1. A Short Presentation of Ongoing AO Work at Lund Observatory Mette Owner-Petersen Lund Observatory Workshop for “Forskarskolen i Rymdteknik” Gothenburg 12/9 – 13/9 Gothenburg Adaptive Optics

2. What is Adaptive Optics? Answer: Real-time Improvement of the Quality of Images which are degraded due to dynamical perturbations of the imaging system

3.  Peak Intensity (Strehl Ratio)  Resolution (FWHM)  Contrast (Background Level) Strehl Ratio: Detection of faint objects FWHM:Resolving bright objects in crowded fields Contrast:Direct Exo-Planet observation What is Meant by Image Quality? Point Image (PSF)

4. A Generic Example of Adaptive Optics

5. The Shack-Hartmann Wavefront Sensor Other design principles are possible

6. How it looks in Reality From the William Herschel telescope on La Palma

7. With and Without Adaptive Optics

8. Different AO Modes  Single Conjugate Adaptive Optics (SCAO). One DM and one guide star -> High Strehl but small corrected field.  Ground Layer Adaptive Optics (GLAO). The easy game. One DM and several guide stars -> Low Strehl but narrow FWHM over large field.  Multi Conjugate Adaptive Optics (MCAO). Several DMs and several guide stars -> High Strehl and large corrected field.  Extreme Adaptive Optics (ExAO). The hard bargain One DM and one Guide Star. Complicated filtering in both image and pupil plane -> Extremely high contrast.

9. SCAO versus MCAO Uncorrected SCAO MCAO

10. How to Make it Work  Analytical performance evaluation  Confirmation by simulations  Lab verifications if needed  Optical modeling  “The real thing”

11.  Simulations of AO perfomance for the Euro50. Integrated modeling PhD project for Anita Enmark  DCAO on the Lunda – Moon and for terrestrial applications Collaboration with Dept. of Applied Optics in Galway and FOI Sweden PhD project for Per Knutsson  DCAO for wide - field retinal imaging Collaboration with Dept. of Ophthalmology in Gothenburg  Previous: Analytical performance evaluations Experimental verification of expected DCAO performance Ongoing AO Work

12. Correction for Atmosphere La Palma 7-Layer Model 0 s < t < 0.1 sNo AO correction 0.1 s < t < 0.6 sSlow correction for Focus & Tip/tilt 0.6 s < t < 1.1 sAO ON Specification for AO: Strehl > 0.58 Euro50 PSF @ λ=2.2 μm Scale 0  0.3

13. The Moon DCAO Experiment Zemax Model Celestron DM1 0 km DM2 10 km Sci. Cam. Tip /Tilt WFS

14. Wide Field Retinal Imaging First light very soon!

15. Goal of the experiment: Emulation of K – band performance of SCAO, GLAO and DCAO on a 7.5 m telescope 5 guide stars in a cross Specific Address: Field gain going from SCAO to DCAO The Lund DCAO Demonstrator