Recent results of the second generation of vector vortex coronagraphs on the high-contrast imaging testbed at JPL

Mawet, Dimitri; Serabyn, Eugene; Moody, Dwight; Kern, Brian; Niessner, Albert F.; Kuhnert, A.; Shemo, David M.; Chipman, Russell A.; McClain, Stephen C.; Trauger, John T.

doi:10.1117/12.896070

Cited by 25 publications

(15 citation statements)

References 8 publications

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“…The HCIT is a state-of-the-art coronagraph simulator installed into a vacuum chamber. Several kinds of coronagraphs have been tested at the HCIT/JPL [16][17][18][19][20][21][22] .…”

Section: The High-contrast Imaging Testbed (Hcit)mentioning

confidence: 99%

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Coronagraph focal-plane phase masks based on photonic crystal technology: recent progress and observational strategy

Murakami

Nishikawa

Traub

et al. 2012

Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave

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Photonic crystal, an artificial periodic nanostructure of refractive indices, is one of the attractive technologies for coronagraph focal-plane masks aiming at direct imaging and characterization of terrestrial extrasolar planets. We manufactured the eight-octant phase mask (8OPM) and the vector vortex coronagraph (VVC) mask very precisely using the photonic crystal technology. Fully achromatic phase-mask coronagraphs can be realized by applying appropriate polarization filters to the masks. We carried out laboratory experiments of the polarization-filtered 8OPM coronagraph using the High-Contrast Imaging Testbed (HCIT), a state-of-the-art coronagraph simulator at the Jet Propulsion Laboratory (JPL). We report the experimental results of 10 -8 -level contrast across several wavelengths over 10% bandwidth around 800nm. In addition, we present future prospects and observational strategy for the photonic-crystal mask coronagraphs combined with differential imaging techniques to reach higher contrast. We proposed to apply the polarization-differential imaging (PDI) technique to the VVC, in which we built a two-channel coronagraph using polarizing beam splitters to avoid a loss of intensity due to the polarization filters. We also proposed to apply the angular-differential imaging (ADI) technique to the 8OPM coronagraph. The 8OPM/ADI mode mitigates an intensity loss due to a phase transition of the mask and provides a full field of view around central stars. We present results of preliminary laboratory demonstrations of the PDI and ADI observational modes with the phase-mask coronagraphs.

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“…The HCIT is a state-of-the-art coronagraph simulator installed into a vacuum chamber. Several kinds of coronagraphs have been tested at the HCIT/JPL [16][17][18][19][20][21][22] .…”

Section: The High-contrast Imaging Testbed (Hcit)mentioning

confidence: 99%

“…2 of Ref. [22]. Several kinds of light sources are available, such as a monochromatic laser of λ=785 nm, or a supercontinuum light with selectable bandpass filters with bandwidths of 2%, 10%, and 20%.…”

Section: The High-contrast Imaging Testbed (Hcit)mentioning

confidence: 99%

Coronagraph focal-plane phase masks based on photonic crystal technology: recent progress and observational strategy

Murakami

Nishikawa

Traub

et al. 2012

Space Telescopes and Instrumentation 2012: Optical, Infrared, and Millimeter Wave

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“…The heart of the system is a high-order deformable mirror (DM) to control higherorder aberration (see Sec. 3.2.3) and a vector vortex coronagraph (OAP3, VVC, and OAP4) in the Mawet 26 configuration with a Lyot stop and camera lenses (SCI L1 and SCI L2) to form the image. The data are recorded using a microwave kinetic inductance detector (SCI camera, see Sec.…”

Section: Telescopementioning

confidence: 99%

“…2 The design of the PICTURE C coronagraph follows that of Mawet. 26 The system uses an f ∕2.5 primary (M1). An afocal, off-axis, Gregorian secondary (M2), two fold mirrors (FM1 and FM2), and an integral wavefront controller (IWC; see Sec.…”

Section: Telescopementioning

confidence: 99%

Planetary Imaging Concept Testbed Using a Recoverable Experiment–Coronagraph (PICTURE C)

Cook

Cahoy

Chakrabarti

et al. 2015

J. Astron. Telesc. Instrum. Syst

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Abstract. An exoplanet mission based on a high-altitude balloon is a next logical step in humanity's quest to explore Earthlike planets in Earthlike orbits orbiting Sunlike stars. The mission described here is capable of spectrally imaging debris disks and exozodiacal light around a number of stars spanning a range of infrared excesses, stellar types, and ages. The mission is designed to characterize the background near those stars, to study the disks themselves, and to look for planets in those systems. The background light scattered and emitted from the disk is a key uncertainty in the mission design of any exoplanet direct imaging mission, thus, its characterization is critically important for future imaging of exoplanets. © The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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“…Already in use with the PALM-3000 system, are the PHARO infrared camera and spectrograph which provides imaging and grism spectroscopy at 0.96-2.5 μm wavelength over a 25-40 arcsec field [3] , the P1640 coronagraphic integral field spectrograph (IFS) built by the American Museum of Natural History with a postcoronagraphic calibration wavefront sensor contributed by JPL which provides spectra over 1.1-1.65 μm wavelengths for a 10 arcsec field [4] , the O-SWIFT I-z band integral field spectrograph which provides spectra over 0.6-1 μm wavelengths for a 4 arcsec field [5] , and the Fiber Nuller high-contrast coronagraphic imager built by JPL which provides images at 1.4-2.2 μm [6] . In addition, a new visible imager from Caltech, TMAS [7] , will be commissioned in fall of 2012 and a calibration system for the PHARO instrument is planned in 2013 to improve contrasts using novel coronagraphic techniques such as the vector vortex [8] .…”

Section: Introductionmentioning

confidence: 99%

Results from the PALM-3000 high-order adaptive optics system

Roberts

Dekany²,

Burruss

et al. 2012

SPIE Proceedings

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The first of a new generation of high actuator density AO systems developed for large telescopes, PALM-3000 is optimized for high-contrast exoplanet science but will support operation with natural guide stars as faint as V ~ 18. PALM-3000 began commissioning in June 2011 on the Palomar 200" telescope and has to date over 60 nights of observing. The AO system consists of two Xinetics deformable mirrors, one with 66 by 66 actuators and another with 21 by 21 actuators, a Shack-Hartman WFS with four pupil sampling modes (ranging from 64 to 8 samples across the pupil), and a full vector matrix multiply real-time system capable of running at 2KHz frame rates. We present the details of the completed system, and initial results. Operating at 2 kHz with 8.3cm pupil sampling on-sky, we have achieved a K-band Strehl ratio as high as 84% in ~1.0 arcsecond visible seeing.

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Recent results of the second generation of vector vortex coronagraphs on the high-contrast imaging testbed at JPL

Cited by 25 publications

References 8 publications

Coronagraph focal-plane phase masks based on photonic crystal technology: recent progress and observational strategy

Coronagraph focal-plane phase masks based on photonic crystal technology: recent progress and observational strategy

Planetary Imaging Concept Testbed Using a Recoverable Experiment–Coronagraph (PICTURE C)

Results from the PALM-3000 high-order adaptive optics system

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