Post on 29-Jan-2016
AOF
The VLT Adaptive Optics Facility
R. Arsenault, P.-Y. Madec, W. Hackenberg, J. Paufique, S. Stroebele, J.-F. Pirard, E. Vernet, D. Bonaccini Calia, I. Guidolin,
M. Quattri, R. Guzman, B. Buzzoni, M. Comin, C. Dupuy, A. Silber, J. Quentin, G. Igl, L. Taylor, J. Argomedo, P. Jolly, A.
Manescau, R. Stuik, M. Downing, J. Reyes, A. Jost, M. Duchateau, N. Hubin, A. Glindemann, P. Amico, M. Lelouarn, J.
Kolb, S. Tordo, E. Fedrigo, R. Donaldson, C. Soenke, R. Conzelmann, B. Delabre, M. Kiekebusch, J.-L. Lizon, P. La
Penna, L. Jochum
27/11/2009 20th Anniversary of AO at ESO 1
AOFAOF: why…what…• To provide improved observing conditions for UT4
Instruments by delivering– A better seeing in a Wide Field of View– Diffraction limited images in one direction
• with as constraints– Not to degrade the Instruments throughput/emissivity– High sky coverage
• To turn-out UT4 in an Adaptive Telescope– To replace M2 by a Deformable Secondary Mirror– To provide a Multi-Laser Guide Star Facility– To build two post-focal LGS/NGS WFS Modules27/11/2009 20th Anniversary of AO at ESO 2
AOFHAWK-I and MUSE
the two (first) customers of AOF• HAWK-I, a Wide FoV IR Imager (0.9 – 2.5 m)
– 7.5 x 7.5 arcmin2 FoV – 0.1 arcsec pixel size– Requirement towards AOF, in K bands
• Gain of ≈2 in EE in 0.1 arcsec (seeing reducer: x0.8)
• MUSE, a visible 3D Spectrograph (465-930 nm)– WFM
• 1 x 1 arcmin2 FoV – 0.2 arcsec spaxel size• Requirements towards AOF: gain of ≈2 in EE in 0.2 arcsec
– NFM• 7.5 x 7.5 arcsec2 FoV – 0.025 arcsec spaxel size• Requirements towards AOF: 5% to 10% Sr at 650 nm under 0.6
arcsec seeing 27/11/2009 20th Anniversary of AO at ESO 3
AOFAOF: how…
• MUSE NFM and WFM requirements– Number of DSM actuators > 1000 (1170 final)– Number of WFS subapertures > 33x33 (40x40 final)– Control frequency ≈ 1 kHz– LGS brightness (at Nasmyth) 5 106 photons/m2/s– WFS camera RoN < 1 e-/pixel/frame
• HAWK-I and MUSE WFM requirements– Number of LGSs 4
• HAWK-I requirements– LGS distance from opt. axis up to 6 arcmin
27/11/2009 20th Anniversary of AO at ESO 4
AOFAOF main subsystems
27/11/2009 20th Anniversary of AO at ESO 5
GRAAL
LGS Unit GALACSI
DSM
AOFDSM/M2 Unit (MG/ADS/OAA)
• Same functions and interfaces as the actual M2 Dornier– Optical diameter 1120 mm– Focus, centering, tilt/chop– Hub interfaces
• 2 mm Zerodur thin shell, with magnets glued on
• 1170 voice coil actuators• DSM response time 0.7 ms• Liquid cooled (1.5 kW)• Delivery date end 2011
27/11/2009 20th Anniversary of AO at ESO 6
AOFDSM development status
12711/2009 20th Anniversary of AO at ESO 7
AOF4 Laser Guide Star Facility• 4 identical LGS Unit, mounted on UT4 Center Piece
– One 40 cm diameter Launch Telescope (TNO)– One Beam Control and Diagnostic System (ESO)
• Control of focusing altitude (70 to 200 km)• Control of LGS position (0 to 6 arcmin from optical axis)• LGS jitter stabilization mirror (controlled by AO modules)• Safety devices (shutters)• Diagnostic tools (power meter, WFS, alignment camera)
– One 20 W CW dual line laser (outsourced)• 18 W in D2a and 2 W in D2b lines (back-pumping scheme)
• Compact, efficient, reliable and maintainable laser27/11/2009 20th Anniversary of AO at ESO 8
AOF4LGSF: development status
27/11/2009 20th Anniversary of AO at ESO 9
TOPTICA Laser FASORtronics Laser
Launch telescope (TNO)
AOF
• GLAO mode: seeing enhancer in 7.5 x 7.5 arcmin2 FoV• 4 LGSs located almost 6 arcmin from the opt. axis• No optics inserted in the HAWK-I scientific FoV
27/11/2009 20th Anniversary of AO at ESO 10
GRAAL: the HAWK-I AO Module
AOF
27/11/2009 20th Anniversary of AO at ESO 11
• WFM• GLAO mode: seeing enhancer
in 1x1 arcmin2 FoV @ 750 nm• 4 LGSs located ≈1 arcmin
from the optical axis• NFM
• LTAO mode: 5% to 10% Sr in a 5arcsec diameter FoV @ 650 nm
• 4 LGSs located ≈10 arcsec from the optical axis
• (Almost) no optics inserted in the MUSE scientific FoV
GALACSI: the MUSE AO Module
AOFAOF: common critical components• SPARTA: real-time architecture for AO control
– Inputs: 4 x (240x240 pixels / 1240 subap.) Shack-Hartmann– Outputs: 1170 commands– Control frequency: 1 kHz – latency: 400 s– WFS measurement algorithm: WCoG– Control algorithm: Matrix Vector Multiplication
27/11/2009 20th Anniversary of AO at ESO 12
AOFSPARTA: development status
27/11/2009 20th Anniversary of AO at ESO 13
RTC box
Co-processing cluster
GB Ethernet Switch
Gigabit Ethernet Switch
LCU
InstrumentWS
VLT Gbit control LAN
RTC box
CSW1
switchand
transc.board
VXS backplane
Gbit LAN (VLT)
VXS serial lines
Gbit LAN (private)serial FPDPDell
1950Dell1950
Dell1950
Co-processing cluster
DSM
Dell1950
Dell1950
Gigabit Ethernet Switch
VPF1
Control,TTS WPU,LGSF IF
VPF1
WavefrontProcessing
LGS
VPF1
WavefrontProcessing
LGS
T2V6
Recon-struction
T2V6
Recon-struction
T2V6
Recon-struction
T2V6
Recon-struction
NGC
NGC
NGC
NGC
Jitter Actuators
VLT computer room
UT area
NGC
NGC
LGS 1
TT (VIS)
IRLOS(GALACSI)
LGS 4
LGS 3
LGS 2
Dell2950(storage)
CODE
FS Actuators
CODE(in 4LGSF)
4LGSF
SPARTA RTC
NGCNGS
(GRAALMCM)
GALACSIonly
AOFAOF: common critical components• SPARTA: real-time architecture for AO control
– Inputs: 4 x (240x240 pixels / 1240 subap.) Shack-Hartmann– Outputs: 1170 commands– Control frequency: 1 kHz – latency: 400 s– WFS measurement algorithm: WCoG– Control algorithm: Matrix Vector Multiplication
• WFS camera– 240x240 pixels – 1000 frames/s– High QE: > 80% @ 589 nm– RoN: < 1e-/pixel/frame
27/11/2009 20th Anniversary of AO at ESO 14
AOFWFS Cameras: development status
27/11/2009 20th Anniversary of AO at ESO 15
E2V CCD 220
Ocam – test camera
WFS camera head: first ESO prototype
AOFAOF: common critical components• SPARTA: real-time architecture for AO control
– Inputs: 4 x (240x240 pixels / 1240 subap.) Shack-Hartmann– Outputs: 1170 commands– Control frequency: 1 kHz – latency: 400 s– WFS measurement algorithm: WCoG– Control algorithm: Matrix Vector Multiplication
• WFS camera– 240x240 pixels – 1000 frames/s– High QE: > 80% @ 589 nm– RoN: < 1e-/pixel/frame
• ASSIST: the AOF test and calibration tool– Optical calibration of the DSM– Full system test of the AOF
27/11/2009 20th Anniversary of AO at ESO 16
AOFASSIST: the AOF test bench• 2.5 arcmin unvignetted fov• Diffraction limited on-axis and stringent pupil imaging quality• Simulation of NGSs and LGSs (including elongation)• 3 phase screens at different altitudes• Simulation of VLT Nasmyth focus (f/15 – pupil at -16 m from focus)
27/11/2009 20th Anniversary of AO at ESO 17
AOFASSIST: development status
27/11/2009 20th Anniversary of AO at ESO 18
AOFAOF on-sky: when…
• Critical path: DSM and laser delivery– DSM end 2011– Laser last one beginning 2013
• Tests of DSM, GRAAL and GALACSI in Garching– One year needed end 2012
• Installation of AOF at Paranal– Beginning 2013 (synchronized with laser delivery)
• AOF first light 2013
27/11/2009 20th Anniversary of AO at ESO 19