A CCD detector for multiple object spectroscopy at the United Kingdom Schmidt Telescope

Details A CCD detector for multiple object spectroscopy at the United Kingdom Schmidt Telescope A CCD detector for multiple object spectroscopy at the United Kingdom Schmidt Telescope

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990spie.1235..272o&link_type=abstract

IN: Instrumentation in astronomy VII; Proceedings of the Meeting, Tucson, AZ, Feb. 13-17, 1990 (A91-29601 11-35). Bellingham, WA

Astronomy and Astrophysics

Astronomy

4

Charge Coupled Devices, Image Processing, Optical Fibers, Schmidt Cameras, Thermal Control Coatings, Pixels, Signal Processing, Signal To Noise Ratios

Scientific paper

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.

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