PYRAMID WAVEFRONT SENSING UPDATE FOR MAGAO-X
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1 PYRAMID WAVEFRONT SENSING UPDATE FOR MAGAO-X LAUREN H SCHATZ 1, JARED MALES 2, MICHAEL HART 1, LAIRD CLOSE 2, KATIE MORZINSKI 2, OLIVIER GUYON 1,2,3,4, MADISON JEAN 1,CHRIS BOHLMAN 2, KYLE VAN GORKOM 1, ALEXANDER HEDGLEN 1, MAGGIE KAUTZ 1, JUSTIN KNIGHT 1, JOSEPH D. LONG 2, JENNIFER LUMBRES 1, KELSEY MILLER 1, ALEXANDER RODACK 1 1 College of Optical Sciences, University of Arizona. 2 Steward Observatory, University of Arizona. 3 National Astronomical Observatory of Japan, Subaru Telescope, National Institutes of Natural Sciences, Hilo, Hawaii. 4 Astrobiology Center, National Institutes of Natural Sciences, Tokyo, Japan. Center for Astronomical Adaptive Optics
2 OUTLINE MagAO-X Pyramid Wavefront Sensor Design Optical design of system Lens Results Lab Results PYRITE GMagAO-X motivation 3 PWFS vs 4 PWFS PYRITE simulator
3 Strehl Ratio MOTIVATION Image of LkCa 15b taken by Kate Follette (Sallum et al., Nature, 2015) High airmass and 11th mag GS demand high performance. Strehl Ratio c/o Kate Follette
4 MAGAO-X MagAO-X: Magellan Extreme Adaptive Optics System P.I. Dr. Jared Males, Steward Observatory First light planned: Early ,000 actuator Boston Micromachines Deformable Mirror 3.6 khz correction speed Pyramid Wavefront Sensor Coronagraph Imagers and Spectrographs Laird Close, Corwynn Sauve
5 MAGAO-X BMC 2K Tweeter DM Custom locking kinematic optical mounts Laird Close
6 MAGAO-X SDI: 2x Princeton Inst EMCCDs OCAM2K Pyramid
7 PYRAMID WAVEFRONT SENSING
8 SENSITIVITY TO PHOTON NOISE Purple: 0.5 arcsec modulation Blue: Real modulation 60mili arcsec Green: No modulation Guyon 2005
9 PYRAMID OPTICAL DESIGN Fold Mirror Pyramid Triplet OCAM2K OAP Designed and Manufactured by Arcetri Schatz et. al. in prep
10 OCAM2K OAP F/69 Pyramid Triplet Fold Beam Splitter Modulator Laird Close
11 SYSTEM DESIGN separation Expected Pixel Illumination MagAO-X bandpass same as MagAO size Schatz et. al. in prep
12 LENS DESIGN Parameter Requirement As Built Wavelength Range nm nm Pupil Size 56 pixels; mm mm Pupil Separation 60 pixels; mm mm Pupil Tolerances Δ < 1/10 th pixel; 4.8 μm Δ size =8 μm, Δ sep =-23 μm, Lens Diameter 10mm < D < 20 mm D=10.1 mm Radius Thickness Material Manufactured by Rainbow Optics Schatz et. al. in prep
13 ALIGNMENT Madison Jean Optical Science Undergrad Pyramid Triplet OCAM2K Schatz et. al. in prep
14 INITIAL RESULTS HeNe Laser Full Pupils White Light, Stopped Down Schatz et. al. in prep
15 7x 3,000 actuator deformable mirrors 3 OCAM2K detectors 240 x 240 mode 2kHz on OCAM2k Look out for Jared s Poster tonight! THE GIANT MAGELLAN TELESCOPE EXTREME ADAPTIVE OPTICS SYSTEM: GMAGAO-X
16 3PWFS VS 4PWFS Benefits of Three Sided PWFS: Easier to manufacture Less pixels = less read noise Benefits of Reflective vs Refractive: Multiple detectors Faster, less read noise 4 sided 3 sided Oli Durney Schatz et. al. in prep
17 PyramidResidualWavefront Experiment Robust Simulation Tool: Simulates atmospheric turbulence. Different Pyramid architectures. Reflective vs Refractive Manufacturing errors. Uses residual wavefront error as a metric. Schatz et. al. in prep
18 Run through a console script. Can select: Number of photons Read noise # Pixels across pupil 16, 32, 64 Schatz et. al. in prep
19 Schatz et. al. in prep Kolmogorov Turbulence Model Random phase screens generated Piston, tip/tilt removed. Plate Scale:!!" # $
20 3PWFS 4PWFS
21 3PWFS 4PWFS
22 3PWFS Input 4PWFS
23 5) RESIDUAL WAVEFRONT Actual Reconstructed Residual Wavefront Fit with Fourier Modes to analyze power spectrum
24 TRADE STUDY 3PWFS vs 4PWFS Reflective vs Refractive Pyramid Manufacturing Errors vs No Errors Read Noise Guide Star Magnitudes
25 PYRAMID WAVEFRONT SENSING UPDATE FOR MAGAO-X LAUREN H SCHATZ 1, JARED MALES 2, MICHAEL HART 1, LAIRD CLOSE 2, KATIE MORZINSKI 2, OLIVIER GUYON 1,2,3,4, MADISON JEAN 1,CHRIS BOHLMAN 2, KYLE VAN GORKOM 1, ALEXANDER HEDGLEN 1, MAGGIE KAUTZ 1, JUSTIN KNIGHT 1, JOSEPH D. LONG 2, JENNIFER LUMBRES 1, KELSEY MILLER 1, ALEXANDER RODACK 1 1 College of Optical Sciences, University of Arizona. 2 Steward Observatory, University of Arizona. 3 National Astronomical Observatory of Japan, Subaru Telescope, National Institutes of Natural Sciences, Hilo, Hawaii. 4 Astrobiology Center, National Institutes of Natural Sciences, Tokyo, Japan. Center for Astronomical Adaptive Optics
26 CANNED SLIDES
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