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In 1970 Celestron introduced its "C8" 8" diameter 2032 mm focal length, ƒ10 telescope, the first of a new line of telescopes built using methods developed by Celestron to produce Schmidt-Cassegrains at a high volume and low cost. [1] These models made significant inroads into the amateur astronomical and educational communities.
This mount is an alternative to the altazimuth mount that has the advantage of not having a blind spot near the zenith, and for objects near the celestial equator the field rotation is minimized. [7] It has the disadvantage of having all the mass, complexity, and engineering problems of its equatorial counterpart, so is only used in specialty ...
One of four auxiliary telescopes belong to the Very Large Telescope array. An optical telescope gathers and focuses light mainly from the visible part of the electromagnetic spectrum. [26] Optical telescopes increase the apparent angular size of distant objects as well as their apparent brightness.
A large German equatorial mount on the Forststernwarte Jena 50cm Cassegrain reflector telescope. An equatorial mount is a mount for instruments that compensates for Earth's rotation by having one rotational axis, called polar axis, parallel to the Earth's axis of rotation. [1] [2] This type of mount is used for astronomical telescopes and cameras.
Comparison of nominal sizes of apertures of the above extremely large telescopes and some notable optical telescopes. An extremely large telescope (ELT) is an astronomical observatory featuring an optical telescope with an aperture for its primary mirror from 20 metres up to 100 metres across, [1] [2] when discussing reflecting telescopes of optical wavelengths including ultraviolet (UV ...
In addition, one of the two eyepieces can be further adjusted to compensate for differences between the viewer's eyes (usually by rotating the eyepiece in its mount). Because the focal change effected by the adjustable eyepiece can be measured in the customary unit of refractive power, the dioptre , the adjustable eyepiece itself is often ...
T Coronae Borealis (T CrB), nicknamed the Blaze Star, is a binary star and a recurrent nova about 3,000 light-years (920 pc) away in the constellation Corona Borealis. [11] It was first discovered in outburst in 1866 by John Birmingham, [12] though it had been observed earlier as a 10th magnitude star. [13]
GALEX used the first ever UV light dichroic beam-splitter flown in space to direct photons to the Near UV (175–280 nanometers) and Far UV (135–174 nanometers) microchannel plate detectors. Each of the two detectors has a 65 mm (2.6 in) diameter. The target orbit is 670 km (420 mi) circular and inclined at 29.00° to the equator.
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