Foucault knife-edge test

The Foucault knife-edge test is an optical test developed 150 years ago to accurately measure the shape of concave curved mirrors. It is commonly used by amateur telescope makers for figuring primary mirrors in reflecting telescopes. It uses a relatively simple, inexpensive apparatus compared to other testing techniques.

Foucault test setup to measure a mirror

Overview

The Foucault knife-edge test was described in 1858 by French physicist Léon Foucault as a way to measure conic shapes of optical mirrors.[1] It measures mirror surface dimensions by reflecting light into a knife edge at or near the mirror's centre of curvature. In doing so, it only needs a tester which in its most basic 19th century form consists of a light bulb, a piece of tinfoil with a pinhole in it, and a razor blade to create the knife edge. The testing device is adjustable along the X-axis (knife cut direction) across the Y-axis (optical axis), and is usually equipped with measurable adjustment to 0.001 inch (25 µm) or better along lines parallel to the optical axis.[2] The test can measure errors in a mirror's curvature to fractions of wavelengths of light (or Angstroms, millionths of an inch, or nanometers).[3][4]

Foucault test basics
From top: Parabolic mirror showing Foucault shadow patterns made by knife edge inside radius of curvature R (red X), at R and outside R.

Foucault testing is commonly used by amateur telescope makers for figuring primary mirrors in reflecting telescopes.[5][6] The mirror to be tested is placed vertically in a stand. The Foucault tester is set up at the distance of the mirror's radius of curvature (radius R is twice the focal length.) with the pinhole to one side of the centre of curvature (a short vertical slit parallel to the knife edge can be used instead of the pinhole). The tester is adjusted so that the returning beam from the pinhole light source is interrupted by the knife edge.

Viewing the mirror from behind the knife edge shows a pattern on the mirror surface. If the mirror surface is part of a perfect sphere, the mirror appears evenly lighted across the entire surface. If the mirror is spherical but with defects such as bumps or depressions, the defects appear greatly magnified in height. If the surface is paraboloidal, the mirror usually looks like a doughnut or lozenge although the exact appearance depends on the exact position of the knife edge.

It is possible to calculate how closely the mirror surface resembles a perfect parabola by placing a Couder mask,[7] Everest pin stick (after A. W. Everest)[8] or other zone marker[9] over the mirror. A series of measurements with the tester, finding the radii of curvature of the zones along the optical axis of the mirror (Y-axis). These data are then reduced and graphed against an ideal parabolic curve.

Other testing techniques
Main articles: Ronchi test and Interferometry

A number of other tests are used which measure the mirror at the center of curvature. Some telescope makers use a variant of the Foucault test called a Ronchi test that replaces the knife edge with a grating (similar to a very coarse diffraction grating) comprising fine parallel wires, an etching on a glass plate, a photograph negative or computer printed transparency. Ronchi test patterns are matched to those of standard mirrors or generated by computer.

Other variants of the Foucault test include the Gaviola or Caustic test which can measure mirrors of fast f/ratio more accurately than the Foucault test which is limited to about (λ/8) wavelength accuracy on small and medium-sized mirrors. The Caustic test is capable of measuring larger mirrors and achieving a (λ/20) wave peak to valley accuracy by using a testing stage which is adjusted from side to side so as to measure each zone of each side of the mirror from the center of its curvature.[10]

The Dall null test uses a plano-convex lens placed a short distance in front of the pinhole. With the correct positioning of the lens, a parabolic mirror appears flat under testing instead of doughnut-shaped so testing is much easier and zonal measurements are not needed.

There are a number of interferometric tests which have been used including the Michelson-Twyman and the Michelson method, both published in 1918, the Lenouvel method and the Fizeau method. Interferometric testing has been made more affordable in recent years by affordable lasers, digital cameras (such as webcams), and computers, but remains primarily an industrial methodology.

gollark: Yes.
gollark: I just think it is *not good* if it's working for someone else, generally seems actively hostile for user control, and also seems to slowly be trying to move to a subscription model.
gollark: Arch is somewhat annoying to set up, but it's probably paid back the time investment by teaching me Linux skills and not arbitrarily wasting my time for Microsoft.
gollark: You shouldn't have to work around it. OSes should let you actually use them and work for you, not for some company.
gollark: Well, it does. Because you have to put effort into that nonsense in the first place and it may break later.

See also

References
  1. Texereau 1984 pp.68-70 section 2.25
  2. Harbour 2008 p 39
  3. Texereau 1984 p.70 section 2.26
  4. Sacek, Vladimir (14 July 2006). "4.5.2. Foucault test". Notes on AMATEUR TELESCOPE OPTICS. Vladimir Sacek. Retrieved 18 December 2010.
  5. Texereau 1984 pp. 55-61 section 2.21
  6. Harbour, David A (July 2001). "Understanding Foucault: A Primer for Beginners (Second Edition)". The ATM's Workshop. Retrieved 18 December 2010.
  7. Designing and calculating Couder screens for Foucault testing Ken Slater and Nils Olof Carlin
  8. Stellafane ATM Build a Couder Mask; Build an Everest Pin Stick
  9. Harbour 2008 pp 49-51
  10. Baldwin, Jeff (September 2000). "The Caustic Test". Valley Skies. Stockton Astronomical Society. Archived from the original on July 28, 2011. Retrieved January 9, 2011.
  • Harbour, David A (July 2013). William J Welker (ed.). Understanding Foucault: A primer for beginners (2nd edition). Sapphire Publications. ISBN 978-1-62374-003-0.
  • Texereau, Jean (1984). How to Make a Telescope (second English edition). Richmond, VA: Willman-Bell. ISBN 0-943396-04-2.
  • Thompson, Allyn J (15 April 1947). Making Your Own Telescope. Cambridge, MA: Sky Publishing. ASIN B0007DK32U.

Further reading
  • L. Foucault, "Description des procedees employes pour reconnaitre la configuration des surfaces optiques," Comptes rendus hebdomadaires des séances de l'Académie des Sciences, Paris, vol. 47, pages 958-959 (1858).
  • L. Foucault, "Mémoire sur la construction des télescopes en verre argenté," Annales de l'Observatoire impériale de Paris, vol. 5, pages 197-237 (1859).
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.