curvature wavefront sensor arbitrary waveform generator
DESCRIPTION
Curvature Wavefront Sensor Arbitrary Waveform Generator. Kenyan Kawauchi Subaru Telescope (NAOJ) Mentor: Stephen Colley. Subaru Adaptive Optics. Without AO. With AO. Earth’s atmosphere distorts light. Removes effects of atmospheric distortion. Telescope images blurred. - PowerPoint PPT PresentationTRANSCRIPT
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Curvature Wavefront Sensor Curvature Wavefront Sensor Arbitrary Waveform GeneratorArbitrary Waveform Generator
Kenyan KawauchiKenyan Kawauchi
Subaru Telescope (NAOJ)Subaru Telescope (NAOJ)
Mentor: Stephen ColleyMentor: Stephen Colley
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Subaru Adaptive OpticsSubaru Adaptive Optics
Earth’s atmospheredistorts light
Telescopeimages blurred
Removes effectsof atmospheric
distortion
Image resolutionimproved
Without AO With AO
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AO System ComponentsAO System Components
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Wavefront SensorWavefront Sensor
Visible light reflectsoff one sideof membrane
Measure lightintensity
APDs count photonsin each lenslet
Calculate wavefrontphase shift
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What vibrates membrane?What vibrates membrane?
Other side of membrane
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ProblemProblem
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SolutionSolution
• Design your own AWG!
• Use DAC40 board
• Field Programmable Gate Array (FPGA)
• Digital-to-Analog Converters (DACs)
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AWG SpecificationAWG Specification Range of period – 100 Hz to 4 kHzRange of period – 100 Hz to 4 kHz Number of points – 1000Number of points – 1000 Voltage resolution – 14 bits (DAC40 DACs) Voltage resolution – 14 bits (DAC40 DACs) Update rate for new waveforms – 0.1 seconds Update rate for new waveforms – 0.1 seconds
(10 Hz)(10 Hz)
Voltage Amplitude
Time
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Logic Block DiagramLogic Block Diagram
AWG
Timing Memory
A B
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Implement using Quartus IIImplement using Quartus II
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Design FlowDesign FlowDesign Entry
(VHDL)Compilation Simulation
ProgramDevice
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Simulate DesignSimulate DesignDesign Entry
(VHDL)Compilation Simulation
ProgramDevice
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ConclusionConclusion
Dual-stroke waveform conceptDual-stroke waveform conceptEfficient – Only 1 wavefront sensorEfficient – Only 1 wavefront sensorAstronomical objects appear 2.5X brighterAstronomical objects appear 2.5X brighter
In the FutureIn the Future- Interface DAC40 to oscilloscopeInterface DAC40 to oscilloscope- Test AWGTest AWG- Implement in next generation AO systemImplement in next generation AO system
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AcknowledgementsAcknowledgements
Stephen ColleyStephen ColleyOlivier Guyon – Subaru AstronomerOlivier Guyon – Subaru AstronomerHideki Takami – AO Project ManagerHideki Takami – AO Project ManagerSubaru Telescope (NAOJ)Subaru Telescope (NAOJ)Center for Adaptive OpticsCenter for Adaptive Optics Funding provided through the Center for Adaptive Funding provided through the Center for Adaptive
Optics, a National Science Foundation Science and Optics, a National Science Foundation Science and Technology Center (STC), AST-987683Technology Center (STC), AST-987683