![]() The conduit now passes through the base of the Cassegrain cage which contains Further down the optical table is the lensĪrray unit, and the fibres pass through the black conduit into a strain-reliefīox in the bottom left and out of the Cassegrain cage. The picture on the right shows the aperture in the primary mirror at the top, Scale of the focal plane so that each lenslet corresponds to 0.5 arcsec on the Which the fore-optics and lens array are mounted. There is an optical table bolted onto the Cassegrain focus of the telescope on The diagram on the left shows the physical set-up of SPIRAL on the telescope. This paper covers all the equations concerned, complete with diagrams. The light from an extended area in the sky onto a long thin slit suitable forįor the "Optical Telescopes of Today and Tomorrow" symposium SPIE 2871 (1997). Means you can produce maps of various emission lines, absorption lines,Ĭontinuum and two-dimensional velocity maps. ![]() Your spectral resolution decreases at the same time.Īn IFU allows you to collect light over an extended area on the sky andĪlso obtain spectral information for each spatial element in that area. Of the entrance slit in ths spectrograph. Mismatch of the image scale in the focal plane of the telescope with the width Telescopes is difficult for a variety of reasons. High resolution (R ~ 8,000) work on faint stars/distant galaxies with large Lenses, and consists of two modes - integral field imaging and Metres of fibre optics to a dedicated spectrograph on the floor of the AAT Spiral is a prototype integral field unit (IFU) connected via eighteen Software for SPIRAL and other IFU's What is SPIRAL?. ![]() ![]()
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