Schmidt corrector plate
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A Schmidt corrector plate, invented by Bernhard Schmidt in 1931[1], is an aspheric lens used to correct spherical aberration in a catadioptric telescope that uses a spherical primary mirror. The corrector is placed in front of the mirror and intercepts the light as it enters the telescope. It is placed at the center of curvature of the mirror for a pure Schmidt camera and just behind the prime focus for a Schmidt-Cassegrain. The Schmidt corrector is thicker in the middle and the edge. This corrects the light paths so light reflected from the outer part of the mirror focuses at the same point as light reflected from the inner portion of the mirror. The Schmidt corrector only corrects for spherical aberration. It does not change the focal length of the system.
The curve of the Schmidt corrector is complex but is produced using a fairly simple method. The thin glass is ground and polished to an accurate flat form (figured) on one side. The plate is placed in a vacuum device with the polished flat-side-down, and a vacuum is used to distort the plate making the unfigured side concave to a precise curve. The unpolished side is then ground and polished flat. When the vacuum is released the plate springs back to its original shape but now the originally flat side is flat again and the other side has the complex shape needed for the corrector. The corrector is mounted with the flat side toward the mirror.
[edit] See also
[edit] References
- ^ Wright, Franklin B. (1959). "Theory and Design of Aplanatic Reflectors Employing a Correcting Lens". in Ingalls, Albert G.. Amateur Telescope Making Advanced. Scientific American. pp. 401-409.
