New PDF release: Reflecting telescope optics. 1 : Basic design theory and its

By Wilson, Raymond N

ISBN-10: 3540589643

ISBN-13: 9783540589648

ISBN-10: 3540603565

ISBN-13: 9783540603566

This publication, written by way of the fashion designer of the worlds biggest telescope, the VLT in Chile, covers the fundamental glossy advancements in telescope optics. within the final 20 years, sleek know-how has revolutionized not just production and try tactics but additionally the complete quarter of caliber specification. as well as those issues, the ebook additionally covers the alignment of telescope optics, atmospheric optics, adaptive optics, reflective coatings, and ancillary apparatus. Richly illustrated, this paintings covers very important smooth options, which makes it some of the most entire references on telescope optics

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Extra info for Reflecting telescope optics. 1 : Basic design theory and its historical development

Example text

The Newton and Fizeau interferometers give fringes of equal thickness measuring directly the variations in an air (or glass) space. In the Haidinger interferometer, the thickness of the air (or glass) space is uniform and the source is of large angular size (Fig. 40). This gives circular fringes of equal inclination, formed at infinity. These are governed by Eq. 26) and are the exact equivalent of the basic circular fringes observed with a Michelson in- 48 1. 3 Test technology 49 Monochromatic source of light 6 Pinhole l>' Eye l:!

44. The beam expander expands the par­ allel laser beam to the beam size of the interferometer. Slight aberration here is uncritical as it is present in both interferometer arms. The beamsplitter operates at the Brewster angle and has a small wedge angle to avoid reflec­ tions from the front face. The beam diverger produces a divergent beam with negligib le spherical aberration at an f/no able to cover the steepest concave spherical mirrors to be tested (Fig. 44(a)). Aspheric test mirrors require a supplementary compensation or null system, whose function it is to produce an aberrated wavefront at the position of the test mirror of the same shape as the aspheric form required (Fig.

Fringes" can be dis­ played in real time, but they are no longer the physical intensity fringes: they are a calculated fringe pattern from the phase map measured. They can be manipulated as desired. The wavelength can be chosen at will, or a pre-defined wavefront can be subtracted. Because of the rapidity of short exposure times of the order of 20 milliseconds and a phase unwrapping time of 40 ms, a genuine real-time presentation is possible. A certain level of vi­ bration becomes an advantage, as it provides a sort of temporal heterodyne overlay which improves the averaging.

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Reflecting telescope optics. 1 : Basic design theory and its historical development by Wilson, Raymond N


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