In astronomical
telescope mounts, the equatorial axis (the
right ascension) is paired with a second
perpendicular axis of motion (known as the
declination). The equatorial axis of the mount is often equipped with a motorized "
clock drive", that rotates that axis one revolution every 23 hours and 56 minutes in exact sync with the apparent diurnal motion of the sky. They may also be equipped with
setting circles to allow for the location of objects by their
celestial coordinates. Equatorial mounts differ from mechanically simpler
altazimuth mounts, which require variable speed motion around both axes to track a fixed object in the sky. Also, for
astrophotography, the image does not rotate in the
focal plane, as occurs with altazimuth mounts when they are guided to track the target's motion, unless a rotating erector prism or other field-derotator is installed. Equatorial telescope mounts come in many designs. In the last twenty years motorized tracking has increasingly been supplemented with computerized object location. There are two main types. Digital setting circles take a small computer with an object database that is attached to encoders. The computer monitors the telescope's position in the sky. The operator must push the telescope. Go-to systems use (in most cases) a worm and ring gear system driven by servo or stepper motors, and the operator need not touch the instrument at all to change its position in the sky. The computers in these systems are typically either hand-held in a control "paddle" or supplied through an adjacent laptop computer which is also used to capture images from an electronic camera. The electronics of modern telescope systems often include a port for autoguiding. A special instrument tracks a star and makes adjustment in the telescope's position while photographing the sky. To do so the autoguider must be able to issue commands through the telescope's control system. These commands can compensate for very slight errors in the tracking performance, such as periodic error caused by the worm drive that makes the telescope move. In new observatory designs, equatorial mounts have been out of favor for decades in large-scale professional applications. Massive new instruments are most stable when mounted in an alt-azimuth (up down, side-to-side) configuration. Computerized tracking and field-derotation are not difficult to implement at the professional level. At the amateur level, however, equatorial mounts remain popular, particularly for astrophotography.
German equatorial mount In the
German equatorial mount, (sometimes called a "
GEM" for short) the primary structure is a
T-shape, where the lower bar is the
right ascension axis (lower diagonal axis in image), and the upper bar is the
declination axis (upper diagonal axis in image). The mount was developed by Joseph von Fraunhofer for the Great Dorpat Refractor that was finished in 1824. The telescope is placed on one end of the declination axis (top left in image), and a suitable counterweight on other end of it (bottom right). The right ascension axis has bearings below the T-joint, that is, it is not supported above the declination axis.
Open fork mount The
Open Fork mount has a
Fork attached to a right ascension axis at its base. The telescope is attached to two pivot points at the other end of the fork so it can swing in declination. Most modern mass-produced
catadioptric reflecting telescopes (200 mm or larger diameter) tend to be of this type. The mount resembles an
Altazimuth mount, but with the azimuth axis tilted and lined up to match earth rotation axis with a piece of hardware usually called a "wedge". Many mid-size professional telescopes also have
equatorial forks, these are usually in range of 0.5-2.0 meter diameter.
English or Yoke mount The
English mount or
Yoke mount has a frame or "
yoke" with
right ascension axis bearings at the top and the bottom ends, and a telescope attached inside the midpoint of the yoke allowing it to swing on the
declination axis. The telescope is usually fitted entirely inside the fork, although there are exceptions such as the
Mount Wilson 2.5 m reflector, and there are no counterweights as with the
German mount. The original
English fork design is disadvantaged in that it does not allow the telescope to point too near the north or south celestial pole.
Horseshoe mount The
horseshoe mount overcomes the design disadvantage of English or Yoke mounts by replacing the polar bearing with an open "horseshoe" structure to allow the telescope to access Polaris and stars near it. The
Hale Telescope is the most prominent example of a horseshoe mount in use.
Cross-axis mount The
Cross-axis It achieves this by having a surface that pivots about a "virtual polar axis". This gives equatorial tracking to anything sitting on the platform, from small cameras up to entire observatory buildings. These platforms are often used with
altazimuth mounted
amateur astronomical telescopes, such as the common
Dobsonian telescope type, to overcome that type of mount's inability to track the night sky. ==See also==