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2. Bath interferometer (common path) - Wikipedia

   en.wikipedia.org/wiki/Bath_interferometer...

   Bath interferometers can be used to test telescope mirrors of any size. A Common path interferometer has the test and reference beams traveling over effectively the same path which has the advantage that you can use an inexpensive semiconducting laser pointer with low coherence versus other interferometers which need a high coherence laser ...

3. Secondary mirror - Wikipedia

   en.wikipedia.org/wiki/Secondary_mirror

   A secondary mirror (or secondary) is the second deflecting or focusing mirror element in a reflecting telescope. Light gathered by the primary mirror is directed towards a focal point typically past the location of the secondary. [1] [2] Secondary mirrors in the form of an optically flat diagonal mirror are used to re-direct the light path in ...

4. List of telescope parts and construction - Wikipedia

   en.wikipedia.org/wiki/List_of_telescope_parts...

   Objective: The first lens or curved mirror that collects and focuses the incoming light. Primary lens: The objective of a refracting telescope. Primary mirror: The objective of a reflecting telescope. Corrector plate: A full aperture negative lens placed before a primary mirror designed to correct the optical aberrations of the mirror.

5. Ritchey–Chrétien telescope - Wikipedia

   en.wikipedia.org/wiki/Ritchey–Chrétien_telescope

   A Ritchey–Chrétien telescope (RCT or simply RC) is a specialized variant of the Cassegrain telescope that has a hyperbolic primary mirror and a hyperbolic secondary mirror designed to eliminate off-axis optical errors . The RCT has a wider field of view free of optical errors compared to a more traditional reflecting telescope configuration.

6. Chopping (astronomy) - Wikipedia

   en.wikipedia.org/wiki/Chopping_(astronomy)

   This telescope utilized its Second Mirror Assembly (SMA) primarily for chopping and also partially for small corrections. The signals that the SOFIA Telescope would be searching for could be tens of thousands of times less significant than the background emission , so the telescope has an average chopping frequency of 2-5 Hz , but can reach ...

7. Schmidt camera - Wikipedia

   en.wikipedia.org/wiki/Schmidt_camera

   The Mersenne–Schmidt camera consists of a concave paraboloidal primary mirror, a convex spherical secondary mirror, and a concave spherical tertiary mirror. The first two mirrors (a Mersenne configuration) perform the same function of the correcting plate of the conventional Schmidt. This form was invented by Paul in 1935. [24]