1. Presented by Ryan Moyé

2. Deuterium + Hydrogen https://archive.stsci.edu/fuse/scisumm/sci_d2h.html http://www.astronomynotes.com/solarsys/s3.htm

3. Where are we? What are we looking at? http://mars.nasa.gov/msl/multimedia/images/?ImageID=5766 http://mars.nasa.gov/msl/mission/timeline/prelaunch/landingsiteselection/ 150 km ~3.6 Ga

4. Drill Hole D/H Analysis Mars Science Laboratory (MSL) – Curiosity Rover instruments: Sample Analysis at Mars (SAM): Quadrupole mass spectrometer Tunable laser spectrometer (TLS) 6-column gas chromatograph Chemistry and Mineralogy (CheMin) instruments *Revealed a smectite clay mineral, an amorphous component, and basaltic minerals  isochemical alteration  authigenic Smectite Mahaffy et al., 2012 ; Mahaffy et al., 2015 http://ssed.gsfc.nasa.gov/sam/curiosity.html

5. Clays on Mars: Smectite http://www.mindat.org/min-11119.html Montmorillonite

6. Reservoir Models Single Reservoir Models: Entire near surface H20 reservoir is exposed to atmospheric loss Equation: Compared to Martian meteorites (assuming a continuous D/H evolutionary timeline, allowing for constraint on near-surface Hesperian age water. Multiple Reservoir Models: There is an exposed surface reservoir and an inaccessible reservoir, most likely in the form of ice caps, where R = amount of water, I = D/H ratio, and f = fractionation factor

7. Evolved Gas Analysis (EGA) – H20

8. TLS – High Temperature Water Evolution

9. TLS - Relative D/H (to SMOW) vs. Temperature

10. Reservoir Models Single Reservoir Models: Entire near surface H20 reservoir is exposed to atmospheric loss Equation: Compared to Martian meteorites (assuming a continuous D/H evolutionary timeline, allowing for constraint on near-surface Hesperian age water., where R = amount of water, I = D/H ratio, and f = fractionation factor

11. Conclusions Assuming a fractionation factor between.016-.4 (diffusion limit), amount of water lost since Yellowknife Bay clay minerals formed would be ~1-1.5 times the current surface/near-surface water reservoirs (including polar ice caps). Current reservoirs are ~50m, so water equivalent global layer (GEL) at the time of formation of Cumberland mudstone would be at least 100-150m. https://en.wikipedia.org/wiki/Geological_history_of_Mars