hydrated minerals mapping briefing hangout · 2020-04-20 · mars water mapping projects april 16th...

Hydrated Minerals Mapping Briefing Hangout

Pre-Decisional Information -- For Planning and Discussion Purposes Only© 2020. All rights reserved

John Carter, Ph.D., Project Scientist, Institut d'Astrophysique Spatiale, Paris-Saclay University

Sydney Do, Ph.D., Systems Engineer, NASA Jet Propulsion Laboratory, California Institute of Technology

Richard (Rick) Davis, Assistant Director for Science and Exploration, Science Mission Directorate, NASA Headquarters

Background: Where should we land humans on Mars?

April 16th 2020 2Pre-Decisional Information -- For Planning and Discussion Purposes Only

• 100km radius site at latitude band: ±50° (to be updated)

• Contains:

• Habitation Site: Flat, stable terrain for emplacement

of infrastructure, located ≤5km from landing site

location

• Landing Site(s): Flat, stable terrain, low rockiness,

clear over length scales greater than landing ellipse

• Resource Regions of Interest

• One or more potential near-surface (≤3m) water resource

feedstocks in a form that is minable by highly automated

systems, and located within ~1-3km of ISRU processing

and power infrastructure. Total extractable water should be

~100MT (supports ~5 missions)

• Show potential for minable metal/silicon resources, mainly

Fe, Al, and Si, located within ~1-2m of the surface

• Science Regions of Interest

• That address MEPAG goals (i.e. Astrobiology, Atmospheric

Science, and Geoscience)

Exploration Zone (EZ) – Current Definition

April 16th 2020 3Pre-Decisional Information -- For Planning and Discussion Purposes Only

Concept Drawing

Concept Drawing

Concept Drawing

Mars Water Mapping Projects

April 16th 2020 Pre-Decisional Information -- For Planning and Discussion Purposes Only 4

Subsurface Water Ice Mapping (SWIM) Hydrated Minerals Mapping

Putzig & Morgan et al. (PSI)

Team

1

Carter et al. (Paris-Saclay Univ.)A Global Aqueous Mineral Abundance Catalog for Mars

Team

2

Seelos et al. (APL)CRISM-Derived Global Map of Hydrated Mineral Bearing Units

Global Map of Areal Extent of Hydrated

Mineral Detections [Carter et al.]

Map of two types of hydrated

minerals and bound water over

the Mars 2020 Nili Site

Candidates [Seelos et al.]

Northern Hemisphere Ice Consistency Map

Northern Hemisphere Map of Base

of Deep Subsurface Ice Layers

Ongoing projects to create the best possible maps of water distribution by combining currently available orbiter data

Mars Water Mapping Projects

April 16th 2020 Pre-Decisional Information -- For Planning and Discussion Purposes Only 5

Subsurface Water Ice Mapping (SWIM) Hydrated Minerals Mapping

Putzig & Morgan et al. (PSI)

Team

1

Carter et al. (Paris-Saclay Univ.)A Global Aqueous Mineral Abundance Catalog for Mars

Team

2

Seelos et al. (APL)CRISM-Derived Global Map of Hydrated Mineral Bearing Units

Global Map of Areal Extent of Hydrated

Mineral Detections [Carter et al.]

Map of two types of hydrated

minerals and bound water over

the Mars 2020 Nili Site

Candidates [Seelos et al.]

Northern Hemisphere Ice Consistency Map

Northern Hemisphere Map of Base

of Deep Subsurface Ice Layers

Ongoing projects to create the best possible maps of water distribution by combining currently available orbiter data

MOCCAS

A Mars Orbital Catalog of Chemical Alteration Signatures

Mapping water minerals

Institut d’Astrophysique Spatiale, Paris-Saclay University, FranceTeam: J. Carter, F. Poulet, L. Riu, G. Alemanno

Remote sensing of Mars mineralogy

Aqueous mineraldeposit

Solar radiation interacts with water in Mars minerals

Remote sensing of Mars mineralogy

Aqueous mineraldeposit

Imaging spectrometersOMEGA (Mars Express - ESA)

CRISM (MRO – NASA)

Mars orbit spectra

Solar radiation interacts with water in Mars minerals

We detect thisfrom orbit

Near InfraredNear Infrared

Remote sensing of Mars mineralogy

Aqueous mineraldeposit

Solar radiation interacts with water in Mars minerals

We detect thisfrom orbit

Mars orbit spectra Earth mineral spectraImaging spectrometers

OMEGA (Mars Express - ESA) CRISM (MRO – NASA)

What orbital near-infrared spectroscopy can tell us

• Identify and map out tens of types of aqueous minerals

Clay and clay-likeSulfate saltsCarbonate saltsHydrated silica

Commonly:Example 10x10 km mineral map

• Identify and map out tens of types of aqueous minerals

Clay and clay-likeSulfate saltsCarbonate salts Hydrated silica

• Provides the major chemical makeup (iron, aluminum, magnesium etc.)

• Qualitative indication on how water is bound to the mineral, as H2O molecules or as hydroxyl (OH-)

Commonly:

We can do this on the 10s to 100s of meters scale, globally

Example 10x10 km mineral map

What orbital near-infrared spectroscopy can tell us

• A ten-year endeavor to map all types of aqueous minerals, globally at Mars

• We implement a sequential approach:

Find aqueous minerals deposits

Characterize their nature

Quantify their mineral abundance

Derive their water abundance

The MOCCAS Project

« abundance » refers to volume% or weight% within a « skin » located in the top <1 mm of the surface It is not a bulk volume abundance of the entire deposit Currently limited to clays and oxides: sulfate salt abundances are not derived yet

Limitations (1 of 2)

• Only a few mm of mantling by dust or ice can obscure signatures• Most aqueous minerals formed early, so 3+ Gyrs of geologic processes have obscured the deposits

Not accessible

Obscured by:- Dust- Ice/frost (H2O and CO2)-Young capping

Ancient surface visible

Only a fraction (<50%) of the ancient surface is accessible to remote sensing:

Limitations (2 of 2)

• We cannot readily infer the rock type in which the mineral of interest is detected

Example: same mineral (clay), two rock types

Left: dry mud (brittle) Right: mudstone (hard)

This is foreseen to impact resource availability & extraction cost

Limitations (2 of 2)

• We cannot readily infer the rock type in which the mineral of interest is detected

Not accessible

How thick ?

• No active means to probe thickness and get a mineral deposit volume

• Thickness estimates rely on high resolution topographic data and rare erosional windows

• Even retrieving the surficial abundance of a mineral in a rock is not trivial, we rely on complex models and laboratory measurements (see later slides)

How much?

Difficult to quantify how much of a mineral (or water) is present

Example: same mineral (clay), two rock types

Left: dry mud (brittle) Right: mudstone (hard)

This is foreseen to impact resource availability & extraction cost

• A ten-year endavour to map all types of aqueous minerals, globally at Mars

• We implement a sequential approach:

Find aqueous minerals deposits

Characterize their nature

Quantify theirmineral abundance

Derive theirwater abundance

Aqueous minerals, composition is color-coded

The MOCCAS Project

At each step, we procude maps at high resolution (200 m/pixel or better)

Landing ellipse

Global scale mapping

Landing ellipse

Local scale mappingJezero crater landing site for Mars 2020

The MOCCAS Project

The MOCCAS Project: 5-step method

1. Tune in to specific mineral absorption bands in the infrared using 2 instruments: OMEGA & CRISM

2. A scouting algorithm looks for most probable mineral signatures, globally at Mars

3. Systematic human supervision: we verify each candidate mineral deposit, globally: so there are no false positives & a high detection sensitivity. The most reliable approach.

4. Perform radiative transfer modelling (Shkuratov theory) on largest mineral deposits to derive the modal abundances of the rocks, except for sulfate salts (for now). Calibrate … validate … repeat !

5. Deduce from these modal abundances the major chemical elements (including H2O)

Clay deposits

Water : 4.3 wt%

Spectra extraction and spectral modelling

Modal abundances Water contentIdentification and mapping

Anhydrousminerals

Mars surface spectrum (CRISM)

Spectral model

Aqueous minerals:

From 2006-2011: pioneering work produced the first global inventory of aqueous minerals

• Roughly 1000 « sites » with aqueous mineral deposits identified• No detailed maps were built: limited knowledge of their spatial extent & composition

Compiled from meta analyses (2006-2011)

State of the Art – at inception

Ref: Bibring+06,Mustard+08,Poulet+09,Murchie+09,Ehlmann+11,Carter+11

Nili Fossae

GaleMeridiani

MawrthVallis

OxiaPlanum

Marineris

DOMINANT MINERAL CLASSES:

10 years of mapping with the MOCCAS project:From 1000s to 100,000s of aqueous mineral

deposits are now found, and analyzed

Results from MOCCAS – Aqueous mineralogy

Nili Fossae

GaleMeridiani

MawrthVallis

OxiaPlanum

Marineris

Results from MOCCAS – Aqueous mineralogy

DOMINANT MINERAL CLASSES:A more perceptible mapping approach:

Areas on Mars where aqueous minerals are found within a 10x10 km region (size of a landing ellipse)

Nili Fossae

GaleMeridiani

MawrthVallis

OxiaPlanum

Marineris

Results from MOCCAS – Aqueous mineralogy

DOMINANT MINERAL CLASSES:

Wherever we have access to the ancient surface, it is altered

The first map of water and chemical elements stored in aqueous minerals. Uses OMEGA/MEx @1km scale.

Results from MOCCAS – Abundances

> 0% > 10%

Surficial abundance of water in minerals (as OH or H2O) weight%

Water in sulfate salts (as H2O)Not quantified yet

Results from MOCCAS – Abundances

Nontronite clay Water in mineralsMawrth Vallis

candidate landing site

> 0% 50% > 0% 13%Weight% Weight%

2.5% 14%

• There is an additional, independent fingerprint for water in the spectral datasets• It is sensitive to water molecules adsorbed or more tightly bound (including in aqueous minerals)• It is not from ice or water clouds

• An average 4wt% water at low latitude throughout, regardless of the distribution of aqueous minerals. • The mode of binding is unclear. It may be more superficial than aqueous mineral deposits.

An additional reservoir of water at the surface ?

Other bound water in the surface regolith, weight%

Audouard+14

Aqueous mineral ressources and landing site constraints

Mantled +/- 40° Lat Alt < 1 km

Aqueous mineral ressources and landing site constraints

Mantled +/- 40° Lat Alt < 1 km Alt < 0 km

Prospect: 1. on deriving abundances (modelling)

Average relative abundance of aqueous minerals in deposits

Clay mineralsHydrated silica Sulfate saltsCarbonate salts Iron hydroxides

Relative water + hydroxyl content of aqueous minerals

< 1% 10s %

Hydrated silica

<30 %

Clay minerals

10-20 %

Iron hydroxides

5 %

Sulfate salts

20-50 %

Carbonate salts

< 1%

1. Additional laboratory measurements are required to infer abundances of sulfate salts. Task: Acquire optical constants using an infrared polarization bench or related setup

2. Additional calibration measurements to better constrain model errors. Total uncertainty is currently estimated to ±12.3 vol% for aqueous minerals.Task: making known mineral mixtures in lab, acquire spectra and compare to abundance modelTask: compare spectral signatures with the other form of bound water from Audouard+14

Expected result: provide ISRU ranking, globally or for a region of interest, which combines the following:

To be coupled with:

Prospect: 2. Abundance mapping from the km scale to the 100s m scale using CRISM

Task: Upgrade abundance mapping from OMEGA to include entire CRISM detection dataset

Expected result: Generate local scale abundance maps at 10-100 m/pix, for landing sites selection purposes

Jezero Delta (Mars 2020)

Prospect: 3. Attempt retrieval of the rock texture

• Orbital data from thermal inertia (OMEGA/Mars Express & TES/MGS) • Laboratory spectro-photometric study of rock texture in the infrared

Expected result: Provide additional insight on suitability of aqueous deposits for resource extraction depending on rock type (hardness, thickness)

Task: Combine

?

1

THANK YOU!

REACH OUT:

NASA-Mars-Exploration-Zones@mail.nasa.gov

FIND MORE INFORMATION AT:

http://www.nasa.gov/journeytomars/mars-exploration-zones