1. Titan H2O Clouds + ISS/UVIS
Water in Titan's Atmosphere
Image Cube Refinements
Application to Enceladus Plume Locations
Dione Example of co-analysis

2. Prediction of H2O Clouds
Barth + Toon Model Predictions
Based on UVIS temperature profile
Maximum H2O abundance at 540 km
N = 0.4 cm-3
H2O Particle size 0.01 microns

3. Data Sets
Spica (Alpha Vir) and Shaula (Lambda Sco) occultations at T-B (December 13, 2004)

4. H2O Absorption Spectrum

5. Hydrocarbon Spectra
CH4
C2H2
C2H4
C2H6
HCN

6. H20 Sensitivity

7. H2O Sensitivity with Hydrocarbons

8. Hints of H2O From Spica Occultation

9. H2O In Shaula Occultation

10. H2O Slopes Slope change at 1100 km Slope change at 900 km
Slope between 1640Å and 1825Å
Slope change at 1100 km
Slope change at 900 km

11. Hydrocarbon analysis
Correction of unattenuated spectrum with only hydrocarbons from Shemansky et al. occultation paper.
At 550 km, log(nl) =
CH4:
C2H2: 17.5
C2H4:
C2H6: 16.5
HCN:

12. Hydrocarbon Correction of Spica

13. Spica Correction

14. Spica Correction with H2O
km spectrum
Hydrocarbon Model
Hydrocarbon + Water

15. Shaula Occultation

16. Corrected Shaula Occultation
km spectrum
Hydrocarbon Model
Hydrocarbon + Water

17. Spatial Variability
H2O clouds needed in northern hemisphere, but not southern.
Future solar/stellar occultations should provide more tests.

18. Enceladus Image Cube Fountains of Enceladus (1688) November 27, 2005
Unknown time or distance
Enceladus Plume Raw Preview (1701)
November 27, 2005
170,600 km distance, 161º phase angle

19. Enceladus Plumes
Based on relative size of moon in image and orbital geometry, image taken at 17:27:00 ± 5 minutes
Plumes assumed to be limb aligned for mapping purposes.

20. Enceladus Plumes

21. Dione ISS/UVIS Analysis
ISS Dione Raw Preview #1 (1564)
October 11, 2005
~09:50:00
UVIS ICYMAP003_PRIME
Start Time - 14:43:28

22. Dione ISS Unwrap

23. Dione ISS/UVIS Pixels