MAORY E-ELT MCAO module project overview

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1 MAORY E-ELT MCAO module project overview Emiliano Diolaiti Istituto Nazionale di Astrofisica Osservatorio Astronomico di Bologna On behalf of the MAORY Consortium AO4ELT3, Firenze, May 2013

2 MAORY overview from Phase A Functions Compensate atmospheric turbulence Relay telescope focal plane to science instrument Main requirements related to client instrument MICADO Wavelength range µm Science field of view 53" 53" Uniform adaptive optics correction with high sky coverage Gravity invariant exit port Other requirements Lateral exit port for another possible instrument TBC Expected AO performance 50% Strehl Ratio averaged over MICADO field at 2.16 µm wavelength with 50% sky coverage at the Galactic Pole 40% Strehl Ratio with 80% sky coverage at the Galactic Pole 2

3 AO basic choices Multi-conjugate adaptive optics Performance uniformity Demonstrated on sky by MAD and GeMS MAD Strehl Ratio maps (2.2 µm) ESO Laser Guide Stars Sky coverage and performance uniformity Demonstrated on sky with MCAO by GeMS SCAO MCAO Wavefront sensors downstream the deformable mirrors Optical feed-back Telescope DM (M4/M5) MAORY DMs WFS 3

4 MCAO module architecture E-ELT Telescope Control System Common Path Optics Deformable Mirrors Real Time Control System Dichroic Science Path Optics LGS Objective MAORY Instrumentation Software E-ELT NGS Wavefront Sensor LGS Wavefront Sensor MAORY Client Instrument Exit Port Light beam MAORY module Client Instrument Instrumentation Software Signal (real-time) Signal (non real-time) 4

5 MCAO module layout Pre-focal station Nasmyth platform MAORY Lateral port Area for detached instrument MICADO Gravity invariant port 5

6 To MICADO Wavefront Sensors Laser Guide Star Wavefront Sensor 6 Sodium Laser Guide Stars LGS fixed with respect to telescope pupil Shack-Hartmann (~80 80 subapertures) Natural Guide Star Wavefront Sensor 3 Natural Stars over 2.6 arcmin field of view Limiting magnitude H Each WFS unit is split into two channels: Tip-Tilt/Focus channel ( µm) Reference channel ( µm) 6

7 Project status Phase A completed (December 2009) Project Management Plan for phases B-E in preparation Consortium consolidation in progress INAF: System level responsibility, platform, NGS WFS, deformable mirrors, auxiliary equipments, science support tools Durham University: Real Time Control System Observatoire de Paris LESIA: LGS Wavefront Sensor ESO: WFS cameras, deformable mirrors, other contributions TBC 7

8 Project status Review of requirements, interfaces and technical choices in collaboration with ESO General technology developments within E-ELT project Cameras for wavefront sensors Deformable mirrors Real Time Control System Led by ESO Specific activities within MAORY project Development of end-to-end simulation code optimised for GPU Study of wavefront sensing issues Design activities 8

9 Height (km) Field of view Wavefront sensing Sodium layer data kindly provided by Paul Hickson, University of British Columbia UTC (hrs) Spurious low-order aberrations seen by LGS WFS Monitored by NGS Reference WFS Preliminary analysis: residual wavefront error compatible with MAORY error budget. More detailed analysis required Detectors for LGS WFS: sampling, field of view Phase A: ~ pixel detector assumed, i.e pixels/subap. Alternative option under analysis: ~ pixel detector Trade-off between sampling and field of view in progress Spurious wavefront map seen by a LGS WFS due to Sodium layer and field truncation (tip, tilt, focus, astigmatism removed) 9

10 Wavefront sensor laboratory prototype Main features Multiple sources Arbitrary Sodium profile Sodium profile simulated by LCD light modulator Dynamic turbulence (2 layers) Low-order deformable mirror 10

11 AO test unit Some options to test AO performance Simulate turbulence by deformable mirrors Test with external turbulence simulator NGS sources Turbulence simulator design Segmented design NGS/LGS sources Turbulence screens M4/M5 emulated by software LGS sources NGS focus LGS focus Poster by Matteo Lombini 11

12 MAORY post-focal relay modified baseline optical design Science path Laser guide star path Light beam from E-ELT Focus for LGS WFS Post-focal deformable mirrors (~400 mm diameter). Baseline piezoelectric actuator technology. Under review. Gravity invariant exit port Development activities Adaptation to new E-ELT optical design Verification of interfaces to E-ELT and science instrument Feasibility of optical components Optimisation of LGS objective 12

13 Optical schemes for alternative deformable mirror technologies Optical designs for small ( 150 mm) deformable mirrors? Deformable mirror Main technical issues Longitudinal de-magnification Intermediate re-imaging is needed between two DMs Large tilt of layer image with respect to DM surface Difficult to obtain diffraction-limited optical performance Off-axis mirror with prime focus corrector 13

14 Optical schemes for alternative deformable mirror technologies Optical designs for large ( mm) deformable mirrors (e.g. voice-coil actuator)? To LGS objective Gravity invariant exit port LGS objective Main technical issue Larger volume than modified baseline design 14

15 Thank you for your attention 15

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