ASTR 511 (O'Connell) Lecture Notes


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 and image blur. 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. In the case of large mirrors or multiple-mirror designs, continual mechanical surface correction and alignment devices must be included.

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 extraordinarily 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 -- e.g. paraboloids and hyperboloids. 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.

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.


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.
GREGORIAN Parabola Ellipse (concave) Primary mirror focus before secondary. Focus below primary.
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 June 2017 by rwo

Copyright © 2000-2017 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.