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Optical Telescope Performance Specifications: PILOT Pathfinder for Advancements in Astronomy

Join the JACARA Science Meeting on March 26 at the Anglo Australian Observatory to explore PILOT's data collected from various sites like the South Pole, Dome C, and Mauna Kea. Discover insights on turbulence, atmospheric parameters like seeing, and adaptive optics systems. Uncover the advancements in optical telescope technology and how PILOT is shaping the future of astronomy research.

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Optical Telescope Performance Specifications: PILOT Pathfinder for Advancements in Astronomy

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  1. PILOT:Pathfinder for an International Large OpticalTelescope-performance specifications Jon Lawrence • JACARA Science Meeting • PILOT • Friday March 26 • Anglo Australian Observatory

  2. DOME C The data South Pole • Turbulence: • SODAR (winter 2000/1) • DIMM (winter 2000/01) • microthermals (winter 1996) • Sky temperature and opacity • SUMMIT (winter 2003/4) • MIR FTI (summer 2002/3) • MISM (winter 1998) • NISM (winter 2000) • Met data • AWS • met balloons • Turbulence: • SODAR (winter 2003/4) • MASS (winter 2004) • DIMM (summer 2003/04) • Sky temperature and opacity • SUMMIT (winter 2003/4) • MIR FTI (summer 2003/4) • Met data • COBBER (winter 2003/4) • ICECAM (summer 2003/4) • AWS (winter 2004) • met balloons (summer 2000-04)

  3. Seeing Data Dome C - 2002/3 DIMM summer 2002: median seeing 1.2 arcsec (Aristidi et al, 2003) SODAR summer/ winter 2003: median seeing ~0.08 arcsec (33 % floor 0.05)

  4. Seeing Data Dome C - 2003/4 • DIMM summer 2003/4: • data not yet reduced • median seeing < 1.1 arcsec (~0.4-0.7 arcsec) • isoplanatic angle ~ 10 arcsec

  5. CN2 profile Dome C Bad iso= 9.5 arcsec fG = 30 Hz iso= 13.5 arcsec fG = 7 Hz r0= 0.05 m (1.8 arcsec seeing) r0= 0.2 m (0.5 arcsec seeing)

  6. CN2 profile Dome C Good iso= 9.5 arcsec fG = 30 Hz iso= 13.5 arcsec fG = 7 Hz iso= 30 arcsec fG = 2Hz r0= 0.05 m (1.8 arcsec seeing) r0= 0.2 m (0.5 arcsec seeing) r0= 0.7 m (0.15 arcsec seeing)

  7. CN2 profile Mauna Kea iso= 9.5 arcsec fG = 30 Hz iso= 13.5 arcsec fG = 7 Hz iso= 30 arcsec fG = 2Hz iso= 2 arcsec fG = 50 Hz r0= 0.05 m (1.8 arcsec seeing) r0= 0.2 m (0.50 arcsec seeing) r0= 0.7 m (0.15 arcsec seeing) r0= 0.20 m (0.50 arcsec seeing)

  8. Atmospheric parameters seeing (arcsec) isoplanatic angle Greenwood (arcsec) Frequency (Hz) Mauna Kea 0.50 2-3 50 Dome C 0.15 - 0.50 10-30 2-10

  9. Atmospheric parameters seeing (arcsec) isoplanatic angle Greenwood (arcsec) Frequency (Hz) Mauna Kea 0.50 2-3 50 Dome C 0.15 - 0.50 10-30 2-10 ? ?

  10. Adaptive Optics object guide star to tip-tilt secondary tip-tilt control telescope optics centroid sensor dichroic beam splitters deformable mirror image camera wavefront control wavefront sensor wavefront analysis

  11. PILOT AO systems • Tip-tilt • tip-tilt mirror + quad sensor • Low Order AO • ds=0.3 (30-50 actuators) • High Order AO • ds=0.08 (500-1000 actuators)

  12. PILOT AO system performance • Low Greenwood frequency: • lower feedback loop frequency • higher integration time • fainter stars lower SNR/bandwidth errors • Large isoplanatic angle • larger fields • brighter stars low anisoplanatic error • Better seeing (lower r0) • less actuators lower fitting error

  13. Strehl ratio - V band On-axis low order DCG DCB MK

  14. Strehl Ratio

  15. Strehl ratio - K band (tip-tilt correction) Off-axis On-axis DCG DCG DCB DCB

  16. Uncomp DCB Uncomp DCG Diff lim 2m

  17. Uncomp DCB Uncomp DCG DCB off-axis DCG off-axis on-axis Diff lim 2m

  18. Uncomp DCB Uncomp MK Uncomp DCG DCB off-axis DCG off-axis Gemini altair Diff lim 8 m on-axis Diff lim 2m

  19. Sky emission MK Emission = 5% @ 0° C

  20. Sky emission SP Emission = 5% @ -63° C

  21. Sky emission DC Emission = 5% @ -66° C

  22. Sky Transmission - NIR/MIR MK

  23. Sky Transmission - NIR/MIR DC

  24. Relative integration time : MK versus SP, DC, DA

  25. Relative integration time : 8m MK versus 2 m DC PILOT diffraction limit

  26. Relative integration time : 8m MK versus 2 m DC PILOT Seeing limit - extended object

  27. Relative integration time : 8m MK versus 2 m DC PILOT Seeing limit - extended object

  28. Possible PILOT Instruments Visible (AO-on) imaging:  4k array (0.03 arcsec/pixel) = 2.3 arcmin FOV NIR wide field imaging JHK bands:  4k array (0.6 arcsec/pixel) = 10 arcmin FOV DF imaging KLM bands:  1k array (0.23 arcsec/pixel) = 4 arcmin FOV MIR imaging N band:  0.5k array (0.7 arcsec/pixel) = 6 arcmin FOV

  29. V band imaging - AO on Point source ext object

  30. Point source K band imaging - tip tilt ext object

  31. Point source N band imaging ext object

  32. Summary • Visible AO system (40-100 actuators plus tip-tilt): • near diff lim for on-axis stars 8-12 mag • off-axis reasonable performance up to 1-2 arcmin • highest ground based resolution!! • mirror figure error is very important < 50 nm rms required • spectroscopy? • Near Infrared K band imaging: • tip-tilt correction is enough for near diff lim (0.2-0.3 arcsec) • equivalent to 8m ML telescope for extended object, 5m for point source • wide field or narrow field science? • Mid-Infrared imaging: • niche is wide field sensitivity

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