S. J. Leeks 1, B. M. Swinyard 2, T. L. Lim 3, & P. E. Clegg 1
1 Queen Mary & Westfield College, London, E1 4NS, U.K.
2 Space Science Department, Rutherford Appleton Laboratory, Chilton, Didcot, Oxon, OX11 0QX, U.K.
3 ISO Science Operations Centre, Space Science Department of ESA, Villafranca, P. O. Box 50727, 28080, Madrid, Spain
We present an outline of various stages of the LWS data pipeline processing, from the conversion of the output from the detectors through to a calibrated spectrum. Normal calibration is based on a linear relationship between the Uranus data from the LWS and a theoretical model of the planet. For strong sources, however, some of the detectors behave non-linearly. We show that, using a strong source for which we have a good model as a calibrator, these data can be corrected. Examples of the resulting spectra are shown.