1. Page 1 Introduction to Adaptive Optics Antonin Bouchez (with lots of help from Claire Max) 2004 Observatory Short Course

2. Page 2 Outline Why do we need adaptive optics?Why do we need adaptive optics? How is it supposed to work?How is it supposed to work? How does it really work?How does it really work? Astronomy with adaptive optics.Astronomy with adaptive optics.

3. Page 3 Why do we need adaptive optics? Even the largest ground-based astronomical telescopes have no better resolution than an 8" telescope! Even the largest ground-based astronomical telescopes have no better resolution than an 8" telescope! Turbulence in earth’s atmosphere makes stars twinkle More importantly, turbulence spreads out light; makes it a blob rather than a point

4. Page 4 Optical consequences of turbulence

5. Page 5 Optical consequences of turbulence Temperature fluctuations in small patches of air cause changes in index of refraction (like many little lenses)Temperature fluctuations in small patches of air cause changes in index of refraction (like many little lenses) Light rays are refracted many times (by small amounts)Light rays are refracted many times (by small amounts) When they reach telescope they are no longer parallelWhen they reach telescope they are no longer parallel Hence rays can’t be focused to a point:Hence rays can’t be focused to a point: Parallel light rays Light rays affected by turbulence  blur  Point focus

6. Page 6 Kolmogorov turbulence cartoon Outer scale L 0 ground Inner scale l 0 h convection solar h Wind shear

7. Page 7 Turbulence arises in several places stratosphere tropopause Heat sources w/in dome boundary layer ~ 1 km 10-12 km wind flow over dome

8. Page 8 Short exposures through the atmosphere What a star really looks like through a large (6 m) telescope.

9. Page 9 Long exposures through the atmosphere

10. Page 10 Light rays and the wavefront Parallel light raysLight rays affected by turbulence  blur  Point focus

11. Page 11 Light rays and the wavefront Parallel light raysLight rays affected by turbulence  blur  Point focus

12. Page 12 Characterize turbulence strength by quantity r 0 “Coherence Length” r 0 : distance over which optical phase distortion has mean square value of 1 rad 2 “Coherence Length” r 0 : distance over which optical phase distortion has mean square value of 1 rad 2 r 0 ~ 15 - 30 cm on Mauna Kear 0 ~ 15 - 30 cm on Mauna Kea Primary mirror of telescope r0r0 “Fried’s parameter” Wavefront of light

13. Page 13 Imaging through a telescope With no turbulence, FWHM is diffraction limit of telescope, ~ / D Example: / D = 0.02 arc sec for / D = 0.02 arc sec for = 1  m, D = 10 m = 1  m, D = 10 m FWHM ~ /D in units of /D 1.22 /D Point Spread Function (PSF): intensity profile from point source 10m 0.02"

14. Page 14 Imaging through a telescope With turbulence, FWHM is diffraction limit of regions of coherent phase, ~ / r 0 Example: / r 0 = 0.80 arc sec for / r 0 = 0.80 arc sec for = 1  m, r 0 = 25 cm = 1  m, r 0 = 25 cm FWHM ~ /r 0 in units of /D Point Spread Function (PSF): intensity profile from point source 10m 0.80"

15. Page 15 How does adaptive optics help? (cartoon approximation) Measure details of blurring from “guide star” near the object you want to observe Calculate (on a computer) the shape to apply to deformable mirror to correct blurring Light from both guide star and astronomical object is reflected from deformable mirror; distortions are removed

16. Page 16 Simplified AO system diagram

17. Page 17 How a deformable mirror works (idealization) BEFORE AFTER Incoming Wave with Aberration Deformable Mirror Corrected Wavefront

18. Page 18 Most deformable mirrors today have thin glass face- sheets Anti-reflection coating Glass face-sheet PZT or PMN actuators: get longer and shorter as voltage is changed Cables leading to mirror’s power supply (where voltage is applied) Light

19. Page 19 Simplified AO system diagram

20. Page 20 How to measure turbulent distortions (one method among many) Shack-Hartmann wavefront sensor

21. Page 21 Simplified AO system diagram

22. Page 22 A real AO system: Keck 1 & 2 Tip-tilt mirror Deformable mirror Wavefront sensor

23. Page 23 Keck II Left Nasmyth Platform Elevation Ring Enclosure with roof removed Electronics Racks Adaptive Optics Bench Nasmyth Platform Science cameras

24. Page 24 The adaptive optics bench Tip/tilt Mirror Deformable Mirror To wavefront sensor IR Dichroic To near-infrared camera

25. Page 25 Deformable mirror Front view Rear view 15cm

26. Page 26 Wavefront Sensor AOA Camera Sodium dichroic/beamsplitterField Steering Mirrors (2 gimbals) Camera Focus Wavefront Sensor Focus Wavefront Sensor Optics: field stop, pupil relay, lenslet, reducer optics

27. Page 27 6 AO systems on Mauna Kea! Summit of Mauna Kea volcano in Hawaii: Subaru 2 Kecks Gemini North CFHT UH 88"

28. Page 28 An adaptive optics system in action: Keck 2

29. Page 29 Neptune in infra-red light (1.65 microns) Without adaptive optics With Keck adaptive optics June 27, 1999 2.3 arc sec May 24, 1999

30. Page 30 Adaptive optics in astronomy Planetary sciencePlanetary science –Volcanoes on Io –Methane storms on Titan Dense star fieldsDense star fields –Black hole at the center of our galaxy –Star population in globular clusters High-contrast imagingHigh-contrast imaging –Faint material around bright stars (disks of dust, etc.) –Extra-solar planets and super-planets Studying very distant galaxies.Studying very distant galaxies.

31. Occultation of a binary star by Titan Hubble Space Telescope image

32. Occultation of a binary star by Titan Images taken with the Palomar Observatory 200" AO system. One image taken every 0.843 seconds - 4700 images total. Titan's atmosphere refracts the starlight, forming multiple images of each star! Result: winds in Titan's stratosphere are very strong: ~250 m/s in a jet-stream type pattern.

33. Orbits of stars around the black hole at the center of our galaxy Result: Black hole at center of the galaxy has a mass of 2.6 million suns.

34. Mid-infrared flares from the black hole at the center of our galaxy Result: Direct detection of heat released by material falling on the accretion disk surrounding the black hole.

35. Searching for planets around Epsilon Eridani

36. Result: They're all background stars!

37. Studying the star populations of galaxies at z~0.5 Result: Galaxies were brighter than today, but about the same size.

38. Page 38 Sodium laser guidestars Rayleigh scattered light Light from Na layer at ~ 100 km Max. altitude of Rayleigh ~ 35 km

39. Page 39 Keck 2 laser

40. Page 40 First images with Keck laser-guidestar adaptive optics HK Tau B hidden behind an edge-on disk of dust. HK Tau A (10 6 yr old T- tauri star)