gemini ao program october 21, 1999gemini science committee1 the gemini adaptive optics program mcao...
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October 21, 1999 Gemini Science Committee 1
Gemini AO Program
The Gemini Adaptive Optics The Gemini Adaptive Optics ProgramProgram
MCAO for Gemini-SouthMCAO for Gemini-South
Gemini Adaptive Optics TeamB. Ellerbroek and F.Rigaut
October 21, 1999 Gemini Science Committee 2
Gemini AO Program
Top Level Perf. Requirement Top Level Perf. Requirement #2#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 scienceenable 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 3
Gemini AO Program
AO and ScienceAO 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 4
Gemini AO Program
• 1989: First AO images w/ Come-On (OHP & ESO) 110mas
A short history of astronomical A short history of astronomical AOAO
• 1992: First Curvature system (UH) 70mas• 1996: First Facility system (CFHT AOB)
October 21, 1999 Gemini Science Committee 5
Gemini AO Program
CFHT Pueo 1996Galactic Center2.2 m
FWHMFWHM
130 mas130 mas
October 21, 1999 Gemini Science Committee 6
Gemini AO Program
A short history of astronomical A short history of astronomical AOAO
• 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 7
Gemini AO Program
Keck AO System1999Vesta 1.5 m
FWHMFWHM<40 mas<40 mas 1’’
October 21, 1999 Gemini Science Committee 8
Gemini AO Program
Gemini’s Gemini’s DedicationDedication
Courtesy C.Roddier, UH-IfA
October 21, 1999 Gemini Science Committee 9
Gemini AO Program
ALFA AO ResultsALFA AO Results(18 Modes, 0.9-1.0’’ seeing, K band)(18 Modes, 0.9-1.0’’ seeing, K band)
NGS AO• 0.42 Strehl
• 0.53 predicted
Open loop
Loop closedwith LGS AO• 4 W dye laser
• 0.23 Strehl
• FWHM dif-fraction limited.
October 21, 1999 Gemini Science Committee 10
Gemini AO Program
Where is AO standing ?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 11
Gemini AO Program
Proposed Baseline AO Proposed Baseline AO ProgramProgram
NORTH
SOUTH
1999
2000
2001
2002
2003
2004
SubaruSubaruKeckKeck
VLTVLT VLT-LGSVLT-LGS CP AOS/LGSCP AOS/LGS
AltairAltair10W LGS10W LGS
Hokupa’aHokupa’a 3636 8585
2W LGS2W LGS
CP Hokupa’aCP Hokupa’a 8585
October 21, 1999 Gemini Science Committee 12
Gemini AO Program
Baseline Program: AltairBaseline Program: Altair
CP AOS/LGS
10W LGS
NORTH
SOUTH
1999
2000
2001
2002
2003
2004
SubaruKeck
VLT VLT-LGS
Hokupa’a 36 85
2W LGS
CP Hokupa’a 85
Altair
•Progresses well (CDR 02/99)•Statement of work for Altair LGS upgrade nearly ready
October 21, 1999 Gemini Science Committee 13
Gemini AO Program
Baseline Program: 10W Baseline Program: 10W LGSLGS
CP AOS/LGS
10W LGS
NORTH
SOUTH
1999
2000
2001
2002
2003
2004
SubaruKeck
VLT VLT-LGS
Hokupa’a 36 85
2W LGS
CP Hokupa’a 85
10W LGS10W LGS
•10 W Laser RFP to go out early October•Power requirements vary from 7 to 23W depending on laser pulse format•Design of the LLT and BTO underway
October 21, 1999 Gemini Science Committee 14
Gemini AO Program
Baseline Program: MK-Baseline Program: MK-Hokupa’aHokupa’a
CP AOS/LGS
10W LGS
NORTH
SOUTH
1999
2000
2001
2002
2003
2004
SubaruKeck
VLT VLT-LGS
Hokupa’a 36 85
2W LGS
CP Hokupa’a 85
Hokupa’aHokupa’a 3636 8585
•Hokupa’a-36 installed on the telescope early June this year•Images fully compatible with expectations (seeing ok but not exceptional), near diffraction limit in K band w/ Strehl ~ 15-30%. Great tool for telescope engineering•85 Actuators upgrade to be done next year by UH team on UH/NSF internal funds. Small transferred field (30’’)
Performance w/ NGS (AO only) (2 fold vs 36 actuators):Seeing Strehl(J) Strehl(K)0.45’’ 50% 80%0.65’’ 25% 62%
October 21, 1999 Gemini Science Committee 15
Gemini AO ProgramCerro PachonCerro Pachon-AOS/LGS -AOS/LGS ForumForumApril 1999, Review Panel April 1999, Review Panel RecommendationsRecommendations1 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.
2 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.
3 The IGPO should lead the conceptual design program of the Gemini-South AO system, including defining the allocation of subsystems across the Gemini Community
4 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.
5 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 16
Gemini AO Program
Baseline Program: CP-Baseline Program: CP-Hokupa’aHokupa’a
CP AOS/LGS
SOUTH
1999
2000
2001
2002
2003
2004
SubaruKeck
VLT VLT-LGS
Hokupa’a 36 85
2W LGS
CP Hokupa’a 85
SOUTH
2W LGS2W LGS
CP Hokupa’aCP Hokupa’a 8585
• AOAO: Duplicate of the MK upgrade of Hokupa’a to 85 actuators. UH AO Team. Proposal submitted to NSF 08/99. Optomechanical upgrades (FoV 60’’) + LGS compatible
Performance w/ NGS (AO only):Seeing Strehl(J) Strehl(K)0.45’’ 50% 80%0.65’’ 25% 62%
• LGSLGS: Off-the-shelf 2W CW laser. Coherent/Spectra physics CW 10W pump laser + ring dye laser (demonstrated in lab)• IR ImagerIR Imager: ABU
October 21, 1999 Gemini Science Committee 17
Gemini AO Program
Baseline Program: CP-Baseline Program: CP-Hokupa’aHokupa’a
CP AOS/LGS
SOUTH
1999
2000
2001
2002
2003
2004
SubaruKeck
VLT VLT-LGS
Hokupa’a 36 85
2W LGS
CP Hokupa’a 85
SOUTH
2W LGS2W LGS
CP Hokupa’aCP Hokupa’a 8585
Rationale:Rationale:• Gives us a 2+ year window of unchallenged AO+LGS capability unchallenged AO+LGS capability in the southern hemispherein the southern hemisphere (comp. NAOS) w/ Adequate JHK performance. • Build expertise on LGS by stepping up gradually (Laser Launch Telescope + Beam Transfer Optics)• Getting AO on CP as soon as possible relieves pressure, allowing us to avoid the rush and do a better job on the final CP system
October 21, 1999 Gemini Science Committee 18
Gemini AO Program
Baseline Program: Facility CP Baseline Program: Facility CP AOSAOS
CP AOS/LGS
10W LGS
SOUTH
1999
2000
2001
2002
2003
2004
SubaruKeck
VLT VLT-LGS
Hokupa’a 36 85
2W LGS
CP Hokupa’a 85
SOUTH
Context:Context:• Simplest case = duplicate Altair -> No AO facility until late 2002.• Other observatories have very capable AOSs in the north (Keck 1999) and in the south (VLT-NAOS 2001) -> Competitiveness issue
Rationale:Rationale: (Why?)(Why?)• Provide the Gemini community with NGST-like capabilities (spatial res. and field), matching the Gemini science goals and instrumentation• 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
CP AOS/LGSCP AOS/LGS
October 21, 1999 Gemini Science Committee 19
Gemini AO Program
Baseline Program: Facility CP Baseline Program: Facility CP AOSAOS
CP AOS/LGS
10W LGS
SOUTH
1999
2000
2001
2002
2003
2004
SubaruKeck
VLT VLT-LGS
Hokupa’a 36 85
2W LGS
CP Hokupa’a 85
SOUTH
Proposal:Proposal: (What?)(What?)• Build a high performance, 2 arcminutes field of view AOS with homogeneous PSF quality over the entire field of view, with very high sky coverage
How ?How ?• Using Multi-Conjugate AO, i.e. 4-5 LGSs and wavefront sensors to measure the turbulence in 3D and 2-3 deformable mirrors to correct it• This uses currently available technology. NO hardware development required other than lasers (same as MK-LGS)
CP AOS/LGSCP AOS/LGS
October 21, 1999 Gemini Science Committee 20
Gemini AO Program
What is Tomography ?What is Tomography ?1. Cone effect1. Cone effect
90 k
m
October 21, 1999 Gemini Science Committee 21
Gemini AO Program
What is tomography ?What is tomography ?2. Multiple guide star and 2. Multiple guide star and tomographytomography
90 k
m
October 21, 1999 Gemini Science Committee 22
Gemini AO Program
What is multiconjugate?What is multiconjugate?
October 21, 1999 Gemini Science Committee 23
Gemini AO Program
What is multiconjugate?What is multiconjugate?
October 21, 1999 Gemini Science Committee 24
Gemini AO Program
What is multiconjugate?What is multiconjugate?
Telescope
DM1 DM2
Turb. Layers#1 #2
Atmosphere
WFS
UP
October 21, 1999 Gemini Science Committee 25
Gemini AO Program
Baseline Program: Facility CP Baseline Program: Facility CP AOSAOS
CP AOS/LGS
10W LGS
SOUTH
1999
2000
2001
2002
2003
2004
SubaruKeck
VLT VLT-LGS
Hokupa’a 36 85
2W LGS
CP Hokupa’a 85
SOUTH
What does MCAO do that another system wouldn’t ?What does MCAO do that another system wouldn’t ?• Sky coverage (50%) increased (50-500x) w/ respect to a NGS system• Increased performance on axis w/ respect to a LGS system because the cone effect is taken care of• Increased field of view (well matched to IRMOS)• Uniform PSF across the FoV -> Easier and more accurate Data Reduc.
CP AOS/LGSCP AOS/LGS
October 21, 1999 Gemini Science Committee 26
Gemini AO Program
Classical AO
MCAO
No AO
165’’
MCAO Performance MCAO Performance SummarySummaryEarly NGS results, MK ProfileEarly NGS results, MK Profile
2 DMs / 5 NGS
320 stars / K band / 0.7’’ seeing
1 DM / 1 NGS
Stars magnified for clarity
October 21, 1999 Gemini Science Committee 27
Gemini AO Program
MCAO Performance MCAO Performance SummarySummaryEarly NGS results, MK ProfileEarly NGS results, MK Profile
Classical AO
MCAO
Guide star location
October 21, 1999 Gemini Science Committee 28
Gemini AO Program
Baseline Program: Facility CP Baseline Program: Facility CP AOSAOS
CP AOS/LGS
10W LGS
SOUTH
1999
2000
2001
2002
2003
2004
SubaruKeck
VLT VLT-LGS
Hokupa’a 36 85
2W LGS
CP Hokupa’a 85
SOUTH
PerformancePerformance
Mode %Sky3 SRJ(0’’) SRJ(48’’) FOV HardwareNGS 1% 0.55 0.04 30’’ 1 1DMLGS 17% 0.47 0.04 32’’ 1 1DM/1LGSMCAO 34% 0.54 0.35 2’ 2 3DM/5LGS
1 50% Strehl ratio attenuation2 limited by the AO-Fold aperture3 Sky coverage at galactic pole
CP AOS/LGSCP AOS/LGS
October 21, 1999 Gemini Science Committee 29
Gemini AO Program
Baseline Program: Facility CP Baseline Program: Facility CP AOSAOS
CP AOS/LGS
10W LGS
SOUTH
1999
2000
2001
2002
2003
2004
SubaruKeck
VLT VLT-LGS
Hokupa’a 36 85
2W LGS
CP Hokupa’a 85
SOUTH
Where are we?Where are we?• Feasibility studyFeasibility study progressing, including:
•First pass on the science drivers•Theoretical analysis of MCAO control/numerical simulations/Performance assessment•A proof-of-concept optical and mechanical layout•Assessment of the need in computing issues•Management plan including schedule and resource needs
CP AOS/LGSCP AOS/LGS
October 21, 1999 Gemini Science Committee 30
Gemini AO Program
MCAO for Gemini-SouthMCAO for Gemini-SouthPerformance, Feasibility, and SchedulePerformance, 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 32
Gemini AO Program
NGS, LGS, and Multi-conjugate NGS, LGS, and Multi-conjugate AOAOPerformance CharacteristicsPerformance Characteristics
•T/T guide star brightness (relaxed)• TBD (new inverse problem)
•T/T guide star brightness (relaxed)• Tilt anisoplanatism• Cone effect
• Guide star brightness• Common anisoplanatism
Fundamental limits
1-2’(Nearly uniform)
20-40”(Nonuniform)
20-40”(Nonuniform)
Compensated field-of-view
Further improved (~34% at galactic
pole)
Good (~17% at galactic pole,SR=0.6 in H)
Poor (0.1-2%)Sky coverage
MCAOLGS AONGS AO
• Sky coverage and field-of-view are for J, H, K bands with 0.5 arc second seeing
October 21, 1999 Gemini Science Committee 33
Gemini AO Program
Analysis and Simulation Analysis and Simulation ModelsModels
• 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 34
Gemini AO Program
MCAO Parameters for MCAO Parameters for Gemini-CPGemini-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 35
Gemini AO Program
Sample Numerical ResultsSample 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 36
Gemini AO Program
Sample Numerical ResultsSample Numerical ResultsVariation with Seeing and Zenith Variation with Seeing and Zenith AngleAngle0 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 37
Gemini AO Program
Sample ResultsSample ResultsSlit Coupling Efficiency at 0 Degrees ZenithSlit 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 38
Gemini AO Program
Why Multiple Tip/Tilt NGS’s?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
r)=ar2
r)=a(cr+d)2
=ac2r2+2acdr+ad2
~ ac2r2
After tilt removal
October 21, 1999 Gemini Science Committee 39
Gemini AO Program
MCAO Sky Coverage with MCAO Sky Coverage with Multiple Tip/Tilt NGSMultiple 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 40
Gemini AO Program
MCAO Implementation-MCAO Implementation-Feasibility study conclusions: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 41
Gemini AO Program
MCAO Science Optical PathMCAO Science Optical Path
•3 DM’s at R=0, 4, and 8 km 3 DM’s at R=0, 4, and 8 km •13 actuators across beamprint13 actuators across beamprint•4 folds, 2 off-axis parabolas,4 folds, 2 off-axis parabolas, 1 dichroic beamsplitter (not shown)1 dichroic beamsplitter (not shown) - Near-minimum number of surfaces for - Near-minimum number of surfaces for facility MCAOfacility MCAO• f/30 output focusf/30 output focus
October 21, 1999 Gemini Science Committee 42
Gemini AO Program
MCAO LGS Optical PathMCAO LGS Optical Path
4 LGS’s sensed with 1 WFS CCDZEMAX optical schematic
• Outgoing: Single launch telescope for all guide stars
• Return: One WFS camera for all guide stars
October 21, 1999 Gemini Science Committee 43
Gemini AO Program
WFS Camera OptionsWFS Camera Options
Supports 5 LGS,
16 by 16 SA1000+6-10128 by
128
MIT/LL CCD
1-2 Cameras for 4-5 LGS, 12 by 12 SA
1000580 by 80EEV CCD
500-10005-10
80 by 80to
128 by 128Requirement
CommentsFrame
rate, Hz
Read noise
electronsPixels
• MIT/LL read noise level is new information since feasibility study
October 21, 1999 Gemini Science Committee 44
Gemini AO Program
Approach to Multiple Tip/Tilt Approach to Multiple Tip/Tilt NGS WFS’sNGS WFS’s
X stage
Y stage
200mm
To APDs
X stage
Focal plane
• 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 45
Gemini AO Program
Laser IssuesLaser 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 46
Gemini AO Program
Baseline ScheduleBaseline Schedule
• Conceptual design review: 3/00
• Preliminary design reviews: 12/00
• Critical design reviews: 12/01
• Subsystems complete: 6/03
• System integration and test: 10/03
• Science handover: 3/04
ID Task Name Duration
1 CP LGS MCAO System 1632 days
2 Conceptual Design 632 days
3 CP Sight Characterization 261 days
4 Science and System Implimentation Review 65 days
5 CoD Forum 1 day
6 Review Forum 22 days
7 System Concept Development 152 days
8 System Requirements Review (Gemini Board) 1 day
9 System Conceptual Design 87 days
10 Conceptual Design Review 0 days
11 Subsystem Requirements and Interface Description 44 days
12 AO Instrument Package 799 days
13 Preliminary Design Phase 141 days
14 Preliminary Design 140 days
15 Lab Demo 140 days
16 Integration and Test Planning 120 days
17 Preliminary Design Review(s) 1 day
18 Detailed Design Phase 258 days
19 Subsystem Detailed Design 257 days
20 Integration and test planning 160 days
21 Critical Design Review(s) 1 day
22 Fabrication Phase 400 days
23 Fabrication of Subsystems 300 days
24 I, T, & C Proceedures 200 days
25 Operational Software Implementation 300 days
26 Integration and Test 100 days
27 Laser System 799 days
28 Preliminary Design Phase 141 days
29 Preliminary Design 140 days
30 Integration and Test Planning 140 days
31 Preliminary Design Review(s) 1 day
32 Detailed Design Phase 258 days
33 Subsystem Detailed Design 257 days
34 Risk Reduction Prototyping 257 days
35 Integration and Test Planning 160 days
36 Critical Design Review(s) 1 day
37 Fabrication Phase 400 days
38 Fabrication of Subsystems 300 days
39 I, T, & C Proceedures 200 days
40 Operational Software Implementation 300 days
41 Integration and Test 100 days
42 System Integration Phase 201 days
43 System Integration and Test 100 days
44 Commissioning 100 days
45 Science Handover 1 day
3/31
12/14
12/11
12/14
12/11
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 M2000 2001 2002 2003 2004
October 21, 1999 Gemini Science Committee 47
Gemini AO Program
Gemini AO Program: Gemini AO Program: Division of Work within Division of Work within PartnershipPartnership
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.