PALM-3000 PALM-3000 Status and the 3388-actuator Xinetics Deformable Mirror A.H. Bouchez, R.G. Dekany, J.R. Angione, C. Baranec, K. Bui, R.S. Burruss, J.R. Crepp, E.E. Croner, J.L. Cromer, S.R. Guiwits, D.D.S. Hale, J.R. Henning, D. Palmer, J.E. Roberts, M. Troy, T.N. Truong, J. Zolkower 2009 CfAO Fall Retreat 11/7/2009

PALM-3000 The PALM-3000 upgrade The Palomar AO system 241 actuators, 16x16 sampling, 2 kHz max frame rate Typical perf.: 190 nm RMS WFE Instruments: –PHARO nIR imager & spectrometer –Project 1640 nIR coronagraphic IFS –SWIFT visible IFS –Visitor instruments The PALM-3000 upgrade 3388 active actuator deformable mirror Wavefront sensor with up to 63x63 pupil sampling Wavefront reconstructor computer to run at up to 2 kHz Expected performance: –95 nm RMS WFE in median conditions (r 0 =9.2 cm) –79 nm RMS WFE in 75th percentile conditions (r 0 =11.0 cm) Palomar AO & SWIFT installed on the 5.1m Hale telescope

PALM Science Drivers Galactic –Hot, young exo-Jupiter studies –Faint debris disks –Mass/luminosity of pre-main sequence binaries Require high contrast in the near-infrared Solar system –Giant planet satellite surface geology –Multiplicity of TNOs and asteroids –Surface minerology of large asteroids Require high Strehl in the visible PALM-3000 will deliver >50% Strehl in V band! 2.5” Brown et al., ApJ 639, 2006 Oppenheimer et al., AJ 679, 2008 Marois et al., Science 322, 2008

PALM P3K-GPI comparison How is PALM-3000 different from GPI? Budget: $9M, including science instrument and calibration WFS –Reusing many components of the current AO system –Planning optimization after delivery (less algorithm development, modeling) Optimized for brighter stars –Contrast of ~10 -7 at 1” around V=7 stars Wider search area –dark hole extends to 2.1” at 1.65 µm Testbed for coronagraphic techniques –APLC + IFS, [Vortex, band-limited] + imager Visible light AO capability Northern hemisphere

PALM The Project 1640 Instrument PI: Ben Oppenheimer, American Museum of Natural History Apodized Lyot coronagraph with a low-resolution ( /  =30) J-H band integral field spectrograph back-end. Post-coronagraphic calibration wavefront sensor being developed by JPL. Expected flux ratio reached at 1.0” radius from bright stars (3  in 1 hr): –PALMAO8 x –P3K5 x –P3K + JPL Cal2 x Raw spectra of a broadband calibration source Project 1640 in the lab at AMNH

PALM-3000 Optical Relay Reuses existing bench, off-axis parabolas, steering mirrors, tip/tilt mirror, science dichroics, DM (DM241). Retain current science focus position New HOWFS, high-order DM (DM3388), Acquisition Camera and Stimulus Passes 120” Ø field DM3388 located at pupil, 10.5° AOI DM241 located at +742 m conjugate, 16.0 ° AOI Requires 4 fold mirrors (meets 50% transmission requirement, incl. telescope) Acquisition camera rides on HOWFS focus stage DM3388 DM241 OAP1 TTM FM3 FM4 FM1 FM2 OAP2 SSM1 SSM2 HOWFS & ACam Science Instrument Volume

PALM-3000 Optical Relay Performance Corner of PHARO (20”, 20”) Corner of P1640 (2”, 2”) M1 aberration (2 µm P-V astigmatism)14 mas1.4 mas Atmosphere (median conditions, 2  ) 21 mas2.1 mas TT anisoplanatism20 mas2 mas Optical Performance On-axis aberrations corrected by DMs (astigmatism from dichroic, alignment errors) Field aberrations 30” off axis are ~32 nm RMS Woofer DM at non-pupil conjugate leads to focal plane distortion, on same scale as tip/tilt anisoplanatism Mechanical Tolerances <5 mas image drift over 300s in the focal plane Image shift induced by applying corrections for these errors at +742 m conjugate J band spot diagrams at science focus, using DMs to correct on-axis aberrations <5% misregistration of finest subaperture in 300s in pupil plane Requires both careful mechanical design and active, open-loop flexure compensation

PALM-3000 High-Order Deformable Mirror Manufactured by Xinetics using a new actuator structure Development funded by an SBIR grant World’s highest actuator count deformable mirror –66 x 66 = 4356 actuators on 1.8 mm pitch –We control 3388 on 112 mm  Very, very late Acceptance testing at Xinetics Inc., Aug. 2009

PALM-3000 DM Actuator Structure Prior to face sheet bonding Actuator Structure Actuators are machined from monolithic blocks of PNM 6x6 mosaic of 11x11 actuator blocks 2mm thick Zerodur facesheet Stroke ~1.4 µm without face sheet, uniform to 9% RMS.

PALM-3000 Deformable Mirror Testing All actuators are functional Influence functions are uniform With face sheet, measured stroke is µm Zygo surface map of a portion of the mirror, with every 4th actuator poked

PALM-3000 Deformable Mirror Status Unpowered surface figure: 0.03 µm RMS, 0.5 µm P-V Mirror is currently being silver coated. Expect to receive it in Pasadena in 2-3 weeks.

PALM-3000 DM Electronics and Cabling Implementation issues Driver electronics dissipate ~4 kW; mounted on telescope due to cable length constraints Cables require redesign to meet observatory operational requirements

PALM-3000 High Order Wavefront Sensor Shack-Hartmann design with selectable 8, 16, 32 or 63 samples across the pupil CCD50 detector (128x128 pixels) in SciMeasure Lil’ Joe camera Uses a tilted spherical collimator and cylindrical lens to match mircrolenses to DM3388 actuators at 10.5º AOI See Baranec, Proc. SPIE 7015, 2008.

PALM-3000 HOWFS microlens arrays Images of the microlens arrays in the assembled HOWFS arrays taken with a CMOS alignment camera.

PALM-3000 HOWFS alignment Spot patterns recorded with the CCD50 camera Preliminary alignment:

PALM-3000 HOWFS Subaperture Alignment 63  6332  3216  168  8 In the 63x63 subaperture mode, the pupil will be shifted with respect to the detector to preserve Fried geometry. In the other modes, we will use use modal control.

PALM-3000 Wavefront Processor Computer Perform full matrix multiplication reconstruction Parallelize, and use off-the-shelf Graphics Processor Units for computation House GPUs in a remote cluster of low-cost desktop PCs (in observatory computer room) Implementation VMM calculations performed on 16 Nvidia GPUs in 8 PCs –Advantages: Low cost, simple software implementation, rapid upgrade cycle PC 0 provides the interface, scheduling, and control of the cluster PC 9 is dedicated to telemetry recording (1 Tb RAID, Berkeley DB) Communication provided by a Quadrics switch (latency measured to be 19 µs) All running Real-Time Linux Publish/subscribe environment Strategy Despite reconstruction problem being 250 times larger than for present-day systems… 8192 slopes x 3631 actuators, vs. 512 slopes x 243 actuators

PALM-3000 Servo Control Architecture Flexible control system Modes: 1.Control DM3388 & TTM, offload to DM241 2.Split modes btw. DM3388 & DM241, offload to TTM 3.Fixed DM241 (good seeing only) 4.Calibration WFS input to centroid offsets & DM3388 positions

PALM-3000 Future Plans PALM-3000 Testbed Demonstrate performance of all new components before taking Palomar AO system offline – Includes all PALM-3000 components except DM241, final optics (eg. off-axis parabolas, stimulus), and steering mirror mounts – Low-cost monochromatic source and refractive optics Testbed integration this month (Nov. 2009) Goal is to demonstrate closed-loop operation at 2 kHz by April 2010 Future Milestones Project 1640 Cal WFS integrated with Palomar AO Dec PALM-3000 pre-ship review planned for June 2010 First light in February 2011

PALM-3000 The End