A5036881839- Adaptive optics and wavefront sensing
- Stellar, planetary, and galactic studies
- Optical Systems and Laser Technology
- Astronomy and Astrophysical Research
- Optical Wireless Communication Technologies
- CCD and CMOS Imaging Sensors
- Astrophysics and Star Formation Studies
- Advanced optical system design
- Astronomical Observations and Instrumentation
- Geomagnetism and Paleomagnetism Studies
- Calibration and Measurement Techniques
- Astro and Planetary Science
- Solid State Laser Technologies
- Geological and Geochemical Analysis
- Atmospheric aerosols and clouds
- Geophysics and Sensor Technology
- earthquake and tectonic studies
- Space Satellite Systems and Control
University of Arizona
2023-2024
University of California, Berkeley
2019-2022
Almost all current and future high-contrast imaging instruments will use a Pyramid wavefront sensor (PWFS) as primary or secondary sensor. The main issue with the PWFS is its nonlinear response to large phase aberrations, especially under strong atmospheric turbulence. Most try increase linearity range by using dynamic modulation, but this leads decreased sensitivity, most prominently for low-order modes, makes it blind petal-piston modes. In push toward of fainter stars deeper contrasts,...
We present 3 years of high-contrast imaging the PDS 70 b and c accreting protoplanets with new extreme AO system MagAO-X as part MaxProtoPlanetS survey H$\alpha$ protoplanets. In 2023 2024 our sharp (25-27 mas FWHM); well corrected (20-26% Strehl), deep (2-3.6hr) images detect compact (r~30 mas; r~3 au) circumplanetary disks (CPDs) surrounding both Starlight scattering off dusty outer edges these CPDs is likely source bright continuum light detected within ~30 planets in simultaneously...
Pyramid wavefront sensors (PWFSs) are the preferred choice for current and future extreme adaptive optics (XAO) systems. Almost all instruments use PWFS in its modulated form to mitigate limited linearity range. However, this modulation comes at cost of a reduction sensitivity, blindness petal-piston modes, limit sensor's ability operate high speeds. Therefore, there is strong interest without modulation, which can be enabled with nonlinear reconstructors. Here, we present first on-sky...
MagAO-X is the coronagraphic extreme adaptive optics system for 6.5m Magellan Clay Telescope. We report results of commissioning first phase MagAO-X. Components now available routine observations include: >2kHz high-order control loop consisting a 97 actuator woofer deformable mirror (DM), 2040 tweeter DM, and modulated pyramid wavefront sensor (WFS); classical Lyot coronagraphs with integrated low-order (LO) WFS using third 97-actuator non-common path correcting (NCPC) DM; broad band...
The success of ground-based instruments for high contrast exoplanet imaging depends on the degree to which adaptive optics (AO) systems can mitigate atmospheric turbulence. While modern AO typically suffer from millisecond time lags between wavefront measurement and control, predictive control (pWFC) is a means compensating those using previous measurements, thereby improving raw in post-coronagraphic science focal plane. A method based Empirical Orthogonal Functions (EOF) has previously...
The Keck Planet Imager and Characterizer (KPIC) is an upgrade to the II adaptive optics system enabling high contrast imaging high-resolution spectroscopic characterization of giant exoplanets in mid-infrared (2-5 microns). KPIC instrument will be developed phases. Phase I entails installation infrared pyramid wavefront sensor (PyWFS) based on a fast, low-noise SAPHIRA IR-APD array. ultra-sensitive PyWFS enable studies infant around cool, red, and/or obscured targets star forming regions. In...
The Keck Planet Imager and Characterizer comprises of a series upgrades to the II adaptive optics system instrument suite improve direct imaging high resolution spectroscopy capabilities facility instruments NIRC2 NIRSPEC, respectively. Phase I KPIC includes NIR pyramid wavefront sensor Fiber Injection Unit (FIU) feed NIRSPEC with single mode fiber, which have already been installed are currently undergoing commissioning. will enable High Dispersion Coronagraphy (HDC) directly imaged...
Almost all current and future high-contrast imaging instruments will use a Pyramid wavefront sensor (PWFS) as primary or secondary sensor. The main issue with the PWFS is its nonlinear response to large phase aberrations, especially under strong atmospheric turbulence. Most try increase linearity range by using dynamic modulation, but this leads decreased sensitivity, most prominently for low-order modes, makes it blind petal-piston modes. In push toward of fainter stars deeper contrasts,...
The MMT Adaptive Optics exoPlanet Characterization System (MAPS) is a comprehensive update to the first generation adaptive optics system (MMTAO), designed produce facility class suite of instruments whose purpose image nearby exoplanets. system's secondary mirror (ASM), although comprised in part legacy components from MMTAO ASM, represents major leap forward design, structure and function. subject this paper operation, achievements technical issues MAPS mirror. We discuss laboratory...
High-contrast imaging data analysis depends on removing residual starlight from the host star to reveal planets and disks. Most observers do this with principal components (i.e. KLIP) using modes computed science images themselves. These may not be orthogonal planet disk signals, leading over-subtraction. The wavefront sensor recorded during observation provide an independent signal which predict instrument point-spread function (PSF). MagAO-X is extreme adaptive optics (ExAO) system for...
The next generation of extreme adaptive optics (AO) must be calibrated exceptionally well to achieve the desired contrast for ground-based direct imaging exoplanet targets. Current wavefront sensing and control system responses deviate from lab calibration throughout night due non linearities in sensor (WFS) signal loss. One cause these changes is optical gain (OG) effect, which shows that difference between actual reconstructed wavefronts sensitive residual errors partially corrected...
The high contrast and spatial resolution requirements for directly imaging exoplanets requires effective coordination of wavefront control, coronagraphy, observation techniques, post-processing algorithms. However, even with this suite tools, identifying retrieving exoplanet signals embedded in resolved scattered light regions can be extremely challenging due to the increased noise from off circumstellar disk potential misinterpretation true nature detected signal. This issue pertains not...
The next generation of extreme adaptive optics (AO) must be calibrated exceptionally well to achieve the desired contrast for ground-based direct imaging exoplanet targets. Current wavefront sensing and control system responses deviate from lab calibration throughout night due non linearities in sensor (WFS) signal loss. One cause these changes is optical gain (OG) effect, which shows that difference between actual reconstructed wavefronts sensitive residual errors partially corrected...
Real-time control (RTC) is pivotal for any Adaptive Optics (AO) system, including high-contrast imaging of exoplanets and circumstellar environments. It the brain AO what wavefront sensing (WFS\&C) techniques need to work with achieve unprecedented image quality contrast, ultimately advancing our understanding exoplanetary systems in context high contrast (HCI). Developing WFS\&C algorithms first happens simulation or a lab before deployment on-sky. The transition on-sky testing often...
The large apertures of the upcoming generation Giant Segmented Mirror Telescopes will enable unprecedented angular resolutions that scale as ∝λ/D and higher sensitivities D4 for point sources corrected by adaptive optics (AO). However, all have pupil segmentation caused mechanical struts holding up secondary mirror (European Extremely Large Telescope Thirty Meter Telescope) or intrinsically, design, in Magellan (GMT). These gaps be separated more than a typical atmospheric coherence length...
Abstract MagAO-X is a recently commissioned extreme adaptive optics instrument for the Magellan Clay 6.5 m telescope at Las Campanas Observatory in Chile. had first light 2019 and subsequent commissioning observations 2022 2023. An essential step of any new calibration conversion detector coordinates to angular sky coordinates, which we accomplish with HD 165054. The background stars adjacent 165054 Baade’s Window are fortuitous configuration astrometric natural-guide-star high-contrast...
MagAO-X is the extreme coronagraphic adaptive optics (AO) instrument for 6.5-meter Magellan Clay telescope and currently undergoing a comprehensive batch of upgrades. One innovation that features deformable mirror (DM) dedicated non-common path aberration correction (NCPC) within coronagraph arm. We recently upgraded 97 actuator NCPC DM with 1000 Boston Micromachines Kilo-DM which serves to (1) correct aberrations hamper performance at small inner-working angles, (2) facilitate focal-plane...
MagAO-X is the coronagraphic extreme adaptive optics system for 6.5 m Magellan Clay Telescope. We report results of commissioning first phase MagAO-X. Components now available routine observations include: >2 kHz high-order control loop consisting a 97 actuator woofer deformable mirror (DM), 2040 tweeter DM, and modulated pyramid wavefront sensor (WFS); classical Lyot coronagraphs with integrated low-order (LO) WFS using third 97-actuator non-common path correcting (NCPC) DM; broad band...
High-contrast imaging data analysis depends on removing residual starlight from the host star to reveal planets and disks. Most observers do this with principal components (i.e. KLIP) using modes computed science images themselves. These may not be orthogonal planet disk signals, leading over-subtraction. The wavefront sensor recorded during observation provide an independent signal which predict instrument point-spread function (PSF). MagAO-X is extreme adaptive optics (ExAO) system for...
The high contrast and spatial resolution requirements for directly imaging exoplanets requires effective coordination of wavefront control, coronagraphy, observation techniques, post-processing algorithms. However, even with this suite tools, identifying retrieving exoplanet signals embedded in resolved scattered light regions can be extremely challenging due to the increased noise from off circumstellar disk potential misinterpretation true nature detected signal. This issue pertains not...
The Keck Planet Imager and Characterizer comprises of a series upgrades to the II adaptive optics system instrument suite improve direct imaging high resolution spectroscopy capabilities facility instruments NIRC2 NIRSPEC, respectively. Phase I KPIC includes NIR pyramid wavefront sensor Fiber Injection Unit (FIU) feed NIRSPEC with single mode fiber, which have already been installed are currently undergoing commissioning. will enable High Dispersion Coronagraphy (HDC) directly imaged...
The MMT Adaptive Optics exoPlanet Characterization System (MAPS) is a comprehensive update to the first generation adaptive optics system (MMTAO), designed produce facility class suite of instruments whose purpose image nearby exoplanets. system's secondary mirror (ASM), although comprised in part legacy components from MMTAO ASM, represents major leap forward engineering, structure and function. subject this paper design, operation, achievements technical issues MAPS mirror. We discuss...