8 september 20151 observational astronomy telescopes, active and adaptive optics kitchin pp.51-129
TRANSCRIPT
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Observational Astronomy
TELESCOPES,Active and adaptive
opticsKitchin pp.51-129
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Optical Schemes
Spherical mirrors cannot focus light properly due to spherical aberrations:
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Optical Schemes
… but a single parabola can produce perfect image on the optical axis:
Off-axis images suffer from coma.
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Ritchey-Chrétien telescope
Hyperbolic primary and hyperbolic secondary solve main aberration problems (sphericaland coma) in a rather large field of view(tens of arcminutes) in Cassegrain focus
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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
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Alternative to RC:Gregorian
system
Concave secondary after the primary focus:
Court
esy
of
AIP
Pots
dam
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Materials
Low thermal expansion: zerodur & sitall
mean linear coefficient of thermal expansion within temperature range-60º to +60º С is <10-8 cm ºC-1
Astro-sitall blank at LZOS(VST, VISTA, SALT, LAMOST, OWL?) Zerodur VLT primary at
REOSC
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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 mirrorWeight: 6.2 kg
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Coatings
Mirrors: Aluminum (forming SiO) on the
top Silver-based coatings. Needs
coating to prevent mechanical damage during washing
Lenses: MgF2
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Hard Gold coating results (from 0.7 µm to 25 µm)
Wavelength (µm)
EXAMPLES OF OPTICAL COATINGEnhanced Silver coating results (from 350 nm to 800 nm)
Wavelength (nm)
Ref
lect
ivit
yR
efle
ctiv
ity
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Point Spread Function
PSF is the intensity distribution in the focal plane produced by a point source.
Ideal PSF (Bessel function)
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Active optics
Large thin mirrors are shaped bysupport system: VLT mirror is8.2m in diameterand only 18 cm thick! •Compensate for
thermal and orientation distortions
•Close loop operation during adjustment
•Low frequency:30 s cycle
•VLT: 150 actuators
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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).
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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
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Wavefront sensor
Shack-Hartmann Curvature sensor Pyramid WFS
Fast steering mirror is neededto get all pixels in focus
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Sensor implementation
A corner of the 1cmx1cm 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!
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Deformable mirror
Various shapes of a deformable mirror with 37 actuators
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Calibrations
Looking for a zero-point of DM:
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Closing the loop
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Laser Guide Star
a b
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Final result
VLT NACO:PSF and resolutionimprovements
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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?
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Next time…
Direct Imaging and Photometry