Phase-induced amplitude apodization of telescope pupils for extrasolar terrestrial planet imaging

By Olivier Guyon. 2003

329 citations recorded by the source corpus.

In this paper, an alternative to classical pupil apodization techniques (use of an amplitude pupil mask) is proposed. It is shown that an achromatic apodized pupil suitable for imaging of extrasolar planets can be obtained by reflection of an unapodized flat wavefront on two mirrors. By carefully choosing the shape of these two mirrors, it is possible to obtain a contrast better than 10 9 at a distance smaller than $2 \lambda/d$ from the optical axis. Because this technique preserves both the angular resolution and light gathering capabilities of the unapodized pupil, it allows efficient detection of terrestrial extrasolar planets with a 1.5 m telescope in the visible.

Subfields: Atomic and Molecular Physics, and Optics, Biomedical Engineering

View Paper: https://www.semanticscholar.org/paper/841cb53398e1274605339da90a0a48748d897057

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In Atomic and Molecular Physics, and Optics

In Biomedical Engineering

Citations in the corpus

Imaging Extrasolar Giant Planets (2016, methodology): “…interferometric science in the visible with VAMPIRES (Norris et al. 2015) and FIRST (Huby et al. 2012), high-contrast integral field spectroscopy (Brandt et al. 2014b), and coronagraphy with phase-induced amplitude apodization (Guyon 2003) and vector vortex coronagraphs (Mawet et al. 2010).”
SPHERE: the exoplanet imager for the Very Large Telescope (2019, background): “…that all present their respective advantages and drawbacks in terms of IWA, band-pass, manufacturing, polarimetric requirements, etc (e.g., Guyon 2003; Mawet et al. 2005, 2009; Kenworthy et al. 2010; Snik et al. 2012; Carlotti 2013; Mawet et al. 2013; N’Diaye et al. 14 More than 120…”
Exoplanet Imaging with a Phase-induced Amplitude Apodization Coronagraph. I. Principle (2004, methodology): “This law applies to both interferometers (Labeyrie et al. 1996) and monolithic pupils (Guyon 2003; Soummer et al. 2003; Traub & Vanderbei 2003) and prevents the PIAAI from directly forming good-quality wide-field images.”
FUNDAMENTAL LIMITATIONS OF HIGH CONTRAST IMAGING SET BY SMALL SAMPLE STATISTICS (2014, background): “…imaging instruments, 1 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA or to efficiently cope with the limited size of spacebased telescopes (Roddier & Roddier 1997; Rouan et al. 2000; Guyon 2003; Mawet et al. 2005; Serabyn et al. 2010).”
Optimal Occulter Design for Finding Extrasolar Planets (2007, methodology): “Several methods (see Kasdin et al. 2003; Kuchner&Traub 2002; Vanderbei 2006;Guyon 2003) have been proposed to do thiswithin the telescope by adjusting the point spread function so that there is very little starlight at the location of the planet in the image plane of the telescope.”
Theoretical Limits on Extrasolar Terrestrial Planet Detection with Coronagraphs (2006, methodology): “This coronagraph uses a lossless amplitude apodization of the pupil performed by geometric redistribution of the light rather than selective absorption (Guyon 2003; Traub & Vanderbei 2003; Guyon et al. 2005; Vanderbei & Traub 2005; Martinache et al. 2006; Vanderbei 2006; Pluzhnik et al. 2006).”