1 Space Science Department, Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, UK
2 Queen Mary and Westfield College, University of London, Mile End Road, London E1 4NS, UK
3 ISO Science Operations Centre, ESA Science Department, Villafranca del Castillo, P.O. Box Apdo 50727, 28080 Madrid, Spain
4 Institute of Space and Atmospheric Studies, University of Saskatchewan, 116 Science Place, Saskatoon, Sask. S7N 5E2, Canada
5 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
A total of ten full LWS grating scans made at different epochs between 15th
July and 27th August 1997 have been carefully reduced and analysed using LWS
pipeline 7 software and the LWS Interactive Analysis tools. The results of a
search for possible diurnal variation in the LWS wavelength range will be
presented, together with a report on the comparison with predictions of
a thermophysical model of the Martian surface.
In order to put limits on instrumental effects and calibration drifts, any detected Martian variability will be checked against S106, a comparably bright non-varying astronomical calibration source observed routinely throughout the mission. The implications of this work on the role of Uranus as the LWS prime flux calibrator will also be discussed.