1. Wet environment reconstruction using IR spectra on Mars Akos Kereszturi Konkoly Astronomical Institute, MTA CSFK Mars Astrobiology Group (ESA RCL) OTKA PD 105970

2. Background: aim: use laboratory analysis to reconstruct wet conditions on Mars this presentation: earlier results + new project idea results: Mars surface morphology  past water (Bolyai Fund: 2011-2012) project: Mars surface IR spectroscopy + laboratory analysis  past wet conditions (OTKA Fund: 2012.09.01.-) Contenst: Martian wet locations paleoenvironment reconstruction examples from morphology examples from volumetric and discharge calculations overview of wet environments IR spectra to understand wet alteration available CRISM, THEMIS data laboratory spectra, FTIR measurements

3. Introduction: evidences for past water on Mars channels, shorelines, Gilber-like deltas, cross-bedding features, lake basins… wet alteration products (Al-clays, hydrated sulfates, zeolites…) inside Mars meteorites (clays, carbonates) ice on and below the surface today + paleoclimate indicators  water OK, but what was it like? Temperature? pH? Salinity? …

4. Surface morphology  channel shape  erosion style Methods: imaging data (MOC, THEMIS, HSRC, CTX, HiRISE), topography (DTMs) GIS software, model computations, error level channel identification: images / databases (some % catalogued) measurements: cross-sectional, longitudinal profiles, network str. reason: different erosion (climate related) Kereszturi 2011 Planetary and Space Science

5. Surface morphology  volume, duration volume estimation: eroded (missing) regolith deposited sediment volume discharge computation (Modified Manning / Darcy- Weisbach equations) sediment transport rate active duration result: water volumes involved, wet periods (climate related) delta-like sediment Example: Gale crater NW valley eroded: 0.34 km 3 deposited: 0.23 km 3 flow speed: 30-50 km/h sed. transp. rate: 0.1 kg/m 3 active duration: 100-500 h fan cross profile Kereszturi 2012 Planetary and Space Science

6. Surface morphology  other temporal parameters relative, absolute ages crater density calculations different erosion style at different ages morphology – age correlation probably climatic forces older sections younger sections

7. Summary: compare different wet environment types: calculations on fluvial activity estimation on polar liquid interfacial water (today) other authors: freezing timescales of lakes, weathering durations results: separate groups with overlapping zones connections with geological evolution but great uncertainty should be improved… Kereszturi 2012 Astrobiology water ice + thin liquid film CRISM spectra

8. Possible solution: IR spectroscopy (project 2012-) OTKA project started Sept. 2012. identify wet alteration products wet conditions  mineral alteration  spectral identification best candidates: phyllosilicates, hydrated sulphates models  past temperature, pH, salininty, water activity, rock/water ratio, duriation fluvial channel delta-like depositional structure weathered minerals phyllosilicates  moderate pH, high a w montmorillonite (Columbia Hills)  alkaline conditions kaloinite (many locations)  acidic sulphates  acidity  low water/rock ratio, short duration assemblages of hydrated minerals

9. Possible solution: IR spectroscopy (project 2012-) CRISM (Compact Reconnaissance Imaging Spectrometer for Mars) onboard Mars Reconnaissance Orbiter multi- / hypespectral 0.4-3.9 µm resolution: 20 m/px 544 wavelengths 200 m/px 72 wavelengths THEMIS (Thermal Emission Imaging System) onboard Mars Odyssey 9 bands: 6.8-14.9 µm (thermal IR) 5 bands: 0.42-0.86 µm (visible - near IR) resolution: global thermal IR bands 100 m 60% in visual bands 18 m influencing factors: aerosols (dust, vapor) surface dust cover particle size fluvial channel delta-like depositional structure weathered minerals

10. Possible solution: IR spectroscopy (project 2012-) mineral identification on Mars using library spectra own data: FTIR at Institute for Geological and Geochemical Research range: 1.5-28 µm spectra of clays, sulphates with known H 2 O content eample: dehydrataion of zeolite 1.9 µm band disappears, also may shift Extrapolation not easy: phyllosilicates  moderate pH, high a w montmorillonite (Columbia Hills)  alkaline conditions kaloinite (many locations)  acidic assemblages of hydrated minerals

11. First targets clay-like smectites (phyllosilicate) characteristic vibrational absorption near 2.3 μm and a 1.9 μm band indicating molecular H2O, also at 1.4 μm not easy  mixed-interlayered, Fe-Mg substitution, diverse particle size… in lab we can „play” with these factors Mars laboratory Used data: FTIR spectrometer (lab): 1.25-28 µm CRISM data (Mars): 0.4-3.9 µm THEMIS data (Mars): 0.4-15 µm

12. First location preliminary example: Nanedi Valles delta 2.1 nm absorption min.  monohydrated minerals elevated clay level? delta lake basin Kereszturi 2007 LPSC