Machine Learning for Planetary Science

Kiri L. WagstaffJet Propulsion Laboratory,

California Institute of Technology

Big Data Task ForceNovember 1, 2017

© 2017, California Institute of Technology. Government sponsorship acknowledged.This work was performed at the Jet Propulsion Laboratory,

California Institute of Technology, under a contract with NASA.

ML for Planetary Science

1. Content-based image classification 2. Onboard data analysis and

discoveries3. Onboard data acquisition4. Information extraction

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon 1, R. Jackson 1, R.C. Wiens2, N. Lanza 2, A. Cousin 2, S. Clegg 2, V. Sautter3, J. Bridges 4, N. Man-

gold 5, O. Gasnault 6, S. Maurice6, C. D’Uston 6, G. Berger 6, O. Forni6, J. Lasue 6, P.-Y. Meslin 7, B. Clark 8, R. Anderson 9, R.

Gellert10, M. Schmidt11, J. Berger11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres15, M.-P. Zorzano16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

MOC, June 2000

1. Content-based image classification• NASA image archives: millions of images

• Goal: enable search by content, not just pointing• Statistical analysis + deep learning classification

Crater Impact ejecta

Dark slope streakBarchan dune

Salience MapKiri Wagstaff, You Lu, Alice Stanboli, Kevin Grimes, Gary B. Doran, Jr., Lukas Mandrake

Find visually salient “landmarks” Train a classifier to label them

http://pds-imaging.jpl.nasa.gov/search/

Content-based image search• Detect landmarks -> image meta-data• Enables search for images containing

landmarks of interestExample results from “crater” searchPlanetary Image Atlas

Dark dunes

Dark slope streaks

Benefits for mission operations

August 2012

December 2013

November 2016

12

Lukas Mandrake, Gary Doran, Brian Bue

DHM field team Nuuk, Greenland Raw Hologram (2D) Detections

Extremophiles

Contamination

Planetary

• Digital Holographic Microscopes• Big data (4D, ~GB/s), rare findings

• Motility ~ Life (composition agnostic!)• HELM ML system detects, tracks, and

classifies in messy, raw 2D holograms

2. Astrobiology: Holographic life detection

2. Onboard science:Dust devil (change) detection

• Analyze sequence of images for motion detection• Operationally qualified on Mars Exploration Rovers (2008)• Consumes no data volume when no activity detected• Achieved significant data reduction for MER

A. Castaño et al., 2007. Machine Vision Applications.

• Thermal anomaly detection• 14,856 THEMIS nighttime images• 143 images > 240K (12.57 um)• Synthetic positives: 100% detection

• Polar cap tracking• Led to first discovery of

north polar water ice annulus in THEMIS data [Wagstaff et al., 2008]

• Future: Europa Clipper

2. Onboard science for new discoveries

Image credit: Mars Odyssey team, ASU, JPL, NASA

Mars south polar capMars north polar cap

R. Castaño et al., 2007. Knowledge Discovery and Data Mining.K. Wagstaff et al., 2008. Planetary and Space Science.

3. Onboard science: Data acquisition

• AEGIS: Autonomous Exploration for Gathering Increased Science

• Find and prioritize rocks• Fire ChemCam laser and collect

spectra• Operational on MSL since 2016• Baselined for Mars 2020

• Automatic pointing refinement• Developed for Mars 2020 (PIXL)

Tara Estlin, Benjamin J. Bornstein, Daniel M. Gaines, Robert C. Anderson, David R. Thompson, Michael Burl, Rebecca Castaño, and Michele Judd

4. Information extraction for planetary science

Millions of observations…

What have we learned?

16

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon1, R. Jackson 1, R.C. Wiens 2, N. Lanza 2, A. Cousin 2, S. Clegg 2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue 6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan12, W. Boynton 13, M. Fisk 14; F. Martin-Torres 15, M.-P. Zorzano16, S.

Karunatillake17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon1, R. Jackson 1, R.C. Wiens 2, N. Lanza2, A. Cousin 2, S. Clegg 2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon 1, R. Jackson 1, R.C. Wiens 2, N. Lanza2, A. Cousin2, S. Clegg2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston 6, G. Berger 6, O. Forni 6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert 10, M. Schmidt 11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano 16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of G RS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon 1, R. Jackson 1, R.C. Wiens 2, N. Lanza2, A. Cousin2, S. Clegg2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston 6, G. Berger 6, O. Forni 6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert 10, M. Schmidt 11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano 16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of G RS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon 1, R. Jackson 1, R.C. Wiens 2, N. Lanza2, A. Cousin2, S. Clegg2, V. Sautter3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston 6, G. Berger 6, O. Forni 6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert 10, M. Schmidt 11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres15, M.-P. Zorzano 16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom1, S. Gordon 1, R. Jackson1, R.C. Wiens2, N. Lanza2, A. Cousin2, S. Clegg2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue6, P.-Y. Meslin7, B. Clark 8, R. Anderson9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain,16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon 1, R. Jackson 1, R.C. Wiens 2, N. Lanza2, A. Cousin2, S. Clegg2, V. Sautter3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston 6, G. Berger 6, O. Forni 6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert 10, M. Schmidt 11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres15, M.-P. Zorzano 16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon1, R. Jackson 1, R.C. Wiens 2, N. Lanza 2, A. Cousin 2, S. Clegg 2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue 6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan12, W. Boynton 13, M. Fisk 14; F. Martin-Torres 15, M.-P. Zorzano16, S.

Karunatillake17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon1, R. Jackson 1, R.C. Wiens 2, N. Lanza2, A. Cousin 2, S. Clegg2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano 16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon 1, R. Jackson1, R.C. Wiens 2, N. Lanza2, A. Cousin2, S. Clegg2, V. Sautter3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston 6, G. Berger 6, O. Forni 6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert 10, M. Schmidt 11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres15, M.-P. Zorzano 16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon 1, R. Jackson1, R.C. Wiens 2, N. Lanza2, A. Cousin2, S. Clegg2, V. Sautter3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston 6, G. Berger 6, O. Forni 6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert 10, M. Schmidt 11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres15, M.-P. Zorzano 16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the vol

ments including H, C, Cl, S, that r

input to the soils andvides a w

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS

tions reflect the integrated abund

0.5 m, but the instrof the r

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon1, R. Jackson1, R.C. Wiens 2, N. Lanza 2, A. Cousin2, S. Clegg2, V. Sautter 3, J. Bridges 4, N. Man-

gold 5, O. Gasnault 6, S. Maurice6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue 6, P.-Y. Meslin 7, B. Clark8, R. Anderson 9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan12, W. Boynton 13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano16, S.

Karunatillake17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map wi

arrows showing Gale (West) and Gusev (E

dichotomy boundary. See Fig 2

G

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon1, R. Jackson1, R.C. Wiens 2, N. Lanza 2, A. Cousin2, S. Clegg2, V. Sautter 3, J. Bridges4, N. Man-

gold 5, O. Gasnault 6, S. Maurice6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue 6, P.-Y. Meslin 7, B. Clark8, R. Anderson 9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano16, S.

Karunatillake17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon1, R. Jackson 1, R.C. Wiens 2, N. Lanza2, A. Cousin 2, S. Clegg2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano 16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no w

to get their unique GRS signatures. The

the two landing sites are o

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon1, R. Jackson 1, R.C. Wiens 2, N. Lanza2, A. Cousin 2, S. Clegg 2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon 1, R. Jackson1, R.C. Wiens2, N. Lanza 2, A. Cousin2, S. Clegg2, V. Sautter 3, J. Bridges 4, N. Man-

gold 5, O. Gasnault 6, S. Maurice6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue 6, P.-Y. Meslin7, B. Clark 8, R. Anderson 9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano16, S.

Karunatillake17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon1, R. Jackson1, R.C. Wiens 2, N. Lanza 2, A. Cousin2, S. Clegg2, V. Sautter 3, J. Bridges 4, N. Man-

gold 5, O. Gasnault 6, S. Maurice6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue 6, P.-Y. Meslin 7, B. Clark8, R. Anderson 9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan12, W. Boynton 13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano16, S.

Karunatillake17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy bou d

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon1, R. Jackson 1, R.C. Wiens 2, N. Lanza2, A. Cousin 2, S. Clegg2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston6, G. Berger 6, O. Forni6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert10, M. Schmidt11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano 16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophil

ements including Al, Si, Fe, Mn, Ca N

represents the rock comments includii

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS sign

Regional trends fr

tions reflect

Example of GRS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

Mars Target Encyclopedia:Geochemical relationships

• Big Sky contains magnetite• Big Sky contains hematite

Mars Target Encyclopedia:Geochemical relationships

EntitiesFind

Elements, Minerals, Targets

Relations Classify pairs

of Target + (Element or

Mineral)

MTE Database

Information Extraction User queries via web

REGIONAL CONTEXT OF SOIL AND ROCK CHEMISTRY AT GALE AND GUSEV CRATERS, MARS.

H.E. Newsom 1, S. Gordon 1, R. Jackson 1, R.C. Wiens 2, N. Lanza2, A. Cousin2, S. Clegg2, V. Sautter 3, J. Bridges 4, N. Man-

gold5, O. Gasnault6, S. Maurice 6, C. D’Uston 6, G. Berger 6, O. Forni 6, J. Lasue6, P.-Y. Meslin7, B. Clark8, R. Anderson9, R.

Gellert 10, M. Schmidt 11, J. Berger 11, S. McLennan 12, W. Boynton13, M. Fisk14; F. Martin-Torres 15, M.-P. Zorzano 16, S.

Karunatillake 17 1Inst. of Meteoritics, Univ. of New Mexico, Albuquerque, NM 87131, USA (Newsom@unm.edu); 2Los

Alamos National Lab., NM, USA; 3MNHN, CNRS Fr; 4Univ. of Leicester, GB; 5Lab. de Planetologie et Geodynamique de

Nantes, FR; 6IRAP/CNRS, FR; 7Univ. Paul Sabatier, Toulouse, FR; 8Planetary Science Inst., Tucson, AZ, USA; 9USGS,

Flagstaff, AZ, USA; 10Univ. of Guelph, Canada; 11Brock Univ., Canada, 12Stony Brook Univ., NY, USA; 13Univ. of Arizona,

AZ, USA, 14Univ. of Oregon, USA. 15Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Granada, Spain, 16Centro de

Astrobiología (INTA-CSIC), Madrid, Spain, 17Louisiana State Univ., LA, USA

Introduction: Geochemical data for both rocks and

soils from Gale Crater, and Gusev Crater, are compared

here with data from the Gamma Ray Spectrometer

(GRS) experiment on the Mars Odyssey Spacecraft [1,

2]. Both Gale and Gusev craters are located near the di-

chotomy boundary between the Noachian Highlands

and the younger volcanics and transitional units to the

north (Fig. 1). Element ratios in these samples may pro-

vide a link between the regional provinces analyzed by

GRS and the materials at the two landing sites. The lith-

ophile data may lead to a better understanding of the

origin and evolution of the martian crust in this region

of Mars, while the volatile element components SO3, Cl,

and water provide information on volcanic aerosols,

weathering processes and potentially recent climate [3].

Fig. 1 – Portion of the Mars Global Geologic map with

arrows showing Gale (West) and Gusev (East) craters on the

dichotomy boundary. See Fig. 2 for scale and reference.

Geochemical components and normalization:

Comparing the chemistry of Gale and Gusev samples

with other martian data must take into account the dif-

ferent geochemical components in the samples. The

most important distinction is between the lithophile el-

ements including Al, Si, Fe, Mn, Ca, Na, Mg, etc. that

represents the rock component, and the volatile ele-

ments including H, C, Cl, S, that represent later external

input to the soils and rocks. Normalization to SiO2, pro-

vides a way to correct the lithophile elements for varia-

ble amounts of the mobile element component, mainly

sulfur, chlorine and water.

Fig. 2 – Areas with distinctive GRS signatures based on 5

x 5 degree binned data.

Fig. 3 – CaO/SiO2 vs. FeO/SiO2 data for areas near Gale

and Gusev Craters (Fig. 2) with distinctive GRS signatures.

Regional trends from GRS: The GRS composi-

tions reflect the integrated abundances to a depth of ~

0.5 m, but the instrument is not collimated, and ~ 50%

of the received gamma rays come from an area ten de-

grees in diameter on the surface below the instrument

[4]. Thus most of the signal from each 5 degree binned

data used in this study comes from outside the nominal

area represented by the data. Because Gale and Gusev

craters are only ~ 3 degrees in diameter, there is no way

to get their unique GRS signatures. Therefore, because

the two landing sites are on the dichotomy boundary,

Example of G RS 10 degree “pixel”

2284.pdf

46th Lunar and Planetary Science Conference (2015)

Kiri L. Wagstaff, Raymond Francis, Thamme Gowda, You Lu, Ellen Riloff, Karanjeet Singh, and Nina Lanza

• Train: 118 manually annotated documents• Deploy: 5,920 automatically analyzed• Speed: 30 minutes/doc => 5 seconds/doc

MTE Integration with the MSL Analyst’s Notebook

How to ↑ support for ML + planetary science

• For research advances• ROSES call for ML+planetary science collaborations

• For spacecraft infusion• Funds for maturing algorithms for onboard use• Funds for infusing algorithms into flight software

• For community impact• Funds for connecting algorithms to data systems (e.g., PDS)