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S. Vicente, M. Roos-Serote (CAAUL/Obs. Ast. de LIsboa ,Portugal), U.A. Dyudina (Caltech, California, USA), P. Drossart (Obser. Meudon, France), R.W. Carlson (JPL , California, USA)
The Near Infrared Mapping Spectrometer (NIMS) on the Galileo spacecraft give us spectra from Jupiter in the 4 - 5 micron window.
The well known and studied 5 micron window (4.6 - 5.2 micron) contains information on the water vapor mixing ratio between 3 and 8 bar and the cloud opacity above 2 bars. The shape of the spectrum in this range contains information on the presence of a possible cloud deck at pressures between 3 and 8 bar. The 4 - 4.5 micron region has been very little studied, as terrestrial CO2 blocks this region, and previous space based instruments (Voyager/IRIS) were not sensitive in this range. The NIMS data set is the first with a good spatial and spectral coverage of this region. It contains strong absorptions of methane on the blue side and phosphine on the red side, with two little windows around 4.3 micron.
In this work we apply the Principal Component Analysis (PCA) method to isolate a small number of Empirical Orthogonal Functions. The EOF represent the (spatial) variance of the spectral intensities at different wavelengths. From this analysis we search to understand the relation between the physical processes which determine the spectra in the well understood 4.5 - 5.2 micron and those which determine the spectra in the 4.0 - 4.5 micron range.
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The author(s) of this abstract have provided an email address for comments about the abstract: svicente@oal.ul.pt