THE IRIS DATA
This appendix presents the IRIS data set itself. All on-planet spectra
with a range of less than 400,000 km are listed, with 5 tables covering
each spacecraft encounter with each icy satellite.
First I give the FDS count, then the spacecraft range, in kilometers,
from the planet center, and the subspacecraft latitude and longitude. Longitudes
are given using the pre-Voyager system, with zero at the sub-Jupiter point.
Then follows postitional information for the center of the IRIS field of
view (corrected values in the case of Voyager 2 Ganymede (see Chapter 3)).
I give, in order, the latitude and longitude, local time in degrees (`LTim'),
solar incidence angle (i), emission angle (e), minimum separation
of the field of view from the limb, in degrees (`LSp': negative values
indicate dark-sky contamination, see Chapter 4), and solar phase angle
(`Phs'). Then, for most Ganymede spectra, `fDk' and `fCt'
give the percentage of the field of view occupied by dark cratered terrain
and bright crater materials respectively (Chapter 3).
Finally I list the spectrum shape and temperature information. T1,
\dt, and \ep\ are the fitted warm-component temperature, effective temperature,
temperature contrast, and emissivity, as defined in Chapter 4. T1
is redundant but it, and thus T2, cannot be derived analytically
from TE, \dt, and \ep, so it is given for convenience.
`Slp' is the standardized slope of the fitted spectrum: the difference
in brightness temperature between 500 and 250 cm-1. A few spectra
(usually those with dark-sky contamination) could not be fitted: for these
only the `raw' 22 microns brightness temperature is listed, in the TE