ASTR 511 (O'Connell) Lecture Notes



TELESCOPE OPTICAL DESIGN


Hevelius 140-foot Telescope (ca. 1675)



Telescope optical design is covered in detail in ASTR 512, so we give only a flavor of what is involved here.


A. Overview

The usual goal of telescope optics design is to bring all light rays, arriving at the primary element from a large range of field angles, to a sharp focus in a flat focal plane. The image should be a faithful one-to-one reproduction of the angular distribution of light in the source with minimal geometric distortion. The image representation should be independent of the wavelength of the light rays (i.e. achromatic).

But it is not possible to accomplish this. One can never build a perfect optical device. Any realized design is always a compromise because it is not possible to control for all optical aberrations at will.

Therefore, modern telescope design is essentially a process of successive approximations in aberration control in 3 dimensions. Fortunately, a number of highly capable software packages are now available to mitigate the pain of doing this.

The picture at the top of this page shows how early telescope builders tried to control for two major aberrations in crude lenses: (1) chromatic aberration and (2) spherical aberration. The effects of both of these aberrations diminish with focal length....hence the very long focal length of Hevelius' telescope.

The modern solution to chromatic aberration in refractive optics is to use mirrors rather than lenses, and most large telescopes employ mirrors as their primary optics. However, most optical instruments must also include refractive elements in order to achieve wavelength selection or wide-field images, so chromatic aberration is still almost always an issue.

The modern solution to spherical aberration (the fact that parallel light rays striking the surface of a sphere do not come to a single focus) is to use non-spherical optics, especially paraboloids. Rays parallel to the axis of a parabolic reflector come to a perfect focus. Unfortunately, off-axis rays do not, and this leads to a comet-shaped aberration known as coma, which becomes worse with field angle.

  • Coma can be reduced by using a refractive corrector near the focal plane of a parabolic primary.

  • A widely-used alternative is the Ritchey-Chretien design, a Cassegrain system that employs two hyperbolic mirrors yielding zero first-order coma and spherical aberration. RC's are affected, however, by third-order coma, astigmatism, and field curvature (at larger field angles).

  • Another famous alternative for control of spherical aberration over a wide field with a spherical primary is to use a special full-aperture refractive correcting plate called a Schmidt corrector. The Schmidt sky-survey telescopes employ these.


B. Sample Ray Traces

Click below for illustrations of ray traces for spherical and parabolic reflectors. These show light paths for parallel incoming rays in a plane containing the symmetry axis of the mirror. They are for fast optical systems (small f/ ratios, where f/ = Focal Length/Diameter), so that aberrations are larger than for typical designs. You can see that, except for the case of a parabola and paraxial rays, it is not possible to find a good focal point anywhere in these systems.




STANDARD TELESCOPE OPTICAL CONFIGURATIONS


TYPE PRIMARY MIRROR SECONDARY MIRROR COMMENTS
PRIME FOCUS Parabola   Focus inside telescope
Add refractive corrector for wide field
NEWTONIAN Parabola Flat Focus at side/top of telescope
CASSEGRAIN Parabola Hyperbola (convex) Focus below primary
RITCHEY-
CHRETIEN
Hyperbola Hyperbola (convex) Focus below primary. Zero coma & spherical aberration
COUDE Various Various Tertiary flat directs light to fixed focus below polar axis
NAYSMITH Various Various (Alt-Az): Tertiary flat directs light to focus outside altitude axis
SCHMIDT Spherical   Catadioptric: Uses refractive corrector to provide wide field without spherical aberration. Focus inside telescope body


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Last modified July 2007 by rwo

Copyright © 2000-2007 Robert W. O'Connell. All rights reserved. These notes are intended for the private, noncommercial use of students enrolled in Astronomy 511 at the University of Virginia.