Gemini AO Program The Gemini Adaptive Optics Program MCAO for Gemini-South Gemini Adaptive Optics Team B. Ellerbroek and F.Rigaut October 21, 1999 Gemini Science Committee 1 Gemini AO Program Top Level Perf. Requirement #2 “ Image quality of better than 0.1 arcsec with AO: Achievement of outstanding image quality will have the highest scientific priority for the project […]” • The proposed evolution of the program at CP will enable unique NGST-class science 4 years ahead of NGST launch. It will keep Gemini competitive during the NGST era. October 21, 1999 Gemini Science Committee 2 Gemini AO Program AO and Science AO is a rather new domain... – First AO instrument for astro. -> Come-on, ESO 1990 – UH curvature system, Mauna Kea 1992 – 1994-1998: Exponential progression of # of systems …but science is already flowing: – Number of Astro paper is growing exponentially – Total of 70+ refereed papers (lost count). Highlights: Discovery of an asteroid satellite, wrap of Pic disk, Surface and orbital parameters of solar system bodies, YSO disks and outflows (e.g. HL and GG Tau), Stellar motions in GC, Stellar multiplicity surveys, Structure in AGNs, Galaxy dynamic (e.g. CFHT AOSIS), etc... October 21, 1999 Gemini Science Committee 3 Gemini AO Program A short history of astronomical AO • 1989: First AO images w/ Come-On (OHP & ESO) 110mas • 1992: First Curvature system (UH) 70mas • 1996: First Facility system (CFHT AOB) October 21, 1999 Gemini Science Committee 4 Gemini AO Program CFHT Pueo 1996 Galactic Center 2.2 m FWHM 130 mas October 21, 1999 Gemini Science Committee 5 Gemini AO Program A short history of astronomical AO • 1989: First AO images w/ Come-On (OHP & ESO) 110mas • 1992: First Curvature system (UH) 70mas • 1996: First Facility system (CFHT AOB) • • • • 1996: First compensation in the visible (Mt Wilson) 58mas 1996: First LGS systems 1998: LGS systems getting closing expectations 1999: First h.order system on a large telescope (Keck) 40mas October 21, 1999 Gemini Science Committee 6 Gemini AO Program Keck AO System 1999 Vesta 1.5 m FWHM <40 mas October 21, 1999 1’’ Gemini Science Committee 7 Gemini AO Program Gemini’s Dedication Courtesy C.Roddier, UH-IfA October 21, 1999 Gemini Science Committee 8 Gemini AO Program ALFA AO Results (18 Modes, 0.9-1.0’’ seeing, K band) Open loop Loop closed with LGS AO • 4 W dye laser NGS AO • 0.23 Strehl • 0.42 Strehl • FWHM diffraction limited. • 0.53 predicted October 21, 1999 Gemini Science Committee 9 Gemini AO Program Where is AO standing ? • AO technology for astronomy is maturing rapidly – Well designed and calibrated NGS AO systems (CFHT Pueo, Hokupa’a, MIT/Lincoln Laboratory, SOR) now closely approach their performance predictions. – Rayleigh beacon LGS AO programs (MIT/LL, SOR) have been technically successful – Astronomical sodium beacon LGS AO systems have progressed from Strehls of 0.03 to 0.30 in two years – Sodium layer variability has been well characterized by numerous LIDAR campaigns October 21, 1999 Gemini Science Committee 10 Gemini AO Program Proposed Baseline AO Program NORTH 1999 Altair 10W LGS Hokupa’a SOUTH CP AOS/LGS CP Hokupa’a 2000 36 Keck 2001 2002 2003 2004 85 Subaru VLT VLT-LGS 85 2W LGS October 21, 1999 Gemini Science Committee 11 Gemini AO Program Baseline Program: Altair NORTH 1999 2000 2001 2002 2003 2004 Altair 10W LGS well (CDR 02/99) •Progresses 36 for Altair 85 LGS upgrade nearly ready Hokupa’a •Statement of work SOUTH CP AOS/LGS CP Hokupa’a Keck Subaru VLT VLT-LGS 85 2W LGS October 21, 1999 Gemini Science Committee 12 Gemini AO Program Baseline Program: 10W LGS NORTH 1999 2000 2001 2002 2003 2004 10W LGS 10W •10 W LGS Laser RFP to go out early October 36 vary from857 to 23W depending on laser pulse Hokupa’a •Power requirements format Keck Subaru •Design of the LLT and BTO underway SOUTH CP AOS/LGS CP Hokupa’a VLT VLT-LGS 85 2W LGS October 21, 1999 Gemini Science Committee 13 Gemini AO Program Baseline Program: MK-Hokupa’a NORTH 1999 Hokupa’a 2000 36 2001 2002 2003 2004 85 •Hokupa’a-36 10W LGS installed on the telescope early June this year •Images fully compatible with85 expectations (seeing ok but not 36 Hokupa’a exceptional), near diffraction limit in K band w/ Strehl ~ 15-30%. Keck Subaru Great tool for telescope engineering SOUTH •85 Actuators upgrade to be done next year team on VLT by UH VLT-LGS internal funds. Small transferred field (30’’) CPUH/NSF AOS/LGS Performance w/ NGS (AO only) (285 fold vs 36 actuators): CP Hokupa’a Seeing Strehl(J) Strehl(K) 2W LGS 0.45’’ 50% 80% 0.65’’ 25% 62% October 21, 1999 Gemini Science Committee 14 Gemini AO Program Cerro Pachon-AOS/LGS Forum April 1999, Review Panel Recommendations 1 2 3 4 5 The IGPO should develop a strategy for its overall adaptive optics program which satisfies the Gemini community. Timing of the program, staff resources, and cost must be addressed. The RP also notes that the experience gained with the Altair AO and Hokupa'a teams are valuable to the overall program and should be folded into the planning. The Project should conduct a significant but time-limited study of a multiconjugate adaptive optics system for Cerro Pachon. This would provide an exciting advancement in capabilities but implementing the system should be conditional on "filling" the AO gap on Gemini-South and addressing the requirements of the coronagraphic imager. The study should address the theoretical analysis, science drivers, technical challenges, systems engineering, and programmatics of such an AO system. With the development of a plan, the RP recommends that Gemini adopt as aggressive a schedule as possible to bring this capability to the community. The IGPO should lead the conceptual design program of the Gemini-South AO system, including defining the allocation of subsystems across the Gemini Community In light of the proposals presented for turn-key laser systems, the RP recommends that the IGPO explore with LiteCycles the manufacture of a Sum Frequency laser. To reduce cost and risk for the laser, procurement through a consortium should be explored, including Keck, and possibly other groups if they can participate on timescales which are consistent with Gemini's schedule for laser deployment. The project should avoid relying on major technological developments such as MEMs, liquid crystals, and other 'advanced' DMs for the CP AOS October 21, 1999 Gemini Science Committee 15 Gemini AO Program Baseline Program: CP-Hokupa’a SOUTH 1999 CP Hokupa’a 2000 2001 2002 2003 2004 85 2W LGS 36 MK upgrade 85 of Hokupa’a to 85 actuators. UH AO Hokupa’a • AO: Duplicate of the Team. Proposal submitted NSF 08/99. Optomechanical upgrades Keck to Subaru (FoV 60’’) + LGS compatible SOUTH Performance w/ NGS (AO only): VLT VLT-LGS Strehl(K) CP Seeing AOS/LGSStrehl(J) 80% 85 CP 0.45’’ Hokupa’a 50% 0.65’’ 25% 62% 2W LGS • LGS: Off-the-shelf 2W CW laser. Coherent/Spectra physics CW 10W pump laser + ring dye laser (demonstrated in lab) • IR Imager: ABU October 21, 1999 Gemini Science Committee 16 Gemini AO Program Baseline Program: CP-Hokupa’a SOUTH 1999 2000 2001 CP Hokupa’a 2002 2003 2004 85 2W LGS Hokupa’a Rationale: 36 85 • Gives us a 2+ yearKeck window Subaru of unchallenged AO+LGS capability in the SOUTH southern hemisphere (comp. NAOS) w/ Adequate JHK performance. VLT VLT-LGS • Build expertise on LGS by stepping up gradually (Laser Launch CP AOS/LGS Telescope + Beam Transfer Optics) 85 CP Hokupa’a • Getting AO on CP as soon as possible relieves pressure, allowing us to avoid LGS the rush and do a better job on the final CP system 2W October 21, 1999 Gemini Science Committee 17 Gemini AO Program Baseline Program: Facility CP AOS SOUTH 1999 2000 2001 2002 2003 2004 CP AOS/LGS 10W LGS Context: 36 85 Hokupa’a • Simplest case = duplicate Altair -> No AO facility until late 2002. KeckhaveSubaru • Other observatories very capable AOSs in the north (Keck 1999) SOUTH and in the south (VLT-NAOS 2001) -> Competitiveness issue VLT VLT-LGS Rationale: (Why?) CP AOS/LGS • Provide the Gemini community with NGST-like capabilities (spatial res. 85 CP Hokupa’a and field), matching the Gemini science goals and instrumentation 2W LGS • Sets up Gemini to be a lead ground-based facility in the NGST era with matching resolution and similar field of view • Future ELTs require “wide” field of view AO October 21, 1999 Gemini Science Committee 18 Gemini AO Program Baseline Program: Facility CP AOS SOUTH 1999 2000 2001 2002 2003 2004 CP AOS/LGS 10W LGS(What?) Proposal: 36 85 • Build a high performance, 2 arcminutes field of view AOS with Hokupa’a homogeneous PSF Keck quality over the entire field of view, with very high Subaru sky coverage SOUTH VLT VLT-LGS How ? CP AOS/LGS • Using Multi-Conjugate AO, i.e. 4-5 LGSs and wavefront sensors to 85 measure the turbulence in 3D and 2-3 deformable mirrors to correct it CP Hokupa’a • ThisLGS uses currently available technology. NO hardware development 2W required other than lasers (same as MK-LGS) October 21, 1999 Gemini Science Committee 19 Gemini AO Program What is Tomography ? 90 km 1. Cone effect October 21, 1999 Gemini Science Committee 20 Gemini AO Program What is tomography ? 90 km 2. Multiple guide star and tomography October 21, 1999 Gemini Science Committee 21 Gemini AO Program What is multiconjugate? October 21, 1999 Gemini Science Committee 22 Gemini AO Program What is multiconjugate? October 21, 1999 Gemini Science Committee 23 Gemini AO Program What is multiconjugate? Turb. Layers #1 Telescope #2 WFS DM1 DM2 Atmosphere UP October 21, 1999 Gemini Science Committee 24 Gemini AO Program Baseline Program: Facility CP AOS SOUTH 1999 2000 2001 2002 2003 2004 CP AOS/LGS 10W What LGS does MCAO do that another system wouldn’t ? 36 increased85(50-500x) w/ respect to a NGS system Hokupa’a • Sky coverage (50%) • Increased performance axis w/ respect to a LGS system because Keck on Subaru the cone effect is taken care of SOUTH • Increased field of view (well matched toVLT IRMOS)VLT-LGS CP AOS/LGS • Uniform PSF across the FoV -> Easier and more accurate Data Reduc. 85 CP Hokupa’a 2W LGS October 21, 1999 Gemini Science Committee 25 Gemini AO Program MCAO Performance Summary Early NGS results, MK Profile No AO 320 stars / K band / 0.7’’ seeing October 21, 1999 Classical AO MCAO 1 DM / 1 NGS 2 DMs / 5 NGS 165’’ Gemini Science Committee Stars magnified for clarity 26 Gemini AO Program MCAO Performance Summary Early NGS results, MK Profile MCAO Classical AO Guide star location October 21, 1999 Gemini Science Committee 27 Gemini AO Program Baseline Program: Facility CP AOS 1999 SOUTH 2000 2001 2002 2003 2004 CP AOS/LGS 10W LGS Performance Hokupa’a Mode NGS SOUTH LGS MCAO CP AOS/LGS 36 %Sky3 Keck 1% 17% 34% 85 SR J(0’’) SRJ(48’’) Subaru 0.55 0.04 0.47 0.04 VLT 0.54 0.35 CP Hokupa’a 1 50% Strehl ratio attenuation FOV Hardware 30’’ 1 1DM 1 32’’ VLT-LGS 1DM/1LGS 2’ 2 3DM/5LGS 85 limited by the AO-Fold aperture 2W LGS 3 2 Sky coverage at galactic pole October 21, 1999 Gemini Science Committee 28 Gemini AO Program Baseline Program: Facility CP AOS SOUTH 1999 2000 2001 2002 2003 2004 CP AOS/LGS 10W LGS Where are we? 36 85 Hokupa’a • Feasibility study progressing, including: Subaru •First pass on Keck the science drivers SOUTH •Theoretical analysis of MCAO control/numerical VLT VLT-LGS simulations/Performance assessment CP AOS/LGS •A proof-of-concept optical and mechanical layout 85 CP Hokupa’a •Assessment of the need in computing issues 2W •Management LGS plan including schedule and resource needs October 21, 1999 Gemini Science Committee 29 Gemini AO Program MCAO for Gemini-South Performance, Feasibility, and Schedule • • • A multi-conjugate AO system for Gemini-south can theoretically provide highly uniform turbulence compensation over a 1-2’ diameter field-of-view System can be implemented with largely existing hardware and technology – Fully acceptable deformable mirrors, tip/tilt mirrors, and wave front reconstructs have been demonstrated – Most recent high-speed 1282 CD's meet wave front sensor requirements with margin – Significant improvements still required in sodium laser power and reliability • Comparable with conventional LGS AO on a per beacon basis Estimated schedule for science handover is spring 2004 October 21, 1999 Gemini Science Committee 30 Gemini AO Program NGS, LGS, and Multi-conjugate AO Performance Characteristics NGS AO LGS AO MCAO Sky coverage Poor (0.1-2%) Good (~17% at galactic pole, SR=0.6 in H) Further improved (~34% at galactic pole) Compensated field-of-view 20-40” (Nonuniform) 20-40” (Nonuniform) 1-2’ (Nearly uniform) Fundamental limits • Guide star brightness • Common anisoplanatism •T/T guide star brightness (relaxed) • Tilt anisoplanatism • Cone effect •T/T guide star brightness (relaxed) • TBD (new inverse problem) • Sky coverage and field-of-view are for J, H, K bands with 0.5 arc second seeing October 21, 1999 Gemini Science Committee 32 Gemini AO Program Analysis and Simulation Models • • • Two approaches available for more detailed modeling of MCAO – Upgraded simulation – Statistical analysis based opon turbulence statistics, MCAO system parameters Both approaches treat laser- and natural guide stars, WFS/DM geometries, CP turbulence profiles – Analysis derives “optimal” wave front reconstructors – Simulation more efficient for standard least-squares approach Both approaches extendable to model WFS noise, servo lag, telescope/instrument aberrations – Simulation can potentially model wave optics effects in wave front sensors and the atmosphere October 21, 1999 Gemini Science Committee 33 Gemini AO Program MCAO Parameters for Gemini-CP • 4 or 5 laser guide stars – 30 to 60” (48”) offset from optical axis – 10 to 20 Watts CW equivalent power, 1.5 XDL • 4 or 5 LGS wave front sensors – 12 by 12 or 16 by 16 subapertures – 80 by 80 to 128 by 128 pixels – 5 to 10 read noise electrons, 500 to 1000 Hz sampling • 2 or 3 deformable mirrors – 13 or 17 actuators across beamprint – Conjugate ranges of 0, 4-4.5, 8-9 km • 3-4 T/T or T/T/F natural guide stars, 1 T/T mirror (Parameters Used for Following Sample Results) (Parameters not Yet Modeled) October 21, 1999 Gemini Science Committee 34 Gemini AO Program Sample Numerical Results 0 degree zenith • 50% seeing • 12 by 12 NGS (black) • 12 by 12 MCAO (red) • 16 by 16 MCAO (blue) • I, J, H, and K bands • K H J I October 21, 1999 Gemini Science Committee 35 Gemini AO Program Sample Numerical Results Variation with Seeing and Zenith Angle 0 Degree Zenith 45 Degree Zenith 12 by 12 NGS (black), 12 by 12 MCAO (red), and 16 by 16 MCAO (blue) • I, J, H, and K spectral bands • October 21, 1999 Gemini Science Committee 36 Gemini AO Program Sample Results Slit Coupling Efficiency at 0 Degrees Zenith •16 by 16 MCAO, I, J, H, and K spectral bands • Horizontal and vertical 0.1 arc second slits October 21, 1999 Gemini Science Committee 37 Gemini AO Program Why Multiple Tip/Tilt NGS’s? – Consider a turbulence profile with a focus aberrations at two ranges (blue) – LGS measurements (yellow) cannot determine range of the aberration • Tip/tilt information lost • Equal focus measurement from each LGS, regardless of aberration range – Tip/tilt NGS measurements can determine range from the differential tilt between stars – Three tip/tilt NGS’s needed for all three quadratic modes – Alternate approaches: Rayleigh LGS’s, or a solution to the LGS tilt indeterminacy problem October 21, 1999 Gemini Science Committee f(r)=a(cr+d)2 =ac2r2+2acdr+ad2 ~ ac2r2 After tilt removal f(r)=ar2 38 Gemini AO Program MCAO Sky Coverage with Multiple Tip/Tilt NGS • Quantitative sky coverage calculations more complex than for conventional AO, but some initial estimates are possible – Only one NGS need be sufficiently bright for correction of high-bandwidth, wind-shake induced tip/tilt jitter – The atmospheric modes corrected by remaining reference stars are lower frequency, allowing lower control bandwidths and dimmer stars (e.g. 30Hz sampling rate) – Preliminary calculation for the galactic pole: • LGS AO sky coverage for 60% Strehl in H: 17% • MCAO coverage with 1 m=18 star and 2 m=20 stars within 1’ radius: 34% October 21, 1999 Gemini Science Committee 39 Gemini AO Program MCAO Implementation- Feasibility study conclusions: • Optics and optics bench – Mass, volume similar to Altair • Wave front sensor camera – Goal of a single camera for all laser guide stars – 80 by 80 to 128 by 128 pixels, 5 to 10 read noise electrons • Deformable mirrors and tip/tilt mirror – Number of actuators, other parameters demonstrated • Wave front reconstruction electronics – Frame rate, number of inputs/outputs demonstrated • Tip/tilt sensors, laser transfer optics and launch telescope – Appear straightforward, feasibility designs in progress – 2-3 T/T sensors + 1 more provided by OIWFS • Laser(s): Technology and engineering development required October 21, 1999 Gemini Science Committee 40 Gemini AO Program MCAO Science Optical Path •3 DM’s at R=0, 4, and 8 km •13 actuators across beamprint •4 folds, 2 off-axis parabolas, 1 dichroic beamsplitter (not shown) - Near-minimum number of surfaces for facility MCAO • f/30 output focus October 21, 1999 Gemini Science Committee 41 Gemini AO Program MCAO LGS Optical Path • Outgoing: Single launch telescope for all guide stars • Return: One WFS camera for all guide stars ZEMAX optical schematic October 21, 1999 4 LGS’s sensed with 1 WFS CCD Gemini Science Committee 42 Gemini AO Program WFS Camera Options Pixels Requirement EEV CCD MIT/LL CCD 80 by 80 to 128 by 128 80 by 80 128 by 128 Read noise electrons 5-10 5 6-10 Frame rate, Hz Comments 5001000 1000 1-2 Cameras for 4-5 LGS, 12 by 12 SA 1000+ Supports 5 LGS, 16 by 16 SA • MIT/LL read noise level is new information since feasibility study October 21, 1999 Gemini Science Committee 43 Gemini AO Program Approach to Multiple Tip/Tilt NGS WFS’s 200mm To APDs Focal plane XX stage stage Y stage • Fiber-fed APD quadrant detectors •2 or 3 T/T WFS’s in AO instrument package • One additional T/T/F WFS in each facility instrument, for a total of 3-4 sensors October 21, 1999 Gemini Science Committee 44 Gemini AO Program Laser Issues • Power requirement: – Equivalent to conventional LGS AO on a per beacon basis – 20-40 Watts per LGS, 80-200 Watts total for short pulse, flashlamp+Nd:YAG-pumped dye lasers (LLNL) • ~20 Watts demonstrated • Scaling a cost/engineering issue (electrical power, heat dissipation, flammable dye) – 7-12 Watts per LGS, 28-60 Watts total for diode-pumped, Nd:YAG sum frequency lasers (MIT/LL and others) • ~5 Watts demonstrated • Scaling a technical issue (Nd:YAG beam quality and sum frequency feasibility at higher powers) October 21, 1999 Gemini Science Committee 45 Gemini AO Program Baseline Schedule 2000 2001 2002 2003 2004 Duration O N D J F M A M J J A S O N D J F M A M J J A S O N D J F M A M J J A S O N D J F M A M J J A S O N D J F M 1632 days ID Task Name 1 CP LGS M CAO System 2 Conceptu al Design 632 days • Conceptual design review: 3/00 3 CP Sight Characterization 4 Science and System Implimentation Review 5 CoD Forum 6 Review Forum 7 System Concept Development 8 System Requirements Review (Gemini Board) • Preliminary design reviews: 12/00 9 System Conceptual Design 10 Conceptual Design Review 11 Subsystem Requirements and Interface Description 12 261 days 65 days 1 day 22 days AO Instru m ent Package 152 days 1 day 87 days 0 days 799 days 13 Prelim inary Design Phase 141 days 14 Preliminary Design 140 days • Critical design reviews: 12/01 15 Lab Demo 140 days 16 Integration and Test Planning 120 days 17 Preliminary Design Review (s) 18 Detailed Design Phase 1 day Subsystem Detailed Design 257 days 20 Integration and test planning 160 days • Subsystems complete: 6/03 21 Critical Des ign Review (s) • System integration and test: 10/03 27 • Science handover: 3/04 October 21, 1999 Fabricatio n Phase 1 day Fabrication of Subsystems 300 days 24 I, T, & C Pr oceedures 200 days 25 Operational Softw are Implementation 300 days 26 Integration and Test 100 days 799 days 28 Prelim inary Design Phase 141 days 29 Preliminary Design 140 days 30 Integration and Test Planning 140 days 31 Preliminary Design Review (s) 32 Detailed Design Phase 1 day Subsystem Detailed Design 257 days 34 Risk Reduc tion Prototyping 257 days 35 Integration and Test Planning 160 days 36 Critical Des ign Review (s) Fabricatio n Phase 12/14 258 days 33 37 12/11 400 days 23 Laser Sys tem 12/14 258 days 19 22 3/31 44 days 1 day 12/11 400 days 38 Fabrication of Subsystems 300 days 39 I, T, & C Pr oceedures 200 days 40 Operational Softw are Implementation 300 days 41 Integration and Test 100 days 42 System In tegration Phase 201 days 43 System Integration and Test 100 days 44 Commissioning 100 days 45 Science Handover 1 day Gemini Science Committee 46 Gemini AO Program Gemini AO Program: Division of Work within Partnership Gemini AO program ambitious, but IGPO is not proceeding alone • • Partnership Workload (including vendors): – Hokupa’a-85 for Gemini-North: UH – Hokupa’a-85 for Gemini-South: • WFS and DM: UH • Commercially supplied dye laser – Altair: HIA – Altair LGS: • WFS upgrades: HIA • Laser source: Contract – Coronograph AO: Instrument supplier Common infrastructure (IGPO): LGS transfer optics, launch telescope, and safety system • MCAO is the focus of IGPO efforts. Outsourcing of work expected after CoDR. October 21, 1999 Gemini Science Committee 47