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GRAAL- GALACSI Comparison

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GRAAL- GALACSI Comparison

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  1. AOF Wave front sensor modulesGALACSI and GRAALbyStefan Ströbelein behalf of the GALACSI and GRAAL Team members:R.Arsenault, R.Conzelmann, B.Delabre, R. Donaldson, M.Duchateau, G.Hess, P.Jolley, A. Jost, M.Kiekebusch, M.Lelouarn, P.Y.Madec, A.Manescau, J.Pirard, J.Quentin, R.Siebenmorgen, C.Soenke, S.Tordo, J.Vernet, SPARTA, DSM, 4LGS, ASSIST, Teams, Integration and IR and CCD detector groups

  2. GRAAL- GALACSI Comparison

  3. AO Types • GLAO: • 4 Laser guide stars, 4 WFSs • 1 Natural guide star, 1 TT Sens. • Average WFS signal High order DM command + tip tilt meas. • LTAO: • 4 Laser guide stars, 4 WFSs (closer together) • 1 Natural guide star, 1 low order sensor • WFS signal + Tomography Algorithm  high order DM command + tip tilt +focus meas. • correction by the DM • SCAO: • 1 Natural guide star, 1 WFS • WFS measures Turbulence • correction by the DM

  4. GRAAL • Integration to a existing instrument •  Strong constraints to space, weight, access, interfaces LGS and NGS pickup outside the science field HAWK-I co-rotates to the sky Matching of the WFS – DSM geometries counter rotation of the LGS WFSs

  5. GRAAL big pieces Alu-structure NGS-TT sensor assembly LGS trombone LGS WFS assembly bearing Hawk-I shutter Torque drive Steel structure Counterweight • Bearing (150Nm friction / 80kg) • Torque drive (500Nm nominal / 70kg) • Encoder (tape / scanning head) • Cable-guide system (110 kg) • Aluminium structure (75 kg) • Steel structure (50 kg) Steel flange MCM assembly

  6. GRAAL as seen from (above) the Nasmyth platform Flange sandwiched between UT-Nasmyth and Hawk-I Aluminum and steel structure for stiffness and weight constraints ICPs for quick-separation Internal co-rotator for pupil derotation, direct drive in torque mode, strip band encoder, control loop using VLT-SW standard library 1kHz, 0-noise LGS WFS, optics and trombone focusing on a Ø500 mm (x4) Retractable focal enlarger x6 (maintenance and commissioning), with WFS pick-up 100 kg counterweight to balance 150 kg of electronics

  7. GRAAL arrangement on UT4 • 2 E-Cabinet on board • (WFS camera electronics) • Uses the HAWK-I cable rotator • Cabinet on the NP • motion control, • Cabinet on Azimuth PF • SPARTA RTC • 5*NGC backend • Cabinet in the computer room • SPARTA cluster

  8. GRAAL Performance • Image improvement x~2 (EE in 0.1” pixel),seeing reducer: x0.8 (in Ks) • Improvement for all seeing conditions J. Paufique

  9. MUSE-GALACSI MUSE: • 3d Spectrograph with 300 by 300 spatial resolution elements • Spectrometer resolution 1500-3000 • 24 spectrographs with 1CCD 4096 by 4096 pixels each • Wavelength range: 465-930nm • Developed by consortium lead by CRA-Lyon, PI: R.Bacon • Nasmyth platform “over” filled (Volume, Weight) extension for cabinets and access

  10. NGS-LGS Configurations 4 Sodium LGSs 1’ MUSE FOV 1 faint NGS within 3.4’ FOV Rayleigh cone WFM NFM

  11. LGS WFS path from VLT Focus compensator LGS dichroic, Reflects 589nm transmits the rest to TTS Pyramid: • LGS separation near LGS focus • On linear stage to switch between modes AIT pupil Telecentricity lens 2nd Pupil relay Pupil relay WFS, LA Annular Mirror, ( no obstruction for MUSE WFM) LGS dichroic inserted for NFM Jitter actuator

  12. GALACSI Main assembly GALACSI at Nasmyth B UT4 5 E-Boxes on board 1 Cabinet on NP 1 Cabinet on AZ P 2 cable chains

  13. IRLOS • HAWAI –I 1024 x 1024 pixels, 4 quadrant geometry  4 sub aperture lenslet array • Frame rate 200/500 Hz for 20by20/8by8 pix RON <15 e-rms

  14. GALACSI Performance specification NFM performance WFM performance

  15. Outlook to GRAAL Commissioning

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