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TMT First Decade Adaptive Optics

TMT First Decade Adaptive Optics. Brent Ellerbroek TMT Instrumentation @ SPIE 2010 San Diego, June 26, 2010. Presentation Outline. Motivations for AO improvements First decade instruments incorporating AO Facility AO upgrades Required technology developments. TMT.AOS.PRE.10.057.REL01.

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TMT First Decade Adaptive Optics

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  1. TMT First Decade Adaptive Optics Brent Ellerbroek TMT Instrumentation @ SPIE 2010 San Diego, June 26, 2010. TMT.AOS.PRE.10.057.REL01

  2. Presentation Outline • Motivations for AO improvements • First decade instruments incorporating AO • Facility AO upgrades • Required technology developments TMT.AOS.PRE.10.057.REL01

  3. Motivations for AO Improvements • New spectral bands • R, I, and Z bands (reduced wavefront error: NFIRAOS+) • L, M, and longer bands not transmitted by NFIRAOS (Mid IR AO -- MIRAO) • Wider fields of view • “Multiplex” observing advantage • Wide field enhanced seeing (Ground Layer AO--GLAO), or… • Moderate field multi-object AO (Multi-Object AO--MOAO) • Higher contrast ratios • Detecting and characterizing planets, other companions (“Extreme” AO--ExAO) TMT.AOS.PRE.10.057.REL01

  4. Possible First Decade Instruments Incorporating AO • IR Multi-Object Spectrograph (IRMOS) • MOAO compensation of ~20 integral field units (IFUs) • 5 arc min FoV, 50 mas sampling • ~8 LGS, one order ~60 MEMS for each IFU • 2006 feasibility studies by Caltech and UF/HIA • Pathfinder Multi-Object Spectrograph (PMOS) • A “mini IRMOS” behind NFIRAOS • Perhaps 5 IFUs plus an on-axis imager • NFIRAOS reduces MEMS stroke requirements to < 1 mm • MEMS could also sharpen tip/tilt stars for improved sky coverage • Planet Formation Instrument (PFI) • Contrast ratios in 107-108 range • Order ~128 correction; coronagraphy, advanced WFS detectors/concepts • 2006 feasibility study by LLNL/JPL TMT.AOS.PRE.10.057.REL01

  5. PFI Block Diagram (Coronagraphic) (MEMS) (Calibration) TMT.AOS.PRE.10.057.REL01

  6. IRMOS Block Diagram (UF Concept) MEMS DM NGS WFS LGS WFS TMT.AOS.PRE.10.057.REL01

  7. MOAO Behind NFIRAOS With two DMs, NFIRAOS Strehl and PSF core degrade off-axis at large zenith angles (left) Correction is theoretically much better with MEMS behind NFIRAOS (right) Would benefit both IFUs and natural guide stars Zenith Angle Distance from Center FoV TMT.AOS.PRE.10.057.REL01

  8. Potential Facility AO Upgrades • Mid IR AO facility (MIRAO) • 300-500 nm RMS WFE • Facility system for 2-3 mid IR instruments • Could be an order 30x30 system with 1 DM, 3 LGS • 2006 feasibility study (UH/NOAO) • NFIRAOS upgrade (NFIRAOS+) • ~120 nm RMS WFE for higher Strehls, shorter wavelengths • Could be an order 120x120 upgrade to existing NFIRAOS • Improvements to lasers, DMs, WFSs, and RTC • Ground layer adaptive optics (GLAO) • Enhanced seeing over a wide field of view (e.g., WFOS) • Adaptive secondary mirror required TMT.AOS.PRE.10.057.REL01

  9. MIRAO Optical Schematic Output to Instrument Light from TMT DM LGS WFSs TMT.AOS.PRE.10.057.REL01

  10. AO Component “Desirements” • Higher power lasers • Pulsed format to defeat LGS elongation • IR detectors • Large, high speed, low noise detectors (full frame readout) • Piezo DMs • Order ~120 with large stroke • MEMS DMs • Order 64 to 128 with moderate to large stroke • Adaptive secondary mirror (AM2) • Large, convex, but only ~500 modes of correction required • 2006 feasibility study (SAGEM) • RTCs • Higher throughput and/or more advanced algorithms • Advanced WFSs: Pyramid, post coronagraphic calibration,. … TMT.AOS.PRE.10.057.REL01

  11. Required AO Component Advances by Application TMT.AOS.PRE.10.057.REL01

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