Held at
Edited by
L. Kirkland, J. Salisbury, J. Mustard,
R. Clark, P. Lucey, and S. Murchie
Sponsored by
Lunar and Planetary Institute
JPL Mars Program Office
Convener
Laurel Kirkland
CLICK HERE FOR THE REPORT AS A PDF DOCUMENT
CONTENTS
Letters
Recommendations for the next spectral data set of Mars
Abstracts (In Adobe Acrobat PDF Format)
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Bell, J., Fifty Years Of Mars Surface and Atmospheric Composition from Telescopes: Highlights and Implications For Spacecraft Studies
Clark, R., Mapping the Surface Mineralogy of Hydrothermal Alteration Systems: Applications to the Geologic History of Mars and the Search for Past Life
Farrand, W., Sub-pixel Detection and Mapping of Spectrally Unique Materials on Mars using ISM Data
Farmer, J., Environmental and Mineralogical Controls on Fossilization: Key Elements in a Strategy for Mars Exopaleontology
Erard, S., What ISM told us about Mars
Erard, S. and J-P. Bibring, OMEGA, the Imaging Spectrometer On Board Mars Express
Hanel, R., 1971 Mariner Mars Infrared Interferometer Spectrometer (IRIS)
Hansen, G., Remote Sensing Spectroscopy of the Polar Regions of Mars
Herr, K. and L. Kirkland, 1969 Mariner Mars Infrared Spectrometer (IRS): Lessons for Future Exploration
Keim, E., The SEBASS Hyperspectral Imaging Spectrograph: Instrument Description and Sample Thermal Images Obtained Near Flagstaff, Arizona and Mesquite, Nevada
Mustard, J., Review of the 1989 ISM Instrument and Results
Pieters, C., J. F. Mustard, and S. L. Murchie, Aladdin Instruments at Mars
Young, S., Use of Thermal Hyperspectral Imagery in Terrestrial Surface Characterization
Members of the Mars infrared spectral community desired to assess what spectral instrument will best serve the Mars program and spectral community after the successful flight of currently planned instruments. It was felt this issue needed to be addressed, given the shift of the NASA Mars program toward a search for regions conducive to the preservation of biomarkers, and the desire for sample return. To this end, leaders of the planetary community with expertise in spectroscopy and remote mineral identification met to discuss the state of understanding of Mars surface composition, and to assess what critical gaps may exist: 1) after the successful completion of planned measurements of Mars; and 2) in research programs to support investigations of the current and planned data sets. Participants also discussed the proposed Mars airplane. This report summarizes our consensus.
To support the selection of landing sites that may preserve biomarkers, participants agreed that the most critical gap that will remain is a spectral data set containing very high information content spectra of targeted regions. Mineralogy is an essential tool to assess ancient and modern environments on Mars that may have been conducive to the support and preservation of life and biomarkers. Reflectance and emission spectroscopy remain the most capable method for remote mineral identification. Experience gained from spectral data sets of Mars and Earth has shown that an unambiguous interpretation requires spectra with both high spatial resolution and very high information content. High information content is obtained by measuring with broad spectral range, high spectral resolution, and high signal to noise ratio.
Participants concluded that there are two critical gaps in the ability of the community to interpret current and planned spectral data sets. First is a lack of a widely accepted method to quantitatively examine remotely sensed spectra. Second is the lack of adequate spectral libraries available to the entire community that contain the needed range of minerals, coatings, and particle sizes.
Selecting among potential landing and sample return sites will be aided by a clear, unambiguous interpretation of spectra measured from orbit. To provide adequate support for the landing site selection process, we recommend the measurement from orbit of high information content spectra of targeted regions, and the development of the two listed research areas. This will provide essential tools in the phased approach to Mars exploration that NASA has developed. Additional details on workshop recommendations are contained in the Letters within this report. We strongly encourage NASA and the Mars community to consider these recommendations in planning for future research programs.
Sincerely,
Participants of the workshop, "Spectroscopy of the Martian Surface: What Next?"
Jim Bell Diana Blaney Phil Christensen Ben Clark Roger Clark Stephane Erard Jack Farmer William Farrand Rudy Hanel Gary Hansen Ken Herr Eric Keim Laurel Kirkland Melissa Lane Paul Lucey Richard Morris Scott Murchie John Mustard Carle Pieters Jack Salisbury Steve Saunders Allan Treiman Steve Young
|
Participant |
Affiliation, and instruments built/building |
|
Jim Bell |
Cornell University |
|
Diana Blaney |
Jet Propulsion Laboratory |
|
Phil Christensen |
Arizona State University; 1997 TES PI; 2001 THEMIS PI; '01, '03, '05 Mini-TES PI |
|
Ben Clark |
Lockheed-Martin |
|
Roger Clark |
USGS; 1997 TES Co-I |
|
Stéphane Erard |
CNES |
|
Jack Farmer |
Arizona State University |
|
William Farrand |
Space Science Institute |
|
Rudy Hanel |
GSFC (retired); 1971 IRIS PI |
|
Gary Hansen |
U. Hawaii |
|
Ken Herr |
Aerospace Corporation; 1969 IRS Co-I |
|
Eric Keim |
Aerospace Corporation |
|
Laurel Kirkland |
Lunar and Planetary Institute; Convener |
|
Melissa Lane |
NASA-JSC |
|
Paul Lucey |
U. Hawaii |
|
Richard Morris |
NASA-JSC |
|
Scott Murchie |
Johns Hopkins U.-Applied Physics Laboratory |
|
John Mustard |
Brown University |
|
Carlé Pieters |
Brown University |
|
Jack Salisbury |
Johns Hopkins University |
|
Steve Saunders |
Jet Propulsion Laboratory |
|
Allan Treiman |
Lunar and Planetary Institute |
|
Steve Young |
Aerospace Corporation |
This workshop had an unusual breadth of researchers present, and included expertise in spectroscopy of Mars, Earth, and the moon; from the both NASA and the DOD/Intelligence community; and in laboratory spectral research and computational spectral analysis.
However, an interesting historical note was the presence of all three builders of the only thermal infrared spectrometers ever sent to Mars. It is the first, and will perhaps be the only time, that all three have been together:
Click here for larger image
Photo Credit: Debra Rueb, LPI Staff Photographer
Taken during the workshop, at the entry to the LPI
Recommendations: Next Spectral Data Set
On June 10 - 11, 1999 the workshop "Spectroscopy of the Martian Surface: What Next?" was held at the Lunar and Planetary Institute in Houston, TX. At this workshop, leaders of the science community with expertise in spectroscopy and remote mineral identification met to discuss the state of understanding of Mars surface composition, and to assess what critical gaps may exist after the successful completion of currently planned Mars missions. Participants agreed that the most critical gap that will remain is a spectral data set containing targeted, very high information content measurements to support the selection of landing sites that may preserve biomarkers. This letter summarizes the consensus of the participants.
Should the currently planned instruments complete their objectives, then we feel that the global reconnaissance mapping of Mars will be completed. The Global Surveyor TES will provide global measurements of Mars using emission spectroscopy (6 - 50 µm) at 3 km spatial resolution. This will be complemented in 2001 by multispectral visible and thermal infrared imaging at <100 m/pixel (MARCI and THEMIS), and in 2003 by hyperspectral visible and near-infrared imaging (0.4 to 5.0 µm) at 2 km/pixel (Mars Express OMEGA).
The next instrument should measure spectra of targeted regions to support lander site selection. Mineralogy is an essential tool to assess ancient and modern environments on Mars that may have been conducive to the support and preservation of life and biomarkers. Reflectance and emission spectroscopy remain the most capable method for remote mineral identification. It is likely that the global data sets (TES, THEMIS, MARCI, OMEGA) can be used to identify many potential sites for lander science measurements and sample return. Experience gained from spectral data sets of Mars and Earth has shown that an unambiguous interpretation of a complex region requires spectra with both high spatial resolution and very high information content. Selecting the most desirable landing site will require this type of data set. High information content is obtained by measuring with broad spectral range, high spectral resolution, and most importantly high signal to noise ratio. The data set should not be global, but should focus on the most promising sites identified from the global data sets. The proposed Ariane piggyback micromissions will lack the payload for an instrument capable of making these measurements.
Neither reflectance nor emission spectroscopy alone is sufficient to uniquely determine the full range of minerals that may be present, as each method is sensitive to different physical processes. Together they provide the best capability to identify the surface mineralogy. The broader the spectral range, the less ambiguous the interpretations, and the more technical the justification for selecting a particular landing site.
Interpretation of current and planned data sets will require access by the community to spectral libraries that contain measurements of materials of interest over the full wavelength range of the spacecraft instruments (0.4 - 50 µm). To facilitate site selection, spectral libraries should be expanded and made available to the community.
On the basis of our extensive experience with laboratory, planetary, and terrestrial spectroscopy, the workshop participants identified the following instrument characteristics required to best select among potential landing sites:
Such an instrument would provide an essential tool in the phased approach to Mars exploration that NASA has developed. We strongly encourage NASA and the Mars community to consider these recommendations in planning for future missions.
Sincerely,
Participants of the workshop, "Spectroscopy of the Martian Surface: What Next?"
|
Jim Bell |
Diane Blaney |
Phil Christensen |
|
Ben Clark |
Roger Clark |
Stéphane Erard |
|
Jack Farmer |
William Farrand |
Rudy Hanel |
|
Gary Hansen |
Kennneth Herr |
Eric Keim |
|
Laurel Kirkland |
Melissa Lane |
Paul Lucey |
|
Richard Morris |
Scott Murchie |
John Mustard |
|
Carlé Pieters |
John Salisbury |
Steve Saunders |
|
Allan Treiman |
Steve Young |
|
Recommendations: Supporting Research
Summary Recommendations: Spectroscopic remote sensing of surface composition has been of critical importance to our current understanding of Mars, as well as other planets. Spectroscopy, especially high resolution spectroscopy, will continue to be of great importance for future Mars exploration and is particularly important for assessing present and past environments in the search for evidence of life. There are two areas that need more emphasis by Research and Analysis Programs: 1) Measurement and public archiving of spectra covering the range 0.4 - 50 µm; and 2) Testing of quantitative mineral analysis methods. Participants also felt there should be additional discussion of what materials should be measured, and how the data should be archived.
Background. On June 10 - 11, 1999 the workshop "Spectroscopy of the Martian Surface: What Next?" was held at the Lunar and Planetary Institute in Houston, TX. At this workshop, leaders of the planetary community with expertise in spectroscopy and remote mineral identification met to discuss the state of understanding of Mars surface composition, and to assess what critical gaps may exist in planned measurements of Mars and supporting research programs. This letter summarizes our consensus about the supporting research programs.
Knowledge of surface composition is an essential tool to assess ancient and modern environments on Mars that may have been conducive to the support and preservation of life and biomarkers. Reflectance and emission spectroscopy are the most capable method for remote compositional mapping. Participants concluded that there remain several critical needs in the ability of the community in order to reliably interpret current and planned spectral data sets. One is the unavailability of supporting spectral libraries that contain diverse measurements over the entire wavelength range measured by current and planned spectrometers (0.4 - 50 µm). Another is the need to test and compare currently available analytical methods that are used to quantitatively examine remotely sensed spectra.
Laboratory spectra. Two factors are essential for detection and quantification of surface materials: high information content spectra of Mars, and high quality laboratory spectra. Participants concluded that a lack of access by the entire community to measurements over the full wavelength range measured by current and planned spectrometers (0.4 - 50 µm) seriously impedes interpretations. Measurement of diverse materials relevant to active processes and the environment of Mars over the full wavelength range should be encouraged by current Research and Analysis Programs. This community effort will be strongly aided by insuring that there is a community measurement facility capable of measuring the entire 0.4 - 50 µm range. It is essential to the success of this integrated approach that spectral data measured under this program are publicly archived, and that the materials measured are well-characterized.
Quantitative methods. Workshop participants concluded that there is a strong need to test and evaluate currently available identification and unmixing algorithms. An important baseline could be established through blind measurements by different algorithm proponents of prepared samples representing increasing degrees of difficulty.
Participants also felt quantitative methods will be advanced by the development of liaisons to similar research programs, such as those developed by Department of Defense and Intelligence agencies. One goal should be to test and incorporate knowledge from these other programs into the NASA community, perhaps by inviting them to participate in the blind measurement program.
Additional discussions. Participants concluded there should be additional public discussion of what materials should be measured, and how the data should be archived. Materials discussed included weathering materials and coatings, and poorly crystalline materials that may be present on Mars. The workshop did not have the goal of addressing these issues, and no consensus was reached, but these issues were felt to be of sufficient importance to warrant further discussion.
Recommendations. Selecting among potential landing sites will be aided by measuring targeted, high information content spectra from orbit, followed by clear, unambiguous interpretations of the spectra. Community access to measurements over the full wavelength range covered by current and planned instruments, and the development and testing of quantitative analysis methods will provide the enabling foundation and data analysis tools that are essential to the phased approach to Mars exploration that NASA has developed. We strongly encourage NASA and the Mars community to consider these recommendations in planning for future research programs.
Sincerely,
Participants of the workshop, "Spectroscopy of the Martian Surface: What Next?"
|
Jim Bell |
Phil Christensen |
Ben Clark |
|
Roger Clark |
Stéphane Erard |
Jack Farmer |
|
William Farrand |
Rudy Hanel |
Gary Hansen |
|
Kennneth Herr |
Eric Keim |
Laurel Kirkland |
|
Melissa Lane |
Paul Lucey |
Scott Murchie |
|
John Mustard |
Carlé Pieters |
John Salisbury |
|
Steve Saunders |
Allan Treiman |
Steve Young |
Recommendations: Mars Airplane
Participants felt that with the successful completion of the currently planned remote sensing instruments (TES on Mars Global Surveyor, THEMIS on Mars '01, and OMEGA on Mars Express '03), the next step for Mars surface spectroscopy is targeted imaging spectroscopy at spatial scales < 100 m.
Participants recognized that the Mars Airplane could act as a science and technology demonstration mission, paving the way for the next generation of observation, provided an appropriate instrument was flown at a good location. This instrument would need to have spatial resolution of a few 10's of meters. The instrument should cover a wavelength range at sufficient spectral resolution (l / l D > 250) and signal to noise ratio (>500) to be able to identify specific diagnostic mineral spectral features. High spectral resolution is needed for definitive mineralogic characterization, because the currently planned global survey products will likely be sufficient to identify candidate locations that may contain mineral deposits conducive to preservation of a fossil record. However, a data product capable of prioritizing and characterizing in more detail an interesting site at higher spatial and spectral resolution than is currently planned is of high interest to the community.
While imaging spectroscopy is desirable, a profiling spectrometer taking spectra along the airplane track would also return scientifically useful data, provided it was registered to images. However, a poorly chosen instrument or one flown to a location where the geologic setting would not predict mineralogical variations could be a serious setback in the overall goal of exploring Martian mineralogy at these spatial scales.
James Bell402 Space Science Cornell University Ithaca, NY 14850 email: [email protected] phone: 607-255-5911 fax: 607-255-9002 Diana Blaney 4800 Oak Grove Dr. M/S 183-501 Pasadena, CA 91109-8099 phone: 818-354-5419 fax: 818-354-0966 email: [email protected] Philip Christensen Mail Code 1404 Dept. of Geology Arizona State University Tempe, AZ 85287-1404 phone: 602-965-1790 fax: 602-965-8102 email: [email protected] Benton Clark Mail Stop 5-8001 Lockheed Martin Astronautics PO Box 179 Denver, CO 80201 phone: 303-971-9007 fax: 303-977-3600 email: [email protected] Roger Clark US Geological Survey P.O. Box 25046, MS 964 Denver, CO 80225 phone: 303-236-1332 email: [email protected] Stéphane Erard IAS bât. 121 Université Paris-Sud F-91405 Orsay, France email: [email protected] Jack Farmer Mail Code 1404 Dept. of Geology Arizona State University Tempe, AZ 85287-1404 phone: 602-965-6748 fax: 602-965-8102 email: [email protected] William Farrand Farr View Consulting Westminster, CO 80234 phone: 303-450-1128 fax: 303-280-1531 email: [email protected] Rudolf A. Hanel 3881 Bridle Pass Ann Arbor, MI 48108-2264 phone: 734-913-2015 Gary Hansen University of Hawaii at Manoa Hawaii Institute of Geophysics and Planetology School of Ocean and Earth Science and Technology 2525 Correa Road Honolulu, HI 96822 phone: 808-956-3163 fax: 808-956-6322 email: [email protected] Kenneth Herr The Aerospace Corporation Mail Station M5/747 2350 East El Segundo Blvd. El Segundo, CA 90245-4691 phone: 310-336-5620 fax: 310-336-6524 email: [email protected] Eric Keim The Aerospace Corporation Mail Station M5/747 2350 East El Segundo Blvd. El Segundo, CA 90245-4691 phone: 310-336-1419 fax: 310-336-1636 email: [email protected] Laurel Kirkland Lunar and Planetary Institute/Rice University 3600 Bay Area Blvd. Houston, TX 77058-1113 phone: 281-486-2107 fax: 281-486-2162 email: [email protected] Melissa Lane Lyndon B. Johnson Space Center NASA, Code SN3 Building: 31, Room 102 2101 NASA Road 1 Houston, TX 77058 email: [email protected] Paul Lucey University of Hawaii at Manoa Hawaii Institute of Geophysics and Planetology School of Ocean and Earth Science and Technology 2525 Correa Road Honolulu, HI 96822 phone: 808-956-3137 fax: 808-956-6322 email: [email protected] Richard Morris Lyndon B. Johnson Space Center NASA, Code SN3 Building: 31, Room 102 2101 NASA Road 1 Houston, TX 77058 phone: 281-483-5040 email: [email protected] Scott Murchie JHU-APL John Hopkins Rd. Laurel, MD 20723-6099 phone: 240-228-6235 fax: 240-228-6670 email: [email protected] John F. Mustard Department of Geological Sciences Box 1846 Brown University Providence, RI 02912 phone: 401-863-1264 fax: 401-863-3978 email: [email protected] Carle Pieters Department of Geological Sciences Box 1846 Brown University Providence, RI 02912-1846 phone: 401-863-2417 fax: 401-863-3978 email: [email protected] John W. Salisbury 84 Cochise Ct. Palm Coast, FL 32137 phone: 904-446-8457 fax: 904-446-1749 email: [email protected] R. Stephen Saunders Chief Scientist Solar System Exploration Office Space and Earth Science Programs Directorate Jet Propulsion Laboratory Mail Stop 180-701 4800 Oak Grove Drive Pasadena, CA 91109 phone: 818-354-2867 fax: 818-393-0712 email: [email protected] Allan Treiman Lunar and Planetary Institute 3600 Bay Area Blvd. Houston, TX 77058-1113 phone: 281-486-2117 fax: 281-486-2162 email: [email protected] Steve Young The Aerospace Corporation Mail Station M5/747 2350 East El Segundo Blvd. El Segundo, CA 90245-4691 fax: 310-336-1636 email: [email protected]
* = presenter
7:45 Registration
8:15 Welcome, Introductory remarks
PRESENTATIONS I
8:30 a.m.
Chair: Carlé Pieters
Format: Each talk is 15-20 minutes, followed by a 15-10 minute discussion/questions period.
Mars program + sample return
8:30 Steve Saunders*, Spectroscopy for Mars Exploration
9:00 Jack Farmer*, Environmental and Mineralogical Controls on Fossilization: Key Elements in a Strategy for Mars Exopaleontology
Past/Current data sets
9:30 Jim Bell*, Fifty Years Of Mars Surface and Atmospheric Composition from Telescopes: Highlights and Implications For Spacecraft Studies
10:00 Ken Herr*, 1969 Mariner Mars Infrared Spectrometer (IRS): Lessons for Future Exploration
10:30 BREAK
10:45 Rudy Hanel*, 1971 Mariner Mars Infrared Interferometer Spectrometer (IRIS)
11:15 John Mustard*, Review of the 1989 ISM Instrument and Results
11:45 Phil Christensen*, Mars Surface Mineralogy and Petrology from 1997 MGS TES Data
LUNCH
12:15
PRESENTATIONS II
1:30 p.m.
Chair: John Salisbury
Format: 15 minute talk + 10 minute questions/discussion. The combined Mini-TES/THEMIS talk is 25 minutes +15 for questions/discussion.
Planned and terrestrial data sets
1:40 Carlé Pieters*, J. F. Mustard, and S. L. Murchie, Aladdin Instruments at Mars
2:05 Phil Christensen*, Overview of the Mini-TES and THEMIS Instruments for the Mars 2001 Surveyor Mission
2:45 Paul Lucey*, A Strategy for Future Mars Spectral Remote Sensing: An Outsider's Opinion
3:10 BREAK
MODERATED PANEL DISCUSSION
3:25 p.m.
Moderator: John Mustard
Format: Each panelist has a 10 minute talk, and 5 minute questions/discussion. Followed by 60 minute discussion.
3:25 Visible/Near-IR: Roger Clark
3:40 Thermal IR: Phil Christensen
3:55 Both: Jack Salisbury
4:10 "Outside the community" spectroscopist: Paul Lucey
4:25 Surface studies: Ben Clark
4:40 Discussion (60 minutes)
GROUP DINNER
6:30
The Italian Café
Friday, June 10, 1999
PRESENTATIONS III
8:15 a.m.
Chair: Allan Treiman
Format: 15 minute talk, then 10 minute discussion/questions.
8:15 Introductory remarks.
8:25 Diana Blaney* and D. Glenar, In Situ Spectrometers for Martian Mineralogy
8:50 Roger Clark* Mapping the Surface Mineralogy of Hydrothermal Alteration Systems: Applications to the Geologic History of Mars and the Search for Past Life
9:15 William Farrand*, Sub-pixel Detection and Mapping of Spectrally Unique Materials on Mars using ISM Data
9:40 Gary Hansen*, Remote Sensing Spectroscopy of the Polar Regions of Mars
10:05 BREAK
10:20 Eric Keim*, The SEBASS Hyperspectral Imaging Spectrograph: Instrument Description and Sample Thermal Images Obtained Near Flagstaff, Arizona and Mesquite, Nevada (15 minutes + 5 for questions)
10:40 Steve Young*, Use of Thermal Hyperspectral Imagery in Terrestrial Surface Characterization (15 minutes + 5 for questions)
LUNCH (brought in)
11:00
WORKSHOP REPORT MODERATED DISCUSSION
11:45 p.m.
Moderator: Paul Lucey
11:45 Discussion
The discussion will begin with any major issues left unresolved from the panel discussion, and then will address submitted questions.
ADJOURN
2:45
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