Laboratory Facility
  • 1900 sq ft in the in the Thimann Laboratories Building in two separate rooms
  • Lab area clean to class 10,000 standards
  • Class 100 cleanroom area
  • Temperature control
  • Light control
images/Photos/LAO_Aug04.jpg
Optical Tables
  • 18 x 4 ft granite optical table (ExAO testbed)
  • 6 x 6 ft granite optical table (cleanroom/assembly/test area)
  • 2 16 x 4 ft Newport optical tables (MCAO testbed, wavefront sensing and control experiments, interferometers)
Interferometers
  • Phase-shifting Diffraction Interferometer (PSDI) - ~0.2 nm rms absolute wavefront accuracy over a 10-20 mm area - ExAO prototype evaluation and calibration
  • Zygo Fizeau Interferometer - 4 inch aperture with 6 x zoom, 1000x1000 resolution, 4" window and flat with lambda/20 certification - general purpose optical testing
  • Veeco White-Light Interferometer - - for testing MEMS devices
  • Quadrature Polarization Interferometer (QPI) - high speed (30 Hz) phase determination on 20 mm square aperture in a Mach-Zehnder configuration - used for testing transmissive optics single-pass and the temporal response of spatial light modulators
images/Photos/QPI_small.GIF
Deformable Mirrors
  • 1020 actuator (32 x 32) continuous face sheet MEMS-technology, high order deformable mirror, manufactured by Boston Micromachines.
  • 2 52-actuator magnetic-actuated membrane, low-order high stroke, deformable mirror manufactured by Alpao.
  • 4 768 x 768 pixel liquid crystal spatial light modulators from Hamamatsu - surrogate very high order DMs for simulating TMT and other Extremely Large Telescope AO systems.
  • Some number of 37-element segmented MEMS devices manufactured by Iris AO - for AO demonstration and laser beam wavefront correction and Laser Guidestar Uplink AO.
  • 1 36 element membrane DM manufactured by Aperture Optical Systems - for AO education, demonstration, and controls research
images/Photos/AODemo_small.GIF
Detectors
  • 3 1024 x 1024 Dalsa 1M30 cameras - wavefront sensors for the MCAO testbed (up to 4 guidestars per camera)
  • 2 additional 1024 x 1024 Dalsa 1M30 cameras - wavefront sensing in the ExAO prototype
  • 1K x 1K Science Grade CCD from Princeton Instruments with E2V CCD47-10 chip - for far-field high-contrast measurements on the ExAO testbed
  • 2 Sci-Measure "Little-Joe" cameras with 80x80 Lincoln Labs CCD39 chip. One will be incorporated as the tip/tilt sensor on ShaneAO.
  • 1 Sci-Measure "Big-Joe" camera with 160x160 Lincoln Labs CCD66 chip - to be incorporated as the wavefront sensor on ShaneAO.

Wavefront Aberration Plates
  • Etched glass 150 x 150 mm area with Kolmogorov spectrum, 40 micron features (4K x 4K), 8 bit resolution, 25 micron peak optical path difference - for testing ExAO or MCAO systems with simulated atmospheric turbulence - we only have 2 of these now but plan to replicate them at various peak optical path specification for use as simulated atmospheric layers.
  • Acrylic spray on optical plastic. These are round 4 to 6 inch plates with a random pattern of aberrations roughly following a Kolmogorov power law.
images/Photos/PhasePlate_small.GIF
Lasers
  • A 2-watt 532 nm short coherence laser for use in the PSDI interferometer.
  • A 10 watt 589 nm Sodium Guidestar laser. Based on fiber-amplifier technology, this laser is adjustable in spectral and pulse format to enable optimal coupling to the sodium atoms. This is now in the LAO cleanroom in preparation for being installed at the Shane telescope in conjunction with the new Shane telescope adaptive optics system, ShaneAO. This laser was developed by a team at Lawrence Livermore National Laboratory under an R&D grant from the CfAO.

Computing
  • Lab-GPU An 8-CPU (Intel i7), running 64bit Linux, and equiped with an NVIDIA Quatro M4000 GPU - for developing real-time MCAO tomography, wavefront control, and running faster than real time simulations of the atmosphere and AO system. A second similar machine runs the AO testbed systems.
  • Lightwave A 24-processor compute server running Linux with IDL, Mathematica, Python, etc. - For running compute intensive AO-project related calculations such as Fresnel wave-propagation and laser guidestar sodium response physics.


Donald Gavel, Director, Laboratory for Adaptive Optics
gavel@ucolick.org