The Four‐Quadrant Phase‐Mask Coronagraph. I. Principle

Rouan, D.; Riaud, Pierre; Boccaletti, A.; Clénet, Y.; Labeyrie, A.

doi:10.1086/317707

Cited by 357 publications

(298 citation statements)

References 14 publications

(6 reference statements)

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“…In the pupil plane coronagraph family, there are: (a) amplitude apodization (via either intensity modification, or pupil shaping), and the phase induced amplitude apodization (PIAA) approach, in which the mirrors are warped to reshape the distribution of light in the pupil to yield an apodized shape, (b) pupil plane phase apodization, and in the focal plane coronagraph family, there are (c) amplitude masks (classical Lyot coronagraphs and band-limited profiles), and (d) phase mask coronagraphs of various types. Unlike "Lyot family" amplitude coronagraphs, focal-plane phase masks such as the four-quadrant phase-mask (FQPM, see [2], and [3] for a recent review on the FQPM) and optical vortex coronagraphs [4,5,6,7] have the great advantage of providing a very small inner working angle (IWA), which is one way of making use of smaller telescope apertures.…”

Section: Introductionmentioning

confidence: 99%

Optical Vectorial Vortex Coronagraphs using Liquid Crystal Polymers: theory, manufacturing and laboratory demonstration

et al. 2009

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Abstract:In this paper, after briefly reviewing the theory of vectorial vortices, we describe our technological approach to generating the necessary phase helix, and report results obtained with the first optical vectorial vortex coronagraph (OVVC) in the laboratory. To implement the geometrical phase ramp, we make use of Liquid Crystal Polymers (LCP), which we believe to be the most efficient technological path to quickly synthesize optical vectorial vortices of virtually any topological charge. With the first prototype device of topological charge 2, a maximum peak-to-peak attenuation of 1.4 × 10 −2 and a residual light level of 3 × 10 −5 at an angular separation of 3.5 λ /d (at which point our current noise floor is reached) have been obtained at a wavelength of 1.55 μm. These results demonstrate the validity of using space-variant birefringence distributions to generate a new family of coronagraphs usable in natural unpolarized light, opening a path to high performance coronagraphs that are achromatic and have low-sensitivity to low-order wavefront aberrations.

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Section: Introductionmentioning

confidence: 99%

Optical Vectorial Vortex Coronagraphs using Liquid Crystal Polymers: theory, manufacturing and laboratory demonstration

et al. 2009

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“…The four-quadrant phase mask [38] and vortex coronagraph known as the AGPM [39] are evolutions of this concept and are used today on VLT/NaCo. The latter has been successfully commissioned on Keck/NIRC2, on VLT/VISIR in the N band and is foreseen to equip VLT/SPHERE.…”

Section: Coronagraphy and Diffraction Controlmentioning

confidence: 99%

Adaptive Optics in High-Contrast Imaging

Milli¹,

Mawet²,

Mouillet³

et al. 2016

Astronomy at High Angular Resolution

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The development of adaptive optics (AO) played a major role in modern astronomy over the last three decades. By compensating for the atmospheric turbulence, these systems enable to reach the diffraction limit on large telescopes. In this review, we will focus on high contrast applications of adaptive optics, namely, imaging the close vicinity of bright stellar objects and revealing regions otherwise hidden within the turbulent halo of the atmosphere to look for objects with a contrast ratio lower than 10 −4 with respect to the central star. Such high-contrast AO-corrected observations have led to fundamental results in our current understanding of planetary formation and evolution as well as stellar evolution. AO systems equipped three generations of instruments, from the first pioneering experiments in the nineties, to the first wave of instruments on 8m-class telescopes in the years 2000, and finally to the extreme AO systems that have recently started operations. Along with highcontrast techniques, AO enables to reveal the circumstellar environment: massive protoplanetary disks featuring spiral arms, gaps or other asymetries hinting at ongoing planet formation, young giant planets shining in thermal emission, or tenuous debris disks and micron-sized dust leftover from collisions in massive asteroid-belt analogs. After introducing the science case and technical requirements, we will review the architecture of standard and extreme AO systems, before presenting a few selected science highlights obtained with recent AO instruments.

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“…In the following, we discuss our recent work with phase masks at JPL, including both laboratory results and initial on-sky testing using our extreme adaptive optics well-corrected subaperture at Palomar. Figure 1 shows the operation of a phase mask coronagraph, together with the phase structure inherent in four-quadrant phase masks [7] and optical vortex masks. In the former, alternating phases of 0 and radians are applied in the four quadrants of the focal-plane point spread function, while in the latter case, an azimuthal phase spiral reaching an even multiple of 2 radians in a circuit about the center is used.…”

Section: Introductionmentioning

confidence: 99%

Phase mask coronagraphy at JPL and Palomar

Serabyn

Mawet

2011

EPJ Web of Conferences

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Abstract. For the imaging of faint companions, phase mask coronagraphy has the dual advantages of a small inner working angle and high throughput. This paper summarizes our recent work in developing phase masks and in demonstrating their capabilities at JPL. Four-quadrant phase masks have been manufactured at JPL by means of both evaporation and etching, and we have been developing liquid crystal vortex phase masks in partnership with a commercial vendor. Both types of mask have been used with our extreme adaptive optics well-corrected subaperture at Palomar to detect known brown dwarf companions as close as ∼ 2.5 /D to stars. Moreover, our recent vortex masks perform very well in laboratory tests, with a demonstrated infrared contrast of about 10 −6 at 3 /D, and contrasts of a few 10 −7 with an initial optical wavelength device. The demonstrated performance already meets the needs of ground-based extreme adaptive optics coronagraphy, and further planned improvements are aimed at reaching the 10 −10 contrast needed for terrestrial exoplanet detection with a space-based coronagraph.

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The Four‐Quadrant Phase‐Mask Coronagraph. I. Principle

Cited by 357 publications

References 14 publications

Optical Vectorial Vortex Coronagraphs using Liquid Crystal Polymers: theory, manufacturing and laboratory demonstration

Optical Vectorial Vortex Coronagraphs using Liquid Crystal Polymers: theory, manufacturing and laboratory demonstration

Adaptive Optics in High-Contrast Imaging

Phase mask coronagraphy at JPL and Palomar

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