  The Cassini Ultraviolet Imaging Spectrograph (UVIS) observed a plume of water
vapor spewing out from the south polar regions of Enceladus in occultation
geometry 7 times during the Cassini mission. Five of them yielded data resolved
spatially that allowed fits to a set of individually modeled jets. We created a
direct simulation Monte Carlo (DSMC) model to simulate individual water vapor
jets with the aim of fitting them to water vapor abundance along the UVIS line
of sight during occultation observations. Accurate location and attitude of
spacecraft together with positions of Enceladus and Saturn at each observation
determine the relationship between the three-dimensional water vapor number
density in the plume and the two-dimensional profiles of water vapor abundances
along the line of sight recorded by UVIS. By individually fitting observed and
modeled jets, every occultation observation of UVIS presented a unique
perspective to the physical properties and distribution of the jets. The
minimum velocity of water vapor in the jets is determined from the narrowest
observed individual jet profile: it ranges from 800 m/s to 1.8 km/s for the
UVIS occultation observations. 41 individual jets were required to fit the
highest resolution UVIS dataset taken during the Solar occultation however, an
alternative larger set of linearly-dependent jets can not be excluded without
invoking additional preferably unrelated data from other instruments. A smaller
number of jets is required to fit the stellar occultation data because of their
spatial resolution and geometry. We identify a set of 37 jets that were
repeatedly present in best fits to several UVIS occultation observations. These
jets were probably active through the whole Cassini mission.
