1. Modern Observational/Instrumentation Techniques Astronomy 500
Andy Sheinis, Sterling 5520,
MW 2:30, 6515 Sterling
Office Hours: Tu 11-12

2. Telescopes What parameters define telescopes? Spectral range Area
Throughput
FOV
Image Quality
Plate scale/Magnification
Pointing/tracking

3. Telescopes Examples of telescopes? Refracting
Galilean (1610)
Keplerian (1611, 1834)
Astronomical
Terrestrial
Reflecting (4x harder to make!)
Newtonian
Gregorian (1663)
Cassegrain (1668)
Ritchey-Cretien (1672)
Catadioptric
Schmidt (1931)
Maksutov (1944)

5. A Omega name diameter FOV A omega M square degrees M^2 sq. degrees
SDSS
2.5
3.9
6.09
CFHT
3.6 1
3.24
Subaru
8.1
0.2
3.28
PanStarrs 7
22.68
LSST
6.5
73.94
SALT 10
0.003
0.07

8. Refractors/ Chromatic Aberration

9. Newtonian

10. Cassegrain

12. Spherical Primary

13. For a classical cassegrain focus or prime focus with a parabolic primary you need a corrector.
The Richey-Chretien design has a hyperbolic primary and secondary designed to balance out coma and spherical in the focal plane.

14. Optics Revisited

15. Where Are We Going? Geometric Optics Reflection Refraction
The Thin Lens
Multiple Surfaces
Matrix Optics
Principle Planes
Effective Thin Lens
Stops
Field
Aperture
Aberrations
Ending with a word about ray tracing and optical design.

16. Snell’s Law
Index = n Q
q’’ q P
Index = n’

17. Focal Length Defined C F F’ A’ Object at Infinity Definition
Application

18. ABCD Matrix Concepts Ray Description Basic Operations Two-Dimensions
Position
Angle
Basic Operations
Translation
Refraction
Two-Dimensions
Extensible to Three
Ray Vector
Matrix Operation
System Matrix

19. Ray Definition a1 x1

20. Translation Matrix
Slope Constant
Height Changes
a1=a2 x2 x1 z

21. Refraction Matrix (1) Height Constant Slope Changes (q Ref. to Normal)

22. Refraction Matrix (2)
Previous Result
Recall Optical Power

23. Cascading Matrices (1) Generic Matrix: Determinant (You can show that
this is true for cascaded matrices) V1 R1
T12 R2
V’2
Light Travels Left to Right, but
Build Matrix from Right to Left

24. The Simple Lens (Matrix Way)
Front Vertex,V
Back Vertex, V’
Index = n
Index = nL
Index = n’
z12

25. Building The Simple Lens Matrix
z12 V V’ n nL n’
Simple Lens Matrix

26. The Thin Lens Again
Simple Lens Matrix

27. Thin Lens in Air Again

28. Thick Lens Compared to Thin
z12 V V’ n nL n’

31. Imaging Cameras
Imagers can be put at almost any focus, but most commonly they are put at prime focus or at cassegrain.

32. The scale of a focus is given by S=206265/(D x f#) (arcsec/mm)
Examples:
3m @f/5 (prime) 13.8 arcsec/mm (0.33”/24µpixel)
1m @f/3 (prime) arcsec/mm (1.56”/24µpixel)
1m @f/17 (cass) arcsec/mm (0.29”/24µpixel)
(prime) 11.5 arcsec/mm (0.27”/24µpixel)
(cass) arcsec/mm (0.03”/24µpixel)
Classical cassegrain (parabolic primary + convex hyperbolic in front of prime focus) has significant coma.

33. Direct Camera design/considerations
LN2 can
Dewar
CCD
dewar window
Preamp
Shielded cable to controller
baffles
shutter
Filter wheel
Field corrector/ADC
Primary mirror

34. Shutters
The standard for many years has been multi-leaf iris shutters. As detectors got bigger and bigger, the finite opening time and non-uniform illumination pattern started to cause problems.
2k x 2k 24µ CCD is 2.8 inches along a diagonal.
Typical iris shutter - 50 milliseconds to open. Center of a 1s exposure is exposed 10% longer than the corners.

35. Shutter vignetting pattern produced by dividing a 1 second exposure by a 30 second exposure.

36. Double-slide system
The solution for mosaic imagers and large-format CCD has been to go to a 35mm camera style double-slide system.

37. Filter Wheel
Where do you put the filter? There is a trade off between filter size and how well focused dust and filter imperfections are.

38. Drift Scanning
An interesting option for imaging is to park the telescope (or drive it at a non-sidereal rate) and let the sky drift by.
Clock out the CCD at the rate the sky goes by and the accumulating charge ``follows’’ the star image along the CCD.

39. Drift Scanning
End up with a long strip image of the sky with a `height’ = the CCD width and a length set by how long you let the drift run (or by how big your disk storage is).
The sky goes by at 15 arcseconds/second at the celestial equator and slower than this by a factor of 1/cos(d) as you move to the poles.
So, at the equator, PFCam, with 2048 x 0.3” pixels you get an integration time per object of about 40 seconds.

40. Drift Scanning What is the point? Problem:
Superb flat-fielding (measure objects on many pixels and average out QE variations)
Very efficient (don’t have CCD readout, telescope setting)
Problem:
Only at the equator do objects move in straight lines, as you move toward the poles, the motion of stars is in an arc centered on the poles.
Sloan digital survey is a good example
Zaritsky Great Circle Camera is another

41. Direct Imaging Filter systems Photometry Point sources
Aperture
PSF fitting
Extended sources (surface photometry)
Star-galaxy separation

42. Filter Systems There are a bunch of filter systems
Broad-band (~1000Å wide)
Narrow-band (~10Å wide)
Some were developed to address particular astrophysical problems, some are less sensible.

43. 1.1µ silicon bandgap
3100Å is the UV atmospheric cutoff

44. Filter Choice: Example
Suppose you want to measure the effective temperature of the main-sequence turnoff in a globular cluster.
color relative time to reach dTeff=100
B-V
V-R
B-I
B-R ,7

45. Narrow-band Filters
Almost always interference filters and the bandpass is affected by temperature and beam speed:
DCWL = 1Å/5˚C
DCWL = 17Å; f/ f/2.8