aof the vlt adaptive optics facility r. arsenault, p.-y. madec, w. hackenberg, j. paufique, s....

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


AOFAOF main subsystems


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


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


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


GRAAL: the HAWK-I AO Module

AOF


• 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


AOFSPARTA: development status


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



• WFS camera– 240x240 pixels – 1000 frames/s– High QE: > 80% @ 589 nm– RoN: < 1e-/pixel/frame


AOFWFS Cameras: development status


E2V CCD 220

Ocam – test camera

WFS camera head: first ESO prototype



• 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


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)


AOFASSIST: development status


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


aof the vlt adaptive optics facility r. arsenault, p.-y. madec, w. hackenberg, j. paufique, s....

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