1. 8 September 20151 Observational Astronomy TELESCOPES, Active and adaptive optics Kitchin pp.51-129

2. 2 Optical Schemes Spherical mirrors cannot focus light properly due to spherical aberrations:

3. 3 Optical Schemes … but a single parabola can produce perfect image on the optical axis: Off-axis images suffer from coma.

4. 4 Ritchey-Chrétien telescope Hyperbolic primary and hyperbolic secondary solve main aberration problems (spherical and coma) in a rather large field of view (tens of arcminutes) in Cassegrain focus

5. 5 Schmidt-Cassegrain RC provides very good image quality in a relatively small field (1º - 2º) When large FoV (up to 5º) is need Schmidt- Cassegrain is the preferred design: Spherical mirror Correction plate

6. 6 Alternative to RC: Gregorian system Concave secondary after the primary focus: Courtesy of AIP Potsdam

7. 7 Materials Low thermal expansion: zerodur & sitall mean linear coefficient of thermal expansion within temperature range -60 º to +60º С is <10 -8 cm º C -1 Astro-sitall blank at LZOS (VST, VISTA, SALT, LAMOST, OWL?) Zerodur VLT primary at REOSC

8. 8 More materials Silicon Carbide Low thermal expansion (not as good as glass) Very light Very hard, keeps the shape well Hard to make in large pieces Fragile, difficult to process SiC 60 cm X-ray mirror Weight: 6.2 kg

9. 9 Coatings Mirrors: Aluminum (forming SiO) on the top Silver-based coatings. Needs coating to prevent mechanical damage during washing Lenses: MgF 2

10. 10 Hard Gold coating results (from 0.7 µm to 25 µm) Wavelength (µm) EXAMPLES OF OPTICAL COATING Enhanced Silver coating results (from 350 nm to 800 nm) Wavelength (nm) Reflectivity

11. 11 Point Spread Function PSF is the intensity distribution in the focal plane produced by a point source. Ideal PSF (Bessel function)

12. 12 Active optics Large thin mirrors are shaped by support system: VLT mirror is 8.2m in diameter and only 18 cm thick ! Compensate for thermal and orientation distortions Close loop operation during adjustment Low frequency: 30 s cycle VLT: 150 actuators

13. 13 Adaptive optics Seeing corrections (PSF): The Strehl ratio is the ratio of peak intensities in the aberrated and ideal point spread functions in the focal plane (Born and Wolf 1999).

14. 14 Why do we need adaptive optics? Atmospheric turbulence distorts the wave front. Three ways of looking at the focal plane image: 1.Non-collimated beams (speckles) 2.Curved wavefront (phase shifts) 3.Changing intensity distribution

15. 15 Wavefront sensor Shack-Hartmann Curvature sensor Pyramid WFS Fast steering mirror is needed to get all pixels in focus

16. 16 Sensor implementation A corner of the 1cm x 1cm wavefront- sensor chip implemented in standard CMOS. The green elements are the position-sensitive detectors. Sensor chip on a printed- circuit board. Wavefronts must measured many at 100 kHz rate!

17. 17 Deformable mirror Various shapes of a deformable mirror with 37 actuators

18. 18 Calibrations Looking for a zero-point of DM:

19. 19 Closing the loop

20. 20 Laser Guide Star ab

21. 21 Final result VLT NACO: PSF and resolution improvements

22. 22 Home work Find a telescope with Silicon Carbide mirror. Why this material was used? When using adaptive optics what are the pluses and minuses of using natural and laser guide star?

23. 23 Next time… Direct Imaging and Photometry