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Optomechanic Design DIF-FUS Universidad de Sonora |
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The main part of the telescope, the mirror of 30 cm of diameter, is polished with the technique that is used for optics of observation in X rays This means a precision that does not allow variations in the major surface of the mirror to an Amstrong (10E-8 cm). Until the moment there's no telescope in a terrestrial observatory with optics worked with this technique. The mirror will be mounted in a vacuum sealed tube to avoid internal turbulences. Instead of a secondary mirror, a flat mirror that will allow to a focal length base of 1200 mm or f/4 will be installed.
At the end of the tube will be the package of instruments in an 'L' shaped. A removible mirror will move perpendicular to the light beam interfering this one to direct the beam towards the solar package of instrumentation or leaving free the path towards the package of stellar instrumentation. In the solar observation way, the light will be directed to two filters of narrow band. One of them will be a tuneable filter to observe in the line of H-Alpha 656 nm with a CCD video camera of 2048 x 2048 pixels with a zoom system lens. The second filter will be for observing in the line of Helium I 1083 nm, where will be a CCD camera of 2048 x 2048 pixels. In the way of stellar observation, the light will be directed to a CCD camera of 2048 x 2048 pixels for obtaining images. Also the light could be directed to a small spectrograph. The telescope will be in an equatorial mount English type modified. Fecha de Ultima actualización: Enero 22, 2000. |
