1. Widening the Scope of Adaptive Optics Matthew Britton

2. The Seeing Limit

3. Atmospheric Turbulence

4. Wavefront phase Seeing limited image Diffraction limited image

5. Long Exposure PSFs Diffraction limit Seeing limit Seeing limit (x40) Angular Resolution ~ D 0 Point source Sensitivity ~ D 2 Angular Resolution ~ D Point source Sensitivity ~ D 4

6. Palomar Seeing on Aug 20, 2005

7. Turbulence Profiles

8. Diffraction Limited PSFs

9. Seeing Limited PSFs

10. Adaptive Optics

12. NGC 7469 (CFHT) Neptune (Keck) NGC 3603 (VLT)

13. Anisoplanatism

15. Modeling the PSF OTF oa = OTF gs * ATF

16. An Experiment at Palomar

17. Observations of a 21” Binary Guide Star Companion OTF gs * ATF = OTF oa Turbulence theory C n 2 profile measurements

18. Why is this experiment important? Establish consistency of DIMM/MASS measurements and AO PSFs Test theoretical formulation of anisoplanatism If successful, allows PSF predictions over wide fields.

19. Observed and Predicted PSFs

20. Strehl Ratios vs. Time

21. Predicted vs. Measured Strehls

22. Differential Photometry and Astrometry M(x,y) = A P(x+  x,y+  y) A - differential photometry  x,  y - differential astrometry

23. Fitting the Observation I(r) = OTF gs (r) + d * OTF oa (r) * exp{i  r} d = differential photometry  = differential astrometry

24. Fit Residuals

25. Differential Photometry 2.12  m.7903 +/-.0004 1.65  m.8316 +/-.0007 Relative Intensity

26. Differential Astrometry 2.12  m 21.3322 +/-.0006282.3923 +/-.0011 1.65  m 21.3306 +/-.0012282.3932 +/-.0023  

27. Observations of a Quadruple

28. Modelling the Observation

29. LGS Adaptive Optics

30. Laser Tilt Indeterminacy Pilkington 1987 (Nature)

31. Adaptive Optics with Lasers

32. LGS PSFs on a 10 m Aperture

33. Keck LGS observation Of M5 (Courtesy of the CfAO Treasury Survey)

34. Advanced Wide Field Adaptive Optics

35. A Preliminary Comment Field dependence of the AO system performance is a function of: Aperture diameter Observing wavelength Guide star configuration How the adaptive mirrors are deployed Zenith angle Turbulence conditions (-> time)

36. Single Laser AO (SLGLAO) Poor to moderate performance over a modest field FOV = 70” (D / 30 m)(90 km / h)

37. Ground Layer AO (GLAO) Poor performance Field uniformity

38. Tomography

39. Laser Tomography AO (LTAO) Good performance on axis

40. Multiconjugate AO (MCAO) Good performance over 30” field

41. Multiobject AO (MOAO) Intermediate performance over 5’ field

42. Conclusions There are a number of ways to provide wide field AO compensation. Postprocessing using turbulence profiles XXAO At least one of them is likely to work for your observations…