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1 July 1990 CCD detector for multiple object spectroscopy at the United Kingdom Schmidt Telescope
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The standard CCD used in the camera installed at the Schmidt Telescope has a poor short wavelength response and so all the CCDs are surface coated with a fluorescent dye to partially overcome this problem. In 1988 it was decided that the system's response around 4000 A could be improved further by replacing the FLAIR (fiber linked array image reformatter) fibers with a set of fibers offering superior transmission properties at this wavelength. The introduction of these larger core diameter fibers would have meant, however, accepting a reduction in signal-to-noise as the fibers illuminate more pixels on the CCD. The CCD sequencing was therefore modified to permit pixel binning across the dispersion direction. Recent modifications also provide a detection capability for approximately twice the number of objects, by appending a second CCD detector and correlated double sample processor to the existing sequencer. Both CCDs are operated via a signal controller which can route clocks and video between the detectors and sequencing electronics. Reduction of galaxy data show that FLAIR, combined with a low noise detector, in both single and dual CCD mode, is easily capable of obtaining cross-correlation redshifts in the blue with a high success rate.
© (1990) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Anthony Patrick Oates "CCD detector for multiple object spectroscopy at the United Kingdom Schmidt Telescope", Proc. SPIE 1235, Instrumentation in Astronomy VII, (1 July 1990);


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