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Advanced Camera Interfaces and Control Systems for ATST

This presentation outlines the Instrument Control System Interfaces and Scripts for ATST Cameras, focusing on standardization through the ATST Control Software Framework (CSF). It highlights the common software architecture that enhances development efficiency and reduces maintenance for instrument builders. Key functionalities include burst mode, frame selection, continuous monitoring, and intelligent focus alignment. The presentation covers various camera sensor requirements and operational parameters, ensuring optimal performance for solar observations.

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Advanced Camera Interfaces and Control Systems for ATST

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  1. ATST Cameras(presentation for HAO only)David Elmore

  2. Instrument Control System Interfaces Scripts OCS 4.2 Users ICD 3.1-4-4.2 DHS 4.3 ICS 3.1.4 TCS 4.4 ICD 3.1.4-3.2 ICD 3.1.4-3.3 ICD 3.1.4-3.4 ICD 3.1.4-3.5 ICD 3.1.2-3.1.4 ICD 3.1.1-4.4 BDT 4.3.1 VBI 3.2 ViSP 3.3 NIRSP 3.4 VTF 3.5 Synchrobus 3.1.2 GOS 3.1.1 ICD 3.2-3.6 ICD 3.3-3.6 ICD 3.4-3.6 ICD 3.5-3.6 ICD 3.1.1-3.1.2 Cameras 3.6 ICD 3.6-4.3 ICD 3.1.2-3.6 Synchrobus Data LAN

  3. Facility • Cameras are an ATST Facility • Interfaces to instruments, modulators, and data transport is standardized via ATST CSF • Common camera software minimizes development time and maintenance • Special cases are minimized • Instrument builders can share camera control software

  4. Virtual • Images • Accumulated modulation states: N frames into M states • Bursts: Collect N frames at a rate faster than BDT can accept – then spool them out • Frame selection: Record frames at a high rate, select only the ‘best’ on the fly and send them to BDT • Monitor: Send frames to BDT at a rate that can be continuously displayed by DHS

  5. Services • Focus: Virtual cameras compute contrast values of identified features and continuously send values back to the controlling instrument to servo focus • Alignment: Virtual cameras compute the pixel coordinates of identified features and continuously send coordinates back to the controlling instrument to servo camera rotation and translation

  6. Synchronization • Virtual cameras contain absolute time board and wave form generator • Controlling experiment sends synchronization information to cameras • modulator start time, modulation rate, and phase at t=0 • time to start accumulations • trigger details such as sign and duty cycle (exposure time) • VCs then produce images according to settings

  7. Sensor requirements • Size • ViSP: 4k X 4k to sample 2’ at 2x diffraction limit at 600nm and handle multiple slits • VBI: 8k X 8k for 2’ diffraction limit at 600nm, 12k x 12k for diffraction limit at 400nm • ISRD indicates a willingness to compromise instantaneous field of view for other camera parameters and ability to raster • VTF: 4k X 4k for 1’ diffraction limit at 550nm • NIRSP: 2k X 2k for 2’ at 2x diffraction limit at 1.2 microns

  8. Sensor requirements • Full well and read noise • 100,000e- full well and <50e- read noise: Gives >40:1 dynamic range over the image

  9. Seeing-induced cross talk I,Q,U,V vary by 100% in 1/8 arc second Solar feature model DST excellent seeing with tip-tilt correction Atmosphere ATST M1 & M2 polarization, Al coated mirrors Telescope polarization Rotating 0.375 wave retarder Polarization modulation Conclusions for ViSP: -100Hz required for dual beam analysis -Many kHz required for single beam Time varying polarization from Gregorian focus to ViSP Relay optics polarization Single or Dual Beam Polarization analyzer 100Hz to 1600Hz Detector

  10. Image Reconstruction • The SWG decided upon speckle reconstruction over Multi-Object Multi-Frame Blind Deconvolution (MOMFBD) or Phase diversity (PD) • Approximately 100 short frames are required that freeze seeing but sample different seeing realizations • solar features change on a time scale of 3 seconds (at VBI resolution) • Conclusion • ~10msec exposures • 30 frames/second for ~3 seconds

  11. Sensor requirements • Frame Rate • 100 frames/second for high polarimetric accuracy (ViSP) • 30 frames/second for imagers using image reconstruction (VBI, VTF, context cameras)

  12. Sensor goals • Many kHz charge-caching • Operationally allows for optimizing polarimetry at multiple instruments • Quantum efficiency > 0.75 over spectral range • Effectively increases the size of the telescope • Snapshot mode readout • Improves ability to perform image reconstruction

  13. Sensor goals • Exposure ‘gate’ • Operationally optimizes exposure times among multiple instruments • Butt-able • VBI can meet field of view requirements without rasterization

  14. Two Pronged Approach • FDR: Meet requirements • Field of view can be sequentially sampled and visible wavelength sensor technology is rapidly evolving, therefore select the best available visible wavelength detectors at the required time of purchase • currently 2352 X 1728 @ 60Hz frame rate • or 2352 X 1000 at 100Hz frame rate • Purchase currently available cameras for NIR • 2k X 2k, 76 frames/sec

  15. Two Pronged Approach • Outside of ATST • Pursue development funding for state of the art cameras meeting goals • 4k X 4k • 100Hz • snapshot mode • butt-able • gated • high QE • Include charge caching design in the development program (2k X 2k)

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