefront-error correction using a deformable mirror requires measuring the wavefront aberrations in the science image with high accuracy and in a shorter time than the duration of the dominant speckle lifetime. Aims. The sel

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24

Rozelot, Jean-Pierre, and Jagdev Singh. "Spectrographic observations of the ionized iron coronal emission lines at Pic du Midi Observatory (F) in the mid-60s." Journal for the History of Astronomy 53, no. 3 (2022): 300–327. http://dx.doi.org/10.1177/00218286221101604.

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This paper is dedicated to the memory of Jean Rösch, a great figure in astronomy in the years 1947–1981 who designed, among several innovative devices, a 15-cm spectro-coronagraph. This instrument was installed at Pic du Midi observatory (south-west France), was in use during the mid-60s, fully dedicated to the observation from the ground of the coronal highly ionized iron lines, which was a true challenge at that time. This program is here reconsidered in the context of the time, at Pic du Midi observatory, which has been the cradle of routine visual coronal observations initiated by Bernard

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25

Ruane, G. J., E. Huby, O. Absil, et al. "Lyot-plane phase masks for improved high-contrast imaging with a vortex coronagraph." Astronomy & Astrophysics 583 (October 30, 2015): A81. http://dx.doi.org/10.1051/0004-6361/201526561.

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26

Itoh, Satoshi, Taro Matsuo, Shunsuke Ota, et al. "Experimental Verification of a One-dimensional Diffraction-limit Coronagraph." Publications of the Astronomical Society of the Pacific 135, no. 1048 (2023): 064502. http://dx.doi.org/10.1088/1538-3873/acdbea.

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Abstract We performed an experimental verification of a coronagraph. As a result, we confirmed that, at the focal region where the planetary point spread function exists, the coronagraph system mitigates the raw contrast of a star-planet system by at least 1 × 10−5 even for the 1-λ/D star-planet separation. In addition, the verified coronagraph keeps the shapes of the off-axis point spread functions when the setup has the source angular separation of 1λ/D. The low-order wave front error and the non-zero extinction ratio of the linear polarizer may affect the currently confirmed contrast. The s

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27

Dorotovič, I., B. Lukáč, T. Pintér, and M. Rybanský. "A New Station of Prominence Patrol Observations in Slovakia." International Astronomical Union Colloquium 167 (1998): 498–501. http://dx.doi.org/10.1017/s0252921100048168.

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AbstractThe data from prominence observations provide an opportunity to study spatio-temporal distribution of prominences over a solar cycle. The Slovak Central Observatory (SCO) at Hurbanovo (South Slovakia) in cooperation with the coronal station at Lomnický Štít (Astronomical Institute of the Slovak Academy of Sciences, Tatranská Lomnica, Slovakia) constructed a Lyot coronagraph with parameters D/f of 90/1250/3750 mm in 1996 for regular prominence patrol at Hurbanovo (112 m above sea level).The aim of this collaboration is a joint annual publication of a catalogue of the observed prominence

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28

Martinez, P., C. Dorrer, M. Kasper, A. Boccaletti, and K. Dohlen. "Design, analysis, and testing of a microdot apodizer for the apodized pupil Lyot coronagraph." Astronomy and Astrophysics 520 (September 2010): A110. http://dx.doi.org/10.1051/0004-6361/201015351.

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29

Martinez, P., C. Dorrer, E. Aller Carpentier, et al. "Design, analysis, and testing of a microdot apodizer for the Apodized Pupil Lyot Coronagraph." Astronomy & Astrophysics 495, no. 1 (2008): 363–70. http://dx.doi.org/10.1051/0004-6361:200810918.

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30

Martinez, P., C. Dorrer, M. Kasper, A. Boccaletti, and K. Dohlen. "Design, analysis, and testing of a microdot apodizer for the apodized pupil Lyot coronagraph." Astronomy & Astrophysics 500, no. 3 (2009): 1281–85. http://dx.doi.org/10.1051/0004-6361/200911824.

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31

Itoh, Satoshi, Taro Matsuo, and Motohide Tamura. "Wide-spectral-band Nuller Insensitive to Finite Stellar Angular Diameter with a One-dimensional Diffraction-limited Coronagraph." Astronomical Journal 167, no. 5 (2024): 235. http://dx.doi.org/10.3847/1538-3881/ad3733.

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Abstract Potentially habitable planets around nearby stars less massive than solar-type stars could join targets of the spectroscopy of the planetary reflected light with future space telescopes. However, the orbits of most of these planets occur near the diffraction limit for 6 m diameter telescopes. Thus, while securing contrast-mitigation ability under a broad spectral bandwidth and a finite stellar angular diameter, we must maintain planetary throughput even at the diffraction-limited angles to be able to reduce the effect of the photon noise within a reasonable observation time. A one-dim

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32

Crepp, Justin R., Jian Ge, Andrew D. Vanden Heuvel, Shane P. Miller, and Marc J. Kuchner. "Laboratory Testing of a Lyot Coronagraph Equipped with an Eighth‐Order Notch Filter Image Mask." Astrophysical Journal 646, no. 2 (2006): 1252–59. http://dx.doi.org/10.1086/504977.

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33

Laginja, Iva, Jean-François Sauvage, Laurent M. Mugnier, et al. "Wavefront tolerances of space-based segmented telescopes at very high contrast: Experimental validation." Astronomy & Astrophysics 658 (February 2022): A84. http://dx.doi.org/10.1051/0004-6361/202142150.

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Context. The detection and characterization of Earth-like exoplanets (exoEarths) from space requires exquisite wavefront stability at contrast levels of 10−10. On segmented telescopes in particular, aberrations induced by co-phasing errors lead to a light leakage through the coronagraph, deteriorating the imaging performance. These need to be limited in order to facilitate the direct imaging of exoEarths. Aims. We perform a laboratory validation of an analytical tolerancing model that allows us to determine wavefront error requirements in the 10−6 − 10−8 contrast regime for a segmented pupil w

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34

Shestov, S. V., A. N. Zhukov, and D. B. Seaton. "Modeling and removal of optical ghosts in the PROBA-3/ASPIICS externally occulted solar coronagraph." Astronomy & Astrophysics 622 (February 2019): A101. http://dx.doi.org/10.1051/0004-6361/201834584.

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Context. ASPIICS is a novel externally occulted solar coronagraph, which will be launched onboard the PROBA-3 mission of the European Space Agency. The external occulter will be placed on the first satellite ∼150 m ahead of the second satellite that will carry an optical instrument. For 6 h per orbit, the satellites will fly in a precise formation, constituting a giant externally occulted coronagraph. The large distance between the external occulter and the primary objective will allow observations of the white-light solar corona starting from extremely low heights ∼1.1 R⊙. Aims. We aim to ana

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35

Thomas, Sandrine J., Rémi Soummer, Daren Dillon, Bruce Macintosh, Donald Gavel, and Anand Sivaramakrishnan. "TESTING THE APODIZED PUPIL LYOT CORONAGRAPH ON THE LABORATORY FOR ADAPTIVE OPTICS EXTREME ADAPTIVE OPTICS TESTBED." Astronomical Journal 142, no. 4 (2011): 119. http://dx.doi.org/10.1088/0004-6256/142/4/119.

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36

Pourcelot, R., A. Vigan, K. Dohlen, et al. "Calibration of residual aberrations in exoplanet imagers with large numbers of degrees of freedom." Astronomy & Astrophysics 649 (May 2021): A170. http://dx.doi.org/10.1051/0004-6361/202040157.

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Imaging faint objects, such as exoplanets or disks, around nearby stars is extremely challenging because host star images are dominated by the telescope diffraction pattern. Using a coronagraph is an efficient solution for removing diffraction but requires an incoming wavefront with good quality to maximize starlight rejection. On the ground, the most advanced exoplanet imagers use extreme adaptive optics (ExAO) systems that are based on a deformable mirror (DM) with a large number of actuators to efficiently compensate for high-order aberrations and provide diffraction-limited images. While s

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37

Bos, S. P. "The polarization-encoded self-coherent camera." Astronomy & Astrophysics 646 (February 2021): A177. http://dx.doi.org/10.1051/0004-6361/202039569.

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Context. The exploration of circumstellar environments by means of direct imaging to search for Earth-like exoplanets is one of the challenges of modern astronomy. One of the current limitations are evolving non-common path aberrations (NCPA) that originate from optics downstream of the main wavefront sensor. Measuring these NCPA with the science camera during observations is the preferred solution for minimizing the non-common path and maximizing the science duty cycle. The self-coherent camera (SCC) is an integrated coronagraph and focal-plane wavefront sensor that generates wavefront inform

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38

Seo, Byoung-Joon, Brian Gordon, Brian Kern, et al. "Hybrid Lyot coronagraph for wide-field infrared survey telescope-astrophysics focused telescope assets: occulter fabrication and high contrast narrowband testbed demonstration." Journal of Astronomical Telescopes, Instruments, and Systems 2, no. 1 (2016): 011019. http://dx.doi.org/10.1117/1.jatis.2.1.011019.

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39

Guseva, S. A., and A. D. Shramko. "Study of the Green Coronal Line with Altitude from Out-of-Eclipse Observations during Solar Cycle 24." Космические исследования 61, no. 2 (2023): 124–33. http://dx.doi.org/10.31857/s0023420622600180.

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The results of studies of the coronal emission line λ = 5303 Å (Fe XIV) for the period of solar cycle 24 are presented. The spectral data were obtained with an out-of-eclipse Lyot coronagraph at the Mountain Astronomical Station of the Pulkovo Observatory, Russian Academy of Sciences (near Kislovodsk). As a result of processing of out-of-eclipse observations, a database of three types of daily coronal maps of green line intensity I5303 was created with a height distribution h from 1R☉ to 1.38R☉ (R☉ is the radius of the Sun). Irregularities along the λ = 5303 Å line were found and identified, w

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40

Haffert, S. Y. "The spectrally modulated self-coherent camera (SM-SCC): Increasing throughput for focal-plane wavefront sensing." Astronomy & Astrophysics 659 (March 2022): A51. http://dx.doi.org/10.1051/0004-6361/202141309.

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Context. The detection and characterization of Earth-like exoplanets is one of the major science drivers for the next generation of telescopes. Direct imaging of the planets will play a major role in observations. Current direct imaging instruments are limited by evolving non-common path aberrations (NCPAs). The NCPAs have to be compensated for by using the science focal-plane image. A promising sensor is the self-coherent camera (SCC). An SCC adds a pinhole to the Lyot stop in the coronagraph to introduce a probe electric field. The pinhole has to be separated by at least 1.5 times the pupil

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41

Galicher, R., E. Huby, P. Baudoz, and O. Dupuis. "A family of phase masks for broadband coronagraphy example of the wrapped vortex phase mask theory and laboratory demonstration." Astronomy & Astrophysics 635 (February 28, 2020): A11. http://dx.doi.org/10.1051/0004-6361/201936971.

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Context. Future instruments need efficient coronagraphs over large spectral ranges to enable broadband imaging or spectral characterization of exoplanets that are 108 times fainter than their star. Several solutions have been proposed. Pupil apodizers can attenuate the star intensity by a factor of 1010 but they only transmit a few percent of the light of the planet. Cascades of phase and/or amplitude masks can both attenuate the starlight and transmit most of the planet light, but the number of optics that require alignment makes this solution impractical for an instrument. Finally, vector ph

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42

Sivaramakrishnan, Anand, and James P. Lloyd. "Spiders in Lyot Coronagraphs." Astrophysical Journal 633, no. 1 (2005): 528–33. http://dx.doi.org/10.1086/432903.

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43

Lloyd, James P., and Anand Sivaramakrishnan. "Tip‐Tilt Error in Lyot Coronagraphs." Astrophysical Journal 621, no. 2 (2005): 1153–58. http://dx.doi.org/10.1086/427719.

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44

Ferrari, Andre. "Analytical Analysis of Lyot Coronagraphs Response." Astrophysical Journal 657, no. 2 (2007): 1201–9. http://dx.doi.org/10.1086/511026.

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45

Sivaramakrishnan, Anand, Rémi Soummer, Laurent Pueyo, J. Kent Wallace, and Michael Shao. "Sensing Phase Aberrations behind Lyot Coronagraphs." Astrophysical Journal 688, no. 1 (2008): 701–8. http://dx.doi.org/10.1086/591957.

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46

Oppenheimer, B. R., R. G. Dekany, M. Troy, T. Hayward, and B. Brandl. "Companion Detection Limits with Adaptive Optics Coronagraphy." Symposium - International Astronomical Union 202 (2004): 99–102. http://dx.doi.org/10.1017/s0074180900217592.

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We present a study of the Palomar Adaptive Optics System and the PHARO near infrared camera in coronagraphic mode. The camera provides two different focal plane occulting masks–opaque circular disks 0.43 and 0.97″ across. Three different pupil plane apodizing masks (Lyot masks) are also provided. The six different combinations of Lyot mask and focal plane mask suppress differently the point spread function of a bright star centered on the focal plane mask. We obtained images of the bright nearby star Gliese 614 with all six different configurations in the K filter. We measured the dynamic rang

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47

Sivaramakrishnan, Anand, and Natalia Yaitskova. "Lyot Coronagraphy on Giant Segmented-Mirror Telescopes." Astrophysical Journal 626, no. 1 (2005): L65—L68. http://dx.doi.org/10.1086/431460.

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48

Aime, C., and R. Soummer. "Cascading properties of Prolate Apodized Lyot Coronagraphs." EAS Publications Series 12 (2004): 281–86. http://dx.doi.org/10.1051/eas:2004041.

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49

Soummer, Rémi. "Apodized Pupil Lyot Coronagraphs for Arbitrary Telescope Apertures." Astrophysical Journal 618, no. 2 (2004): L161—L164. http://dx.doi.org/10.1086/427923.

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50

Yaitskova, N. "Peculiarity of Lyot Coronagraphy for Highly Segmented Apertures." EAS Publications Series 22 (2006): 223–37. http://dx.doi.org/10.1051/eas:2006135.

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