The Reflecting telescope reference article from the English Wikipedia on 24-Apr-2004 (provided by Fixed Reference: snapshots of Wikipedia from wikipedia.org)

Reflecting telescope

A reflecting telescope (reflector) is an optical telescope which uses mirrors, rather than lenses, to reflect light. The British scientist Sir Isaac Newton (1643-1727) designed the first reflector; in order to solve problems, such as chromatic aberration, which occurred with the refracting telescopes of the time before the perfection of achromatic lenses. The traditional two-mirrored reflector is known as a Newtonian reflector.

While still used in amateur astronomy, professionals now tend to use prime focus, Cassegrain focus, and coudé focus designs. On Earth (by 2001), there were at least 49 reflectors with primary mirrors having diameters of 2m+.

Table of contents

1 Technical Difficulties 2 Notable Reflectors 3 The Prime Focus 4 The Cassegrain Focus 5 The Coudé Focus

Technical Difficulties

Reflecting telescopes do not have as many technical issues, as do the refracting telescopes; they are also less expensive for the same light-gathering power. In addition, reflectors which have spherical mirrors (rather than parabolic mirrors) tend to suffer from spherical aberrations. These aberrations can be corrected with a Schmidt corrector plate; however, corrected non-parabolic reflectors still lack the magnification-power of parabolic reflectors.

Nearly all large research-grade astronomical telescopes are reflectors. This is for several reasons:

• In a lens the entire volume of material has to be free of imperfection and inhomogeneities, whereas in a mirror, only one surface has to be perfectly polished.
• Light of different colors travels through a medium other than vacuum at different speeds. This causes chromatic aberration in uncorrected lens and creating an aberration-free large lens is a costly process.
• There are technical difficulties involved in manufacturing and manipulating large-aperture lenses. One of them is that a lens can only be held by its perimeter such that the sag due to gravity is sufficient to distort the image. A mirror, on the other hand, can be supported by the whole side opposite to its reflecting face.

Notable Reflectors

• W.M. Keck telescopes (Hawaii)

The Prime Focus

In a prime focus design, the astronomer, nowadays the CCD camera, sits inside the telescope, at the focal point of the reflected light.

The Cassegrain Focus

Designs with a Cassegrain focus have a hole drilled through the primary mirror and a mirror, placed where the astronomer would sit in a prime focus telescope, refleces light through the hole.

The Coudé Focus

In a coudé design, the design is similar to the Cassegrain except no hole is drilled in the primary mirror; instead, a third mirror reflects the light to the side.

• The Newtonian has a parabolic primary mirror, and a flat secondary that reflects the focal plane to the side of the top of the telescope tube. It is one of the simplest and least expensive designs for a given size of primary, and is popular with amateurs. Since the light path is unfolded, the tube is quite long and heavy. The parabolic mirror is difficult to produce with accuracy. Some amateurs produce a spherical mirror, and live with the spherical aberration. The spider supporting the secondary mirror often introduce diffractive effects that cause stars to appear to "flare" in four or six directions.

• The Cassegrain has a spherical primary mirror, and a spherical secondary mirror that reflects the light back down through a hole in the primary. This is one of the most attractive designs. The folded optics make the telescope compact. The secondary corrects spherical aberration introduced by the spherical primary. The secondary mirror introduces a diffraction pattern that seems to create a ring around stars. The spherical mirrors are easy to produce with automatic equipment. On smaller telescopes, and camera lenses, the secondary is often mounted on an optically-flat, optically-clear glass plate that closes the telescope tube. This support eliminates the "star-shaped" diffraction effects caused by a support spider. The closed tube stays clean, and the primary is protected, at some loss of light-gathering power.

• The Maksutov is similar to the Cassegrain. It starts with an optically transparent corrector lens that is a section of a hollow sphere. It has a spherical primary mirror, and a spherical secondary that is often just a mirrored section of the corrector lens. Maksutovs are mechanically simpler than small Cassegrains, have a closed tube and all-spherical optics.
  • One very popular luxury telescope design was the Celestron. It ran a "finder" scope and the main scope to the same eyepiece. It had a 10cm Maksutov reflector as the main telescope. The finder was a 2.5 cm refractor. The focal plane of the reflector and refractor were the same (probably the refractor had a factory adjustment). A flat-mirror near the bottom reflected light to the finder's primary, and a movable mirror at the back of the 10-cm cassegrain hole switched the optical path of the large telescope between the eyepiece and the camera attachment on the back. When the camera was engaged, the finder-scope was operational.

• The Ritchey-Chrétien is a specialized Cassegrain reflector with the advantage that it is coma free. This is why almost every professional reflector telescope in the world is of the Ritchey-Chrétien design. It was invented by George Willis Ritchey and Henri Chrétien in the early 1910s.

• The Schmidt-Cassegrain is a classic wide-field telescope. 30 inch Schmidt-cassegrains are used for sky surveys at astronomical observatories and satellite tracking stations. The first optical element is a "schmidt corrector plate." The plate is figured by placing a vacuum on one side, and grinding the exact correction required to fix the spherical correction. The primary mirror is spherical.

• One exception to the supremacy of Ritchey-Chrétien telescopes for professional use are Schmidt cameras. These instruments have a very wide field, a sharp focus, about 30 times greater than Ritchey-Chrétien, with the drawbacks that the focus is inaccessible, making them usable only as cameras, and contrary to Cassegrain, they have their physical length at least twice their focal length. Their optical performance comes from the use of a spherical mirror which reintroduces the spherical and field curvature aberrations, but avoids all the others. The spherical aberration is overcome by using a corrector lens in front of the telescope at the radius of the curvature of the mirror. The field curvature are compensated with a film-holder that stretches the film into a mild spherical shape.

An unusual variant of the Cassegrain is the Schiefspiegler telescope which uses tilted mirrors to avoid the secondary mirror casting a shadow on the primary, however, while eliminating diffraction patterns, this leads to several other abberations that must be corrected for.

Radio telescopes have a parabolic metal surface that reflects the radio waves, rather than light rays, towards the actual antenna. The largest single-piece antenna is the Arecibo radio telescope in Puerto Rico.

This is the "Reflecting telescope" reference article from the English Wikipedia. All text is available under the terms of the GNU Free Documentation License. See also our Disclaimer.