Holographic aperture masking (HAM) is an imaging technique in which a conventional telescope pupil is made into an interferometric array by means of a diffractive liquid-crystal phase mask. HAM allows for angular resolution that approaches and goes within the classical diffraction limit, while simultaneously increasing the throughput on the detector compared to traditional SAM, which uses a simple transmissive pupil plane mask. HAM creates interference fringes that provide phase and power information for each pair of holes in the mask, making the technique especially useful for the detection of close-in asymmetric structures surrounding stars, such as stellar or planetary companions, or protoplanetary disks. We present on-sky tests of an upgraded HAM mask installed in the Keck I OSIRIS imager. Observations were taken at J-band (1.28μm) of the known binary HD 44927 and single star HD 13249, the latter being used as a reference for calibration of instrumental errors. Using the SAMpy data reduction pipeline and modifying it for the Keck I HAM mask, Fourier observables were extracted and analyzed. We constrained astrometric and photometric measurements of the HD 44927 companion relative to its host star using a grid-fit companion model, producing orbital parameters to compare to previous measurements made with other interferometric imaging techniques.
A multiple-wave lateral shearing interferometer extends upon the traditional lateral shearing interferometry by producing multiple sheared copies of the incoming light. By using a special grating instead of a shear plate, it is able to produce fringes in multiple directions at the same time. This makes it possible to do single-shot reconstruction of both phase and amplitude aberrations.
Instead of a surface relief grating, we propose to use a patterned half-wave plate manufactured using direct-write techniques that acts as a liquid-crystal geometric phase grating. We demonstrate its wavefront sensing capabilities with laboratory measurements with an ALPAO-97 deformable mirror in monochromatic light. Finally, we present on-sky measurements performed at the William Herschel Telescope, showing broadband operation in unpolarized light.
The Leiden EXoplanet Instrument (LEXI) is a bench-mounted high-contrast spectrograph (HCS) and high- contrast imager(HCI). Both science instruments are mounted behind a common adaptive optics (AO) system. The AO can be controlled by several new wavefront sensors for which we will show the first on-sky results. There is a new pupil-plane wavefront sensors; the Generalized Optical Differentiation Wavefront sensor(g-ODWFS). LEXI can switch between two observing modes, the HCI mode or the HD-IFS mode. The spectrograph is very compact because it is fed by single-mode fiber. The HD-IFS is an IFS that covers the spectral range of 600 800 nm with a constant spectral resolving power of 96000. The 2kx3k detector makes it possible to deliver diffraction limited spectra of up to 20 input fibers. The high-dispersion spectra of the HD-IFS allow for robust post-processing technique to remove residual stellar speckles and allows for direct characterization of the faint stellar environment. We will show the first sucesful on-sky results of the injection into a single-mode fiber with LEXI. In HCI mode an Apodizing Phase Plate (APP) is used to create a dark region around the star with an average design contrast of 1E-4. The APP is multiplexed with holographic modes to create the Coronagraphic Modal Wavefront sensor (cMWS) for non-common path error (NCPE) correction. The cMWS creates holographic copies in the focal plane that react linearly to aberrations. The holographic copies are measured simultaneously with the science target. There is no downtime for NCPE correction. We will show the first on-sky closed-loop correction of (NCPEs) with the cMWS.
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