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The database employed in the analysis contains the same images used for quick-look sensitivity monitoring and consists of several hundred low-dispersion point source and trailed observations distributed amongst the sensitivity monitoring standard stars. Each image was carefully examined for defects such as data dropouts, cosmic ray hits, etc. and any corrupted spectra were discarded. All of the data were uniformly reprocessed using the prototype final archive processing software (Nichols-Bohlin 1990) and the updated line library and wavelength calibration (Bushouse 1991a). The original databases include images taken through early 1992 for the SWP, mid-1993 for the LWP, and late 1994 for the LWR.

Karen Levay