Ground- and Space-Based Telescopes. Dr. Vithal Tilvi

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1 Ground- and Space-Based Telescopes Dr. Vithal Tilvi

2 Telescopes and Instruments Astronomers use telescopes to gather light from distant objects and instruments to record the data

3 Telescopes gather light and resolve detail A telescope is sometimes called a light bucket. Number of photons collected per second is proportional to the area of the lens/ mirror: Area = π/4 x D 2 where D = diameter of the lens/mirror.

4 Focal Points and Focal Lenghts Snell s law: the angle of incidence measured between two media (air, glass) is given by n1λ sin θ1= n2λ sin θ2 Focal point: the point where all light rays converge (or from where they diverge) Focal Length, fλ: given by 1 f λ =(n λ 1) 1 R R 2

5 Focal Points and Focal Lenghts Sign of convention for R (radii of curvature) in 1 f λ =(n λ 1) 1 R R 2 In case (a), R1 > 0, R2 > 0 and in case (b), R1 < 0, R2 < 0

6 Focal Points and Focal Lenghts Two kinds of mirrors: (a) a converging mirror, f > 0, (b) a diverging mirror, f < 0.

7 Focal Points and Focal Lenghts Focal Plane (out of the page) Focal Plane: a plane passing through the focal point and oriented perpendicular to the optical axis of the system. All light rays are essentially parallel at the focal plane.

8 Focal Points and Focal Lenghts Focal Plane (out of the page) Plate scale: relates the angular separation of the objects with linear separation of their images at the focal plane. As the focal plane is increased, the linear separation of the images of two point sources separated by an angle θ also increases.

9 Focal Points and Focal Lenghts Focal Plane (out of the page) For two point sources separated by a distance θ, simple geometry gives their distance on the focal plane as: y = f tan( θ ), or y fθ where the approximation is valid if the field of view of the telescope is small. The Plate Scale is: dθ dy = 1 f

10 Resolution Resolution: Our ability to see two objects separated by an angle θ. For two light rays traveling to the focal plane, if they are one-half wavelength (λ/2) destructive interference occurs: D 2 sin θ = λ 2 Now consider dividing the aperture (given by D) into 4 pieces, where we pair up a light ray from the edge of the opening with one passing through a point one-quarter of a slit width away. Destructive interference occurs for: In general, destructive interference occurs from light passing through an aperture if the following is met: D 4 sin θ = λ 2 or sin θ =2 λ D sin θ = m λ D

11 Resolution In general, destructive interference occurs from light passing through an aperture if the following is met: Intensity sin θ = m λ D Dark fringes occur when m=integers m= Circular apertures act the same way, but involved more complicated math to compute locations of peaks. The intensity and locations of the minima and maxima are given by: Ring m I / I0 central max st minimum nd max nd min rd max rd min 3.238

12 Resolution Circular apertures act the same way, but involved more complicated math to compute locations of peaks. The intensity and locations of the minima and maxima are given by: Ring m I / I0 central max st minimum nd max nd min rd max rd min 3.24 This gives a minimum resolution to resolve two point sources: (a) sources are resolved. (b) sources are barely resolved (c) sources are unresolved

13 Resolution This gives a minimum resolution to resolve two point sources: (a) sources are resolved. (b) sources are barely resolved (c) sources are unresolved Rayleigh criterion is the minimum angular separation to resolve two point sources, given (for small angle approximation) at location of first minimum, where m = 1.22 for circular apertures: θ min =1.22 λ D where λ is the wavelength of light, and D is the diameter of the telescope mirror This is the Diffraction Limit

14 Resolution 10 o 1 o 10 1

15 What is the resolution of the human eye? Get together in groups On a piece of paper, draw two small dots very close together Move the paper away until another group member can no longer see that there are two dots Calculate the angular resolution of your eye by estimating the separation between the dots and dividing by the distance from your eye to the unresolved dots on the piece of paper Convert this number (which is in radians) to arcminutes

16 Seeing Unfortunately, the Earth s atmosphere usually sets the limit to how refined we can make the resolution. This is set by Turbulence in the atmosphere, which blurs light. We call this Seeing. Good sights in the world normally achieve seeing ~1. At the best sights in the world, like Mauna Kea in Hawaii or the mountains in Northern Chile, the median seeing is ~ The Hubble Space Telescope, which is most of the atmosphere, achieves the diffraction limit. It has a D=2.4 m primary mirror. At a wavelength of 1 micron (10-6 m) HST achieves a diffraction limit of: θ min =1.22 λ D = m 2.4m = rad = 0.10 which is 5-10x better than what is achievable on Earth.

17 Two types of telescopes: refractor vs. reflector Galileo s telescope Newton s telescope

18 Refracting telescopes A convex lens (thicker in the middle) focuses light to a point: Light from a large area is funnelled into a small area.

19 Refracting telescopes Galilean telescope design

20 The world s largest refracting telescope Yerkes Observatory, Wisconsin 1 meter diameter Completed 1897

21 Reflecting telescopes Newtonian telescope, 1668

22 Cassegrain telescope design Secondary Primary Focus

23 Gregorian telescope design Secondary Primary Focus

24 Reflecting telescopes Reflective mirrors, rather than large lenses, are often used for large telescopes who can think of why this might be?

25 The world s biggest telescopes are reflectors (mirrors), not refractors (lenses). The problem with lenses: 1) Lenses absorb light. 2) Lenses sag. 3) Lenses have chromatic aberration: colors do not focus at same point.

26 Reflecting telescopes A mirror shaped like a parabola focuses light to a point: Light from a large area is funneled into a small area. Lenses and mirrors (if shaped correctly) produce an accurate image of an object.

27 Historical telescopes Astronomers have been using telescopes to study the night sky since Galileo s time

28 Historical telescopes Astronomers have been using telescopes to study the night sky since Galileo s time Remember: bigger mirrors = more collecting power and higher angular resolution

29 Herschel Telescope (1789) Newtonian Wilson design Fig metal primary mirror

30 Mt. Wilson 100 Hooker telescope (1917)

31 Palomar 200 Hale telescope (1949)

32 Modern optical telescopes

33 Modern optical telescopes Bigger mirrors = more collecting power and better angular resolution

34 Modern optical telescopes Bigger mirrors = more collecting power and better angular resolution

35 McDonald Observatory

36 Gemini, VLT Gemini: 2x8m VLT: 4x8.2m

37 Keck Telescopes Twin 10 meter telescopes on Hawaii s Mauna Kea. Built by U California and Cal Tech. Commissioned 1992, 1996.

38 SDSS

39 Large Binocular Telescope 2x8.4m on single mount

40 Magellan

41 Giant Magellan Telescope 25 meter diameter, first light in 2018 Texas A&M is a founding partner in GMT! (Prof Papovich is at a meeting at Harvard about this right now)

42 Infrared, UV, X-ray, Radio Telescopes The Atmosphere has different windows that are transparent and opaque to light at different wavelengths: We can observe in the Visible, certain spots in the IR, and in the Radio easily. Other wavelengths (far-ir, UV, X-ray) we have to go to space.

43 NASA s Great Observatories Compton γ-ray Observatory Gamma Ray Telescope Hubble Space Telescope 1990-? UV, optical some IR Chandra X-ray Observatory 1999-? X-ray. Spitzer Space Telescope 2003-? Mid/Far-Infrared.

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