SciMeasure Wavefront Sensor Cameras and their Application in the 5m Palomar Adaptive Optics System SciMeasure Analytical Systems, Inc. Ray DuVarney, Charlie Bleau, Garry Motter Emory University, Department of Physics Ray DuVarney* NASA/JPL, Palomar AO Team Rich Dekany, Mitch Troy, Gary Brack * has a financial interest in SciMeasure Analytical Systems, Inc.
History
Camera System Overview Camera Control Unit Power Supply Camera Head CCD Enclosure Clocks Biases TEC Video 1.2 Ghz Bi-directional Control/data Fiber-optic Link RS-232 Control Halt Signal RS-170 Video Data Out 4 12-bit Data Ports Overflow/handshake Port (SOF/SOL/DRDY) Stopped Status FIBER COMM & DATA REALTIME DISPLAY GRAPHICS DISPLAY VIDEO OVERLAY DATA CAPTURE SEQUENCER +5V DIGITAL ±12V ANALOG +24V ANALOG CLOCK DRIVERS FIBER COMM & DATA ANALOG PROCESSOR PREAMPLIFIER CCD
Future Camera Overview I Control Unit Power Supply Camera Head CCD Enclosure Clocks Biases TEC Video 1.2 Ghz Bi-directional Control/data Fiber-optic Link RS-232 Control Halt Signal Data Out/Handshake 16-bit Data Ports SOF/SOL/DRDY Stopped Status FIBER COMM/DEMUX POWER/BIASES CONTROLLER/SEQUENCER CLOCK DRIVERS FIBER COMM/MUX ANALOG PROCESSOR(S) 12, 14 or 16-bit options PREAMPLIFIER CCD 160 mm 3U cards DATA OUTPUT
Future Camera Overview II Power Supply Camera Head CCD Enclosure Clocks Biases TEC Video RS-232 Control Halt Signal 16-bit Data Ports & SOF/SOL/DRDY Stopped Status POWER/BIASES CONTROLLER/SEQUENCER CLOCK DRIVERS ANALOG PROCESSOR(S) 12, 14 or 16-bit options PREAMPLIFIER CCD 160 mm 3U cards DATA OUTPUT
4-3 Sequencer Address Bus Data Bus ProgramsSubroutinesPatterns bit 32-bit Address Generator Addr Mux 32K Static RAM Data Mux Addr Mux 32K Static RAM Data Mux Addr Mux 32K Static RAM Data Mux Address Generator 50 MHz Clock ISA Bus Inter- face Data O/P Address Generator Ext. Select & Sync
Sequencer Programming Programs Subroutines Patterns define program 0;# 1100 Hz Nominal subroutine start_of_frame; repeat 32; subroutine read_line; end repeat; repeat 2; subroutine integrate; end repeat; end define; define subroutine read_line; pattern send_start_of_line1; pattern shift_line1; pattern wait10; pattern shift_pixel17; pattern read_pixel32; end define; define pattern read_pixel; # # t = /turbo, c = /clamp, S = sample, V = *DCAV # RG IA BS OR xxx t c S CCCC FV xx # ; # ; # ; # ; # ; # ; # ; # ; # ; # ; # ; # ; # ; # ; # ; # ; # end define;
Fiber Link CAMERA CONTROL UNIT (CCU) CAMERA HEAD UNIT (CHU) Filter Offset Gain CCD Clocks Clamp Sample Turbo Digital Video Ports Digital Data Ports External Sequencer Data 1.2 Ghz Bidirectional Control/data Fiber-optic Link MUXMUX MUXMUX DEMUXDEMUX DEMUXDEMUX ONBOARD SEQUENCER TRANS- CEIVER ONBOARD SCAN CONVERTER TEMP/VACUUM STATUS, ETC DATA TRANS- CEIVER CONTROL CLOCKS
Clock Driver Board 12 Individually Programmable Clocks ±11V Range 16V Maximum Swing 20 ns Switching Time -12V +12V TTL InVout V low V span Variable Regulator Level Shifter EL 7182
Preamplifier Board A=5 75 ohm drivers Video Outputs Temperature CCD Clocks CCD Biases TEC Power Clock Filters Bias Filters TEC Filters CCD Peltier Pack
Analog Processor Sample Offset Clamp Video Gain Filter Turbo Data 1 of 4 channels 75 ohms HIGH SPEED SHUNT TIME CONST. 1 of 4 GAIN 1 of 4 CLAMP OFFSET A/D
Data Output/Display/Capture Data R G B S RS-170 Video Data Stream Realtime Data Ports ISA Bus Data Capture Card Realtime Display Card Fiber Link Card 1 MEGAPIXEL DUAL PORT STATIC RAM ISA BUS INTERFACE RS- 422 STATIC RAM REALTIME SCAN CONVERTER INTERNAL SCAN CONVERTER DEMUXDEMUX
Control Panel
Camera Performance EEV CCD x64 pixel frame size - Read Noise calculated from Photon Transfer curve MIT/LL CCID19 achieved Mpix/sec/port and 600 frames/sec
Palomar AO System
PALAO Performance
PALAO Results
AO Loop Open FWHM = 1.2" AO Loop Closed FWHM = 0.097" (Strehl = 20%) QS Aql (HR 7486) Binary Star with 0.185" Separation
PALAO Results Trapezium Cluster in the Orion Nebula The left image was taken with the AO system off; the seeing was about 1 arcsec. With the AO system locked on Theta 1 Ori C (brightest star), the stellar images were about 0.2" across, with the brightest stars saturated. Each image is represents approximately 40 arcsec x 40 arcsec field.
Acknowledgements SBIR Phase I Grant NAS SBIR Phase II Grant NAS Jim Beletic and the ESO Optical Detector Team Mike Shao - Director, Interferometry Center of Excellence, NASA/JPL Eric Bloemhof - Mt. Palomar Observatory Horace Dale - Physics Dept, Emory University