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Introduction to Portable--CGS4DR
The fourth generation COOLED GRATING SPECTROMETER, CGS4, is
designed to operate on UKIRT in the 1--5 m region of the
electromagnetic spectrum at resolutions in the range
/ 300--20000 (Mountain et al. 1990,
Ramsay 1993). To reduce background noise, it is maintained on the
telescope in vacuum at cryogenic temperatures. It achieved first light
at UKIRT on 4 February 1991 (Carswell et al. 1991). On 22 April 1995 a
new InSb 256 256 array was commissioned into the instrument.
The new array having a dark current of << 1 and a
read noise of 40 per integration, is much more sensitive
than previous detectors. On any given spectroscopic night, an observer
can expect to acquire and reduce 100 Mb of high quality data
with CGS4.
To an observer, the system appears as two black boxes: the data
acquisition system and the data reduction system (Wright et al. 1994).
Both are under the direct control of the observer and can be
manipulated to deal with a wide variety of astronomical configurations.
The data is, therefore, both acquired and reduced in real-time at the
telescope.
This document describes the CGS4 data reduction system now called
Portable--CGS4DR. The software has been carefully designed and tested
under the Figaro (Shortridge 1993) and ADAM (Lawden & Hartley 1992)
environments under Unix. The data files produced by Portable--CGS4DR
are readable by standard Figaro applications although not all may
handle the quality and error arrays correctly.
For best results, Portable--CGS4DR should be run on a single user
workstation having at least 32 Mb of main memory and a colour monitor.
It can, of course, run on a dumb terminal and display to any STARLINK supported graphics device.
If you think you have discovered a bug, please report it by e-mail to
ussc star.rl.ac.uk.
Last Modification Date 1996/03/12 - Last Modification Author: frossie
Phil Daly (pnd@jach.hawaii.edu)
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