Peter Wizinowich is the Optical Systems Manager at the W. M. Keck Observatory (WMKO). He has been at WMKO since 1991, and has led the telescope optics installation and alignment, the adaptive optics development program and the Keck interferometer development activities. Prior to coming to WMKO, Peter was a Staff Scientist at Steward Observatory, an instrumentation technician at the Canada-France-Hawaii Telescope and resident astronomer at the University of Toronto Southern Observatory.
Peter received his Ph.D. from the University of Arizona's Optical Sciences Center, his M.A.Sc. from the University of Toronto Institute for Aerospace Studies, and his B.Sc. in physics and astronomy from the University of Toronto.
Peter received his Ph.D. from the University of Arizona's Optical Sciences Center, his M.A.Sc. from the University of Toronto Institute for Aerospace Studies, and his B.Sc. in physics and astronomy from the University of Toronto.
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In this paper we present the results of the latest upgrades to the KPIC instrument. Among these upgrades, a second fiber bundle with related injection/extraction optics and new dichroics were added to extend KPIC’s science capabilities to y through H band, and to provide access to laser frequency combs for spectral calibration from y-K. Additionally, the charge 2 vortex mask for fiber nulling was supplemented with a charge 1 mask to enable spectroscopy of low mass companions at very small angular separations. Other upgrades included an atmospheric dispersion corrector, a new calibration source switching system, and an optimized tip/tilt control system. Here we show preliminary results of on-sky tests performed in the first few months of re-commissioning, along with the next steps for the instrument.
Enhanced high-dispersion coronagraphy with KPIC phase II: design, assembly and status of sub-modules
This paper describes the implementation of the algorithms, and the design and development of the prototype operational tools for automated PSF reconstruction. On-sky performance is discussed by comparing the reconstructed PSFs to the measured PSF’s on the NIRC2 science camera. The importance of knowing the control loop performance, accurate mapping of the telescope pupil to the deformable mirror and the science instrument pupil, and the telescope segment piston error are highlighted. We close by discussing lessons learned and near-term future plans.
The new laser has been implemented on the telescope’s elevation ring with its electronics installed on a new Nasmyth sub-platform, with the capacity to support up to three laser systems for future upgrades. The laser is projected from behind the telescope’s secondary mirror using the recently implemented center launch system (CLS) to reduce LGS spot size. We will present the new laser system and its performance with respect to power, stability, wavelength, spot size, optical repumping, polarization, efficiency, and its return with respect to pointing alignment to the magnetic field. Preliminary LGSAO performance is presented with the system returning to science operations. We will also provide an update on current and future upgrades at the WMKO.
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