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the vlt adaptive optics facility

The VLT Adaptive Optics Facility

R. Arsenault, P.-Y. Madec, W. Hackenberg, J. Paufique, S. Stroebele, J.-F. Pirard, E. Vernet, D. BonacciniCalia, 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

20th Anniversary of AO at ESO

aof why what
AOF: 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 Modules

20th Anniversary of AO at ESO

hawk i and muse the two first customers of aof
HAWK-I and MUSEthe two (first) customers of AOF
  • HAWK-I, a Wide FoV IR Imager (0.9 – 2.5 mm)
    • 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

20th Anniversary of AO at ESO

aof how
AOF: 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

20th Anniversary of AO at ESO

aof main subsystems
AOF main subsystems

GRAAL

DSM

GALACSI

LGS Unit

20th Anniversary of AO at ESO

dsm m2 unit mg ads oaa
DSM/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

20th Anniversary of AO at ESO

dsm development status
DSM development status

20th Anniversary of AO at ESO

4 laser guide star facility
4 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 laser

20th Anniversary of AO at ESO

4lgsf development status
4LGSF: development status

FASORtronics Laser

TOPTICA Laser

Launch telescope (TNO)

20th Anniversary of AO at ESO

graal the hawk i ao module
GRAAL: the HAWK-I AO Module
  • 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

20th Anniversary of AO at ESO

galacsi the muse ao module
GALACSI: the MUSE AO Module
  • 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

20th Anniversary of AO at ESO

aof common critical components
AOF: 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 ms
    • WFS measurement algorithm: WCoG
    • Control algorithm: Matrix Vector Multiplication

20th Anniversary of AO at ESO

sparta development status
SPARTA: development status

GB Ethernet Switch

RTC box

Co-processing cluster

20th Anniversary of AO at ESO

aof common critical components1
AOF: 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 ms
    • 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

20th Anniversary of AO at ESO

wfs cameras development status
WFS Cameras: development status

E2V CCD 220

WFS camera head: first ESO prototype

Ocam – test camera

20th Anniversary of AO at ESO

aof common critical components2
AOF: 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 ms
    • 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

20th Anniversary of AO at ESO

assist the aof test bench
ASSIST: 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)

20th Anniversary of AO at ESO

assist development status
ASSIST: development status

20th Anniversary of AO at ESO

aof on sky when
AOF 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

20th Anniversary of AO at ESO

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