CCSD3ZF0000100000001NJPL3IF0PDS20000000001 = SFDU_LABEL RECORD_TYPE = STREAM INSTRUMENT_HOST_NAME = ("NASA DC-8", "NASA C-130", "NASA ER-2" , "FIELD EXPERIMENT") INSTRUMENT_ID = ("ASAR", "ASAS", "AVIR", "AWND", "DAED", "GPSM", "HSTP", "PARB", "PFES", "REAG", "RMTR", "SHYG", "SIRS", "THRM", "TIMS", "WTHS") TARGET_NAME = EARTH FILE_TITLE = "GEOLOGIC REMOTE SENSING FIELD EXPERIMENT DATA" END Archive of Geologic Remote Sensing Field Experiment Data Release 1.0 May 13, 1991 Raymond E. Arvidson, Mary A. Dale-Bannister, Edward A. Guinness, Susan H. Slavney, and Thomas C. Stein Planetary Data System Geosciences Node Department of Earth and Planetary Sciences McDonnell Center for the Space Sciences Washington University St. Louis, Missouri With input from: Ronald Greeley, Arizona State University Nicholas Lancaster, Desert Research Institute, Reno, Nevada Lisa Gaddis, Arizona State University James R. Irons, Goddard Space Flight Center David Harding, Goddard Space Flight Center Don Deering, Goddard Space Flight Center James B. Garvin, Goddard Space Flight Center Diane L. Evans, Jet Propulsion Laboratory Thomas Farr, Jet Propulsion Laboratory Bruce Jakosky, University of Colorado Fred A. Kruse, University of Colorado William Farrand, University of Arizona Jeffrey J. Plaut, Washington University Shelley B. Petroy, Washington University Kathy Young, University of Colorado Robert Singer, University of Arizona James Conel, Jet Propulsion Laboratory Carol Bruegge, Jet Propulsion Laboratory i TABLE OF CONTENTS 1. INTRODUCTION ................................................... 1 2. GRSFE OBJECTIVES ............................................... 3 3. OVERVIEW OF GRSFE REQUIREMENTS AND IMPLEMENTATION .............. 7 3.A. SITE SELECTION ............................................... 7 3.B. AIRBORNE CAMPAIGN ............................................ 10 3.C. FIELD CAMPAIGN ............................................... 11 3.D. NARRATIVE OF FIELD CAMPAIGN ACTIVITIES ....................... 12 4. MODELING SITE DESCRIPTIONS ...................................... 17 5. UNIVERSITY OF COLORADO DIRECTIONAL EMISSIVITY EXPERIMENT ....... 21 6. FIELD DATA SETS ................................................ 25 6.A. PHOTOGRAPHS .................................................. 25 6.B. SAMPLES ...................................................... 26 6.C. VISIBLE AND REFLECTED INFRARED SURFACE DATA .................. 26 6.C.1. DAEDALUS SPECTROMETER ...................................... 26 6.C.1.1. INSTRUMENT DESCRIPTION ................................... 26 6.C.1.2. DATA SET DESCRIPTION ..................................... 27 6.C.2. PARABOLA ................................................... 28 6.C.2.1. INSTRUMENT DESCRIPTION ................................... 29 6.C.2.2. DATA SET DESCRIPTION ..................................... 31 6.C.3. SIRIS SPECTROMETER ......................................... 33 6.C.3.1. INSTRUMENT DESCRIPTION ................................... 33 6.C.3.2. DATA SET DESCRIPTION ..................................... 34 6.D. THERMAL INFRARED SURFACE DATA ................................ 36 6.D.1. PORTABLE FIELD EMISSION SPECTROMETER (PFES) ................ 36 6.D.1.1. INSTRUMENT DESCRIPTION ................................... 36 6.D.1.2. DATA SET DESCRIPTION ..................................... 38 6.E. ATMOSPHERIC DATA ............................................. 39 6.E.1. REAGAN RADIOMETER .......................................... 39 6.E.1.1. INSTRUMENT DESCRIPTION ................................... 39 6.E.1.2. DATA SET DESCRIPTION ..................................... 39 6.E.2. SPECTRAL HYGROMETER ........................................ 40 6.E.2.1. INSTRUMENT DESCRIPTION ................................... 40 6.E.2.2. DATA SET DESCRIPTION ..................................... 40 6.E.3. ARIZONA STATE UNIVERSITY WIND EXPERIMENT ................... 41 6.E.3.1. INSTRUMENT DESCRIPTION ................................... 41 6.E.3.2. DATA SET DESCRIPTION ..................................... 41 6.E.4. WEATHER STATION ............................................ 42 6.E.4.1. INSTRUMENT DESCRIPTION ................................... 42 6.E.4.2. DATA SET DESCRIPTION ..................................... 42 6.F. GEOPOSITIONAL SATELLITE PROFILES ............................. 42 6.G. PROFILES FROM HELICOPTER-BORNE STEREOPHOTOGRAPHY ............. 44 7. AIRBORNE DATA SETS ............................................. 44 7.A. ASAS ......................................................... 44 7.A.1. INSTRUMENT DESCRIPTION ..................................... 44 7.A.2. DATA SET DESCRIPTION ....................................... 46 7.B. AVIRIS ....................................................... 47 7.B.1. INSTRUMENT DESCRIPTION ..................................... 47 7.B.2. DATA SET DESCRIPTION ....................................... 48 7.C. TIMS ......................................................... 49 7.C.1. INSTRUMENT DESCRIPTION ..................................... 49 ii 7.C.2. DATA SET DESCRIPTION ....................................... 51 7.D. AIRSAR ....................................................... 52 7.D.1. INSTRUMENT DESCRIPTION ..................................... 52 7.D.2. DATA SET DESCRIPTION ....................................... 52 8. SOFTWARE ....................................................... 54 9. FLIGHT LINE LOCATOR MAPS ....................................... 54 10. GRSFE SAMPLER DATA SETS ........................................ 54 11. INDEX TABLES ................................................... 55 12. DATA SET LABEL AND FILE ORGANIZATION ........................... 56 13. DISK DIRECTORY STRUCTURE AND FILE NAMES ........................ 58 14. RELEVANT BIBLIOGRAPHY .......................................... 60 APPENDIX A - CD-ROM VOLUME, DIRECTORY AND FILE STRUCTURES .......... 67 A.1 VOLUME AND DIRECTORY STRUCTURES ............................... 67 A.2 FILE STRUCTURE ................................................ 67 A.2.1 FIXED-LENGTH FILES .......................................... 67 A.2.2 STREAM FILES ................................................ 67 A.2.3 EXTENDED ATTRIBUTE RECORDS .................................. 68 APPENDIX B - SYNTACTIC RULES OF KEYWORD ASSIGNMENT STATEMENTS ...... 69 B.1 INTEGER NUMBERS ............................................... 69 B.2 REAL NUMBERS .................................................. 69 B.3 DATES AND TIMES ............................................... 70 B.4 LITERAL VALUES ................................................ 70 B.5 TEXT CHARACTER STRINGS ........................................ 70 APPENDIX C - KEYWORD DEFINITIONS ................................... 71 APPENDIX D - GRSFE AIRBORNE AND FIELD INSTRUMENTS .................. 76 TABLE D.1 GRSFE AIRBORNE REMOTE SENSING INSTRUMENTS ............... 76 TABLE D.2 ATMOSPHERIC INSTRUMENTS DEPLOYED DURING GRSFE FIELD CAMPAIGN ....................................................... 76 TABLE D.3 GROUND TRUTH INSTRUMENTS DEPLOYED DURING GRSFE FIELD CAMPAIGN ....................................................... 77 TABLE D.4 AVIRIS FLIGHT LINES ..................................... 78 TABLE D.5 ASAS AND TIMS FLIGHT LINES .............................. 80 TABLE D.6 AIRSAR FLIGHT LINES ..................................... 85 TABLE D.7 AVIRIS CROSS-REFERENCE TABLE ............................ 88 TABLE D.8 AIRSAR CROSS-REFERENCE TABLE ............................ 89 TABLE D.9 ASAS CROSS-REFERENCE TABLE .............................. 89 TABLE D.10 TIMS CROSS-REFERENCE TABLE .............................. 90 TABLE D.11 GRSFE TEAM PARTICIPANTS ................................. 91 APPENDIX E - WASHINGTON UNIVERSITY EXPERIMENT -- THERMAL MEASUREMENTS AT LUNAR CRATER VOLCANIC FIELD .................... 93 TABLE E.1 LUNAR LAKE THERMISTOR DATA ............................... 93 TABLE E.2 LUNAR LAKE THERMISTOR DATA ............................... 93 TABLE E.3 TEMPERATURE AND RELATIVE HUMIDITY AT THERMAL TEST SITE ... 94 TABLE E.4 LUNAR LAKE THERMISTOR DATA FOR MANTLED FLOW SITE PITS .... 95 TABLE E.5 RADIOMETER DATA COLLECTED AT MANTLE FLOW SITE PITS ....... 95 TABLE E.6 RADIOMETER DATA COLLECTED DURING TIMS OVERFLIGHTS ........ 96 APPENDIX F - SAMPLES COLLECTED DURING GRSFE ........................ 98 TABLE F.1 SUMMARY OF SAMPLES COLLECTED DURING GRSFE CAMPAIGN ....... 98 TABLE F.2 SOIL ANALYSES ............................................ 99 APPENDIX G - EPPLEY PYRANOMETER DATA ACQUIRED TO SUPPORT PARABOLA DATA ANALYSES .................................................. 101 APPENDIX H - GRSFE CD-ROM ARCHIVE VOLUME AND DIRECTORY STRUCTURE.... 107 1 1. INTRODUCTION This document provides an overview of the objectives, requirements, implementation, data processing, and archiving for the Geologic Remote Sensing Field Experiment (GRSFE). It also describes GRSFE sampler data sets that provide examples of the products that can be generated from the airborne observations. GRSFE consisted of coordinated airborne remote sensing and field observations over geological targets in the Mojave Desert, California, and the Lunar Lake Volcanic Field, Nevada in July, September and October of 1989. GRSFE was funded by NASA's Planetary Geology and Geophysics Program, the Geology Program, the Planetary Data System, the Pilot Land Data System, the Mars Observer Project, and the Magellan Project. The GRSFE archive is maintained and updated by the Planetary Data System Geosciences Node at Washington University, in collaboration with the Pilot Land Data System. Release of Version 1.0 of the GRSFE archive on a set of CD-ROMs is meant to provide a well documented data set collection for research and teaching. Release on CD-ROMs also provides concrete examples of archived data using Planetary Data System and Pilot Land Data System standards (e.g. Martin et al., 1988). The intent of this document is to provide information needed for researchers to understand why and how GRSFE was implemented, the structure and content of the data sets that comprise the archive, and how the various observations can be used in a synergistic fashion to address geological remote sensing problems. We note that the GRSFE archive is dynamic, and release of Version 1.0 on CD-ROMs should be viewed as a convenient way to ensure wide distribution. A few data sets were not ready for this release. These data sets include: (a) ATLAS laser altimetric profiles of selected sites; (b) AIRSONDE balloon measurements of atmospheric temperature, pressure, and relative humidity, (c) PIDAS field spectral reflectance observations, (d) vegetation analyses of sites in the Lunar Crater Volcanic Field, Nevada; and (e) a number of topographic profiles extracted from helicopter-borne stereophotography. We hope to release these data sets in the future as an addendum to Version 1.0. We will also concurrently release an updated version of this VOLINFO.TXT document. GRSFE was possible because of the expertise and interest of the Science Steering Group (SSG), field participants, and personnel who have been involved in data reduction, processing, and documentation. These personnel are listed in Table 1.1 and are hereby thanked for their advice and work. Special thanks are extended to the Science Steering Group for their advice and work throughout GRSFE. We thank Joseph Boyce, Theodore Maxwell, and Miriam Baltuck, NASA Headquarters, for insight and support, and we also thank the High and Medium Altitudes Branches of the Ames Research Center for their efforts during the data acquisition phase of GRSFE. Finally, we thank Susan McMahon, Gail Woodward, and Jason Hyon, Planetary Data System, for their support and work, and Blanche Meeson, Pilot Land Data System, for her interest in the GRSFE archive. 2 GRSFE objectives and requirements are described in the next two sections of this document. Summaries of the airborne and field campaigns are then provided, followed by data set descriptions. This document ends with a discussion of the formats and the directory structure used for the data sets, and CD-ROMs, respectively. Appendices provide specific details on formats and keywords used on the CD-ROM, and also contain some data tables and ancillary information. TABLE 1.1 GRSFE PARTICIPANTS Arizona State University ------------------------- Ronald Greeley - Science Steering Group (SSG) Member Lisa Gaddis Nicholas Lancaster Goddard Space Flight Center ------------------ James R. Irons - SSG Member Don Deering - SSG Member James B. Garvin - SSG Member David Harding Jet Propulsion Laboratory --------------------- Diane Evans - SSG Co-Chair Elsa Abbott Carol Bruegge Fred Burnette James Conel Pascal Dubois Thomas Farr - SSG Member Rob Green Gordon Hoover John Holt Phil Hughes Howell Johnson Anne Kahle - SSG Member Mike Kobrick Joel Norris Jeff Plescia Jakob van Zyl - SSG Member Gregg Vane Michele Vogt Steve Wall - SSG Member Cathy Weitz Rich Zurek Stanford University ----------------------- Richard Simpson - SSG Member 3 USGS -------- John Dohrenwend University of Arizona ------------------------ Bill Farrand Paul Geissler Jeff Kargel Robert Singer - SSG Member University of California ------------------------ Susan Ustin University of Colorado ------------------------ Jose Aguirre Bruce Jakosky - SSG Member John Dietz Gary Finiol Alex Goetz Bradley Henderson Fred Kruse - SSG Member Kathy Young University of Nevada, Reno -------------------------- John Perry University of Washington ------------------------- Alan Gillespie Washington University ----------------------- Raymond E. Arvidson - SSG Co-chair Kristy Chamberlain Mary A. Dale-Bannister Glen Green Edward A. Guinness - SSG Member Shelley B. Petroy Jeffrey J. Plaut Susan H. Slavney Thomas C. Stein 2. GRSFE OBJECTIVES The primary GRSFE objectives were: (a) to acquire airborne remote sensing and field data in a coordinated campaign for key geological targets, e.g., alluvial fans, dunes, lava flows, volcanoes, etc.; (b) to reduce and document the data and deliver the archive to the Planetary 4 Data System (PDS) and the Pilot Land Data System (PLDS); (c) to take advantage of the multisensor approach, allowing cross-comparison of results acquired with different wavelengths and facilitating rigorous characterization of surfaces using multiple wavelength intervals; (d) to use results to test quantitative models for the extraction of surface property information from remote sensing data for Earth (e.g., Earth Observing System), Moon (e.g., Lunar Observer), Mars (e.g., Mars Observer), and Venus (e.g., Magellan); and (e) to use data in prototype EOS studies focused on the nature and ages of geological features and implications for regional climatic and tectonic histories. Table 2.1 shows relevant remote sensing instruments currently flying or scheduled to be flown on upcoming missions. The spaceborne missions will acquire new, detailed information about materials exposed on the surfaces of Venus, Mars, and Earth, respectively. For example, multiple incidence angle observations with the Magellan radar system and altimeter provide information about the Fresnel reflectivity and the roughness of the Venusian surface. The EOS SAR and its precursor, the Shuttle Imaging Radar (SIR-C), will provide multiple frequency, multiple incidence angle polarimetric data for the Earth's surface. The French ISM instrument on PHOBOS II measured the reflected infrared spectrum of Mars with approximately 22 km footprint widths for the equatorial latitudes. VIMS on some Mars mission, and HIRIS on EOS, are imaging spectrometers that will acquire detailed spectral reflectances in an image context. Similar capabilities will exist in the thermal infrared, with TES on Mars Observer. The EOS MODIS-T and MISR instruments will acquire multi-emission angle data to help in deciphering atmospheric and surface scattering and absorption. The TES system will also be used to acquire multi-emission angle data for given areas. The visible through microwave data to be acquired by the various spaceborne instruments will be used to extract information on mineralogy and composition (e.g., from locations, depths, shapes of absorption features due to electronic and vibrational processes) and on selected physical properties (e.g., grain size and degree of packing, macro-scale roughness) associated with surface materials. Appendices D-1, D-2, and D-3 contain detailed information about the airborne and field instruments used in the GRSFE campaign. GRSFE was designed to use, to the extent possible, instruments similar to those used or to be used on the space missions discussed in the last paragraph. Further, the GRSFE instruments acquired data for surfaces that are roughly analogous to those found on Mars and Venus, and that are likely to be regions of study with EOS data. Also, the GRSFE airborne and ground campaign was designed to ensure that the objective of testing quantitative data reduction models for regions with extensive ground truth would be met. For reference, Table 2.2 illustrates the types of analyses that the NASA-supported science community is currently pursuing using GRSFE data. The spaceborne missions of the 1990s will result in high volume, complex data sets that will present major archiving challenges. Thus, another major GRSFE objective was to explore the extent to which PDS and PLDS standards and guidelines could be used to facilitate archiving a 5 modestly complex set of data. The extent to which the Version 1.0 release of the GRSFE archive will be used by the research community will provide direct information on the utility of the standards and guidelines, and our overall archiving approach. TABLE 2.1 SELECTED EARTH AND PLANETARY REMOTE SENSING INSTRUMENTS Instrument Brief Description EOS HIRIS Earth Observing System Imaging (High Resolution Spectrometer with 192 bands covering 0.4 Imaging Spectrometer) to 2.5 micrometer with 10 nm sampling. 30 km swath with 30 m pixels. Pointable +60 degrees +/-30 degrees along track and 24 degrees cross track. EOS ASTER Broad band EOS thermal IR mapper. (Advanced Spaceborne Thermal Emission and Reflectance Radiometer) EOS MODIS EOS moderate resolution imaging (Moderate Resolution spectrometer. Two optical packages, Imaging Spectrometer) including MODIS-T (tilt) and MODIS-N (nadir view). MODIS-T capable of 60 degrees pointing along track. 52 bands between 0.4 to 12 micrometer. 1500 km width with 0.5 to 1.0 km pixels. To be augmented with MISR. EOS SAR EOS radar system operating at 3.5 cm (X- (Synthetic Aperture band), 5.66 cm (C-band), 23.98 cm Radar) (L-band). Incidence angles between 15 to 55 degrees. C, L bands have polarimetric capability. High resolution mode will have 20 to 30 m pixels, 30 to 50 km cross track widths. Magellan Radar S-band (12.6 cm) altimeter. Allows Altimeter estimates of elevation, quasi-specular roughness, and Fresnel reflection coefficient. Magellan Radar System S-band SAR with approximately 150 m best radar resolution. HH (or VV) polarization. Multiple incidence angle coverage during extended mission by 6 rotating spacecraft for given area. Incidence angle varies with latitude. TES Mars Observer instrument covering (Thermal Emission thermal IR with high spectral Spectrometer) resolution. Also broad band channel for VISIR radiance. Three km pixels. VIMS Imaging Spectrometer covering (Visible and Infrared approximately 0.3 to 5.0 micrometers Mapping Spectrometer) with high spectral resolution. Will fly on some Mars Mission. TABLE 2.2 EXAMPLES OF USE OF GRSFE DATA - To test multi-spectral radiative transfer models for scattering and emission from planetary surfaces, including: - Use data to evaluate procedures for separation of macroscale roughness (Hapke rms; grain size, packing; radar-derived roughness) from other surface properties (dielectric constant, refractive index, emissivity). - Use AVIRIS, ASAS, TIMS to understand mixed pixels (including shade and aeolian components) for studies to determine the composition of the upper 100 micrometer of an outcrop. - Use TIMS data collected four times in one diurnal cycle to understand the physics of thermal emission. - Use multi-incidence angle C, L, P polarimetric SAR to test models for radar backscatter from planetary surfaces. - Use data to help establish the paleoclimatic history of the arid S.W. United States. - Use data to understand remote sensing signatures of basalt flows of varying ages and depth of aeolian fill. - Use data to develop models for crater degradation (rille development, wall slumping, etc.). - Use SAR to pursue understanding of the correlation between radar roughness and aerodynamic roughness. - Use data to support landing site selection procedures for Mars Rover Sample Return (MRSR) Mission, concentrating on extraction of roughness information. 7 3. OVERVIEW OF GRSFE REQUIREMENTS AND IMPLEMENTATION 3.A. SITE SELECTION A major task of the SSG was the selection of GRSFE sites for the coordinated airborne and field campaign. A number of site requirements were imposed, including relevance to planetary surfaces. Clearly there are no sites on Earth that simulate surface properties of Mars or Venus in detail. The surface of Mars, for example, is highly desiccated and probably has been for millions, if not billions, of years. The 750 degrees K, 90 bar carbon dioxide conditions at the Venusian surface probably lead to unique surface properties. Rather, the approach was to select sites that are roughly analogous to what we expect on planetary surfaces and, as discussed in the last section, to use GRSFE data to test models for extraction of surface property information. Volcanic terrains, aeolian deposits (e.g., sand dunes), and fluvial landscapes exist on Mars, as do an abundance of craters. Certainly, volcanic terrains and craters abound on Venus. Aeolian deposits are also seen and ancient fluvial landforms are a possibility. Thus, reasonable analog sites for Mars and Venus include volcanic, aeolian, and fluvial surfaces. The terrestrial sites also needed to be as dry as possible, relatively free of vegetation, and accessible by aircraft and from the ground. Finally the sites needed to have relevance for EOS prototype tasks, which the SSG decided were best focused on neotectonic and paleoclimatic studies. Two specific site types were defined for GRSFE. Modeling sites were designated for concentrated airborne and field observations and resultant detailed modeling of GRSFE data. These areas were characterized on the ground in enough detail to provide first-order quantitative simulations of how electromagnetic radiation interacts with geological surfaces and materials in the visible and reflected infrared, thermal infrared, and microwave wavelengths. Surface topography was obtained at a variety of length-scales. Samples were collected so that composition, mineralogy, and physical properties could be characterized close enough together and at sufficient depth intervals to be useful in modeling interactions of radiation with the sites. Various in-situ field measurements were made of both the surface and the atmosphere at the same time as the airborne campaign was underway. The modeling sites thus needed to be where extensive field work and sample collection could be accomplished. Further, the collection of sites needed to be simple enough to allow modeling of remote sensing signatures from ground data. Table 3.1 gives an overview of all GRSFE sites. The modeling sites are located in the Lunar Crater Volcanic Field. Detailed locations are given in Table 3.2. The modeling sites are discussed in more detail in Section 4 of this document. Calibration sites were defined to be regions where ground measurements were obtained to be able to calibrate the airborne data independently of any instrument-specific procedures, e.g. pre-flight and post-flight AVIRIS instrument radiometric calibrations. Logistical and financial constraints limited both the number of calibration sites and 8 the ground measurements that could be acquired at each site. We focused on field spectrometer measurements to characterize the reflectance and emittance of various surfaces. Corner reflectors were also deployed to calibrate AIRSAR. The specific calibration sites are summarized in Table 3.2. TABLE 3.1 OVERVIEW OF GRSFE FIELD SITES Lunar Crater Volcanic Field, Nevada Location: 250 km northwest of Las Vegas, NV (38 deg. 15'N, 116 deg. W). Age: Middle to late Pliocene and Pleistocene (0.015 to 4.2 m.y.). Features: - The field contains about 95 vents and at least 35 associated lava flows within a northeast-trending zone, up to 10 km wide and about 40 km long. - Vents include cinder cones, elongate fissures, and at least two maar craters. - Lava flows range up to 1.9 km wide and 6.1 km long with thicknesses of less than 3 to as much as 25 m. - Progressive degradation of the cones and flows is very similar to that displayed by other basaltic volcanic fields in the southwest Basin and Range (including the Cima, Crater Flat, and Coso fields). - Many of the flows in the northeast and central parts of the field are veneered with various thicknesses of air-fall tephra. - In other areas, all but the youngest flows are mantled with extensive deposits of aeolian silt and fine sand. - Full range of igneous (volcanic) rocks present. Sites of interest: Lunar Lake (a playa) was used as modeling site because it has fan on one side, transition to cobble-strewn playa, then to playa, and on other side are volcanic materials of various ages and compositions. Death Valley, CA Location: 300 km northeast of Los Angeles, CA (36 deg 31'N, 116 deg 50'W). Age: Alluvial fan units are as old as 800,000 years. Features: A variety of rock types (metamorphosed Precambrian Paleozoic limestones, quartzites, and shales and Miocene volcanic rocks) are present. 9 Sites of interest: - Basaltic lava flows and fanglomerates have been exhumed to form a bouldery surface appearing much like the surface of Mars as observed by Viking Lander 2. Informally called "Mars Hill". - Sand dunes, about three kilometers across, rise to 50 m and are located to the northwest and east of Stovepipe Wells. - Ubehebe crater, approximately 700 m in diameter, and about 150 m deep, is located in the northern end of Death Valley. A small amount of basaltic tephra that erupted during the explosion that created Ubehebe blankets the area. Southern Mojave Desert, CA Location: Southeast of Baker, California (35 deg 15'N, 116 deg 45'W). Age: Variable. Features: Sand dunes, alluvial fans, basaltic volcanic flows. Sites of interest: - Kelso dune field: an extensive, complex dune field. - Cima volcanic field: basaltic flows and tephra cones ranging from recent to several million years in age. - Providence Mountains: alluvial fans of granitic and carbonate provenances. TABLE 3.2 GRSFE SITE SUMMARY Specific site names are given in left-hand column. The next two columns provide the approximate latitude and longitude of each site. Line and sample locations for each site are then given for ASAS, AVIRIS or TIMS images that cover the relevant locations. Line and sample coordinate origin is in the upper left of the image data; lines are rows and samples are columns in the image arrays. See Section 13 for a discussion of file naming conventions for the airborne products. See Section 3.D for discussion of calibration site descriptions. Lat. Lon. Finder Image, deg. N deg. W Line, Sample ----- ----- ------------ Modeling Sites Lunar Crater Volcanic Field, NV ASASLL05F.IMG - Playa 38.38 116.02 203, 301 - Disturbed Playa 38.38 116.02 205, 244 - Cobble Strewn Playa 38.38 116.02 242, 279 - Mantle Lava Flow 38.38 116.02 23, 105 10 Calibration Sites Death Valley, CA - Death Valley Dunes - Bright Target TIMDD03A.IMG 36.65 117.13 4628, 335 - Devil's Golf Course - Bright Target AVRDG04A.IMG 36.3 116.83 370, 315 - Trail Canyon Fans - Dark Target AVRDG04A.IMG 36.3 116.92 354, 550 - Ubehebe Maar - Dark Target TIMUB01A.IMG 37.0 117.45 2824, 363 Cima Volcanic Field, CA - Bright Target AVRCM05A.IMG 35.2 115.75 284, 336 Cima Volcanic Field, CA - Dark Target AVRCM05A.IMG 35.2 115.75 246, 341 Kelso Dune Field, CA - Dark Target AVRPV29A.IMG 34.9 115.73 173, 143 3.B. AIRBORNE CAMPAIGN The airborne component of the GRSFE campaign was conducted on July 17, 1989 for ASAS; September 28-29 and October 4, 1989 for AVIRIS; July 17, September 27-29, 1989 for TIMS; and September 13-14, 1989 for AIRSAR (see Table D.1 for brief instrument descriptions; Tables D.4 to D.6 summarize coverage by these instruments.). Schematic maps showing flight lines covered by each airborne instrument are provided in three image files in the LOCATOR directory on the Volume 1 CD-ROM. AVIRIS flew on the NASA ER-2; ASAS and TIMS both flew on the C-130 on July 17. TIMS flew alone on the C-130 during September. AIRSAR was on board the NASA DC-8 aircraft. The airborne campaign was organized by flight lines and runs. The lines denote the azimuthal direction and start and stop positions for acquisition. The runs indicate the number of acquisitions along a given line that occurred during a given data acquisition period. Section 11 of this document describes the index files that provide detailed tabular descriptions of the airborne data. Tables D.7 to D.10 provide conversions between GRSFE file names, lines, and runs, and information used by each instrument archive. These tables are needed to obtain data directly from the data producers, e.g. from the AVIRIS processing facility at JPL. However, remember that these data are also contained on the GRSFE CD-ROMs. The intent of the airborne campaign was to fly all four instruments at the same time over the modeling sites and within a day or so of one another for the calibration sites. In fact, ASAS and TIMS collected data throughout the day of July 17 until engine trouble on the C-130 forced cessation of operations. The ER-2 flew on July 17 with AVIRIS, but operational difficulties with the instrument precluded data collection. The DC-8 was unable to fly on July 17 because of scheduling problems, so it was not possible to get AVIRIS and AIRSAR coverage until September. It was decided to refly TIMS during September, but prior commitments for ASAS precluded its use during that month. Thus, despite 11 best intentions, and a field campaign focused on the July 17 date, instrumental difficulties forced the full airborne campaign to be spread out over three months. We also note that a sun photometer from the NASA Ames Research Center flew on the C-130 during the July deployment. However, it proved to be impossible to extract reduced data records. Thus, these data were not included in the GRSFE archive. For the modeling sites the intent was to acquire multitemporal, multiangle (incidence and emission) AVIRIS, ASAS, and TIMS data. In fact, during the July deployment, TIMS data were collected over the modeling sites at approximately 4:17 (pre-dawn), 8:05 (early morning), 12:16 (noon), and 13:55 (afternoon) Pacific Daylight Time (PDT). ASAS data were acquired during the latter three times. AVIRIS data were acquired over these sites at 9:44, 11:43, and 13:44 PDT on September 29, 1989. For ASAS, data were acquired both along the principal solar plane and perpendicular to it. The multiple angle ASAS and AVIRIS data for the modeling sites will allow tests of radiative transfer models for surface reflectance. The multitemporal TIMS data will allow pursuit of emissivity and thermal inertia studies. AVIRIS and TIMS data were acquired for the calibration sites during one pass. Finally, ASAS also acquired data for a portion of a lava flow north of the modeling sites and for the Ubehebe site. AIRSAR observations over the modeling sites were focused on multiple incidence angle coverage with values of approximately 25, 35, and 45 degrees. Perpendicular tracks were also acquired. A mix of single and multiple angle coverage was acquired for the calibration sites, as noted in Table D.6. The multiple incidence angle AIRSAR data will allow detailed scattering models to be evaluated. 3.C. FIELD CAMPAIGN The GRSFE field campaign supported the July and September airborne observations. A base camp was set up at Lunar Lake for the July campaign focused on the modeling sites. Personnel were also deployed at the various calibration sites listed in Table 3.2. Activities were divided into five functions: (a) atmospheric measurements at Lunar Lake; (b) detailed ground observations at the modeling sites; (c) thermal emission experiments at the Lunar Crater Volcanic Field in July by researchers from the University of Colorado; (d) calibration site measurements in the visible, reflected infrared, and thermal infrared wavelengths; and (e) deployment of corner reflectors at the microwave calibration sites. The calibration team focused on acquiring measurements for bright and dark (in VISIR) surfaces at each calibration site. The University of Colorado radiometry and thermistor experiments are described in Section 5 of this document. Table D.2 summarizes the atmospheric instruments used during the field campaign, and Table D.3 summarizes the other field instruments that were utilized, including field spectrometers and corner reflectors. Table D.11 summarizes the participants involved in various aspects of the field campaign. The locations of the modeling sites at the Lunar Crater Volcanic Field are given relative to an ASAS frame in Table 3.2. Table 3.3 provides 12 location information for the other activities that took place on Lunar Lake. TABLE 3.3 LOCATIONS OF SELECTED GRSFE ACTIVITIES ON LUNAR LAKE Locations are given relative to ASAS frame ASALL05F.IMG. Activity Line Sample -------- ---- ------ Lunar Base Camp 170 198 Univ. Colorado Directional Emissivity Experiment 178 221 Washington Univ. Thermistor and Radiometry Experiments 271 279 (see Section 3.D) Reagan Radiometer and Spectral Hygrometer 177 201 Weather Station 237 337 3.D. NARRATIVE OF FIELD CAMPAIGN ACTIVITIES This section is a chronological sequence of the field campaign activities. This master sequence, together with the other parts of this section, Sections 4 and 5, and the data set descriptions, should allow the reader to understand how the airborne and field campaigns were implemented and how the resultant data can be used in synergistic fashions. Times are given in PDT. July 15, 1989 (Lunar Lake) Greeley and Lancaster set up and began measurements of wind velocity with ASU wind velocity experiment. Arvidson and Plaut set up weather station, which began measuring air temperature, wind velocity, and direction. Weather station was located approximately 700 m ENE of cobble site. Wind velocity experiments (2 towers) were located NNE of cobble site. Deering (PARABOLA, GSFC sun photometer, pyranometer), Zurek and Norris (Reagan Radiometer and Spectral Hygrometer) arrived at Lunar Lake in PM to check out site and equipment. (Note: GSFC sun photometer data not included on version 1 release of GRSFE archive.) July 15, 1989 (Calibration sites) CALTEAM arrived at Kelso Dunes about 11 am. Found a "bright" area on the nominal AVIRIS Afton-Kelso and Providence fans lines at the first parking area on road to dunes. Appeared on TM image as eastern "lump" in road. Site name: Bright Target. (Note: Target not covered during airborne GRSFE campaign.) Took several SIRIS, Daedalus, and PFES spectra. Done about 1 pm. SIRIS, Daedalus moved at about 12:30 pm to a dark area at the pumping station near the intersection of Kelso Dunes Road with Kel-Baker Road. Site is Dark Target. Obtained several spectra. Surface samples collected at both sites. 13 Moved to Cima Volcanic Field at Cone I, measured tephra (dark). Started about 2 pm. Obtained SIRIS, Daedalus, PFES spectra and surface samples. Site called Dark Target. Found bright area on southeast flank of Cone I in a dry stream channel. Site called Bright Target. Done about 5 pm. July 16, 1989 (Lunar Lake) Four modeling sites staked out by Arvidson and Plaut. Disturbed playa site generated by driving automobile around in circles, churning up playa. July 17, 1989 (Lunar Lake) Note: ASAS, TIMS acquired data. Modeling sites characterized using random grid approach. Reagan Radiometer and Spectral Hygrometer obtained data. PARABOLA measurements of atmosphere and surface at cobble site obtained. SIRIS, Collins, Daedalus, PFES spectra were acquired over selected playa, volcanic, fan and vegetated surfaces at modeling sites. Performed SIRIS and Daedalus field spectrometer intercomparison at playa, varnished rock, and disturbed playa sites. Corner Reflector Team arrived at Lunar Lake with a truck full of corner reflectors. July 18, 1989 (Lunar Lake) PARABOLA obtained data at playa and mantled flow modeling sites. Irons examined sites and collected soil samples. July 18, 1989 (Calibration sites) Arrived Trail Canyon fan site about 11:45 am. Site name is Dark Target. SIRIS and Daedalus obtained data along traverses. PFES died from heat. Surface samples collected. Descended to first clean, salt covered flood plain area on Devil's Golf Course at about 1 pm. Obtained SIRIS and Daedalus measurements and surface samples. Site name is Bright Target. Moved to Death Valley dunes site. SIRIS spectra acquired at sand dunes picnic area, Daedalus spectra at main dunes off Stovepipe Road. Samples obtained. Called Bright Target. July 18, 1989 (Corner reflector sites) Corner Reflector deployment team deployed reflectors and acquired soil moisture and dielectric constant data. Reflectors were placed in a number of locations and in two orientations to cover the several parallel and one crossing swath. Note: Detailed field measurements were conducted in May 1988 at the Pisgah lava flow and adjacent Lavic Lake as part of airborne polarimetric SAR coverage associated with the Mojave Field Experiment. Analysis of these data show that topographic variations largely control variations in cross section. Spatial variations in dielectric constants were found to be much less important. Thus, the emphasis for the radar part of GRSFE was to deploy corner reflectors to allow calibration of the data, and to acquire helicopter stereophotographs. 14 The main objective of the Corner Reflector Team was to place trihedral corner reflectors within the image swaths for calibration of the aircraft SAR data. In this technique, the known phase characteristics and backscatter cross-sections of the corner reflectors are used to find the transfer function from image pixel values to surface backscatter cross-section. Typically, several corner reflectors are placed spanning the swath to determine the transfer function as a function of incidence angle. Near-surface samples were also collected for determination of soil moisture. July 17 - 18, 1989 (Lunar Lake Subsurface Temperature Experiments) Temperature data were collected from the playa and cobble modeling sites. This work was led by Petroy, Washington University, and is a separate experiment from the University of Colorado experiment described in Section 5. Eight (8) thermistors were buried 4 m apart by Arvidson and Plaut, each to 3 cm depth, in a continuous line starting in the cobble site and extending south into the adjacent playa. The emplacement was done by noon. A thermistor is an electrical resistor which makes use of a semiconductor whose resistance varies sharply in a known manner with temperature. Each probe is approximately 2 mm in diameter and is placed in direct contact with the soil, usually buried. The resistance across the surface of the thermistor is measured; that resistance is then connected to the temperature of the soil. The thermistor probes used in this experiment were manufactured by Yellow Springs Instruments (YSI) and are accurate to 0.2 degrees C. Temperatures were recorded by Petroy from each site every hour over a 25 hour period, beginning on July 17, at 6:00 pm and concluding on July 18, at 6:00 pm. Results are presented in Table E.1. In addition to these shallow test sites, at approximately 1 pm, thermistors were buried to greater depths in the playa just to the south of the cobble site, and at the southern edge of the cobble site, to measure the depth of the diurnal temperature wave. Thermistors were buried at 30, 10, and 3 cm depths at both locations. In all cases soil was tamped back in place and cobbles returned to their original positions. Temperatures were recorded at these sites every hour over the same 25 hour period. Results are shown in Table E.2. A thermometer and hygrometer were mounted approximately 0.7 m off the ground just to the north of the cobble site. Air temperature and relative humidity were recorded every hour over the same 25 hour period. Results are given in Table E.3. July 19, 1989 (Calibration sites) Arrived at Ubehebe crater about 10 am. Collected SIRIS and Daedalus spectra at Dark Target on north flank of Ubehebe Crater. SIRIS obtained spectra of small playa just to north of dark site, but it seemed too small for calibration, so SIRIS team chose another site where Ubehebe Crater Road crossed stream to east of crater. Clouds began moving in from east. Surface samples collected. July 20, 1989 (Corner Reflector sites) Reflectors were deployed at Death Valley. Four corner reflectors were placed at Trail Canyon fan: one at the base and three distributed 15 along the road going up the fan. Areas of desert pavement were chosen for their smooth background. At Mars Hill, near the exit of Artist's Drive, one corner reflector was placed south of the hill and one north. At Stovepipe Wells, four corner reflectors were distributed along Highway 190 from just east of Stovepipe Wells, east to sand dune picnic rd. At Ubehebe Crater, three corner reflectors were distributed along the crater access road from about 1.4 mile west of its junction with North Highway, west to near the crater. One additional corner reflector was placed about 1 mile down Racetrack Valley Rd. July 21, 1989 (Corner Reflector sites) Reflectors were deployed at Kelso. Four corner reflectors were placed along the Kel-Baker Rd.; two north of the railroad tracks and two south. July 26, 1989 (Corner Reflector sites) Checked orientation of corner reflectors at Kelso. July 27-28, 1989 (Corner Reflector sites) Checked corner reflectors at Death Valley, Ubehebe, and Lunar Crater. September 10, 1989 (Corner Reflector sites) Arrived Kelso about 3 pm. All four corner reflectors were OK. Arrived Death Valley about 18:00. Checked corner reflectors at Mars Hill. Corner reflector 1 was loose and off its base and its vertical sides were bowed inward. September 11, 1989 (Corner Reflector sites) Checked corner reflectors at Stovepipe Wells and found westernmost corner reflector (corner reflector 1) slightly off base. Corner reflector 2 needed minor adjustment. Corner reflector 3 was near a public turnout and was therefore most disturbed. Corner reflector 4 was OK. Proceeded to Ubehebe Crater about 10:30. Started with corner reflector 1 on Racetrack Rd. Corner reflector 1 was turned over due to soft ground. Corner reflector 2 (next to east) also blown over due to soft ground. Corner reflectors 3 and 4 OK. September 12, 1989 (Corner Reflector sites) Lunar Crater corner reflectors were checked and found to be OK. September 26, 1989 (Lunar Lake) A second thermistor-based experiment was conducted by Petroy, Washington University, during the September GRSFE field campaign at Lunar Lake. In addition, a radiometer was used to obtain brightness temperatures as part of this experiment. Petroy and Plaut dug two pits on mantled flow modeling site at 1 p.m. Three stakes left over from July campaign were found to be still standing on SE, NW, NE corners of site, as well as small stakes from random sampling. Pit A dug 25m south of site. Three samples obtained at different depths after which thermistors were placed at 10, 20, and 30 cm depths. Rock hammer point was used to make holes for the thermistors. Soil was tamped back into hole and rocks placed on top in approximately natural density. At 1:30 16 pm, pit B was dug at about 12 m from south boundary of site. Three samples were obtained at different depths, after which thermistors were placed at 3, 10, 20, and 30 cm depths. Soil was tamped back into hole and rocks placed on top in approximately natural density. Pictures were taken before, during, and after the activity. At 2:10 pm, visited disturbed playa modeling site. Surface was found to be back to normal, except for a few faint skid marks still visible. Clouds built up all morning to about 50% cover. Altimeter set for altitude of Lunar Lake: 5760 feet (from topographic map) = 1756 m. Barometric pressure based on altimeter at 9:00 a.m. was 622 mm. 10:00 a.m.: clouds from south, 20% cover. 10:05: Deployed weather station and began recording data. At 12:40, 50% cloud cover, dust kicking up on east side of lake. At 14:10, 55% cloud cover. At 16:00, 35% cloud cover. At 17:45, 40% cloud cover, wind dying slightly. Barometric pressure at 12:40 was 622 mm, at 14:10 it was 620 mm, at 17:45 it was 619 mm. September 27, 1989 (Lunar Lake) Note: TIMS data acquired on September 27 and 29, 1989. At 6:30, 75% cloud cover. At 8:05 barometric pressure was 621 mm with clouds to E, N, S, and wind picking up. By 11:00 there was 100% cloud cover. At 18:24, clouds clearing, wind dying. September 26-27, 1989 (Lunar Lake Surface and Subsurface Temperature Measurements) Temperature data were collected from the mantled flow modeling site using the thermistors buried to 30, 20, 10, and 3 cm depth. Temperature data were collected every hour over a 25 hour period beginning at 6:00 pm on September 26 and concluding at 6:00 pm on September 27. This period was originally to coincide with the TIMS overflight, however, weather precluded acquisition of good data for two days. It should be noted that during the 25 hour monitoring period, the sky was generally overcast and it was extremely windy (up 30 km/hr). Table E.4 provides the temperature data. In addition to the subsurface temperature data, surface temperature data were collected using a Raynger Radiometer at both pit sites during the same 25 hour period. Temperature measurements were made by holding the instrument vertically over the site about 1 meter above the surface (emission angle = 0 degrees), setting the emissivity variable on the instrument to 1.0, and collecting two temperature measurements. Then, the instrument was positioned vertically over an adjacent undisturbed surface and two more brightness temperature measurements were collected. Data are presented in Table E.5. Additional data: On the day of the TIMS overflight (September 29, 1989) surface temperature data were also collected on the playa at two sites - an undisturbed playa site and a cobble site (not the same sites as described during the July GRSFE) located within meters of Lunar base camp. Data were collected every hour for four (4) hours. At the playa 17 site, two sets of temperature data were collected - one set with the emissivity=1.0 and one set with the emissivity=0.95. Unless otherwise noted, all data collected with the Raynger instrument were collected with the emissivity=1.0. Also, one surface temperature measurement was collected at the mantled flow test sites at 1:00 pm during the day of the overflight. Table E.6 presents these data. September 28, 1989 (Lunar Lake) At 6:30, 75% cloud cover, cold, and no wind. At 7:25 barometric pressure was 624 mm; at 9:05 it was 625 mm, with clearing to E, S, 60% cloud cover. September 29, 1989 (Lunar Lake) At 6:30 it was clear and calm. Set up Reagan Radiometer. Sunrise at 6:50, started measurements at 6:52 a.m. with Reagan Radiometer and two Spectral Hygrometers. At 10:58 barometric pressure was 623.5 mm. At 11:00, wind strong, kicking up dust on lake. 4. MODELING SITE DESCRIPTIONS As noted in the previous section, four modeling sites were selected in the Lunar Crater Volcanic Field. The modeling sites are representative of the range of surface compositions and terrain types found in the area. The sites selected were: a) undisturbed playa, b) disturbed playa, c) cobble-strewn section of the playa, and d) a mantled lava flow. Locations of the sites are given in Table 3.2. The disturbed playa was generated by driving a vehicle around in circles until the playa material was thoroughly churned up. The cobble site is a mix of basalt cobbles and playa. The mantled flow site is an old flow that has been partly buried by aeolian debris and covered with a desert pavement of basalt cobbles and boulders. For each site, a 50 m by 50 m area was delineated using stakes, with boundaries approximately aligned with north-south and east-west directions. Each site was characterized in terms of its general surface composition and particle size, vegetation cover, soil moisture status, and compositional "end" members. Note: The following material was edited from contributions by Greeley and Lancaster. Sub-areas within each site were selected randomly within the 50 m by 50 m squares using the following method. Each 50 m by 50 m square was divided into 25 5 m by 5 m sub-sites. Five squares were randomly selected for sampling and characterization, and were located using the coordinate system below. Sub-site numbers refer to the squares numbered as below. NW NE 5 10 15 20 25 4 9 14 19 24 18 3 8 13 18 23 2 7 12 17 22 1 6 11 16 21 SW SE At each sub-site, photographs (black and white and color) were taken to show: a) the general nature of the sub-site, b) a close up of the surface, and c) a near vertical view of the surface. The particle size composition of each sub-site was estimated visually for a 1 m by 1 m quadrant. A 1200 g sample of the surface materials was taken for soil moisture determination, and placed in a sealed can. Field determinations of soil moisture were made by Hughes (JPL) at selected sub-sites at the disturbed playa, undisturbed playa and cobble sites, using a "Speedy" soil moisture tester. Samples of the compositional end members were collected at one sub-site location for each site. Detailed descriptions of each site follow. Times are in PDT. A. Undisturbed playa (July 17th, 10:05-10:40 am) General characteristics: This was a smooth, flat, silty-clay playa surface displaying major 20-30 cm polygons with fine cracks, and clay "sheen" to surface. Within 20-30 cm polygons were finer cracks that formed 2-3 cm polygons. A few scattered clusters of 2-3 cm basalt gravel were visible. There were also some very small craters on the surface in places caused by degassing or water escape. Particle size: silty clay Vegetation: one green Atriplex bush End member samples: Basalt pebbles; Silty clay playa surface Sub-site 3: There was smooth playa soil; a moisture sample was taken. Sub-site 5: The sub-site had smooth playa soil; a moisture sample was taken. Sub-site 7: Here there was smooth playa with scattered 1-2.5 cm basalt pebbles covering < 5% of surface. A soil moisture sample was taken, resulting in measurements of 1.38 wt.%, 1.56 wt.%. Sub-site 12: This area was smooth playa soil, and a moisture sample was taken. Soil moisture measurements were 1.73 wt.%, 1.88 wt.%. Sub-site 17: This sub-site was smooth playa. A soil moisture sample was taken, resulting in measurements of 1.64 wt.%, 1.83 wt.%. Sub-site 19: This area was smooth playa containing very scattered 1-2 cm basalt pebbles. End member samples of basalt and silty-clay were taken here. A soil moisture sample was also taken. B. Disturbed Playa (July 17th, 9:00-9:56 am) 19 General characteristics: Playa surface was disturbed by driving an automobile around the site for several tens of minutes to "roughen" surface and destroy original surface. End member samples : undisturbed playa surface within this site disturbed playa surface within this site Particle size: silty clay Vegetation: A total of six Atriplex bushes, each 0.4-1 m in diameter occurred at this site. Only two were green. Most bushes have accumulated silt and clay around their lower stems to form a small mound. Sub-site 3: There was well disturbed surface soil; a moisture sample taken. Field soil moisture measurements were 0.50 wt.%, 0.22 wt.%. Sub-site 10: End members and soil moisture samples were taken here. The surface was only lightly disturbed. Soil was largely silty clay, with 10-20 cm polygonal cracks and rare basalt pebbles. Soil moisture measured by Farr's instrument 1.75 weight %. Sub-site 18: This surface was well disturbed, mostly powder and a few clods up to 5 cm across; a soil moisture sample was taken. Sub-site 19: The surface was well disturbed, and a soil moisture sample was taken. Sub-site 22: This was a well disturbed surface. Soil moisture sample was taken, resulting in measurements of 1.59 wt.%, 1.78 wt.%. Sub-site 25: Very few car tracks here; the surface was virtually undisturbed. A soil moisture sample was taken. C. Cobble site (July 17th, 10:50 am -12:03 pm) General characteristics: The site was east of 4-5 m high basalt knob that formed an "island" in the playa. Also, the site had numerous blocks and clasts derived from basalt, together with silt matrix. There was poorly developed desert pavement in many areas. See table given below for particle sizes. Area percentage of: Sub-site Clay/silt Sand Gravel Cobbles ------------------------------------------- 5 75 5 15 5 8 27 3 65 5 9 78 5 15 2 14 37 10 45 8 16 15 2 75 8 23 18 10 70 2 20 Vegetation: Atriplex bushes were scattered about; they were up to 1.5 m across and 40 cm high. Some had silt-clay accumulations at their base. End member samples: Playa silts; Basalt pebbles; Basalt cobbles. Sub-site 5: This area had a silt-clay playa surface with scattered basalt gravel and cobbles; scattered Atriplex bushes measured 20 cm high, 50-60 cm across, spacing 2-3 m. A soil moisture sample was taken, resulting in measurements of 0.92 wt.%, 1.04 wt.%. End member samples were taken here. Sub-site 8: This sub-site consisted of gravel-sized basalt clasts resting on a silty substrate. This incipient desert pavement surface contained two dead 5 cm high Atriplex, 40 cm apart. A soil moisture sample was taken, resulting in measurements of 0.47 wt.%, 0.59 wt.%. Sub-site 9: This was a silty-clay surface containing scattered gravel. Two Atriplex bushes were there, 40 cm high, 1-1.5 m across, 1 m spacing. Sub-site 14: Silty-clay playa material and gravel clasts were at this site, but no vegetation. PARABOLA Sub-site was 10 m east of here. Sub-site 16: This was a gravel surface containing dead herbs, 10-15 cm high, 25 cm spacing, 10 cm diameter. A soil moisture sample was taken. This was PFES Sub-site. Sub-site 23: Here there was gravel having occasional cobbles; a silty surface was below basalt clasts, but no vegetation. A soil moisture sample was taken, resulting in measurements of 0.62 wt.%, 0.83 wt.%. D. Mantled Lava Flow (17th July 1:00-2:30 pm). General Characteristics: The site was north of Lunar Lake, and consisted of lava flow with surface of boulders to gravel with windblown silt cover, forming a well developed desert pavement surface. The flow formed a scarp approximately 12 m high to the southeast overlooking Lunar Lake. The basalts forming the flow were "layered", with each unit having a thickness of ~1.5 m. Basalt clasts on the surface were vesicular, with a well developed desert varnish on their surface. The sub-site is fairly flat, dipping 1-2 degrees to the southeast. There were some silt mounds around bushes, and some caliche chips on the surface. See table given below for particle sizes. Area percentage of: Sub-site Clay/silt Sand Gravel Cobbles Boulders ------------------------------------------------------------------------ 8 28 1 60 10 1 9 60 2 20 10 8 10 43 2 30 15 10 18 15 65 20 21 19 37 1 45 15 2 20 60 15 15 10 Boulders are all < 30 cm in diameter. Vegetation: Sage brush and rabbit brush. End member samples: Basalt cobbles, silt, caliche, red varnished basalt. Sub-site 10: This area had boulders and gravel having silty cover; a soil moisture sample was taken. Sub-site 9: Basalt gravel formed a desert pavement surface with large silt patches here. A soil moisture sample was taken. Sub-site 8: Here there was basalt gravel with smaller silt patches. A soil moisture sample was taken. Sub-site 18: This area had basalt gravel and cobbles having some silt and desert pavement formation. A soil moisture sample was taken. Sub-site 19: This site had basalt gravel and a cobble surface. A soil moisture sample was taken. Sub-site 20: Basalt boulders, cobbles, and gravel with silt were here; a soil moisture sample was taken. 5. UNIVERSITY OF COLORADO DIRECTIONAL EMISSIVITY EXPERIMENT Note: The following material was edited from text and data from Jakosky, Finiol, and Henderson. Thermal emission from geologic surfaces is known to be non- isotropic due to the presence of surface rocks and slopes (which have non-uniform kinetic temperatures) as well as emissivity effects arising from the non-uniform Fresnel emission from a flat or a rough surface. These effects have been observed on the Moon, Mars and other rough surfaces in the solar system. Observations of directional effects can tell us something about the surface roughness and structure of a planet's surface; because most spatially resolved thermal infrared observations of the earth or planets are done with near-nadir viewing only, the magnitude of such effects must also be known to properly interpret the diurnal energy balance (and derivation of thermal inertia) and emission spectra. As part of GRSFE we investigated the directional variations in thermal emission of different surfaces. Results obtained using hand- held thermistor probes (to determine local kinetic temperature) and a ground-based, hand-held infrared radiometer (to determine scene-averaged infrared brightness temperature from multiple view angles) are reported. The text of this document describes the experimental protocol and some 22 of the results and conclusions. The radiometer observations are provided in the file RMTLL001.TXT, in the DIREMISS directory on GRSFE Volume 1. The thermistor data are located in the file THMLL001.TXT in the same directory and volume. Field work took place in the Lunar Crater Volcanic Field. Three natural sites were selected, and four artificial sites were constructed. The natural sites included: (1) Dry playa. The selected site was relatively smooth and flat, with a very small number of interbedded rocks less than 0.5 cm in size. Although a number of dessication cracks were present, they occupied a small fraction of the radiometer field of view; observations at multiple viewing angles and directions suggests they are not important in the thermal emission from the ensemble surface. (2) Rocky playa. This surface consisted of dry playa material, with approximately 10 % of the surface covered by rocks with size 1-10 cm. (3) A'a lava flow. A 3-m square, vegetation-free surface was selected within the Black Rock Lava Flow; the surface was extremely rough, with 1-m variations in heights occurring. Four artificial sites were constructed on the Lunar Lake playa close to GRSFE base camp. The artificial sites consisted of a 1-m- square patch of material overlying undisturbed playa material. The sites were: (1) Smooth sand. Overturned playa material was covered to a uniform depth of about 10 cm with sand. (2) Smooth sand plus a single rock. A similar sand surface was constructed, and a single 13-cm cubical rock was placed on top. (3) Pebble surface. Smooth playa material was covered to a depth of about 10 cm with 1- to 3-cm rounded pebbles. (4) Rocky surface. Playa material was covered with a close- packed single layer of 15- to 30-cm slightly weathered and rounded rocks. After construction, each site was allowed to partially equilibrate with sunlight and ambient temperatures for 36 hours prior to beginning measurements. Infrared brightness temperature measurements for each surface were obtained with a hand-held 8- to 14-micron broadband infrared radiometer obtained from the Cole-Parmer Instrument Co. Manufacturer's specifications indicate an absolute calibration to about 3 K, with relative uncertainties between measurements of better than 2 K; field investigation suggests a relative calibration that was usually better than this over short time spans. As we were investigating variations in emission as a function of viewing geometry, the absolute calibration of the instrument was not a limiting factor. Although the field of view of the radiometer is small, an internal averaging function allowed the instrument to be swept over the entire site in a boustrophedonic pattern in order to obtain a reading of the brightness temperature of the ensemble surface. Measurements were made of each site at emission angles of 0, 30 and 60 deg, and, for the latter two emission angles, every 45 deg of azimuth; measurements of the sand and playa sites were obtained at additional emission angles. Experiments were performed to determine the radiometer field of view using adjacent surfaces which had differing temperatures; the field of view was sufficiently well-defined that no significant emission was thought to come from regions outside of the specific sites. 23 Measurements of the actual surface kinetic temperature were made with a hand-held thermistor probe. The probe was thermally connected to the surface only at the time of the measurement and insulated from the atmosphere by a molded piece of styrofoam. The probe itself had a time constant of 10 s in air, and was held in contact with each surface for up to 30 s to obtain a stable temperature. For the rocky and rough surfaces, temperatures were obtained for a representative sampling of surface orientations (typically, about 30), and the strike and dip of each local surface was recorded. In order to obtain measurements of all surfaces at the same local times, we obtained data over a span of three days, partially overlapping with other GRSFE field and aircraft investigations. Logistical and weather problems prevented our obtaining complete diurnal coverage of each site; 10 a.m. observations and variations with emission angle are explicitly discussed in the text of this report. Results and discussion: The angular variations in 10 a.m. brightness temperature for the pebble, rocky, and a'a lava flow surfaces show the same general trend of the warmest temperatures occurring on the side of the roughness elements which face toward the sun, as expected. The a'a lava flow, with the largest rock masses, shows the largest variation with viewing angle; the pebble surface, with the smallest rocks, shows the smallest. This is as expected since the timescale for energy to conduct through a rock is approximately 2 minutes for a 1-cm pebble, 3 hours for a 10-cm rock, and 1 day for a 30-cm rock (e.g., Carslaw and Jaeger, 1959); the pebble surface should be nearly isothermal. The radiometer observations of the a'a lava flow show a nearly 15 K variation in brightness temperature depending on viewing geometry. This variation is a significant fraction of the total diurnal variation because the sunlit faces have heated to nearly their maximum temperature while the shaded faces have not been heated except by conducted or radiant heat; clearly, viewing geometry will affect interpretation in terms of the thermal inertia of the surface. These observations at 10 a.m. local time should show the largest variation with viewing azimuth; temperatures should be more uniform at other times of day. The data set includes the thermistor-probe measurements of these same surfaces. Temperatures are included as a function of local solar incidence angle, as calculated from the known location of the sun and the orientation of each rock face. The data for the rocky surface also includes the temperatures measured at the center of the five visible faces of the rock cube. Scatter results partly from uncertainties in the probe measurement and partly from variations in actual temperature which result from differences in local rock thickness (and, hence, conductive loss) and radiant heating. As expected, the largest variation occurs with the large rock masses in the a'a lava flow, and the smallest with the pebble surface. Within the sand and playa surfaces, individual sand and playa particles should be isothermal, due to the rapid conduction time across 24 mm and smaller grains (less than 1 s) and the dominance of solid over radiative conduction through individual grains. Any variations of the brightness temperature seen at different emission angles should represent pure directional emissivity effects. Relative instead of absolute emissivity is used due to uncertainties in calibration of both the radiometer and thermistor; normal emissivities are expected to be approximately 0.9-1.0 (e.g., Conel, 1969). Relative emissivity is calculated by converting the measured brightness temperature to an energy flux, using a numerical integration over the instrument passband, and normalizing to the nadir-viewing flux; values greater than 1 result from uncertainty in the relative calibration. The data set also includes observations made of the playa and sand surfaces at additional times of day and at additional emission angles and azimuths. Each set of data was normalized separately, and the remaining scatter results from calibration uncertainties. Notice that data collected simultaneously at low and high phase angles produce the same trend of decreased flux at higher emission angles. Jakosky et al. (1990) analyzed the data discussed above. They show normalized emissivity for a surface which is smooth and flat at the scale of the wavelength, i.e., the Fresnel emissivity for transmission through a smooth dielectric boundary (taken as the average of the transmission for parallel and perpendicular polarizations). They also show the measured flux from a smooth pane of glass, which should be a Fresnel emitter. Both the playa and sand surfaces exhibit a smaller decrease in emissivity with increasing emission angle than the Fresnel surface, although both do show a decrease. This effect can be understood as a result of surface roughness at the scale of the individual sand and playa grains. Each grain is itself much larger than the wavelength, so that emission is generated within the grain and the emissivity is governed by the Fresnel relation at the grain surface. At high emission angles, the radiometer preferentially views those parts of the grains that are tilted toward it, so that the normal to the grain surface is also tilted toward it; the local emission angle is thus smaller than that calculated using the normal to the average surface, and the Fresnel emissivity is correspondingly higher. Jakosky et al. (1990) also show model results of the Fresnel emissivity of an isothermal surface which is rough at scales much larger than the wavelength. The model assumes a gaussian distribution of surface slopes (characterized by an r.m.s. slope), and involves a numerical integration over all slopes and azimuths. For each geometry, the Fresnel emissivity (again, the average of the two polarizations) is calculated for the local emission angle and weighted by the projected area of the surface facet and the relative probability of a facet having that geometry; the average or effective emissivity is then calculated from the sum over geometries. Scattering by grains comparable in size to the wavelength is ignored, as are multiple reflections. In Jakosky et al. (1990), r.m.s. slopes up to 20 deg are expected at scales larger than centimeters (McCollom and Jakosky, 1990), and values up to 50 deg might occur at the scale of the individual grains for the sand-covered surface. The model confirms our intuition that rougher surfaces have a 25 smaller decrease in emissivity toward larger emission angles than do smoother surfaces. Notice also that the sand surface has a smaller decrease in emissivity at high emission angles than does the playa surface. This is consistent with the formation of the playa in the presence of water and the presumed more-efficient packing of surface grains. Conclusions: The data suggest that all surfaces emit in a non- Lambertian manner. For surfaces which are rough at scales larger than the thermal conduction depth, such as the a'a lava flow, different faces of the surface will be at different temperatures; observations of the sunlit sides of rocks then will show higher temperatures than observations of the shaded sides. For surfaces which are rough at scales much smaller than the conduction depth, such as the sand surface, the surface will be isothermal, but emissivity will be governed by the roughness; oblique emission will be from grain faces tilted preferentially in that direction, such that the Fresnel emissivity from the grain will be at a lower local emission angle relative to the grain normal, and the average emissivity will be higher than the Fresnel emissivity calculated using the emission angle relative to the average surface. Interestingly, a surface composed entirely of grains much smaller than the wavelength of emission, such as the dust-covered regions on Mars (grain size ~ 1 micron) will emit as if from a uniform half-space, and should show a much more dramatic drop-off with emission angle. The next decade will see a large number of thermal infrared radiometers and spectrometers being flown on spacecraft. By acronym, these include ITIR on the Earth Observing System, PPR on the Galileo mission to the Jupiter system, TES on the Mars Observer, and TIREX on the Comet Rendezvous/Asteroid Flyby mission. In addition, the Magellan mission to Venus includes a microwave radiometer. Most of these will usually operate pointed nearly toward the nadir; clearly, additional useful information can be obtained if they do scans of the surface at multiple emission angles; this will be important in defining the structure of the surface, deriving accurate thermal inertias, and providing input for corrections for the non-isotropic character of the thermal emission in thermal emission spectroscopy. 6. FIELD DATA SETS 6.A. PHOTOGRAPHS It was not possible within existing resources to digitize the field photographs, most of which were acquired on 35mm film. Field photographs are archived at the Geosciences Node, Washington University. Orders for color slides and black and white prints may be placed with Mary Dale-Bannister, via telephone at 314-889-6652 or via electronic mail at WURST::DALE (NASA Science Internet). The cost for part or all of the photographs will be based on reproduction and distribution costs. 26 6.B. SAMPLES Appendix F.1 contains information about samples collected during the GRSFE field campaign. Subsets of this sample collection can be made available if needed. Contact Mary Dale-Bannister. In addition, Jim Irons took a few samples at Lunar Lake on July 18, 1989. They were sent to the Cornell Soil Characterization Lab. One sample was taken from the playa modeling site. A second sample was taken from the cobble modeling site, below the surface cobbles. In both cases samples were acquired within 15 cm of the surface. The other two samples were taken from a hole within the mantled flow modeling site. One sample was taken from the top 3 cm of soil, and the other sample was taken from a distinct B horizon at a depth greater than 3 cm. In all cases, analyses were performed on sieved samples for particle sizes less than 2 mm in diameter. Table F.2 consists of data provided by Cornell University under Jim Irons' auspices. The units for the particle size fractions, the Fe and Al contents, and the organic carbon content are percent by weight. The cation exchange capacity (CEC) is expressed in centimoles of charge per kg of dry soil. The carbonate content is expressed in centimoles of charge per kg of dry soil relative to the calcium carbonate equivalent (CaCO3). The results of the Fe and Al extractions are strange for the following reason. The first extraction was performed with heated citrate-dithionite-bicarbonate following pretreatment with pH 5.0 sodium acetate. This extraction is supposed to remove all of the free irons (crystalline plus amorphous or paracrystalline). The oxalate extraction is only supposed to extract amorphous or paracrystalline iron and aluminum. The oxalate extract, however, contains more iron and aluminum. Regardless, both methods indicate that the samples contained very little free iron. 6.C. VISIBLE AND REFLECTED INFRARED SURFACE DATA 6.C.1. DAEDALUS SPECTROMETER Note: The following material was provided by Guinness. 6.C.1.1. INSTRUMENT DESCRIPTION The Daedalus AA440 Spectrafax is a portable field spectrometer. The important features of the instrument are summarized in the table below. The Daedalus measures radiance between the wavelengths of 0.45 and 2.4 micrometers. The measured radiance values are digitized to values in the range of 0 to 1023 (10 bits). The instrument also has a variable gain setting to adjust the dynamic range. The gain scale is a logarithmic scale in which one step represents about a 16 percent change in gain. A change in gain of 4 units is approximately a factor of 2 change in the digitized output signal. Reflectance values are derived 27 by ratioing the signal of a sample to that of a pressed and bonded halon standard viewed at the same lighting angle. Note that a difference in gain setting for the standard and the target must be accounted for when computing reflectance. The derived reflectance values are radiance coefficients. Daedalus AA440 Spectrafax Instrument Features --------------------------------------------- Dynamic range: Radiance digitized to values between 0 and 1023 (10 bits). Variable gain setting. Wavelength range: 0.452-2.398 micrometers in 280 channels. Wavelength resolution: Varies from 0.01 micrometers (visible) to 0.04 micrometers (infrared). Field of view: 2.5 centimeters when instrument is about 1 meter above target (1.5 degree angular field of view). Detectors: Silicon detector sensitive to wavelengths of 0.4 to 1.1 micrometers; lead sulfide detector sensitive to wavelengths of 1.1 to 2.4 micrometers. Filters: Circular filter wheel with 360 optical interference filters in three overlapping wavelength segments. Overlapping segments must be edited to properly display a Daedalus spectrum. 6.C.1.2. DATA SET DESCRIPTION The Daedalus AA440 spectrafax data set consists of over 500 data files. The purpose of these measurements was to provide ground calibration for AVIRIS and ASAS data. A number of reflectance measurements were made at all sites to estimate the average reflectance of an area about 50 by 50 meters in size (i.e., the size of several AVIRIS pixels). In addition, measurements were made at Lunar Lake to characterize the reflectance of the spectral components at each modeling site. The detached PDS labels for each spectrum contain a brief description of the site and purpose of the measurement. The Daedalus instrument was used during the July 1989 field campaign. The reflectance of a bright and dark target area was characterized with the Daedalus instrument at Kelso Dunes and the Cima Volcanic Field. The reflectance of Trail Canyon Fan, the salt deposit at the Devil's Golf Course, Death Valley Dunes, and the tephra deposit at Ubehebe Crater were also characterized with the instrument. At each site measurements were made along 2 or 3 traverses. The reflectance of the natural surface was measured at points along the traverse. Samples were spaced about 3 meters apart with 10 to 12 samples per traverse. The spectra halon calibration standard was generally measured at the beginning and end of each traverse. Additional samples of vegetation and other significant components of the site (e.g., coated rocks) were also measured. The measurements were made with the operator facing 28 toward the sun and holding the spectrometer at a height of approximately 94 cm above the ground. Nearly 200 measurements were made at Lunar Lake for the purpose of calibrating the airborne data, characterizing the reflectance of end- member materials in the modeling sites, and comparing reflectance spectra made by the various spectrometers used during GRSFE. The procedure used to collect data for the calibration of airborne data was the same as describe in the previous paragraph. Data for this purpose were collected at the playa, disturbed playa, and cobble sites at about 8:00am, 9:30am, and 11:00am (local time). Daedalus measurements were also made for characterizing spectral end-members at the disturbed playa and the cobble site. Three grid locations were sampled at the disturbed playa site. The end-members that were measured were cloddy playa material, fine powder, and undisturbed playa material. One grid location was sampled at the cobble site. The end-members that were measured were silt, basalt fragments, brown-coated rocks, and red-coated rocks. The smooth playa site was not characterized because the instrument batteries wore down. However, the playa site is very uniform and there should be sufficient data from the airborne calibration experiment to characterized the spectral components of this playa. Also, there are no Daedalus measurements of the lava flow site, again because the instrument batteries wore down before visiting that site. Several measurements were made at Lunar Lake to compare spectra from the Daedalus and SIRIS instruments. In this experiment, both spectrometers measured the same calibration standard and then measured the same sample of undisturbed and disturbed playa, along with a large basalt cobble. Finally, a few Daedalus spectra were collected to support the thermistor experiment by measuring the reflectance of the surface near each thermistor. Measurements made with the Daedalus instrument during GRSFE were hand held with the instrument height only approximately fixed. Thus, there can be a small difference in the height used to measure the calibration standard and a given sample. Such a height difference will produce a systematic error in the absolute reflectance value. Each centimeter difference in height will produce about a 2% change in reflectance. During GRSFE the Daedalus instrument showed two operating problems. One problem was the result of saturation in the electronics that affected channels in the wavelength range of about 0.73 to 0.97 micrometers. This problem can be readily seen in the spectra of the calibration standard. The radiance values in the affected wavelength range are approximately constant and well below the values expected for these wavelengths. Data in this wavelength range should be considered bad. The second problem involved the filter wheel not properly rotating during data collection. Measurements with the filter wheel problem have been removed from the GRSFE archive. 6.C.2. PARABOLA Note: The following material was provided by Deering and edited by Michael Shepard, Washington University. 29 6.C.2.1. INSTRUMENT DESCRIPTION The Portable Apparatus for Rapid Acquisition of Bidirectional Observations of the Land and Atmosphere, or PARABOLA instrument was designed to overcome important limitations of previously existing field instruments for obtaining the adequate sampling needed to analyze the bidirectional reflectance angular distributions of earth surface targets and the sky. The key previous major instrumentation limitation was determined to be the difficulty in obtaining multiple viewing angle measurements of ground surfaces in a very short period of time to eliminate, or at least sufficiently minimize, the effects of changing sun position, sky conditions, and the vegetation's dynamic biophysical conditions during the sampling period. A second important previous limitation was the capability to measure the downwelling sky radiance distribution concurrent with measurements of the ground target. The PARABOLA is a battery-powered, two-axis scanning head three-channel (visible, near infrared, and mid-infrared; 0.650-0.670, 0.810-0.840, and 1.620-1.690 micrometers, respectively), motor-driven radiometer that enables the acquisition of radiance data for almost the complete (4 pi) sky- and ground-looking hemispheres in 15 degree instantaneous field-of- view sectors in only 11 s. The detectors, two silicon and one germanium, are temperature regulated (by cooling or heating) through thermoelectric proportional control circuits. Also, due to the tremendous range in target brightness that can be expected in scanning a 4 pi sr field of view, an auto-ranging amplifier is used to switch the gain levels back-and-forth by factors of 1, 10 and 100 to maintain maximum radiometric sensitivity. In designing the PARABOLA for maximum sensitivity for the range of reflectances typically experienced for earth surfaces, including vegetation and snow, the direct solar disk measurement had to be sacrificed. Thus, the direct solar beam saturates the PARABOLA detectors for the pixel at that view angle, and therefore a separate measurement of the sun is required for computations of direct and total irradiant flux. Neutral density filters have been designed for mounting over the detector cones of the PARABOLA for this purpose to obtain periodic measurements when the instrument is placed in its manual (or "calibration", as opposed to scanning) mode. The radiometer is then pointed directly at the solar disk to acquire the necessary measurement to complete the missing data point. Calibration: Radiometric laboratory calibration of the PARABOLA is performed at GSFC on a 1.8 m spherical integrator employing 12 200- W quartz halogen lamps (2950K at 6.5A). The number of lamps is varied to produce 12 radiance levels for calibration. Three separate calibration runs are made to fully calibrate the PARABOLA at the three gain levels of the instrument. Neutral density filters (0.1 and 0.01 density levels; precisely calibrated) are used for the two lowest gain settings. The voltage response to the radiance level relationship is linear in all three spectral channels for each gain setting with linear correlation coefficients of 0.999, and has been found to be very stable from year to year. Calibrations are typically performed at the beginning and at the end of each seasonal field campaign. 30 Data recording and processing: The PARABOLA data system was originally designed to transform the analog data and record the records onto digital cassette tapes, providing a "rugged" recording medium with unlimited data storage capability. The data were then transferred to computer diskettes via a microcomputer and serially linked tape reader. The original data system has been upgraded to enable direct transmittal of the data onto computer disks via a field-hardy laptop portable computer. The original cassette recording system is maintained as a redundant backup. Specially developed software programs are then used to apply geometric computations and system calibration coefficients to the data to generate an output file that can be handled by a variety of commercial software packages, as well as those designed in-house. Mounting system: The primary mounting device is a lightweight, collapsible boom apparatus, called the Transportable Pickup Mount System or TPMS, whose primary unit consists of an aluminum triangular truss that decouples as four 2-m long sections. At the top end resides a detachable, two-axis motorized PARABOLA radiometer head mounting and leveling head with a camera mounting attachment. All operations of the PARABOLA/TPMS, except for raising and lowering the boom, are controlled from the PARABOLA data system control panel. For the GRSFE study the complete PARABOLA/TPMS system was mounted on a large tripod, as the system is adapted for the field measurements where motorized vehicles either cannot go or where traversing the terrain would be potentially damaging to the pickup-mounted equipment (such as the rough lava site on the GRSFE study area). Field deployment: The PARABOLA design provides multidirectional viewing, but the geometry of the systems does not allow the same "spot" on the ground to be measured at each view direction. Thus, considerable care must be taken in locating the instrument at a field site to ensure that the data acquired will actually represent the kind of surface that is desired; and some assumptions about the homogeneity of the area must be made. One approach to increasing the sampling density, which has been found to particularly effective, was employed at the GRSFE site. This involves the rotation of the radiometer boom by + and - 7.5 degrees from the solar principal plane axis and acquiring two additional complete scans. The three scans are combined in a special program that has been written to analyze the bidirectional reflectance distribution characteristics of a site. This procedure also enables more accurate sampling of the "hot spot" effects and the aureole surrounding the solar disk. In more spatially heterogeneous sites three or more (n) complete PARABOLA replicate scans are occasionally acquired by moving the instrument within the site. The replicates are then averaged for each viewing angle position to minimize the within-field inhomogeneity effects. With proper site selection three to five subsamples have been found to be generally adequate for most herbaceous vegetation, since the measurement pixel instantaneous fields of view are large (ranging from approximately 2 meters squared at nadir to 5.7 meters squared at a 45 degree off-nadir angle) relative to the canopy spatial structure. The average of the n values is taken as the canopy radiance for a particular view direction. Directional reflectances are normally computed as hemispherical-directional reflectance factors using the PARABOLA 31 directional radiance measurements from the ground-looking hemisphere divided by the PARABOLA-derived incident irradiance as computed from the PARABOLA sky irradiance data or from a calibrated painted BaSO4 reference standard panel. Supporting Instrumentation: A pair of Eppley Pyranometers was used to obtain broad-band (visible, reflected IR) sky irradiance and the irradiance reflected from the ground. The instrument was deployed at PARABOLA height. These data are in Appendix G. 6.C.2.2. DATA SET DESCRIPTION PARABOLA data were obtained at three modeling sites in the Lunar Crater Volcanic Field. The playa site, the cobble site, and the mantled flow site. Each site was "imaged" by PARABOLA at a variety of solar incidence angles to characterize the scattering properties of the surface completely. This information can be used as a reference to correct airborne data from ASAS and AVIRIS from any lighting and viewing geometry, or as a base data set to test radiative transfer models. Six sets of data from the playa site were gathered primarily on July 17, 1989 with solar incidence angles that varied from 28 to 71 degrees. Five sets of cobble site data were gathered during the morning of July 18, 1989 with incidence angles from 19 to 57 degrees. Data from the mantled flow site was obtained six times during the afternoon of July 18 with incidence angles from 21 to 73 degrees. In all, over 1000 data points exist for each site to characterize its scattering properties. Additionally, an equal number of points exist for the sky above the sites. The data are presented in two formats. The first set of files contain the complete, though filtered, data set consisting of almost all the individual pixels from the three replicate scans of the same site. Because of the scanning pattern of PARABOLA, the pixels are not at equidistant angles in the off-nadir or azimuth viewing planes. These files are on GRSFE Volume 1 in directory PARABOLA, and have names in the format PRBxxxxF.DAT. The files have the following information in each record: 1. Hemisphere i.e. 'GR' or 'SK' 2. Sequence number of data record 3. Off-nadir (view zenith angle, or emission angle) value of the center of a bin assigned to the pixel 4. Azimuth (view azimuth angle) value of the center of a bin assigned to the pixel 5. Actual off-nadir view zenith angle (relative to normal) of pixel 6. Actual view azimuth angle in the 0-360 degree coordinate system, where the sun is at zero and backscatter direction is at 180 degrees 7. Actual view azimuth angle in 0-180 and -180-0 degrees coordinate system; negative azimuth refers to boomside where equipment or shadow of the instruments obstruct the scan 32 8,9,10. Radiance value (W/m2/ster/um) for channels 1,2,3, resp. For users who prefer average sets of data binned into even intervals, the second set of files were created. In these files, the "raw" data of the first set of files has been averaged into bins with centers every 15 degrees in off-nadir and 30 degrees in azimuth. In these files, the last column gives the number of points used to compute the average of the bin. If there are gaps due to instrument shadows, instrument "noise", or other causes, the value of the bin is taken from its mirror bin (this assumes symmetry of data across the solar principal plane). To identify these cases, the number of data points averaged is assigned a negative (mirror image) value. If for some reason, there is no data for substitution, an interpolated value is used. Since interpolated values are not real data, the user is cautioned by placing a zero in the last column. These files are found on GRSFE Volume 1 in the PARABOLA directory, and have names in the format PRBxxxxA.DAT. The files contain the following information in each record: 1. Hemisphere, i.e. 'GR' or 'SK' 2. Sequence number of data records 3. Azimuth (view azimuth angle) value of the center of a bin assigned to the pixel 4. Off-nadir (view angle zenith, or emission angle) value of the center of a bin assigned to the pixel 5. Actual off-nadir view zenith angle (relative to local normal) of the pixel 6. Actual view azimuth angle in the 0-360 deg coordinate system, where the sun is at zero and backscatter direction is at 180 deg 7. Actual view azimuth angle in 0-180 deg and -180-0 deg coordinate system; negative azimuth refers to boomside where equipment or shadow of the instrument obstruct the scan 8,9,10. Radiance value (W/m2/ster/um) for channels 1,2,3, resp. 11. Data "flag" - indicates the number of samples averaged (see above description) Throughout the days during which PARABOLA data were being gathered, a white Barium Sulfate reference plate was periodically measured by PARABOLA. This plate is known to be Lambertian within a correctable amount. The measured radiance of this plate was plotted as a function of the time of day (or solar zenith angle) and fit to a sinusoid. In this way, the radiance from a Lambertian reference is known at any time during the data gathering period. The Lambertian radiances at the time each data set was obtained are tabulated in Table 6.1. TABLE 6.1 LAMBERTIAN SURFACE RADIANCES Col Description --- ----------- 1. Site i.e. playa, cobble, or lava 2. Date of data acquisition 3. Original data file name 33 4. Solar zenith or incidence angle 5. Local time of data acquisition 6,7,8. Radiance of reference plate (corrected to Lambertian) for channels 1,2,3 respectively in (W/m2/ster/um). Dividing the radiance of any bin in the data files by the radiance of the reference plate (taken the same time of day) gives a value of reflectance, sometimes called radiance coefficient. GRSFE89 CORRECTED BASO4 ------------------------------------------------------------------------ SITE DATE FILE NAMES SZA TIME(PDT) CH 1 CH 2 CH 3 ------------------------------------------------------------------------ PLAYA 7/17 PRBLL23,24 27.8 14:32 408.29 275.31 67.70 " " PRBLL25,26 43.7 15:58 331.43 223.79 55.89 " " PRBLL27,28 53.8 16:41 268.48 181.59 46.22 " " PRBLL29,30 62.6 17:34 206.45 140.02 36.69 " " PRBLL31,32 70.9 18:17 143.21 97.64 26.98 " 7/19 PRBLL33,34 48.8 09:17 301.40 197.18 48.61 ------------------------------------------------------------------------ COBBLE 7/18 PRBLL09,10 57.6 08:29 210.98 164.49 38.71 " " PRBLL07,08 48.7 09:14 264.65 202.95 47.74 " " PRBLL06,05 37.7 10:14 317.77 241.02 56.67 " " PRBLL04,03 28.5 11:07 356.91 269.06 63.25 " " PRBLL02,01 19.3 12:14 382.71 287.55 67.58 ------------------------------------------------------------------------ LAVA-FLOW 7/18 PRBLL11,12 21.4 13:45 440.17 304.43 68.97 " " PRBLL13,14 32.6 14:56 402.20 278.11 62.93 " " PRBLL15,16 42.1 15:47 350.79 242.48 54.76 " " PRBLL17,18 52.2 16:45 289.27 199.83 44.98 " " PRBLL19,20 62.7 17:32 222.34 153.44 34.33 " " PRBLL21,22 73.2 18:27 144.58 99.54 21.97 ------------------------------------------------------------------------ 6.C.3. SIRIS SPECTROMETER Note: The following material was edited from a contribution by Kruse. 6.C.3.1. INSTRUMENT DESCRIPTION The Single beam visible/InfraRed Intelligent Spectroradiometer (SIRIS) is a field-portable grating spectrometer manufactured by Geophysical and Environmental Research, Inc. The system is controlled by a portable MS-DOS compatible computer and spectra are saved in digital format on 3 1/2" computer disks. Data acquisition can be custom programmed, however, for this application the instrument was used in the standard mode. The SIRIS measures radiance using three separate gratings on a single stepper motor driven mount. The standard operating mode (from 0.35 to 2.5 micrometers) consists of a scan from 0.35 micrometer to 1.08 micrometer using the first grating, from 1.08 micrometer to 1.8 micrometer with the second grating, and from 1.8 micrometer to 2.5 micrometer with the third grating. Grating 1 uses a silicon detector with sensitivity out to about 1.1 m. A PbS detector is 34 used for the 1.1 to 2.5 micrometer portion of the spectrum. Both detectors are temperature stabilized on the same thermal electric cooler. Three blocking filters are used to prevent 2nd order contamination effects. The first blocking filter cuts off at about 0.65 micrometer, the second at approximately 1.05 micrometer, and the third at approximately 1.7 micrometer. Analog output signals are processed through phase sensitive detector systems with narrow band electronic filtering (Collins, written communication, 1989). Analog to digital conversion in the microcomputer results in 12 bit digital data. Because the SIRIS is a single-beam instrument, it is necessary to measure reference and sample radiance spectra separately. Spectra are typically measured using solar illumination and HALON as a reflectance standard. HALON is a highly reflective material with no absorption features in the 0.4 to 2.5 micrometer range (Weidner and Hsia, 1981). The reference spectrum is measured first and stored on disk. Depending on sky conditions, a reference spectrum should be measured before each sample spectrum unless atmospheric conditions are clear and dry, in which case a new reference spectrum may not be needed each time. The sample is measured next and both the reference and the sample radiance spectra are automatically stored together in a disk file that can later be reduced to reflectance. The reflectance spectrum can be viewed on the MS-DOS computer prior to proceeding to the next measurement. The SIRIS spectral sampling interval varies continuously with wavelength. In all cases, the actual resolution (sampling interval x 2) is greater than the AVIRIS resolution of 10 nm. 6.C.3.2. DATA SET DESCRIPTION The SIRIS measurement objectives were: 1) to measure reflectance spectra of a bright and dark target at each GRSFE site for potential use in AVIRIS calibration; 2) to fully characterize selected sites at the GRSFE modeling site (Lunar Lake, NV) using visible/infrared reflectance; 3) to collect reflectance spectra for selected endmember materials at each of the GRSFE sites; and 4) to make reflectance measurements for inter-instrument calibration. Visible/Infrared field spectral measurements using the SIRIS were made on 15-19 July, as described in Section 3.C of this document. The SIRIS was set up with standardized geometry; a nadir view from 75 cm above the ground surface, facing towards the sun. Undisturbed surfaces were measured including rock outcrops, surface coatings where present, and soils. All measurements were made using the HALON standard, which makes conversion to absolute reflectance based on NBS standard HALON possible. This conversion was not routinely performed for the SIRIS data and all spectra provided for GRSFE are relative to HALON. No additional SIRIS measurements were made for September AVIRIS flights. SIRIS spectra were reduced to reflectance using software provided by GER. This procedure consists of simple division of the sample radiance spectrum by the reference radiance spectrum. The GER grating- match adjustment was applied to correct for offsets at the grating 35 boundaries and grating overlaps were removed by deleting overlap channels. Previous experience with the instrument and inspection of raw data plots indicated that noisy channels between 1.32 - 1.42 micrometers and 1.78 - 1.95 micrometers should be deleted. Deleted points were coded as 9.99999999. Spectra for some measurement sites were discarded completely because of excess noise and other problems. Measurements made with the SIRIS at the Lunar Lake modeling site for comparison of instrument response. These measurements were made using the JPL SPECTRALON plate as a reference standard. Additionally, several instrument artifacts (or atmospheric bands) are apparent in the SIRIS data. First, there are small instrument glitches near 0.6, 0.76, 0.93, 1.06, and 1.49 micrometers. Secondly, there are commonly prominent CO2 absorption features near 2.005 and 2.05 micrometers that are probably caused by changing atmospheric conditions between measurement of the reference and the sample spectra. Spectra measured with the SIRIS in the lab for the Lunar Lake materials do not show many of these features. Kelso, California, site Spectra were measured on 15 July 1989 along the road and parking lot south of the sand dunes in the center of the valley. These measurements were averaged to constitute the Bright Target. The Dark Target measurement is the average of two spectra taken of the gravel at the power station along the main KelBaker road. Cima, California, site Spectra were measured on 15 July 1989 for basalt and basalt gravel and averaged as the Dark Target. The average of two stream wash spectra constitute the Bright Target. Lunar Crater Volcanic Field, site Spectra were measured periodically throughout the day of 17 July, 1989 for the playa, disturbed playa surface, and cobble modeling sites. Ubehebe Crater, Nevada, site Spectra of a Dark Target (basalt gravel) and Bright Target (small playa surface) were measured on 19 July 1989. Spectra of additional targets were not measured because of rapidly changing, cloudy, weather conditions. Death Valley, California, site Spectra of the Trail Canyon fan, the salt flat in the center of Devil's Golf Course adjacent to the fan, and sand dunes near Stovepipe Wells were measured on 18 July 1989. 36 6.D. THERMAL INFRARED SURFACE DATA 6.D.1. PORTABLE FIELD EMISSION SPECTROMETER (PFES) Note: The following material was provided by Petroy. 6.D.1.1. INSTRUMENT DESCRIPTION The PFES was built for the purpose of measuring the ambient spectral thermal emission of geologic materials in situ, thus avoiding the disturbance of the natural setting which occurs during sample collection. This instrument was designed and built at the Jet Propulsion Laboratory (JPL). The spectral range covered is 5 to 14.5 micrometers and the resolution is approximately 1.5% of the wavelength (0.1 - 0.2 micrometers). The PFES system consists of two main parts, the sensor head and the data recorder. Accessories include a gas bottle, signal monitoring box, reference hot and cold blackbodies, and connecting cables. The sensor head contains the optics, the detector, and the preamplifiers. During operation, the sensor head is connected by a hose to a tank that supplies high pressure argon gas for cooling the detector. The data recorder consists of a lap-top computer, signal processing circuitry, scan sequencing logic circuits, and the power supply. The analyzing element of the spectrometer is a filter wheel containing three filter segments (continuously variable multilayer interference filters). The detector is a MCT (mercury-cadmium- telluride) photoconductor. Spectral measurements of the target are made relative to the spectrum of a reference blackbody at ambient temperature. The kinetic temperature of this blackbody is measured using an attached thermistor (Hoover and Kahle, 1987). Usually about two to three spectra of each target are measured to provide a check of consistency and to reduce noise by averaging. Each spectrum takes about thirty seconds to scan. The digital output from the detector, N, is related to the input by the following simplified equation: N = K[L(t)T(l) + L(l)] (1) where: N = digital output K = constant L(t) = radiance from the target L(l) = radiance from the lens T(l) = transmission of the lens Applying this relationship to measurements of the target and the external blackbody: N(t) = K[L(t)T(l) + L(l)] (2) 37 N(bb) = K[L(bb)T(l) + L(l)] (3) where the variable L(bb) represents the radiance from the external blackbody. Since the two measurements (surface and external blackbody) are made close together in time, the radiance contribution due to the lens is essentially constant. Taking the difference between Equations 2 and 3: N(t) - N(bb) = KT(l) [L(t) - L(bb)] (4) from which L(t) (the target radiance) can be derived: L(t) = [L(bb) + (N(t) - N(bb))] / KT(l) (5) In this equation L(bb) is calculated from the Planck formula and the KT(l) divisor is drawn from a table which has been generated from measurements made on blackbodies at different temperatures. The instrument response function is checked during each operation by measuring a second blackbody at a much lower temperature (the "cold" blackbody) and comparing this measured radiance against calculated radiances at that temperature from the tables of instrument responses (Hoover and Kahle, 1986; 1987). Emissivity can be calculated by dividing the target radiance by the radiance of a blackbody at the same temperature. Target kinetic temperature is determined as the lowest temperature which produces a calculated blackbody curve that is greater than the curve of the target spectral radiance and tangent to the target spectral radiance curve in the region between 7.0 and 7.5 micrometers (in general, most silicates closely approach blackbody behavior in this wavelength region). However, in the case of field spectroscopy, in addition to radiance from the surface, the instrument is also sensitive to the emitted skylight radiance. The skylight radiance is reflected from the surface and scattered into the instrument's field of view. Also, the signal from the surface is modified by attenuation, scattering and emission during transit through the atmosphere (Vincent and Thompson, 1972a). These complications can be modeled as: L(tot) = [e(t)L(bb,T)+r(t)L(sky)]trans(A) + L(A) (6) where: L(tot) = the total spectral radiance received by the detector e(t) = emissivity of the target surface L(bb,T) = the spectral radiance of a blackbody at the same temperature (T) as the target surface r(t) = the reflectivity of the target surface L(sky) = the spectral radiance from the sky, incident on the rock surface trans(A) = the spectral atmospheric transmissivity 38 L(A) = the spectral radiance from atmospheric emission and scattering in the path between the detector and the target surface L(A) and trans are generally considered negligible in field spectroscopy measurements because of the relatively short distances between the target surface and the detector (usually less than one meter). However, the effect of reflected skylight radiance (L(sky)) can not be dismissed. To correct for the reflected skylight term, the radiance of a texturized aluminum plate (e=0.01 to 0.05) is measured to obtain L(sky)), with the assumptions given: L(tot) = e(t)L(bb,T) + [1-e(t)]L(D) (7) where L(D) is the measured spectral radiance from the texturized aluminum plate. The radiance measured from the aluminum plate is representative of the skylight radiance sensed by the detector. Using Kirchhoff's Law, 1-e(t) yields the reflectance of the target. Rewriting equation (7) to solve for target emissivity: [L(tot) - L(D)] / [L(bb) - L(D)] = e(t) (8) Note: the emissivity of the aluminum plate is high for wavelengths shorter than 8 micrometers. Thus, the technique discussed above is only applicable for the 8 to 12 micrometer wavelength range. 6.D.1.2. DATA SET DESCRIPTION PFES data were acquired on July 15 and 17, 1989. A total of 31 measurements were collected for GRSFE. Of these measurements, 13 were calibrations and 18 were of representative surfaces. The data were collected primarily to support the calibration of the TIMS data and to assist in interpreting spectral mixing in the mid-infrared. Sites were selected for calibration that covered a range of emissivities. On July 15, PFES data were collected at Kelso Dunes and the Cima Volcanic Field as part of the Calibration Team effort. Daedalus and SIRIS data were collected over the same sites. For the PFES data, the Kelso Dunes Bright Target site represented the silica-rich endmember and the Cima basalt tephra Dark Target site represented the more silica-poor endmember. On July 17, PFES data were collected at two of the modelling sites at Lunar Lake (the bright and the cobble sites). Several spectra were also collected at the playa surface next to the Lunar Lake thermistor site. PFES data files in this release of the GRSFE archive consist of tables of wavelength, emissivity, measured radiance, gain of internal Blackbody calibration source (not used), Blackbody radiance fit to data, and measured radiances of external cold and hot Blackbodies. Note that emissivities have not been corrected for atmospheric effects. However, data acquired over the aluminum target (called CALIBRATION READING in PDS labels) are provided for users who want to do the corrections. 39 6.E. ATMOSPHERIC DATA 6.E.1. REAGAN RADIOMETER Note: The following material was edited from contributions by Bruegge. 6.E.1.1. INSTRUMENT DESCRIPTION In order to characterize the optical depth over a given site and at a given time and wavelength, a spectrally filtered, solar-pointing radiometer is typically used. The Reagan Sunphotometer, operated by JPL, was used during GRSFE. This photometer was built under the supervision of Dr. John Reagan, University of Arizona, Tucson. The characteristics are summarized in the table given below. It has 10 spectral channels, each about 10 nm in bandwidth, fast response, low noise, and an internal filter wheel. The output voltages of the instrument are proportional to the incident irradiances within a given band, although no calibration relating voltage to physical units is required. Features of the JPL Reagan Sunphotometer ---------------------------------------- Number of Channels 10, internal filter wheel Wavelengths (um) 0.37, 0.40, 0.44, 0.52, 0.61 (Ozone), 0.67, 0.78, 0.87, 0.94 (Water Vapor), 1.03 Bandpass (nm) ~10 Field-of-view 2 degrees, full-field Detector Photodiode, temperature stabilized to 40+/- 0.5 degrees C Response Time < 1 Second Output 2.0-0.2 V Tracking Manual, tripod mounted To prepare the Reagan sunphotometer for data collection, the instrument was mounted to a tripod, the detector heater turned on, and the detector temperature monitored to verify stability at 40 +/- 0.5 degrees C. Operator time clocks were set to the nearest second using a portable radio tuned to WWV. The instrument was then aligned such that the solar disk passes through a site at the front of the optical barrel and onto a cross-hair reticle. Alignment was verified by observing that the output voltage was maximized for this position. Next the start time was recorded to the nearest second, the filter wheel sequenced through its ten positions, a gain and voltage recorded for each channel, and a final stop time recorded. Data were then obtained repeatedly during the observing runs in July and September. 6.E.1.2. DATA SET DESCRIPTION Total instantaneous optical depth was obtained from the data through use of Beer's Law, as follows. The equation in this section are given in Fortran-like notation. 40 V = V0 * exp(-(tau/cos i)) where V = instrument voltage for one channel V0 = equivalent voltage that would be obtained above atmosphere tau = optical depth i = solar incidence angle Taking the natural logarithms of both sides and plotting ln V versus sec i (i.e. Langley Plot) for the set of observations for one channel allows one to solve for V0 = intercept and tau = slope. Instantaneous optical depths were then derived by using this intercept and solving for tau using pairs of voltage values acquired close together in time. The GRSFE data files consist of tables of time and optical depth values computed for each of the 10 Reagan Radiometer channels. The data were also further processed to separate aerosol optical depth from the total, but results are not included in this GRSFE archive release. 6.E.2. SPECTRAL HYGROMETER Note: The following material was edited from contributions by Bruegge and Conel. 6.E.2.1. INSTRUMENT DESCRIPTION Two spectral hygrometers were used simultaneously at Lunar Lake base camp. Their serial numbers are SH015 and SH004. The spectral hygrometers provide the ratio Rsh = L(935)/L(880), where L(935) is irradiance at 935 nm and L(880) is the irradiance at 880 nm. The measurement is acquired by aiming the optics at the sun and keeping the sun's image near the center of a ground-glass screen while the ratio is read from the display. Note that 935 nm is in the middle of an atmospheric water band, whereas 880 nm is not. The principle of operation is that the greater the water vapor abundance, the lower the ratio. 6.E.2.2. DATA SET DESCRIPTION The conversion from spectral hygrometer ratio to column water abundance was calibrated prior to GRSFE for column water abundance using more than 100 radiosonde observations. The line of sight precipitable water, WLOS, in centimeters, is: WLOS = W + (W/6.8)**3 where W = 13.7/((10**1.38)*Rsh) The uncertainty is +/- 10%. To adjust the expression for site elevation: WLOS(corr) = WLOS * SQRT (P0/P), where P0 = pressure at sea level and P = pressure at site elevation. 41 The Spectral Hygrometer data files consist of data acquired on September 29, 1989. Columns are time in PDT, ratio of L(935)/L(880) for instrument SH015, time in PDT and corresponding ratio for instrument SH004. For the July campaign, the Reagan Radiometer data could be used to extract WLOS, since: Rrr = L(940)/L(870) and Rsh = 0.08703 + 1.07992 * Rrr with r**2 = 0.9999 where Rrr = Reagan Radiometer ratio r = correlation coefficient 6.E.3. ARIZONA STATE UNIVERSITY WIND EXPERIMENT Note: The following material has been edited from contributions by Greeley and Lancaster. 6.E.3.1. INSTRUMENT DESCRIPTION Boundary layer wind profiles were measured using field-portable anemometer masts with a total height of 9.8 m. Cup anemometers (Tradewinds) were placed at heights with a logarithmic spacing of 0.75, 1.25, 2.07, 3.44, 5.72, and 9.5 m. Pairs of AD590 temperature sensors were placed in a shielded and ventilated mounting at heights of 1.3 and 9.6 m. Wind directions were measured with WD1 instruments from Remote Measurement Systems at heights of 9.7 m and 1.5 m. Data were recorded using an ADC-1 analog to digital converter and a Tandy 102 computer as a data logger. A recording interval of 20 minutes was adopted, so all data represent a 20 minute average of wind speed and temperature conditions. Data were stored in the field on cassette tapes and transferred to a Macintosh computer at Arizona State University. 6.E.3.2. DATA SET DESCRIPTION Near surface winds were studied at two sites on Lunar Lake Playa: a) Lunar Lake North (LLN) is at the northeast end of the playa, on a smooth clay-silt surface; and b) Lunar Lake South (LLS) is toward the center of the playa, just east of the area of prominent basalt gravel bars on the playa. In addition to providing data on surface winds to GRSFE, these investigations will provide input to studies of the relationships between the radar backscatter and aeolian roughness characteristics of desert surfaces (Greeley et al. 1988). Data were recorded at Lunar Lake North between 13:32 on 16 July 1989 and 17:16 on 18 July 1989 for a total of 52 hours; and at Lunar Lake South between 16:51 on 16 July 1989 and 16:13 on 18 July 1989 for a 42 total of 48 hours. During these periods, wind speeds recorded at a height of 9.6 m varied between 1.36 and 8.16 m/sec. The 20 minute averages of wind speed recorded do not reflect the very unsteady and gusty wind conditions that were observed during GRSFE. Wind directions during periods of winds above 4m/sec were mostly from south to southeast. Note: wind data are presented in degrees clockwise from magnetic north. Temperatures at a height of 1.5 m above the surface ranged from a minimum of 9.25 degrees C around 05:00 on 17 July, to a maximum of 35.62 degrees C on the afternoon of 18 July. Unfortunately, a malfunction in the analog to digital converter resulted in no temperature or wind direction data being recorded at Lunar Lake South. The wind experiment data set is divided into two files, one for each wind tower. The data are in tabular form, with column descriptions and listed results. 6.E.4. WEATHER STATION 6.E.4.1. INSTRUMENT DESCRIPTION The weather station was a portable station designed and built by Meteorological Research, Inc. Cup anemometer and thermistor thermometer measurements of wind speed and direction, dry-bulb air temperature, and rainfall were monitored continuously on a strip chart recorder. The instrument was mounted on a tripod approximately two meters above the surface. 6.E.4.2. DATA SET DESCRIPTION The weather station data consist of wind velocity, direction, and air temperature collected at Lunar Lake during the July and September field campaigns. Data were digitized at 30 minute intervals from stripchart recordings. 6.F. GEOPOSITIONAL SATELLITE PROFILES Note: The following material was edited from a contribution by Garvin. A field differential GPS survey team which included Jim Garvin, Jack Bufton, Bill Krabill, and Earl B. Frederick deployed a pair of Motorola Eagle II GPS receivers to the southern flanks of the feature known as Mars Hill (an alluvial boulder field superimposed on a major lobe of alluvial and colluvial material in Eastern Death Valley) on Oct. 19, 1989. The objective was to measure the 5-20 cm scale microrelief of the boulder field at pixel scales (30-50 m long transects), with vertical control to the few cm level. These microterrain profiles were to be used to help calibrate radar scattering models, and to compare with helicopter stereo data for the same location. The GLOTAS technique, as implemented at the time of GRSFE, involves recording GPS carrier phase data for at least 4 satellites simultaneously with two 8-channel receivers. In this approach, one 43 (master) receiver/antenna is fixed at a reference point (which can be surveyed in using GPS itself), and after a suitable calibration period, the second GPS receiver/antenna system is moved from its position beside the fixed master in whatever pattern is desired to develop a topographic profile or grid. The mobile GPS receiver/antenna permits positional data in all three axes (x,y,z) to be recorded at a rate of once per second, which can then be cross-referenced to the fixed master, and later tied to an absolute geodetic positional reference system. The primary interest was in relative horizontal position and in relative relief at each position. Hence, an inverter was attached to a jeep battery to power a COMPAQ 386 computer to record all the GPS tracking data from both receiver/antenna systems. Data were collected by cabling the mobile GPS system to the computer by means of a 150-foot cable, which limited profiling length to just under 50 m. The system was deployed to the southern flanks of Mars Hill, and a profile position was randomly chosen with a bearing of 040 degrees from true magnetic N (measured from the base of Mars Hill using a Brunton). A 100 m long tape measure was used to demark the measurement positions, which were spaced every 5 cm except for flat inter-boulder regions, at which time measurements were made every 10 or 20 cm (our "fractal" assumption). The initial profile extended for 37 m on a heading of 040 degrees, and the resampled average measurement spacing was ~ 10 cm. Measurements were made at 10 sec intervals (10 samples) at each data point, and moved the mobile GPS unit as rapidly as possible between ground sampling points. The antenna was mounted on a fibreglass pole and attached on a circular plate at the top of the 6-foot long pole to minimize interference due to intervening people etc. The first profile took approximately 50 minutes to collect, and the error analysis suggests that 2-3 cm RMS vertical precision was achieved over the length of a 37 m long GLOTAS profile (we were tracking 6-7 satellites during this operation). After the success of the initial profile, a second profile position was chosen at random, to extend from the base of the hill to about 30 m distant. The true bearing of this profile was 320 deg. (relative to magnetic N), and it was chosen so as to begin at the same starting location as Profile 1. Identical conventions were used on this profile, and the average resampled data point spacing was 11 cm. The vertical RMS was again 2-3 cm (max), and if a few of the suspect data points are removed, the vertical RMS precision is as good as 1 cm. This profile required only 35 minutes to collect. The column headings for the GPS data are: Column 1: Time (sec) GMT Column 2: Time hhmmss.sss (GMT) Column 3: Ellipsoid Height (meters) -- relative to WGS-84 (this is microrelief) Column 4: Latitude (deg. North) Column 5: Longitude (deg. East) Column 6: Along track sampling distance in meters 44 Column 7: no. of GPS samples at spot height position (# sec. dwell time) Note that ellipsoid heights are below sealevel and hence negative in Death Valley at Mars Hill. 6.G. PROFILES FROM HELICOPTER-BORNE STEREOPHOTOGRAPHY Selected sites, including those areas chosen for calibration and modeling purposes, were photographed via helicopter-borne 70 mm stereophotography using the JPL Hasselblad system flown by Farr. Some of the data have been reduced to vertical profiles and arrays at a spacing and accuracy required to meet topography requirements. These data cover approximately 5x10 meter square areas. For GRSFE archive Release V1.0, three profiles are located over or close to the mantled lava flow modeling site and one is located over the playa modeling site. The files contain two data columns. The first column contains position along track in centimeters and the second contains relative elevations in centimeters. For each location there are 15 profile files. The first five are along-track, and the remaining ten are cross-track. The profiles are approximately one meter apart. 7. AIRBORNE DATA SETS 7.A. ASAS Note: The following is edited from material contributed by Irons. 7.A.1. INSTRUMENT DESCRIPTION The Advance Solid-State Array Spectroradiometer (ASAS) was flown aboard the NASA/Ames C-130 on July 17, 1989, in support of GRSFE. ASAS is an airborne, off-nadir pointing, imaging spectroradiometer used to acquire multispectral and multi-view angle bidirectional radiance data for terrestrial targets. The sensor employs charge-injection-device (CID) detector array technology operated in the "pushbroom" fashion to acquire digital image data for 29 spectral bands (Irons and Irish, 1988; Irons et al., 1991; Stewart et al., 1985). The bands cover the range of 465 nm to 871 nm with a resolution of approximately 15 nm. At an altitude of 5000 m, the cross-track sensor field-of-view is 2200 m (25 degrees spanned by 512 pixels) and the cross-track spatial resolution is 4.25 m. A gimballed mounting bracket allows ASAS to be pointed up to 45 degrees off nadir either fore or aft of the platform aircraft. ASAS is able to track and image a target site through a sequence of fore-to-aft view angles as it flies over the site. The basic ASAS data product is a sequence of multispectral digital images acquired from multiple view directions and consisting of calibrated spectral radiance values. To produce these calibrated images each of the 15,000 detector elements in the CID array must be spectrally and radiometrically calibrated. The spectral calibration is performed by exposing the ASAS aperture to narrow-band energy from a laboratory 45 monochrometer. The radiometric calibration is accomplished by exposing the ASAS aperture to known levels of spectral radiance from an integrating hemisphere reference source maintained at the NASA/Goddard Space Flight Center. The digitized response of each detector element to incident radiant flux is characterized as a piecewise linear function of spectral radiance on the basis of the laboratory calibration data. The data acquired by each detector in flight are then converted to units of spectral radiance by inverting the appropriate response function. The resulting values are stored as binary integers in units of 0.1 watts / (meter squared * micrometer * steradian) in a band sequential digital image format. The uncertainty associated with spectral radiance values is approximately 6 percent. Note that the values represent the radiant flux received by the sensor at the altitude of the platform aircraft. The calibration and correction procedures are discussed in greater detail by Irons and Irish (1988) and Irons et al. (1991). ASAS Spectral Band Centers and Full-Width-Half-Maximum (FWHM) Points Band FWHM FWHM Channel Center(nm) Minimum(nm) Maximum(nm) ------------------------------------------------------------------- 2 465 458 472 3 479 472 486 4 493 486 500 5 507 500 514 6 521 514 528 7 535 528 542 8 549 542 556 9 563 556 570 10 577 570 585 11 591 584 599 12 606 599 613 13 620 613 628 14 635 627 642 15 649 642 656 16 663 656 671 17 678 671 685 18 693 685 700 19 707 700 715 20 722 714 729 21 738 731 746 22 753 745 760 23 767 760 775 24 782 774 790 25 797 789 805 26 812 804 819 27 826 818 834 28 841 833 849 29 856 848 864 30 871 863 879 46 Note: Channel 1 is inoperable, but digitized signals from channel 1 are still included in ASAS data sets. Thus, the list of channels begins with Channel 2. The Channel 1 values are meaningless and will eventually be omitted from ASAS data sets when the data processing software is revised. 7.A.2. DATA SET DESCRIPTION Most of the ASAS data acquired for GRSFE were taken during flights over Lunar Lake, Nevada, at a nominal altitude of 5000 m above ground level. Flights over Lunar Lake were repeated to acquire data for a range of solar zenith angles and to obtain data for several view azimuth angles (i.e., for several flight headings relative to the solar principal plane). On most flights, the sensor field of view was initially pointed forward 45 degrees as the aircraft approached the site. The sensor then imaged the site through a sequence of seven fore- to-aft view directions ranging from 45 degrees forward to 45 degrees aftward in 15 degree increments as the aircraft flew over the site. The primary target of interest was the Lunar Lake playa, but the digital images also include data for the lava flow and cobble areas within and around the playa. Data were acquired in a similar manner on one flight over the Ubehebe Crater. One flight over Lunar Lake was also flown approximately along the solar principal plane with the ASAS view zenith angle fixed at the solar zenith angle. The purpose of this flight was to observe the opposition effect. Several characteristics of the ASAS digital image data should be noted by investigators and analysts. First, the image data are geometrically distorted. One reason for the distortion is the roll, pitch, and yaw of the platform C-130 aircraft during data acquisition. A second reason is the rectangular, instead of square, dimensions of the surface area represented by each image pixel. The pixel dimensions depend on the aircraft speed, the instrument scan rate, and the pointing angle of the instrument. Two of the ASAS scenes (with GRSFE product IDs ASALL04D and ASALL05D) were acquired at 48 scan lines per sec. Given the nominal aircraft speed of 100 meters per second, the along-track pixel dimension in these two scenes is 2 meters. The rest of the ASAS scenes were acquired at a scan rate of 64 scan lines per second and the along-track pixel dimension for these scenes is 1.5 meters. The across- track dimensions of the pixels in all of the ASAS scenes are 4.3 meters, 4.5 meters, 5.0 meters, and 6.1 meters for pointing angles of 0 (nadir), 15, 30, and 45 degrees, respectively. No attempt has been made to geometrically rectify the ASAS digital image data provided for the GRSFE CD-ROMs. Another intermittent distortion has been observed during initial inspections of ASAS imagery acquired for GRSFE. The scan lines occasionally appear to shift laterally by one or two pixels with the direction of the shift alternating every scan line. This distortion is most clearly exhibited at a smooth boundary between a bright area and a dark area within a scene. Such smooth boundaries will occasionally appear jagged in ASAS imagery particularly when the image around the 47 boundary is magnified. The cause of this distortion has not yet been determined. Investigators and analysts should also note that the ASAS data are stored as binary integers in units of 0.1 watts/(meter squared * micrometer * steradian). In other words, any integer ASAS datum should be divided by 10 to recover a real number radiance value in units of watts/(meter squared * micrometer * steradian). The factor of 10 for all ASAS channels was chosen for the convenience of analysts. Analysts should not infer that the radiometric resolution of each ASAS detector is 0.1 watts/(meter squared * micrometer * steradian) per raw digital count. The actual radiometric resolution varies from channel to channel and, to a lesser degree, from detector to detector for the 512 detectors per channel. 7.B. AVIRIS 7.B.1. INSTRUMENT DESCRIPTION The AVIRIS instrument is essentially a group of four spectrometers that view the surface through a scanner while being carried over a site in an aircraft. Blocking filters help partition reflected light amongst the spectrometers. At any one moment the spectrometers are viewing a spot on the ground 20 meters square. This pixel is viewed simultaneously in 224 spectral bands. A spatial image is built up through the scanner motion, which defines an image line 614 pixels wide perpendicular to the aircraft direction, and through the aircraft motion, which defines the length of the image frame. The data are collected on a tape recorder for later analysis. There is an on-board calibrator which checks the spectral and radiometric alignment of the spectrometers during the operation of the instrument to ensure the accuracy of the spectral data. To do this the calibrator's output must be invariant over the small temperature excursions around the operating temperature (-23 degrees C) and stable during the time period of the instrument operation. Light from a filament lamp is imaged by a concave metal mirror through a filter wheel onto the fiber optics leading to the spectrometers. The fibers are at the meridional focus so the astigmatism of the mirror blurs the filament image, reducing the sensitivity of the system to movement. The mirror and structure are monometallic so thermal effects are minimized. The rotating shutter in the foreoptics enables the light from the foreoptics to be shut off during calibration. The filter wheel in the calibrator has four positions, one of which cuts the light off. Two of the positions are used for neutral density filters to provide two radiometric levels, and the other position is used for a didymium rare earth filter to provide a reference spectrum. This spectrum is relatively independent of the operating temperature, unlike a dichroic. 48 7.B.2. DATA SET DESCRIPTION AVIRIS data are divided into 10x10 square kilometer scenes for purposes of standard product generation. More than 40 scenes were generated during GRSFE, more than 20 of which are included on the CD- ROMs, covering a variety of surfaces. Further, Lunar Crater was covered several times in one day (under clear atmospheric conditions) in order to evaluate atmospheric scattering and absorption removal algorithms and to explore extraction of roughness information using variable incidence angle AVIRIS data. The AVIRIS multi-temporal data were acquired at the same time that ground-based, multi-spectral measurements of atmospheric optical depth, and sky radiance at varying scattering angles were acquired, along with surface bidirectional reflectance data. Accurate wavelength calibration of AVIRIS was performed by JPL using laboratory measurements acquired before and after the AVIRIS flights. An additional check on the wavelength calibration can be made by comparing the positions of known atmospheric absorption features to their locations in actual AVIRIS data. Each AVIRIS scene is calibrated to radiance. The radiance values are stored as 16-bit integers in units of 100 microwatts / (centimeters squared * nanometers * steradians). Each AVIRIS scene is accompanied by 7 ancillary files. They are the navigation, engineering, dark current, offset, dropout, radiometric calibration, and raw spectral calibration files. The navigation file contains the data from the aircraft navigation system. It is recorded by the AVIRIS instrument every major frame. However, it is only updated by the aircraft system every five seconds (60 major frames). It contains the following information: flight id, run id, date, time, latitude, longitude, N-S velocity, E-W velocity, true heading, ground speed, vertical velocity, altitude, true air speed, pitch and roll. The engineering file is from the AVIRIS instrument. It is recorded every major frame and contains the following information: detector temperatures, spectrometer temperatures, scanner optics mount temperature, scan voltages, calibration lamp current, hardware status indicators, scan mirror readings, instrument roll gyro readings, instrument yaw gyro readings, and instrument firmware status indicators. The dark current file contains data taken with the fore-optics shutter closed during scanner flyback and is recorded every major frame. This data has had the initial dark current (offset) data subtracted from it onboard the aircraft. It is therefore a record of how the dark current varies with time over a flight line with respect to the initial dark current. The offset file contains the initial, raw, dark current data taken once, prior to each flight line. It is taken with the fore- optics shutter closed and recorded without any on-board subtraction performed (the same values are recorded every major frame throughout a flight line). This data is subtracted from the image data onboard the aircraft during a flight line in order to keep the image signal level on scale in the signal chain. It is also onboard subtracted from the dark current measurements taken during a flight line. 49 The dropout file contains the data compiled during the logging process. Anomalies in the recording process can cause some lines to contain unintelligible data. These lines are flagged at 4096 DN, and are called dropped lines. The dropout file is a list of those lines that have been flagged. The radiometric calibration file contains the real number calibration coefficients which transform the DN values of the raw image into units of radiance. The units of these coefficients are microwatts per square centimeter per nanometer per steradian per DN. Note that the AVIRIS image data on the GRSFE CD-ROMs are already calibrated and given as radiance values. This data has been adjusted for cross-track vignetting and for offsets between the spectrometers. The raw spectral calibration file contains two real numbers per channel. The first number is the wavelength position corresponding to the channel number, and the second is the full width half max number for the spectral response function of each channel. 7.C. TIMS Note: The following is edited from material contributed by Shelley Petroy. 7.C.1. INSTRUMENT DESCRIPTION The TIMS instrument is a six-channel thermal infrared spectrometer with a spectral range between 8.0 and 12.0 um. Cross-track scanning is achieved through rotation of a 45 degree flat scan mirror that reflects incident energy to a 19 cm diameter, 33 cm focal length parabolic primary mirror. The energy is then directed into the spectrometer section of the instrument by a flat secondary mirror. Both the primary and secondary mirrors are aluminum coated with an overcoating of silicon oxides. At the entrance to the spectrometer section and at the focal plane of the primary mirror is a 0.8 mm field stop aperture which defines the instrument's 2.5 mrad Instantaneous-Field-of-View (IFOV). After passing through the field stop the energy is collimated by an off- axis parabolic section mirror and directed to a replica grating of 12 grooves per mm with a blaze angle of 3.4 degrees, which produces the spectral dispersion. A germanium triplet image lens is used to form an image of the field stop in the detector plane. The image size is 0.38 mm in this plane. The detector consists of a linear array of six MCT (mercury-cadmium-telluride) detector elements mounted on a cold finger from the inner flask of a liquid nitrogen dewar. The width of these detectors (0.43 mm) is a little larger than the image of the field stop aperture and the length is set by the desired bandwidth. The channel wavelengths and Full Width at Half Maximum (FWHM) points are shown in the table below. The thermal reference sources are mounted on the scan head so the scan mirror views one after scanning across the Field-of- View (FOV). This permits line-by-line calibration of the TIMS data. TIMS Channels and Full Width at Half Maximum (FWHM) Points 50 Channel Wavelengths FWHM ------- ---------- ---- 1 8.2 - 8.6 0.4 2 8.6 - 9.0 0.4 3 9.0 - 9.4 0.4 4 9.6 - 10.2 0.8 5 10.3 - 11.1 1.0 6 11.3 - 11.7 1.0 The TIMS optical system consists of a 19 cm diameter Newtonian reflector telescope mounted behind an object-plane 45 degree flat scanning mirror and followed by a Czerny-Turner spectrometer. The primary optical system uses a f1.9 parabolic primary mirror with a field determining aperture located in its focal plane. An off-axis parabolic mirror is used to collimate the energy emerging from the aperture which is then dispersed by the diffraction grating and re-imaged on the detector array by a fast f0.6 germanium lens. All of the primary optical elements, the field stop, the off-axis collimator, and the detector dewar are mounted on sliding blocks controlled by Invar metering rods to provide the active thermal compensation for scan head ambient temperature changes. The three element germanium imaging lens is also internally thermally compensated for changes in ambient temperature. Two thermal references sources are mounted in the TIMS scanner head; thus the scan mirror views one before and one after scanning across the Field-of-View (FOV). As mentioned previously, this permits line-by-line calibration of TIMS data. Each reference source is a 20.3 cm square copper plate coated with Krylon 1602 ultra-flat black paint (paint layer is 0.64 cm thick). Thermistors are mounted in slots cut into the rear of these plates. Reference source 1 can be heated or cooled and is used as the lower temperature reference source. Reference source 2 can be heated only and is used for the higher temperature reference source. The emissivities of the thermal reference sources are known (presumably emissivity=1.0 for the black paint surface). The temperatures of both references are set before the flight (usually 10 and 30 degrees C) and are measured independently throughout the flight using the embedded thermistors (temperatures of both reference sources are recorded from the thermistors during each scan of the instrument). At the same time the thermistor temperatures are recorded, the scanner head records a DN value for each reference source through all of the six channel filters, consecutively. Each DN value recorded for the reference sources for each of the six channels can then be related directly to a radiance value through the following relationship which translates the scene DNs for each scan line into physical units using the internal reference sources. This also allows any scan to scan differences in the system operation to be easily detected. TIMS was designed such that the output data numbers Dx are linearly related to the input radiance Rx through the relationship 51 Rx = a + bDx For each scan line, the radiance and data number for the two internal reference sources are known and can be used to determine the constants a and b. It is then possible to solve for Rx from Dx, both channel-by- channel and scan-by-scan. Rx is in physical units (watts/(meter squared * steradian) and to first order is independent of the TIMS system state at the time of measurement. For a more detailed description of TIMS data reduction, see Palluconi and Meeks (1985). The accuracy of brightness temperatures or emissivities calculated from TIMS data depends on the accuracy with which the brightness temperature of the reference sources can be established. To determine this relationship, laboratory measurements involving two different external blackbodies have been made. The first set of measurements indicated that the brightness temperature of the internal reference sources agreed with the external blackbody to within +/- 1.8 degrees C at all internal reference source temperatures checked (24 to 51 degrees C). The second set of measurements covering a wider range (10 to 55 degrees C) have not yet been fully reduced; however, preliminary results do not appear to agree with the first set. It may be that encoded radiance values vary somewhat with the temperature of the TIMS itself. During data acquisition, the TIMS instrument is exposed to the atmosphere. A direct consequence of this experimental set-up is an overestimation of the blackbody temperatures, due to the presence of condensation on the blackbodies and additional radiant cooling of the blackbody surfaces. This results in an underestimation of the radiance of the blackbodies and of the ground surface being imaged. The absolute effects of this problem are being presently studied by researchers at the Jet Propulsion Laboratory. 7.C.2. DATA SET DESCRIPTION During the July, 1989, TIMS flights, the reference sources did not maintain a constant temperature. Instead, the temperature of the sources appeared to vary periodically (3 degrees on average) about a mean temperature (usually the initial preset temperature) as tracked by the thermistors. Unfortunately, this temperature periodicity was not tracked accurately by the scanner - it was more rapid than the scanning period. Thus, the scanner sampled different pieces of the temperature wave during the time of data collection. In addition to this problem, the temperature variation was often insufficient to trigger the scanner to record a higher DN value, so two or more temperatures (as recorded by the thermistors) are often represented by a single DN value. In other words, at no time was the true temperature or the corresponding DN value known precisely. As a result of these calibration problems, the TIMS data are presented in values of DN only. Each image file contains 6 bands in band-interleaved format, 8 bits per pixel. Each image is accompanied by an auxiliary file which contains the line by line temperature values of the references sources as recorded by the thermistors during each data 52 take as well as the corresponding radiance values (in all six bands) for each thermistor as recorded by the scan head. Principal-component decorrelation stretches of these data are still useful for relative comparisons between materials in one scene, because this processing technique is not dependent on a calibrated data set. For users who are only interested in this type of product, it is not necessary to calibrate the data. However, for users who are interested in extracting temperature or emissivity values from the images, additional work is necessary before using these data. The TIMS data are in the [TIMS] directory on several GRSFE CD-ROM volumes. The image files have names in the format TIMxxxxA.IMG, and the auxiliary files have names in the format TIMxxxxB.DAT. 7.D. AIRSAR Note: The following material is edited from contributions by Evans and Plaut. 7.D.1. INSTRUMENT DESCRIPTION AIRSAR is a synthetic aperture radar that operates in a polarimetric mode in C (5.66 cm), L (23.98 cm) and P (68.13 cm) wavelengths and is a prototype of the radar that will fly on the Earth Observing System. Its multifrequency, full polarimetric capability is augmented by acquiring multiple incidence angle views of a scene. The data can be used to evaluate the utility of polarimetric SAR in multiple frequency and incidence angle domains. Calibration is provided by on-board systems and by use of corner reflectors located in scenes. AIRSAR flies on NASA's DC-8. Signals are derived from a stable local oscillator source operating at the L-band center frequency (1250 MHz). The P-band center frequency is derived from this source by down-converting, while the C- band center frequency is derived by up-converting. 7.D.2. DATA SET DESCRIPTION External calibration of relative amplitude, relative phase, absolute amplitude, and system cross-talk using the radar return from natural targets and at least one trihedral corner reflector was done using the procedure described by van Zyl (1990). The calibration technique involves four steps, 1) phase calibration using the phase equalization based on a relatively homogeneous area where the HH-VV phase difference is assumed to be zero based on the small perturbation model (Zebker and Lou 1989); 2) cross-talk calibration which assumes that the cross-talk parameters are reasonably small and that the average co- and cross- polarized components of the scattering matrix are uncorrelated; 3) co- polarized channel amplitude and phase imbalance calibration using trihedral corner reflectors deployed in the scene prior to imaging; and 4) an overall radiometric calibration using the measured absolute radar cross section of the trihedral corner reflectors in the scene. The location and orientation of each of the corner reflectors used in calibration of the GRSFE Lunar Lake / Lunar Crater data are listed in the table below. X=data sample number, Y=data line number, AZ=the angle of the front edge of the corner reflector with respect to true north, 53 EL=Elevation angle of the base of the corner reflector, size=length of the side of the corner reflector in meters. Line, sample coordinate origin is in upper left; lines correspond to rows whereas samples correspond to columns in the data array. Contact Diane Evans, Jet Propulsion Laboratory, via telephone at 818-354-2418 or via electronic mail at BERLIN::EVANS (NASA Science Internet), for information on the specific locations of other corner reflectors deployed during GRSFE. The AIRSAR calibration software (POLCAL) derives calibration parameters based on corner reflector information. These parameters include the phase of the co-channel imbalance, the amplitude of the co- channel imbalance, the correlator gain and the signal to background ratio. Note that for all of the GRSFE data, the phase of the co-channel imbalance was sufficiently close to zero after applying Step 1 above that they were not adjusted further based on the corner reflector data. The co-channel amplitude balance and correlator gain may change across the radar swath, and a polynomial fit is generated which best matches the ensemble of corner reflector data in the scene. In all GRSFE data a zero-order polynomial was used for both corrections. In the Lunar Crater data, a constant value was used to correct for correlator gain in each of the frequency bands since all of the corner reflector data were so similar (4.97 dB for C-band, 4.37 dB for L-band, and 4.22 dB for P- band). In order to test the accuracy of the calibration, corner reflector polarization signatures were compared with theoretical values. See the POLCAL User's Manual (van Zyl et al., 1990) for further information about calibration procedures. CORNER REFLECTORS USED FOR LUNAR LAKE/LUNAR CRATER GRSFE PRODUCT ID: AIRLV001 JPL ID: LUNAR2061 X Y AZ EL SIZE (M) CR4 692 616 205.4 10.1 1.828 CR15 850 770 205.5 12.1 2.438 CR2 754 872 205.0 10.7 1.828 CR13 1008 1062 205.6 10.1 2.438 GRSFE PRODUCT ID: AIRLV002 JPL ID: LUNAR2062 X Y AZ EL SIZE (M) CR7 996 296 205.0 11.5 2.438 CR14 886 554 205.5 11.2 2.438 CR4 398 752 205.4 10.1 1.828 CR15 560 912 205.5 12.1 2.438 CR2 462 1020 205.0 10.7 1.828 GRSFE PRODUCT ID: AIRLV003 JPL ID: LUNAR2063 X Y AZ EL SIZE (M) CR7 948 498 205.0 11.5 2.438 CR14 844 788 205.5 11.2 2.438 CR4 330 1002 205.4 10.1 1.828 CR15 504 1176 205.5 12.1 2.438 54 GRSFE PRODUCT ID: AIRLV005 JPL ID: LUNAR2066 X Y AZ EL SIZE (M) CR7 896 119 205.0 11.5 2.438 CR14 787 331 205.5 11.2 2.438 CR4 298 506 205.4 10.1 1.828 CR15 459 655 205.5 12.1 2.438 CR2 360 756 205.0 10.7 1.828 CR13 617 940 205.6 10.1 2.438 GRSFE PRODUCT ID: AIRLV006 JPL ID: LUNAR2065 X Y AZ EL SIZE (M) CR14 330 242 205.4 10.1 1.828 CR15 498 364 205.5 12.1 2.438 CR2 396 454 205.0 10.7 1.828 CR13 672 617 205.6 10.1 2.438 CR12 670 918 206.5 10.5 2.438 8. SOFTWARE Included in this GRSFE release is a VAX/VMS Fortran program to convert AIRSAR data from the compressed Stokes matrix format in which it is stored to images suitable for display. The program, called SYNTHESIZE, is found in the file SYNTHESZ.FOR in the SOFTWARE directory on CD-ROM volume 1. Questions about this software should be directed to Diane Evans, JPL, who provided it for publication on the GRSFE CD-ROMs. 9. FLIGHT LINE LOCATOR MAPS Include in this GRSFE release is three schematic maps stored as raster images. These maps can be used to locate the flight lines of the airborne instruments. AVIRIS flight lines are shown in AVRLOC.IMG; AIRSAR flight lines are shown in AIRLOC.IMG; and ASAS and TIMS flight lines are shown in TIMLOC.IMG. The image files are found in the LOCATOR directory on CD-ROM volume 1, along with detached PDS labels describing their contents. 10. GRSFE SAMPLER DATA SETS To help the user understand the utility of GRSFE, a selected set of ASAS, TIMS, and AIRSAR data over Lunar Lake and surroundings were geometrically registered to AVIRIS frame AVRLV02A.IMG. The registration involved selection of three or four ground control points and use of bilinear interpolation procedures to do the geometric rectification. The registered ASAS, TIMS, and AIRSAR images are in the SAMPLER directory on CD-ROM Volume 2. The AVIRIS image to which they are registered is in the [AVIRIS.AVRLV02] directory, also on Volume 2. Three tie points were used to register, using bilinear interpolation, ASAS scene ASALL05D.IMG to the AVIRIS scene. The ASAS 55 data are provided as radiance-at-sensor values: DN/10 = watts/m**2/sr/um at the sensor. For AIRSAR we chose HH (horizontal transmit and receive) and HV (horizontal transmit, vertical receive) polarizations and show C, L and P band data. AIRSAR scene AIRLL05C/L/P were converted to ground range (rather than slant range), and four tie points were used to register the image to the AVIRIS scene. To convert the DNs to units of radar cross section in dB, using the gains and offsets shown in the table below, subtract the offset value and divide the result by the gain. The HV images show some scattered zero values that are an artifact of the compression (to dB) processes. Polarization: HH Band C: Offset 161.0 Gain 3.5 Band L: Offset 178.5 Gain 3.5 Band P: Offset 177.0 Gain 3.0 Polarization: HV Band C: Offset 250.0 Gain 2.5 Band L: same as band C Band P: same as band C For TIMS data we include a principal-components enhancement of bands 1, 3, and 5. The TIMS scene used was TIMLL02A.IMG. Bands 1, 3, and 5 were converted into principal component images, stretched 1%, converted back into bands 1, 3, and 5. Seventeen points were used to register the images to the AVIRIS image. There is some distortion evident in the registered TIMS images which could not be corrected. 11. INDEX TABLES For those data sets that include many files, index tables have been created to allow the user to search for subsets of the data more efficiently. All index tables are located in the INDEX directory on GRSFE Volume 1. Table 11.1 shows the GRSFE data sets that have index tables. An index table is an ASCII text file that lists the important label parameters for each file in a data set. The information is in a format that can be easily loaded into a data base management system. The table has one row for each file in the data set. The columns are comma- delimited, with text fields surrounded by double quotation marks ("). Each index table is accompanied by a detached PDS label that describes the columns, including the byte offset and number of bytes for each column (not including the commas and quotation marks). TABLE 11.1 INDEX TABLES FOR GRSFE DATA SETS Data Set Index Table -------- ----------- 56 AIRSAR AIRINDEX.TAB ASAS ASAINDEX.TAB AVIRIS AVRINDEX.TAB Daedalus DAEINDEX.TAB Helicopter Stereo Photography Profiles ELEINDEX.TAB PARABOLA PRBINDEX.TAB PFES PFSINDEX.TAB SIRIS SIRINDEX.TAB TIMS TIMINDEX.TAB 12. DATA SET LABEL AND FILE ORGANIZATION The data sets on this CD-ROM are accompanied by detached PDS labels to describe and point to data files. In some cases the image files also have embedded VICAR2 labels. The reader is referred to the file VICAR2.TXT in the DOCUMENT directory and to LaVoie et al. (1987) for discussion of VICAR2 labels. The remainder of this section describes the detached PDS labels. The PDS label contains descriptive information about the data file and objects within the file. The label consists of keyword statements that conform to the Object Description Language (ODL) developed by the PDS project. There are three types of ODL statements within a label: structural statements, keyword assignment statements, and pointer statements. Structural statements provide a shell around keyword assignment statements to delineate which data object the assignment statements are describing. The structural statements are: 1) OBJECT = object_name 2) END_OBJECT 3) END The OBJECT statement begins the description of a particular data object and the END_OBJECT statement signals the end of the object's description. All keyword assignment statements between an OBJECT and its corresponding END_OBJECT statement describe the particular object named in the OBJECT statement. The END statement terminates a label. It must appear as a single statement that contains only the word END. A keyword assignment statement contains the name of an attribute and the value of that attribute. Keyword assignment statements are described in more detail in Appendix B of this document. These statements have the following format: name = value Values of keyword assignment statements can be numeric values, literals, or text strings. 57 Pointer statements are a special class of keyword assignment statements. These pointers are expressed in the ODL using the following notation: ^object_name = location If the object is in the same file as the label, the location of the object is given as an integer representing the starting record number of the object, measured from the beginning of the file. The first label record in a file is record 1. Pointers are useful for describing the location of individual components of a data object. Pointer statements are also used for pointing to data or information stored in separate files. An example of a pointer to information stored in a separate file is shown below: ^DESCRIPTION = "logical_file_name" The value of "logical_file_name" is the name of the file containing the description. An example of a pointer to a record within a file is: ^IMAGE = ("logical_file_name",2) This indicates that image data begins at record 2 in file "logical_file_name". Each keyword assignment is stored as a single variable-length record. An example of a label is shown below. Appendix C of this document provides a detailed description of each keyword found in the labels. EXAMPLE OF A DETACHED PDS IMAGE LABEL CCSD3ZF0000100000001NJPL3IF0PDS20000000001 = SFDU_LABEL /* PDS label for an AVIRIS image */ RECORD_TYPE = FIXED_LENGTH RECORD_BYTES = 1228 FILE_RECORDS = 114689 /* Pointers to image objects */ ^IMAGE_HEADER = ("AVRLV14A.IMG",1) ^IMAGE = ("AVRLV14A.IMG",2) /* Image description */ DATA_SET_ID = 'ER2-E-AVIR-3-RDR-IMAGE-V1.0' PRODUCT_ID = "AVRLV14A" INSTRUMENT_NAME = 'AIRBORNE VISIBLE/IR IMAGING SPECTROMETER' TARGET_NAME = EARTH FEATURE_NAME = "LUNAR CRATER VOLCANIC FIELD" IMAGE_TIME = 1989-09-29T20:46:11Z FLIGHT_LINE_NUMBER = 2 FLIGHT_RUN_NUMBER = 3 CENTER_LATITUDE = 38.378 CENTER_LONGITUDE = 116.023 INCIDENCE_ANGLE = 44.3 58 EMISSION_ANGLE = 0.0 /* Description of objects */ OBJECT = IMAGE_HEADER BYTES = 1228 RECORDS = 1 TYPE = VICAR2 ^DESCRIPTION = "VICAR2.TXT" END_OBJECT = IMAGE_HEADER OBJECT = IMAGE LINES = 512 LINE_SAMPLES = 614 SAMPLE_TYPE = VAX_INTEGER SAMPLE_BITS = 16 SAMPLE_BIT_MASK = 16#FFFF# BANDS = 224 BAND_STORAGE_TYPE = LINE_INTERLEAVED END_OBJECT = IMAGE END 13. DISK DIRECTORY STRUCTURE AND FILE NAMES The volume and directory structure of this CD-ROM conforms to the level-1 standard specified by the International Standards Organization (ISO). The ISO standard was used so that the disks can be accessed on a wide variety of computer systems. Information on the ISO CD-ROM standard is provided in Appendix A of this document. Appendix H is a list of the directories and files on each CD-ROM volume. The directory structure is discussed further below. The top level directory of each GRSFE CD-ROM contains two text files. The first is a brief description of the structure and contents of the disk called AAREADME.TXT. The second is a file called VOLDESC.SFD, which is meant to be read via computer and which contains a broad description of the structure and contents of the disk, written using a structured Standard Data Format Unit convention. All other files on the disks are contained in directories below the top level directory. On Volume 1, the directory DOCUMENT contains the text file you are currently reading, VOLINFO.TXT. The DOCUMENT directory also includes text files that describe the format of some of the data files. These files are referenced in the detached labels that accompany the data files. The directory INDEX, also on Volume 1, contains the index tables described in Section 11. The SOFTWARE directory, also on Volume 1, contains the AIRSAR conversion software described in Section 8, and the LOCATOR directory contains the three locator images described in Section 9. The SAMPLER directory, on Volume 2, contains the data sets discussed in Section 10. Separate directories exist for each instrument that acquired data for GRSFE. Each of these directories contains data set files and associated detached labels. Some instrument directories are further 59 subdivided to manage a large number of files or to logically group a collection of files. The ground-based data sets are all located on Volume 1, and the airborne data sets are spread over Volumes 1 through 9. See Appendix H for locations of specific data files. The following approach was used to name files in ways that allow the user to infer the type of data in a reasonably straightforward manner, while maintaining the 8 character limit for file names. The convention uses codes for the instrument that acquired the data, the location, and a 3 character ID number. The file extension (three characters following a period) indicates the type of data in the file. The codes are shown below in Table 13.1, followed by several examples. TABLE 13.1 FILENAME STRUCTURE FOR GRSFE FILES Instrument Site ID AIR=AIRSAR AF=Afton nnn=3 digit sequence ASA=ASAS CM=Cima nna=2 digit sequence AVR=AVIRIS DD=Death Valley Dunes + 1 alpha sequence DAE=DAEDALUS DG=Devil's Golf Course aaa=3 alpha sequence ELE=HEL ST PHOT KL=Kelso GPS=MICROTERRAIN LL=Lunar Lake HYG=HYGROMETER LV=Lunar Crater PFS=PFES Volcanic Field PRB=PARABOLA MH=Mars Hill REG=REAGAN RAD PV=Providence RMT=RADIOMETER SM=Sample registered images SIR=SIRIS TC=Trail Canyon Fan THM=THERMISTOR UB=Ubehebe TIM=TIMS WND=WIND EXP WTH=WEATHER ST Examples: a. AIRSAR over Ubehebe Crater, File One = AIRUB01C.IMQ b. AVIRIS over Cima, Scene Five Image file = AVRCM05A.IMG Navigation calibration file = AVRCM05B.DAT Engineering calibration file = AVRCM05C.DAT Dark Current calibration file = AVRCM05D.DAT Offset calibration file = AVRCM05E.DAT Dropout calibration file = AVRCM05F.DAT Radiometric calibration file = AVRCM05G.IMG Raw spectral calibration file = AVRCM05H.DAT c. 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Boardman, Mineral mapping at Cuprite, Nevada with a 63 channel imaging spectrometer, Photogram. Eng. Rem. Sensing, in press. LaVoie, S., C. Avis, H. Mortensen, C. Stanley, and L. Wainio, VICAR - User's Guide, JPL Document D-4186, Jet Propulsion Laboratory, Pasadena, CA, 1987. Macenka, S. A., and M. P. Chrisp, AVIRIS Spectrometer Design and Performance, Int. Soc. Opt. Eng., 834, 1987. Martin, T. Z, M. D. Martin, R. L. Davis, R. Mehlman, M. Braun, and M. Johnson, Standards for the Preparation & Interchange of Data Sets, Version 1.1, October 3, 1988. 64 Martonchik, J. V., Sulphuric acid cloud interpretation of the infrared spectrum of Venus, Ph.D. Dissertation, Univ. Texas, Austin, 1974. McCollom, T., and B. M. Jakosky, Slope properties of some terrestrial surfaces and implications for planetary radar studies, submitted for publication. McFadden, L. D., S. G. Wells, and J. C. Dohrenwend, Influences of Quaternary climatic changes on processes of soil development on desert loess deposits of the Cima volcanic field, California, Catena, 13, 361-389, 1986. McFadden, L. D., S. G. Wells, and M. J. Jercinovich, Influences of eolian and pedogenic processes on the origin and evolution of desert pavements, Geology, 15, 504-508, 1987. McKeague and Day, Canadian Journal of Soil Science, 46, 13-22, 1966. Mehra and Jackson, 7th National Conference on Clays and Clay Minerals, 317-327, 1960. Palluconi, F. D., and G. R. Meeks, Thermal Infrared Multi-spectral Scanner (TIMS): An investigator's guide to TIMS data, 14 pp., JPL Pub. 85-32, Jet Propulsion Laboratory, Pasadena, CA, 1985. Parker, R. B., Recent Volcanism at Amboy Crater, San Bernardino County, California, Special Report 76, 22 pp., Calif. Div. Mines Geol., 1963. Quinlivan, W. D., C. L. Rogers, and H. W. Dodge, Geologic map of the Portuguese Mountain Quadrangle Nye County, Nevada, Misc. Geo. Inv. Map I-804, U.S. Geological Survey, 1974. Raynger II Plus Operating Manual, Revision D, Raytek Incorporated, Santa Cruz, CA, 1989. Roberts, D. A., Y. Yamaguchi, and R. J. P. Lyon, Calibration of Airborne Imaging Spectrometer data to percent reflectance using field spectral measurements, Proceedings, Nineteenth International Symposium on Remote Sensing of Environment, Ann Arbor, Michigan, October 21-25, 1985. Schaber, G. G., G. L. Berlin, and W. E. Brown, Jr., Variations in surface roughness within Death Valley, California: Geologic evaluation of 25-cm-wavelength radar images, Geol. Soc. Amer. Bull., 87, 29-41, 1976. Sharp, R. P., Wind ripples, J. Geol., 71, 617-66, 1963. Sharp, R. P., Kelso Dunes, Mojave Desert, California, Geol. Soc. of Amer. Bull., 77, 1045-1074, 1966. 65 Sharp, R. P., Geology Field Guide to Southern California, 208 pp., Kendall/Hunt Pub., Dubuque, IA, 1976. Sharp, R. P., The Kelso Dune Complex, in Aeolian Features of Southern California: A Comparative Planetary Geology Guidebook, edited by R. Greeley, M. Womer, R. Papson and P. Spudis, NASA Planetary Geology Program, 24-52, 1978. Shaw, G. E., J. A. Reagan, and B. M. Herman, Investigations of atmospheric extinction using direct solar radiation measurements made with a multiple wavelength radiometer, J. Appl. Meteorol., 12, 374-380, 1973. Stewart, S. E., R. R. Buntzen, and J. Carbone, Advanced CID array multispectral pushbroom scanner, Laser Focus/Electro-Optics, 21, 88- 100, 1985. Turrin, B. D., J. C. Dohrenwend, R. E. Drake, and G. H. Curtis, K-Ar ages from the Cima volcanic field, eastern Mojave Desert, California, Isochron/West, 44, 9-16, 1985. Van Zyl, J. J., H. A. Zebker, and C. Elachi, Imaging radar polarization signatures: Theory and observations, Radio Sci., 22, 529-543, 1987. Van Zyl, J. J., Calibration of polarimetric radar images using only image parameters and trihedral corner reflector responses, IEEE Transactions on Geoscience and Remote Sensing, 28, 337-348, 1990. Van Zyl, J. J., C. F. Burnette, H. A. Zebker, A. Freeman, and J. Holt, NASA/JPL DC-8 Aircraft SAR POLCAL User's Manual, 127 pp., JPL Publication D-7715, Jet Propulsion Laboratory, Pasadena, CA, 1990. Vane, G. (Ed.), Airborne visible/infrared imaging spectrometer (AVIRIS), 97 pp., JPL Publication 87-38, Jet Propulsion Laboratory, Pasadena, CA, 1987. Vane, G. (Ed.), Proceedings of the Third Airborne Imaging Spectrometer Data Analysis Workshop, June 2-4, JPL Publication 87-30, Jet Propulsion Laboratory, Pasadena, CA, 1987. Vincent, R. K., and F. J. Thompson, Spectral compositional imaging of silicate rocks, J. Geophys. Res., 77, 2465-2472, 1972. Vincent, R. K., and F. J. Thompson, Recognition of exposed quartz sand and sandstone by two-channel infrared imagery, J. Geophys. Res., 77, 2473-2477, 1972. Wall, S. D., T. G. Farr, J. P. Muller, P. Lewis and F. W. Leberl, Measurement of surface microtopography, Photogram. Eng. Rem. Sensing, in press. 66 Weidner, V. R., and J. J. Hsia, Reflection properties of pressed polytetrafluoroethylene powder, Jour. Opt. Soc. Am., 71, 856-859, 1981. Wells, S. G., J. C. Dohrenwend, L. D. McFadden, B. D. Turrin, and K. D. Mahrer, Late Cenozoic landscape evolution on lava flow surfaces of the Cima volcanic field, Mojave Desert, California, Geol. Soc. of Amer. Bull., 96, 1518-1529, 1985. Zebker, H. A., J. J. van Zyl, and D. N. Held, Imaging radar polarimetry from wave synthesis, J. Geophys. Res., 92, 683-701, 1987. Zebker, H. A. and Y. Lou, Phase calibration of imaging radar polarimeter Stokes matrices, IEEE Transactions on Geoscience and Remote Sensing, 28, 246-252, 1989. Zebker, H. H., J. J. van Zyl, D. N. Held, Imaging polarimetry from wave synthesis, J. Geophys. Res., 92, 683-701, 1987. 67 APPENDIX A - CD-ROM VOLUME, DIRECTORY AND FILE STRUCTURES A.1 VOLUME AND DIRECTORY STRUCTURES The volume and directory structures of this CD-ROM conform to the standard specified by the International Organization for Standardization (ISO) [Information processing -- Volume and file structure of CD-ROM for information interchange, 1987, ISO/DIS document number 9660, International Organization for Standardization, 1 Rue de Varembe, Case Postale 56, CH-1121 Geneva 20, Switzerland.]. This CD-ROM disk conforms to the first level of interchange, level-1. A.2 FILE STRUCTURE The files on this CD-ROM are of two types: fixed-length files and stream files. The characteristics of each type are described in the following sections. A.2.1 FIXED-LENGTH FILES The records in a fixed-length file are all the same length, and there is no embedded information to indicate the beginning or end of a record. Fixed-length records allow any part of a file to be accessed directly without the need to pass through the file sequentially. The starting byte of any record can be calculated as follows: offset = (record-1)*length where: offset = offset byte position of record from start of file record = number of desired record length = length of record in bytes On this CD-ROM, images and table files are fixed-length. Image file names have the extension ".IMG", and table file names have the extensions ".DAT" (for data tables) and ".TAB" (for index tables). Image files contain binary data with no carriage-control information in them. Table files, however, contain ASCII text that can be printed or displayed on a terminal. Each record in a table file has the ASCII characters for carriage return and line feed (hex 0D and 0A) in the last two bytes. A.2.2 STREAM FILES Stream files are used to store ASCII text such as documentation and source code. A stream file may have records of varying lengths. The end of a record is marked by two bytes containing the ASCII carriage return and line feed characters (hex 0D and 0A). Stream files are different from variable-length files, which store the record size in the first two bytes of each record. This CD-ROM contains no variable-length files. 68 On this CD-ROM, documentation files and detached label files are in stream format. They may be printed or displayed on a terminal. Their file names have the extensions ".TXT" and ".LBL". Also, the file VOLDESC.SFD in the top-level directory is a stream file. A.2.3 EXTENDED ATTRIBUTE RECORDS An extended attribute record (XAR) contains information about a file's record format, record attributes, and record length. The extended attribute record is not considered part of the file and is not seen by programs accessing a file with high-level I/O routines. Not all computer operating systems support extended attribute records. Those that do not will simply bypass the XAR when accessing a file. On this CD-ROM, fixed-length files have XARs, but stream files do not. 69 APPENDIX B - SYNTACTIC RULES OF KEYWORD ASSIGNMENT STATEMENTS A keyword assignment statement, made up of a string of ASCII characters, contains the name of an attribute and the value of that attribute. A keyword assignment statement has the general form shown below: name = value [/* comment */] The format of each keyword assignment statement is free-form; blanks and tabs are ignored by a parsing routine. An attribute name is separated from its value by the equal symbol (=). Each keyword assignment statement may be followed by a comment that more completely describes the entry. The comment begins with a slash character followed by an asterisk character (/*), and terminates with an asterisk character followed by a slash character (*/). Comments may also exist on a line without a keyword assignment statement. Note that the brackets indicate that the comment and its delimiters are optional. Values associated with an attribute can be integers, real numbers, unitized real numbers, literals, times, or text strings. B.1 INTEGER NUMBERS An integer value consists of a string of digits preceded optionally by a sign (+ or -). Non-decimal based integers are expressed according to the Ada language convention: b#nnnnnnn#, where 'b' represents the base of the number, and '#' delimits the number 'nnnnnnnn'. For example, the number expressed as 2#111# represents the binary number 111, which is 7 in base 10. B.2 REAL NUMBERS A real number has the form: [s]f.d[En] where: s = optional sign (+ or -) f = one or more digits that specify the integral portion of the number. d = one or more digits that specify the fraction portion of the number. n = an optional exponent expressed as a power of 10. A unitized real number is a real number with an associated unit of measurement. The units for a real number value are enclosed in angle brackets (< >). For example, 1.234 indicates a value of 1.234 seconds. 70 B.3 DATES AND TIMES A special form of a numeric field is a time value. The following format of date/time representations is used: yyyy-mm-ddThh:mm:ss.fffZ where: yyyy = year mm = month dd = day of month hh = hour mm = minute ss = seconds fff = fraction of a second Z = The Z qualifier indicates the time is expressed as Universal Time Coordinated (UTC). B.4 LITERAL VALUES A literal value is an alphanumeric string that is a member of a set of finite values. It can also contain underscore character (_). A literal value must be delimited by single quote (') characters if it does not begin with a letter (A-Z). If the literal begins with a letter, it does not have to be enclosed in single quotes. If a literal appears within single quotes, the literal may contain any printable ASCII character. For example, the literal value '1:1' is legal as long as the single quoted format is used. A keyword assignment statement using a literal value might look like the examples shown below: FILTER_NAME = CLEAR IMAGE_ID = '122S01' These statements say that the CLEAR filter was used to acquire an image and that the image_id was 122S01. B.5 TEXT CHARACTER STRINGS Text strings can be any length and can consist of any sequence of printable ASCII characters including tabs, blanks, carriage-control, or line-feed characters. Text strings are enclosed in double quote characters. If the text string comprises several lines, it continues until a double quote character is encountered and includes the carriage- control and line-feed characters. 71 APPENDIX C - KEYWORD DEFINITIONS The definitions of the keywords used in the detached PDS labels on this CD-ROM are given below. Where applicable the definitions are taken from the Planetary Science Data Dictionary Document (Cribbs and Wagner, 1990) or the PDS Standards for the Preparation and Interchange of Data Sets (SPIDS) document (Martin et al., 1988). BAND_STORAGE_TYPE The internal storage format of a multiple-band image. Valid values for GRSFE data are BAND_SEQUENTIAL and LINE_INTERLEAVED. An image with band sequential storage contains all the lines for band 1, followed by all the lines for band 2, followed by all the lines for band 3, etc. ASAS images are stored in this manner. An image in line interleaved format contains line 1 for all the bands, followed by line 2 for all the bands, followed by line 3 for all the bands, etc. TIMS and AVIRIS data are stored in line interleaved manner. BANDS The number of bands in a multiple-band image. BYTES The number of bytes containing a data item. COLUMNS The number of items of information in each row of a data table. DATA_SET_ID A unique alphanumeric identifier for a data set. It is used as a primary key in the PDS catalog. DATA_TYPE The data type of a data item. Valid values are INTEGER, REAL, DATE, TIME, and CHARACTER. DESCRIPTION Text describing an object. Sometimes this is expressed as a pointer to another file containing the descriptive text; e.g., ^DESCRIPTION = "VICAR2.TXT" indicates that the file VICAR2.TXT contains a description of the object. EMISSION_ANGLE The angle between the surface normal vector and the vector to the observer. ENCODING_TYPE The format or algorithm used to store data in an image. END_OBJECT This keyword is used by ODL to indicate the end of a data object definition. FEATURE_NAME 72 The name of a feature. For planets, it is the IAU approved name. For the Earth, it can be the common name of a geographic feature. FILE_RECORDS The number of physical records in a data file. FLIGHT_LINE The line along which an aircraft flew while acquiring data. Flight lines are defined by a starting latitude-longitude and ending latitude- longitude, in Section 3.B of the GRSFE document VOLINFO.TXT. FORMAT The Fortran 77 representation of the format statement needed to read a data item. IMAGE_HEADER The embedded label information at the beginning of an image file, expressed as a pointer to the record in the file where the header begins; e.g., ^IMAGE_HEADER = ("filename",1) indicates that a header begins in record 1 of file "filename". IMAGE The data in an image file, expressed as a pointer to the record where the data begins. For example, ^IMAGE = ("filename",3) indicates that image data begins in record 3 of file "filename". IMAGE_TIME The time of the image acquisition in PDS standard (UTC) format. INCIDENCE_ANGLE The angle of the incoming radar beam relative to the local surface normal. Note this definition is different from the PDS data dictionary definition, which is specific to optical images. INSTRUMENT_NAME The full name of an instrument. INSTRUMENT_POINTING_DIRECTION The direction that the airborne instrument was pointing with respect to the aircraft at the time of data acquisition. Possible values are FORWARD, BACKWARD, and NADIR. INTERCHANGE_FORMAT The type of data stored in a data table, such as ASCII or BINARY. ITEM_BYTES The number of bytes in a single item described by an OBJECT construct. ITEM_TYPE The data type of an item. Valid values are the same as for DATA_TYPE. 73 ITEMS The number of items described by an OBJECT construct. LATITUDE The value of the planetographic latitude of a point of interest. Latitude is defined in terms of the IAU convention that identifies the north pole as that pole of rotation that lies on the north side of the invariable plane of the solar system. Latitude values range from -90 degrees at the south pole to +90 degrees at the north pole. LINES The number of lines in an image. LINE_SAMPLES The number of samples contained in each image line. LONGITUDE The value of the planetographic longitude of a point of interest. Values are positive in the direction opposite to the rotation. For example, east longitudes are positive for Venus and west longitudes are positive for Mars and Mercury. NAME The name of a column in a table. OBJECT This keyword specifies the name of a data object. It is used by ODL to indicate the start of a data object definition. PRODUCT_ID A unique identifier for a data product. RECORDS The number of records in the object being described; for example, the number of records in a header object. RECORD_BYTES The number of bytes in each record of a data file. RECORD_TYPE The record structure type of a data file. Valid values are FIXED_LENGTH, VARIABLE_LENGTH, and STREAM. Images and data tables usually have fixed-length records, whereas text files have stream format records. ROWS The number of logical records in a data table. ROW_BYTES The number of bytes in each row (i.e., logical record) of a data table. RUN_NUMBER 74 A specific instance of a flight along a flight line. SAMPLE_BIT_MASK A bit mask indicating which bits in a sample are valid. A bit set to 1 indicates valid data; a bit set to 0 indicates invalid data. SAMPLE_BITS The number of bits of data comprising one sample or pixel in an image. Common values are 8, 16, and 32. SAMPLE_TYPE The data type of an image sample or pixel. The table below lists the values used on this CD-ROM: UNSIGNED_INTEGER An unsigned integer value. Samples with a length of 16 bits are in most-significant- byte first order. VAX_INTEGER A signed integer value in least-significant- byte first order. VAX_REAL A real (floating point) value in VAX format. START_BYTE The byte position of the beginning of a data item within a row of data. START_TIME Date and time at which data collection began for a particular data product. SITE_NAME The name designating an area where ground measurements were made in support of airborne data. SPECTRUM_HEADER The embedded label information at the beginning of a spectrum file, expressed as a pointer to the record in the file where the header begins; e.g., ^SPECTRUM_HEADER = ("filename",1) indicates that a header begins in record 1 of file "filename". SPECTRUM The data in a spectrum file, expressed as a pointer to the record where the data begins. For example, ^SPECTRUM = ("filename",3) indicates that the image data begins in record 3 of file "filename". STRUCTURE Text that describes the structure of a data file or header. Sometimes this is expressed as a pointer to another file containing the text; e.g., ^STRUCTURE = "DAEDALUS.TXT" indicates that the file DAEDALUS.TXT contains a description of the object in question. The description may be in ODL format, in which case the file pointed to has the extension ".FMT"; e.g. ^STRUCTURE = "PFES.FMT". TABLE_HEADER 75 The embedded label information at the beginning of a table, expressed as a pointer to the record in the file where the header begins; e.g., ^TABLE_HEADER = ("filename",1) indicates that a header begins in record 1 of file "filename". TABLE The data in a table file, expressed as a pointer to the record where the data begins. For example, ^TABLE = ("filename",3) indicates that the table data begins in record 3 of file "filename". TARGET_NAME The name of a planetary body, such as a planet or satellite. TYPE The type of header in a data file, such as a VICAR2 label embedded in the image file. UNIT The units of measure of a data item. 76 APPENDIX D - GRSFE AIRBORNE AND FIELD INSTRUMENTS TABLE D.1 GRSFE AIRBORNE REMOTE SENSING INSTRUMENTS Instrument Brief Description AIRSAR Flew on DC-8. C, L, P-band (68 cm) polarimetric SAR. Multiple incidence angle coverage is possible by acquiring data on multiple passes. 10 m pixels with 10 to 20 km swath width. ASAS Flew on C-130. 29 channel (0.47 to (Advanced Solid-state 0.87 micrometer) imaging system. Array Acquires multi-emission angle data of Spectroradiometer) surface 45 degrees from nadir along ground track. Footprint about 2 by 3 km and pixel width of about 4 m. AVIRIS Flew on ER-2. Covers 0.4 to (Airborne Visible and 2.45 micrometer wavelength region with Infrared Imaging 224 channels, 20 m pixels (20 km Spectrometer) altitude), with 11 km cross track swath width. TIMS Flew on C-130. Six broad bands in 8 to (Thermal Infrared 12 micrometer region. 2.5 mrad Multi-spectral instantaneous field of view; total field Spectrometer) of view of 76 degrees. TABLE D.2 ATMOSPHERIC INSTRUMENTS DEPLOYED DURING GRSFE FIELD CAMPAIGN (Specific sections of this document where detailed instrument and data set descriptions can be found are listed under the instrument column.) Instrument Location, Purpose Dates of Observations ---------- --------------------- ------- Reagan Radiometer, Lunar Lake Optical depth Section 6.E.1 July 17, 1989 Sept. 29, 1989 Spectral Hygrometer, Lunar Lake Column water abundance Section 6.E.2 July 17, 1989 Sept. 29, 1989 Weather Station, Lunar Lake Wind velocity & direction, 77 Section 6.E.4 July 15-18, 1989 air temperature Sept. 28-29, 1989 Arizona State Lunar Lake Wind velocity profiles at University Wind July 15-18, 1989 two locations on playa Velocity Experiment, Section 6.E.3 PARABOLA, Lunar Lake Visible, near-infrared, and Section 6.C.2 July 17-18, 1989 mid-infrared wavelength sky radiance at various scattering angles TABLE D.3 GROUND TRUTH INSTRUMENTS DEPLOYED DURING GRSFE FIELD CAMPAIGN (Specific sections of this document where detailed instrument and data set descriptions can be found are listed under the instrument column.) Instrument Locations, Purpose Dates of Observations ---------- --------------------- ------- Daedalus AA440 Kelso Dunes, Cima Spectral reflectance of Field Spectrometer, Volcanic Field, end-member surfaces at Section 6.C.1 Death Valley, calibration and modeling Ubehebe, Lunar Crater sites Volcanic Field modeling sites, July 15-19, 1989 SIRIS Field Same as Daedalus Same as Daedalus Spectrometer, Section 6.C.3 PFES, Kelso Dunes, Cima Spectral emittance of Section 6.D.1 Volcanic Field, Lunar end-member surfaces at Crater Volcanic Field calibration and modeling modeling sites, sites July 15-17, 1989 PARABOLA, Lunar Crater Volcanic Spectral reflectance Section 6.C.2 Field modeling sites, (visible, near-infrared July 17-18, 1989 and mid-infrared) of surface at various scattering angles Radiometers Lunar Lake, Brightness temperatures of Sections 3, 5 Sept. 26-29, 1989 various surfaces Thermistors Lunar Lake Kinetic temperatures of Section 3 July 17-18, 1989 subsurface 78 Sept. 26-27, 1989 TABLE D.4 AVIRIS FLIGHT LINES Flights correspond to NASA Ames Research Center ER-2 flights 89-19, 20, 22. Table is arranged by GRSFE site, flight number, and runs. Beginning and ending line locations are given as latitudes and longitudes. Brief descriptions of lines are provided. Times of start of runs are given in parentheses in PDT. Note that AVIRIS scenes cover 10 km by 10 km areas within the flight lines. Specific AVIRIS files associated with each line are given. See Section 13 for file naming convention. I. Lunar Crater Volcanic Field Sites Sept 29, 1989: Line 2: Run 1 (09:44) start: 38 deg 40.0', 115 deg 44.5' end: 38 deg 15.0', 116 deg 08.5' AVIRIS files: AVRLV02A.IMG, AVRLV06A.IMG, AVRLV07A.IMG. Run 2 (11:43) start: 38 deg 15.0', 116 deg 08.5' end: 38 deg 4 0.0', 115 deg 44.5' AVIRIS files: AVRLV01A.IMG, AVRLV27A.IMG, AVRLV31A.IMG, AVRLV32A.IMG, AVRLV33A.IMG, AVRLV34A.IMG. Run 3 (13:44) start: 38 deg 15.0', 115 deg 44.5' end: 38 deg 40.0', 116 deg 08.5' AVIRIS files: AVRLV14A.IMG. Oct 4, 1989 Line 1: Run 1 (12:30) start: 38 deg 40.0', 115 deg 53.7' end: 38 deg 05.0', 16 deg 15.5' AVIRIS files: AVRLV26A.IMG, AVRLV35A.IMG. Notes: Line 1 covers Lunar Crater Volcanic Field and Lunar Lake. Line 2 mosaics with line 1 and covers Lunar Lake and alluvial fans and varied rock types on the western side of Railroad Valley. II. Ubehebe Maar Sept 29, 1989: Line 5: Run 1 (13:02) start: 36 deg 55.0', 117 deg 27.0' 79 end: 37 deg 15.0', 117 deg 27.0' AVIRIS files: No data this release. Notes: Covers Ubehebe Crater (37 deg 05', 117 deg 27') with north- south line. 10% clouds were observed on entire line. III. Death Valley Fans/Dunes Sept 29, 1989: Line 1: Run 1 (12:17) start: 36 deg 45.0', 117 deg 03.5' end: 36 deg 00.0', 116 deg 51.0' AVIRIS files: AVRTC15A.IMG, AVRTC16A.IMG Line 2: Run 1 (12:30) start: 36 deg 15.0', 116 deg 42.5' end: 36 deg 45.0', 117 deg 15.0' AVIRIS files: AVRDG04A.IMG, AVRDG18A.IMG, AVRTC19A.IMG, AVRTC20A.IMG, AVRDG36A.IMG, AVRDG37A.IMG. Notes: Line 1 covers all the alluvial fans on the west side of Death Valley. Line 2 covers "Mars Hill" at Artist's Drive and Death Valley Dunes. 10% clouds were observed on last 12 nautical miles for line 2. IV. Cima Volcanic Field: Sept 28, 1989: Line 1: Run 1 (12:37) start: 35 deg 09.0', 115 deg 54.0' end: 35 deg 16.0', 115 deg 30.0' AVIRIS files: AVRCM13A.IMG Line 2: Run 1 (12:25) start: 35 deg 30.0', 115 deg 44.0' end: 35 deg 05.0', 115 deg 44.0' AVIRIS files: AVRCM05A.IMG Notes: Line 1 trends E-NE whereas line 2 trends N-S. V. Providence Fans: Sept 28, 1989: Line 1: Run 1 (13:06) start: 35 deg 00.0', 115 deg 14.5' end: 34 deg 47.5', 116 deg 00.0' 80 AVIRIS files: AVRPV23A.IMG, AVRPV29A.IMG. VI. Kelso Dunes Sept 28, 1989: Line 1: Run 1 (13:24) start: 34 deg 55.0', 115 deg 37.0' end: 35 deg 05.5', 116 deg 25.0' AVIRIS files: No data in this release. TABLE D.5 ASAS AND TIMS FLIGHT LINES Flights correspond to NASA Ames Research Center C-130 flight numbers 89- 08-01, 02, 03, 04, 05, and 06. Table is arranged by GRSFE site, flight number, and runs. Beginning and ending line locations are given as latitudes, longitudes. Brief descriptions of lines are provided. Times of start of runs are given in parentheses in PDT. Specific files associated with each line are given. See Section 13 for file naming conventions. The asterisk (*) present in some file names is a wildcard character, indicating multiple files with similar names; e.g. ASALV01*.IMG refers to files ASALV01A.IMG, ASALV01B.IMG, ASALV01C.IMG, etc. I. Lunar Crater Volcanic Field July 17, 1989: Line 1: Run 1 (04:03) start: 38 deg 04', 116 deg 15.8' end: 38 deg 39.8', 115 deg 53.3' TIMS files: TIMLV03A.IMG Run 2 (07:27) start: 38 deg 03', 116 deg 16.3' end: 38 deg 40', 115 deg 53.2' TIMS files: TIMLV09A.IMG ASAS files: No data in this release. Run 3 (14:11) start: 38 deg 40.5', 115 deg 53.2' end: 38 deg 05.3', 115 deg 14.6' TIMS files: TIMLL06A.IMG ASAS files: ASALV01*.IMG Line 2: Run 1 (04:17) 81 start: 38 deg 40.9', 115 deg 43.4' end: 38 deg 15.1', 116 deg 09.5' TIMS files: TIMLV04A.IMG Run 2 (08:05) start: 38 deg 41.3', 115 deg 43.3' end: 38 deg 14.9', 116 deg 09.1' TIMS files: TIMLL03A.IMG ASAS files: ASALL05*.IMG Run 3 (12:16) start: 38 deg 42.2', 115 deg 44.3' end: 38 deg 39.9', 115 deg 45' TIMS files: No data in this release. ASAS files: ASALL03*.IMG Run 4 (13:55) start: 38 deg 13', 116 deg 10.7' end: 38 deg 39.7', 115 deg 45.2' TIMS files: TIMLL05A.IMG ASAS files: ASALL01*.IMG Line 15: Run 1 (07:50) start: 38 deg 23.3', 116 deg 07.3' end: 38 deg 24.2', 115 deg 54' TIMS files: TIMLL02A.IMG ASAS files: ASALL04*.IMG Run 2 (08:18) start: 38 deg 23', 116 deg 08.4' end: 38 deg 24.1', 115 deg 52.7' TIMS files: No data in this release. ASAS files: No data in this release. Line 16: Run 1 (12:30) start: 38 deg 30.5', 116 deg 02.4' end: 38 deg 18.4', 115 deg 58.7' TIMS files: TIMLV06A.IMG ASAS files: ASALL02*.IMG Notes: Lines 15 and 16 are approximately perpendicular to lines 1 and 2, and cross Railroad Valley, Lunar Lake and Lunar Crater Volcanic Field. Sept 27, 1989: Line 1: Run 1 (05:33) 82 start: 38 deg 04.3', 116 deg 16.40.6' end: 38 deg 05', 115 deg 52.4' TIMS files: TIMLV07A.IMG Notes: Scattered clouds observed at Citadel Mtn. Line 2: Run 1 (05:14) start: 38 deg 40.1', 115 deg 44.3' end: 38 deg 14.2', 116 deg 09.1' TIMS files: TIMLL07A.IMG Notes: Scattered clouds observed over most of line. Run 2 (05:50) start: 38 deg 40.4', 115 deg 45' end: 38 deg 10.2', 116 deg 12.1' TIMS files: TIMLL08A.IMG Notes: 90% clouds at beginning of line, 2 mi later clear. Sept 27, 1989 Line 2: Run 1 (10:02) start: 38 deg 15.5', 116 deg 08.3' end: 38 deg 40.1', 115 deg 44.4' TIMS files: TIMLL09A.IMG Notes: Shadows on Lunar Lake, rest of line heavily clouded. Sept 29, 1989: Line 1: Run 1 (12:58) start: 38 deg 41.7', 115 deg 52.7' end: 38 deg 20.8', 116 deg 05.8' TIMS files: No data in this release. Notes: Required to leave track just N of Citadel Mtn, ~38°20'. Line 2: Run 1 (13:17) start: 38 deg 13.7', 116 deg 09.7' end: 38 deg 39.8', 115 deg 43.1' TIMS files: TIMLV02A.IMG Notes: A few shadows at beginning of line, but overall good. 83 Line 2a: Run 1 (13:33) start: 38 deg 37.1', 115 deg 48.9' end: 38 deg 04.5', 116 deg 16.5' TIMS files: TIMLV08A.IMG Notes: Line extended to pick up southern part of Line 1 not imaged. II. Ubehebe Maar July 17, 1989: Line 5: Run 1 (03:11) start: 37 deg 16.2', 117 deg 26.7' end: 36 deg 54.5', 117 deg 26.9' TIMS files: TIMUB01A.IMG Run 2 (13:23) start: 37 deg 15.9', 117 deg 27.6' end: 36 deg 54.9', 117 deg 27.4' TIMS files: TIMUB02A.IMG ASAS files: ASAUB01*.IMG III. Death Valley Fans/Dunes Sept 27, 1989: Line 1: Run 1 (04:06) start: 36 deg 46', 117 deg 03.8' end: 35 deg 59.1', 116 deg 51' TIMS files: No data in this release. Notes: 80-100% cloud cover observed. Line 2: Run 1 (04:25) start: 36 deg 14.4', 116 deg 41.9' end: 36 deg 45.5', 117 deg 15.6' TIMS files: No data in this release. Notes: 100% cloud cover. Sept 29, 1989: Line 1: Run 1 (14:47) 84 start: 36 deg 00.7', 116 deg 50.6' end: 36 deg 45.9', 117 deg 02.1' TIMS files: TIMTC02A.IMG Notes: Last 6 mi of line 75% obscured by clouds. Line 2: Run 1 (15:08) start: 36 deg 45', 117 deg 16.3' end: 36 deg 14.6', 116 deg 42' TIMS files: TIMDG02A.IMG Line 16: Run 1 (14:25) start: 36 deg 53.4', 116 deg 43.4' end: 36 deg 33.7', 117 deg 10.7' TIMS files: TIMDD03A.IMG Notes: A few clouds over site. IV. Cima Volcanic Field: Sept 29, 1989: Line 1: Run 1 (16:17): start: 35 deg 09.5', 115 deg 53.4' end: 35 deg 14.9', 115 deg 35.5' TIMS files: TIMCM01A.IMG Notes: Channel 2 coming in & out. Line 2: Run 1 (16:44) start: 35 deg 05.3', 115 deg 44' end: 35 deg 30.7', 115 deg 44' TIMS files: No data in this release. Notes: Channel 2 coming in & out. V. Providence Fans: Sept 29, 1989: Line 1*: Run 1 (16:26) start: 35 deg 21.4', 115 deg 21.9' end: 34 deg 44.9', 115 deg 42.5' 85 TIMS files: TIMPV01A.IMG Notes: Channel 2 coming in & out. Line 1* is parallel to the strike of the Providence Mountains. VI. Kelso Dunes Sept 29, 1989: Line 1: Run 1 (15:56) ABORTED Run 2 (15:59) start: 35 deg 04.3', 116 deg 25' end: 34 deg 53.7', 115 deg 33.6' TIMS files: TIMKL02A.IMG TABLE D.6 AIRSAR FLIGHT LINES Table is arranged by GRSFE site, flight number, and runs. JPL tape numbers and AIRSAR run numbers are also given. Beginning and ending line locations are given as latitudes and longitudes. Brief descriptions of lines are provided. Times of start of runs are given in PDT. Specific GRSFE AIRSAR files associated with each line are given. See Section 13 for file naming conventions. The asterisk (*) present in some file names is a wildcard character, indicating multiple files with similar names; e.g. AIRLV01*.IMG refers to files AIRLV01C.IMG, AIRLV01L.IMG, and AIRLV01P.IMG. September 13, 1989 I. Lunar Crater Volcanic Field Line 1: start 38 deg 40', 115 deg 53.7'; end 38 deg 05', 116 deg 15.5' AIRSAR Run #206-1, tape HDDT 89-167. Data acquired at 25 degree incidence angle. GRSFE AIRSAR scene: AIRLL01*.IMQ Time: 22:42:12 (PDT) AIRSAR Run #206-2, tape HDDT 89-167. Data acquired at 35 degree incidence angle. GRSFE AIRSAR scene: AIRLL02*.IMQ Time: 22:58:48 (PDT) AIRSAR Run #206-3, tape HDDT 89-168. Data acquired at 45 degree incidence angle. GRSFE AIRSAR scene: AIRLL03*.IMQ Time: 23:15:46 (PDT) 86 Line 2: start 38 deg 40', 115 deg 46.5'; end 38 deg 05', 116 deg 08' AIRSAR Run #206-7, tape HDDT 89-169. Data acquired at 25 degree incidence angle. GRSFE AIRSAR scene: No data in this release. AIRSAR Run #206-8, tape HDDT 89-169. Data acquired at 35 degree incidence angle. GRSFE AIRSAR scene: No data in this release. AIRSAR Run #206-9, tape HDDT 89-170. Data acquired at 45 degree incidence angle. GRSFE AIRSAR scene: No data in this release. Line 3: start 38 deg 30', 116 deg 13.3'; end 38 deg 10.2', 115 deg 35' AIRSAR Run #123-1, tape HDDT 89-170. Data acquired at 25 degree incidence angle. GRSFE AIRSAR scene: No data in this release. AIRSAR Run #123-2, tape HDDT 89-171. Data acquired at 35 degree incidence angle. GRSFE AIRSAR scene: No data in this release. AIRSAR Run #123-3, tape HDDT 89-171. Data acquired at 45 degree incidence angle. GRSFE AIRSAR scene: No data in this release. Line 4: start 38 deg 38.8', 115 deg 51.5'; end 38 deg 05', 116 deg 11.9' AIRSAR Run #206-4, tape HDDT 89-168. Data acquired at 25 degree incidence angle. GRSFE AIRSAR scene: No data in this release. AIRSAR Run #206-5, tape HDDT 89-168. Data acquired at 35 degree incidence angle. GRSFE AIRSAR scene: AIRLL05*.IMQ Time: 23:49:15 (PDT) AIRSAR Run #206-6, tape HDDT 89-169. Data acquired at 45 degree incidence angle. GRSFE AIRSAR scene: AIRLL06*.IMQ Time: 00:05:38 (PDT) Notes: Line 1 covers parts of the Lunar Crater Volcanic Field and Lunar Lake. Line 2 mosaics with Line 1 and Line 4 and covers alluvial fans and varied rock types on the western side of Railroad Valley. Line 3 is approximately perpendicular to lines 1, 2, and 4, and crosses Railroad Valley, Lunar Lake and Lunar Crater Volcanic Field. Line 4 covers Lunar Lake, crossing Line 3 near the southern end of the playa. II. Ubehebe Maar 87 Line 1: start 37 deg 15', 117 deg 27'; end 36 deg 55', 117 deg 27' AIRSAR Run #180-1, tape HDDT 89-171. Data acquired at 25 degree incidence angle. GRSFE AIRSAR scene: AIRUB01*.IMQ Time: 3:05:00 (PDT) AIRSAR Run #180-2, tape HDDT 89-172. Data acquired at 35 degree incidence angle. GRSFE AIRSAR scene: AIRUB02*.IMQ Time: 2:36:33 (PDT) AIRSAR Run #180-3, tape HDDT 89-173. Data acquired at 45 degree incidence angle. GRSFE AIRSAR scene: No data in this release. Time: 3:03:45 (PDT) III. Death Valley Fans/Dunes: September 14, 1989 Line 1: start 36 deg 45', 117 deg 03.5'; end 36 deg 00', 116 deg 51' AIRSAR Run #167-1, tape HDDT 89-174. Data acquired at 25 degree incidence angle. GRSFE AIRSAR scene: No data in this release. AIRSAR Run #167-3, tape HDDT 89-175. Data acquired at 45 degree incidence angle. GRSFE AIRSAR scene: No data in this release. Line 2: start 36 deg 45', 117 deg 15'; end 36 deg 15', 116 deg 42.5' AIRSAR Run #139-1, tape HDDT 89-175. Data acquired at 25 degree incidence angle. GRSFE AIRSAR scenes: AIRMH01*.IMQ, AIRMH02*.IMQ Times: 11:57:16, 12:14:35 (PDT) AIRSAR Run #139-3, tape HDDT 89-176. Data acquired at 45 degree incidence angle. GRSFE AIRSAR scene: AIRDD01*.IMQ Time: 11:54:11 (PDT) Line 3: start 35 deg 55', 116 deg 33'; end 35 deg 35', 116 deg 33' AIRSAR Run #154-1, tape HDDT 89-176. Data acquired at 45 degree incidence angle. GRSFE AIRSAR scene: No data in this release. AIRSAR Run #154-3, tape HDDT 89-176. Data acquired at 25 degree incidence angle. GRSFE AIRSAR scene: No data in this release. 88 Notes: Line 1 covers alluvial fans on the west side of Death Valley. Line 2 covers "Mars Hill" and Death Valley Dunes. Line 3 covers Confidence Mill playa (35 deg 49', 116 deg 33'). IV. Providence Fans: September 13, 1989 Line 1: start 35 deg 00', 115 deg 14.5'; end 34 deg 47.5', 116 deg 00' AIRSAR Run #251-1, tape HDDT 89-173. Data acquired at 45 degree incidence angle. GRSFE AIRSAR scene: No data in this release. V. Afton Canyon-Kelso Dunes: September 13, 1989 Line 1: start 35 deg 05', 116 deg 25'; end 34 deg 55', 115 deg 37' AIRSAR Run #104-1, tape HDDT 89-172. Data acquired at 45 degree incidence angle. GRSFE AIRSAR scene: No data in this release. TABLE D.7 AVIRIS CROSS-REFERENCE TABLE This table cross-references GRSFE AVIRIS image IDs (identified by time in GMT, line and run) to their original JPL IDs (given by flight, run and segment). The JPL tape ID for each image is also listed. Dates are all in 1989. Note that some Lunar Crater Volcanic Field scenes include Lunar Lake. GRSFE JPL ID Site GRSFE Product Date Time LN/RN FL/RN/SG Tape -------- ------------- -------------- ----- ----------------- Cima AVRCM05A.IMG 09-28 19:28:08 02,01 19/03/04 AS0710 Volcanic AVRCM13A.IMG 09-28 19:37:43 01,01 19/04/01 AS0780 Field Devil's AVRTC04A.IMG 09-29 19:32:07 02,01 20/08/03 AS0714 Golf AVRTC18A.IMG 09-29 19:32:49 02,01 20/08/04 AS0786 Course AVRDG36A.IMG* 09-29 19:30:41 02,01 20/08/01 AS0983 AVRDG37A.IMG 09-29 19:21:34 02,01 20/08/02 AS0984 Kelso AVRKL38A.IMG 09-28 20:25:44 01,01 19/07/02 AS0767 Dunes Lunar AVRLV01A.IMG 09-29 18:45:36 02,02 20/06/03 AS0709 Crater AVRLV02A.IMG 09-29 16:46:14 02,01 20/02/03 AS0766 Volcanic AVRLV06A.IMG 09-29 16:47:39 02,01 20/02/05 AS0769 Field AVRLV07A.IMG 09-29 16:44:48 02,01 20/02/01 AS0742 AVRLV14A.IMG 09-29 20:46:11 02,03 20/10/03 AS0782 AVRLV26A.IMG 10-04 19:39:53 01,01 22/05/02 AS0842 AVRLV27A.IMG 09-29 18:44:10 02,02 20/06/01 AS0845 AVRLV31A.IMG 09-29 18:46:18 02,02 20/06/04 AS0848 AVRLV32A.IMG 09-29 18:47:01 02,02 20/06/05 AS0849 AVRLV33A.IMG 09-29 18:47:44 02,02 20/06/06 AS0850 89 AVRLV34A.IMG 09-29 18:44:53 02,02 20/06/02 AS0846 AVRLV35A.IMG 10-04 19:40:35 01,01 22/05/03 AS0841 Provi- AVRPV23A.IMG 09-28 19:53:15 1*,01 19/05/06 AS0810 dence AVRPV29A.IMG 09-28 19:53:58 1*,01 19/05/07 AS0811 Fans Canyon AVRTC15A.IMG 09-29 19:20:42 01,01 20/07/05 AS0783 Fans AVRTC16A.IMG 09-29 19:21:24 01,01 20/07/06 AS0784 AVRTC19A.IMG 09-29 19:33:32 02,01 20/08/05 AS0787 AVRTC20A.IMG 09-29 19:34:57 02,01 20/08/06 AS0788 * The navigation data file for this image is not included on this release. TABLE D.8 AIRSAR CROSS-REFERENCE TABLE This table cross-references GRSFE AIRSAR image IDs (identified by time in GMT, line and run) to their original JPL IDs (given by run). The JPL far and near tape numbers (CM numbers) for each image are also listed. Dates are all in 1989. Note that some Lunar Crater Volcanic Field scenes include Lunar Lake. GRSFE JPL CM# Site GRSFE Product Date Time LN/RN JPL Run Near Far ---- ------------- -------------- ----- ------- --------- Death Valley AIRDD01C.IMQ 09-14 18:54:11 02,02 139-3 1192 1193 Dunes Lunar Crater AIRLL01C.IMQ 09-13 05:42:12 01,01 206-1 1204 1205 Volcanic AIRLL02C.IMQ 09-13 05:58:48 01,02 206-2 1226 1227 Field AIRLL03C.IMQ 09-13 06:15:46 01,03 206-3 1208 1209 AIRLL05C.IMQ 09-13 06:49:15 04,02 206-5 1162 1163 AIRLL06C.IMQ 09-13 07:05:38 04,03 206-6 1089 1090 Mars Hill AIRMH01C.IMQ 09-14 18:57:16 02,01 139-1 1137 1138 AIRMH02C.IMQ 09-14 19:14:35 02,01 139-1 1403 1404 Ubehebe Maar AIRUB01C.IMQ 09-13 09:36:33 01,01 180-1 1222 1223 AIRUB02C.IMQ 09-13 09:50:06 01,02 180-2 1120 TABLE D.9 ASAS CROSS-REFERENCE TABLE This table cross-references GRSFE ASAS image IDs (identified by time in GMT, line and run) to their original GSFC IDs (given by line and run). Dates are all in 1989. GRSFE Site GRSFE Product Date Time LN/RN GSFC Line/Run 90 ---- ------------- -------------- ----- ------------- Lunar Crater ASALV01D.DAT 07-17 21:15:24 01,03 1/ 3 Volcanic Field Lunar Lake ASALL01D.DAT 07-17 20:58:20 02,04 2/ 4 ASALL02D.DAT 07-17 19:22:23 02,03 2/ 3 ASALL03D.DAT 07-17 19:32:34 16,01 16/ 1 ASALL04D.DAT 07-17 14:51:33 15,01 15/ 1 ASALL05D.DAT 07-17 15:11:11 02,02 2/ 2 Ubehebe ASAUB01D.DAT 07-17 20:26:46 05,02 5/ 2 TABLE D.10 TIMS CROSS-REFERENCE TABLE This table cross-references GRSFE TIMS image IDs (identified by time in GMT, line and run) to their original JPL IDs (given by flight, line and run). Dates are all in 1989. GRSFE JPL JPL Site GRSFE Product Date Time LN/RN Flight LN/RN ---- ------------- ------------- ----- -------- ----- Cima TIMCM01A.IMG 09-29 23:17:10 01,01 89-08-06 10, 1 Volcanic Field Death Valley TIMDD03A.IMG 09-29 21:25:33 16,01 89-08-06 16, 1 Dunes Devil's Golf TIMDG02A.IMG 09-29 22:08:20 02,01 89-08-06 7, 1 Course Kelso Dunes TIMKL02A.IMG 09-29 22:59:28 01,02 89-08-06 13, 2 Lunar Crater TIMLV02A.IMG 09-29 20:17:10 02,01 89-08-06 2, 1 Volcanic Field TIMLV03A.IMG 07-17 11:02:53 01,01 89-08-01 1, 1 TIMLV04A.IMG 07-17 11:17:11 02,01 89-08-01 2, 1 TIMLV06A.IMG 07-17 19:30:30 16,01 89-08-03 16, 1 TIMLV07A.IMG 09-27 12:33:43 01,01 89-08-04 1, 1 TIMLV08A.IMG 09-29 20:33:55 2A,01 89-08-06 15, 1 TIMLV09A.IMG 07-17 14:27:43 01,02 89-08-02 1, 2 Lunar Lake TIMLL02A.IMG 07-17 14:50:08 15,01 89-08-02 15, 1 TIMLL03A.IMG 07-17 15:05:03 02,02 89-08-02 2, 2 TIMLL05A.IMG 07-17 20:55:45 02,04 89-08-03 2, 4 TIMLL06A.IMG 07-17 21:11:44 01,03 89-08-03 1, 3 TIMLL07A.IMG 09-27 12:14:57 02,01 89-08-04 2, 1 TIMLL08A.IMG 09-27 12:50:18 02,02 89-08-04 2, 2 TIMLL09A.IMG 09-27 17:02:38 02,01 89-08-05 2, 3 Providence Fans TIMPV01A.IMG 09-29 23:26:41 1*,01 89-08-06 12, 1 Trail Canyon TIMTC02A.IMG 09-29 21:47:35 01,01 89-08-06 6, 1 91 Fan Ubehebe Maar TIMUB01A.IMG 07-17 10:11:27 05,01 89-08-01 5, 1 TIMUB02A.IMG 07-17 20:22:43 05,02 89-08-03 5, 2 TABLE D.11 GRSFE TEAM PARTICIPANTS CALIBRATION SITE TEAM John Dietz Collins Tom Farr Site Descriptions, Samples, Photography Bill Farrand PIDAS Lisa Gaddis Site Descriptions, Samples, Photography Glen Green Vegetation Rob Green PIDAS (16, 17 July) Ed Guinness Daedalus Gordon Hoover PFES Phil Hughes Soil moisture samples Fred Kruse SIRIS Shelley Petroy PFES, Daedalus Jeff Plaut Site Descriptions, Samples, Photography (25-29 Sept) Cathy Weitz PFES Gregg Vane PIDAS (17, 18, 19 July) Kathy Young Collins CORNER REFLECTOR TEAM Placement: 17 - 21 July Jakob van Zyl Fred Burnette John Holt Pascale Dubois Jeff Plaut Check: 26 - 28 July Steve Wall Fred Burnette Check/Pickup: 10 - 14 September Tom Farr Jeff Plaut Fred Burnette Jakob van Zyl MODELING SITE TEAM Ray Arvidson Jim Conel Diane Evans Ron Greeley Glen Green 92 Dave Harding Jim Irons Nick Lancaster Joel Norris John Perry Bob Rousseau Susan Ustin Rich Zurek Plus various members of the Calibration and Corner Reflector teams UNIVERSITY OF COLORADO RADIOMETRY EXPERIMENT TEAM Bruce Jakosky Gary Finiol Bradley Henderson Jose Aguirre 93 APPENDIX E - WASHINGTON UNIVERSITY EXPERIMENT -- THERMAL MEASUREMENTS AT LUNAR CRATER VOLCANIC FIELD TABLE E.1 LUNAR LAKE LINE ARRAY THERMISTOR DATA Thermistor Array Subsurface Site Data. July 17-18, 1989. Times in PDT. Temperatures in degrees Celsius. Station 1 is southernmost station; i.e., furthest from cobble site. Playa sites: stations 1-4 Cobble sites: stations 5-8 TIME 1 2 3 4 avg stdev 5 6 7 8 avg stdev 18:00 30.7 28.8 30.4 31.1 30.3 1.0 33.2 36.0 34.1 35.9 34.8 1.4 19:00 28.8 28.4 28.7 29.2 28.8 0.3 31.7 33.7 32.0 33.4 32.7 1.0 20:00 25.9 26.8 25.9 26.4 26.3 0.4 28.8 30.2 29.6 31.0 29.9 0.9 20:56 23.0 24.6 22.9 23.2 23.4 0.8 25.4 26.5 26.4 27.0 26.3 0.7 21:57 21.2 22.9 21.2 21.8 21.8 0.8 23.8 24.2 24.9 25.0 24.5 0.6 22:57 20.5 22.0 20.9 20.9 21.1 0.6 22.8 23.2 23.9 23.8 23.4 0.5 23:57 18.9 20.8 19.0 19.0 19.4 0.9 20.9 21.2 22.1 22.0 21.6 0.6 01:00 17.3 19.2 17.2 17.3 17.8 1.0 19.0 19.3 20.2 19.9 19.6 0.5 02:00 16.0 18.2 16.0 16.1 16.6 1.1 18.6 18.0 19.1 18.3 18.5 0.5 03:00 15.0 17.2 14.9 15.0 15.5 1.1 16.1 16.6 18.1 17.0 17.0 0.9 04:00 14.2 15.6 14.1 14.0 14.5 0.8 15.2 15.5 17.0 16.2 16.0 0.8 05:00 12.9 15.1 13.0 13.0 13.5 1.1 14.1 14.2 15.5 14.9 14.7 0.7 06:00 12.4 14.9 12.8 12.7 13.2 1.1 13.8 13.9 15.2 14.3 14.3 0.6 07:00 14.2 15.2 14.3 13.9 14.4 0.6 15.3 16.0 16.7 15.2 15.8 0.7 08:00 17.0 16.6 17.2 17.1 17.0 0.3 18.5 20.0 19.1 18.8 19.1 0.6 09:00 21.0 19.2 21.3 21.0 20.6 1.0 23.2 24.9 22.9 23.8 23.7 0.9 10:00 25.0 22.1 25.2 25.9 24.6 1.7 28.2 30.0 27.0 29.5 28.7 1.3 11:00 28.5 24.9 29.0 29.8 28.1 2.2 32.8 35.0 30.8 34.9 33.4 2.0 12:00 30.9 27.8 31.8 32.2 30.7 2.0 35.9 39.3 34.0 38.5 36.9 2.4 13:00 32.9 29.2 33.5 34.2 32.5 2.2 38.1 41.5 36.2 40.8 39.2 2.5 14:00 34.8 31.0 35.1 36.0 34.2 2.2 40.1 44.0 38.2 42.9 41.3 2.6 15:00 35.1 32.0 35.9 36.9 35.0 2.1 41.0 44.2 39.2 43.8 42.1 2.4 16:00 35.0 32.2 35.1 36.4 34.7 1.8 40.2 44.1 39.2 43.1 41.7 2.3 17:00 34.9 31.5 35.2 36.1 34.4 2.0 40.2 43.5 38.4 43.2 41.3 2.5 18:00 33.4 31.2 33.1 34.2 33.0 1.3 38.2 41.3 38.0 41.4 39.7 1.9 TABLE E.2 LUNAR LAKE DEPTH ARRAY THERMISTOR DATA Thermistor Depth Arrays -- Cobble and Playa Areas July 17-18, 1989. Times in PDT. Temperatures in degrees Celsius Just south of Playa south of cobble modeling site cobble modeling site 94 ---- DEPTH ---- ---- DEPTH ---- TIME 30 cm 10 cm 3 cm 30 cm 10 cm 3 cm 18:00 26.0 28.2 36.9 22.2 20.3 28.2 19:00 26.2 28.8 34.9 21.0 22.1 27.5 20:00 26.6 29.0 32.1 21.8 23.3 26.5 20:56 26.0 28.7 28.5 20.9 22.2 23.8 21:57 26.2 28.8 26.2 21.1 22.8 22.0 22:57 26.1 28.8 25.0 21.1 22.1 21.0 23:57 26.2 28.4 23.8 21.2 23.4 19.9 01:00 26.4 28.1 22.0 21.1 22.1 18.7 02:00 26.3 28.0 20.7 21.2 22.0 17.8 03:00 26.5 27.9 19.0 21.2 21.9 16.8 04:00 26.5 27.2 18.4 21.1 21.5 16.0 05:00 26.1 27.1 17.0 21.0 21.1 15.0 06:00 26.2 26.8 16.3 20.9 20.8 14.4 07:00 26.3 26.4 16.7 20.8 20.7 14.6 08:00 26.0 25.7 19.5 20.5 20.0 15.8 09:00 26.0 25.4 23.9 20.3 19.8 17.9 10:00 25.9 24.9 28.8 20.2 19.8 21.0 11:00 25.9 25.2 33.8 20.1 19.4 24.1 12:00 25.9 25.1 37.9 20.0 20.0 26.9 13:00 25.9 25.8 40.1 20.0 20.0 29.1 14:00 25.9 25.9 42.0 20.0 20.1 30.9 15:00 25.8 26.2 43.1 20.0 21.0 30.9 16:00 25.1 26.8 43.1 20.0 21.1 31.9 17:00 25.1 26.9 42.8 20.2 21.3 31.8 18:00 25.9 27.8 41.3 21.0 22.7 31.3 TABLE E.3 TEMPERATURE AND RELATIVE HUMIDITY AT THERMAL TEST SITE July 17-18, 1989. Times in PDT. Temperatures in degrees Celsius. TIME TEMP % RH NOTES 18:22 29.0 32.0 18:55 28.0 33.0 19:54 25.0 33.0 21:10 20.0 35.0 21:52 21.0 35.0 23:50 18.0 35.5 missed measurements between 21:52 and 23:50 01:15 14.0 38.0 moved thermometer/hygrometer to south end of array 02:00 14.0 40.0 03:00 13.0 42.0 04:00 11.0 45.0 05:00 9.5 44.0 06:00 10.0 44.0 sunrise at 5:55 a.m. 07:00 21.0 41.0 08:00 23.0 40.0 95 08:56 28.0 39.0 09:55 32.0 36.0 10:58 33.0 34.0 wind shifted; now blowing from the south 11:57 30.5 34.5 12:58 30.0 34.0 14:00 33.0 33.0 14:55 33.0 33.2 16:00 31.0 32.5 17:00 36.5 31.5 18:00 32.0 31.0 TABLE E.4 LUNAR LAKE THERMISTOR DATA FOR MANTLED FLOW SITE PITS September 26-27, 1989. Times in PDT. Temperatures in degrees Celsius PIT A SITE PIT B SITE ----- DEPTH ----- ----- DEPTH ----- TIME 30 cm 20 cm 10 cm 3 cm 30 cm 20 cm 10 cm 3 cm 18:00 20.9 21.4 24.6 26.0 19.2 20.5 22.8 25.0 19:00 21.8 22.0 24.6 24.3 19.8 21.0 22.9 23.7 20:00 21.1 22.1 23.9 23.2 19.8 21.0 22.6 22.0 21:00 21.1 22.0 23.1 22.2 19.5 21.0 21.9 20.9 22:00 21.3 22.0 22.9 21.1 19.8 21.0 21.4 19.8 23:00 21.2 22.1 22.1 20.3 19.8 20.8 20.7 18.9 00:00 21.3 22.0 21.3 20.0 19.9 20.7 20.3 18.9 01:00 21.2 21.8 21.0 19.4 19.3 20.3 20.0 18.3 02:00 21.2 21.6 20.5 18.2 19.9 20.0 19.2 17.0 03:00 21.3 21.5 20.2 17.8 19.0 19.9 19.1 16.4 04:00 21.5 21.5 19.9 17.2 19.8 19.9 18.9 16.0 05:00 21.3 21.2 19.5 16.6 19.8 19.8 18.2 15.0 06:00 21.5 21.2 19.1 16.4 19.8 19.2 18.0 14.9 07:00 21.3 21.0 18.8 16.2 19.7 19.1 17.7 15.0 08:00 21.2 20.9 18.4 16.6 19.8 18.9 18.2 15.2 09:00 21.2 20.8 18.3 17.7 19.7 18.7 17.3 17.0 10:00 21.1 20.6 18.4 19.1 19.7 18.7 17.5 18.8 11:00 21.2 20.5 18.9 21.0 19.3 18.2 17.8 20.2 12:00 20.9 20.0 19.2 21.3 19.2 18.5 18.2 21.1 13:00 20.8 20.0 20.0 22.5 19.2 18.9 19.3 22.5 14:00 20.8 19.9 20.6 23.2 18.9 18.6 19.7 23.0 15:00 20.5 20.0 20.6 23.6 19.2 19.0 20.1 23.4 16:00 21.0 20.3 21.6 24.5 19.0 19.0 20.2 24.1 17:00 20.9 20.8 22.2 24.4 19.2 19.3 20.9 23.8 18:00 20.9 20.9 22.2 23.4 19.5 19.8 21.0 22.8 TABLE E.5 RADIOMETER DATA COLLECTED AT MANTLE FLOW SITE PITS 96 September 26-27, 1989. Times in PDT. Surface temperatures in degrees Celsius * indicates surface disturbed during emplacement of thermistors # indicates undisturbed surface adjacent to thermistor sites; i.e., tens of centimeters away. PIT A SITE PIT B SITE TIME 1* 2* 3# 4# 1* 2* 3# 4# 18:00 20.0 20.0 20.0 20.0 20.0 20.0 17.0 18.0 19:00 17.0 18.0 18.0 17.0 17.0 17.0 17.0 17.0 20:00 16.0 18.0 17.0 17.0 17.0 17.0 16.0 16.0 21:00 17.0 15.0 15.0 15.0 14.0 13.0 13.0 13.0 22:00 13.0 15.0 12.0 15.0 13.0 13.0 12.0 12.0 23:00 17.0 17.0 17.0 17.0 16.0 17.0 18.0 16.0 00:00 15.0 15.0 15.0 14.0 13.0 13.0 15.0 14.0 01:00 13.0 14.0 13.0 13.0 13.0 13.0 12.0 12.0 02:00 11.0 10.0 11.0 10.0 10.0 10.0 11.0 10.0 03:00 11.0 10.0 10.0 10.0 9.0 10.0 9.0 8.0 04:00 12.0 11.0 11.0 11.0 11.0 11.0 11.0 11.0 05:00 9.0 10.0 11.0 11.0 10.0 10.0 10.0 8.0 06:00 10.0 10.0 9.0 9.0 8.0 10.0 8.0 8.0 07:00 12.0 12.0 12.0 12.0 12.0 11.0 11.0 11.0 08:00 14.0 14.0 16.0 16.0 14.0 15.0 13.0 14.0 09:00 17.0 17.0 19.0 18.0 18.0 18.0 18.0 17.0 10:00 26.0 26.0 27.0 27.0 26.0 26.0 27.0 27.0 11:00 24.0 23.0 24.0 23.0 22.0 22.0 23.0 23.0 12:00 26.0 26.0 27.0 27.0 25.0 26.0 25.0 26.0 13:00 28.0 27.0 28.0 29.0 27.0 27.0 27.0 27.0 14:00 27.0 27.0 27.0 27.0 26.0 25.0 25.0 26.0 15:00 27.0 26.0 27.0 27.0 25.0 25.0 24.0 25.0 16:00 27.0 26.0 26.0 27.0 24.0 25.0 23.0 24.0 17:00 21.0 22.0 22.0 22.0 19.0 19.0 20.0 19.0 18:00 19.0 20.0 19.0 18.0 18.0 18.0 16.0 17.0 TABLE E.6 RADIOMETER DATA COLLECTED DURING TIMS OVERFLIGHTS Surface Temperatures During TIMS Overflight -- Cobble site adjacent to Lunar base camp September 29, 1989. Times in PDT. Temperatures in degrees Fahrenheit, as measured, with Celsius equivalents in parentheses. SITES TIME 1 2 3 4 10:00 89.0 (31.7) 95.0 (35.0) 86.0 (30.0) 92.0 (33.3) 11:00 97.0 (36.1) 100.0 (37.8) 90.0 (32.2) 95.0 (35.0) 12:00 94.0 (34.4) 95.0 (35.0) 91.0 (32.8) 97.0 (36.1) 13:00 100.0 (37.8) 91.0 (32.8) 89.0 (31.7) 94.0 (34.4) 97 Surface Temperatures During TIMS Overflight -- Mantled flow site September 29, 1989 Temperatures in degrees Fahrenheit, as measured, with Celsius equivalents in parentheses. PIT A SITE PIT B SITE TIME 1 2 3 4 1 2 3 4 13:00 91 94 96 92 93 90 97 92 (33) (34) (36) (33) (34) (32) (36) (33) Surface Temperatures During TIMS Overflight -- Playa site adjacent to Lunar base camp September 29, 1989 Temperatures in degrees Fahrenheit, as measured, with Celsius equivalents in parentheses. * indicates emissivity set for 0.95 on thermal radiometer Emissivity set to 1.0 unless otherwise noted PLAYA SITES TIME 1 2 3 4 10:00 75.0 (23.9) 75.0 (23.9) 74.0 (23.3) 74.0 (23.3) 10:00 75.0 (23.9)* 77.0 (25.0)* 76.0 (24.4)* 78.0 (25.6)* 11:00 79.0 (26.1) 80.0 (26.7) 80.0 (26.7) 82.0 (27.8) 11:00 83.0 (28.3)* 82.0 (27.8)* 81.0 (27.2)* 81.0 (27.2)* 12:00 84.0 (28.9) 84.0 (28.9) 85.0 (29.4) 86.0 (30.0) 12:00 85.0 (29.4)* 84.0 (28.9)* 85.0 (29.4)* 84.0 (28.9)* 13:00 85.0 (29.4) 85.0 (29.4) 84.0 (28.9) 85.0 (29.4) 13:00 85.0 (29.4)* 84.0 (28.9)* 85.0 (29.4)* 84.0 (28.9)* 98 APPENDIX F - SAMPLES COLLECTED DURING GRSFE TABLE F.1 SUMMARY OF SAMPLES COLLECTED DURING GRSFE CAMPAIGN LUNAR LAKE MODELING SITES Collected during July campaign Playa sub-site 19 end member bag sub-site 3 sealed can sub-site 5 sealed can sub-site 7 sealed can sub-site 12 sealed can sub-site 17 sealed can sub-site 19 sealed can Disturbed playa sub-site 10 disturbed end member bag sub-site 10 undisturbed end member bag sub-site 3 sealed can sub-site 10 sealed can sub-site 18 sealed can sub-site 19 sealed can sub-site 22 sealed can sub-site 25 sealed can Mantled flow sub-site 20 end member bag sub-site 10 end member bag sub-site 8 sealed can sub-site 9 sealed can sub-site 10 sealed can sub-site 18 sealed can sub-site 19 sealed can sub-site 20 sealed can Cobble sub-site 5 cobble and pebbles end member bag sub-site 5 playa end member bag sub-site 5 sealed can sub-site 8 sealed can sub-site 9 sealed can sub-site 14 sealed can sub-site 16 sealed can sub-site 23 sealed can CALIBRATION SITES SITE DATE DESCRIPTION 99 Death Valley Dune Field 18 Jul 89 Loose sand from dune surface Devil's Golf Course 18 Jul 89 crust of salt pan on valley bottom- Bright Target Trail Canyon 18 Jul 89 pebble pavement on Trail Canyon fan- Dark Target Ubehebe Maar-1 19 Jul 89 pebble-sized black tephra on north flank of Ubehebe Crater- Dark Target Ubehebe Maar-2 19 Jul 89 scraping of coarse sand north of road to Ubehebe Crater and east of crater- meant to be Bright Target, but no field spectra obtained Cima Volcanic Field-1 15 Jul 89 top layer of tephra from east flank of cone I - Dark Target at Cima Cima Volcanic Field-2 15 Jul 89 rock from same location as Cima Volcanic Field-1 Cima Volcanic Field-3 15 Jul 89 Stream bed sample next to I cone - Bright Target Kelso Dune Field-1 15 Jul 89 upper few mm of granule surface at Kelso Bright Target (parking lot at dunes) Kelso Dune Field-2 15 Jul 89 surface of road just south of Kelso Dune Field-1 sample location TABLE F.2 SOIL ANALYSES PARTICLE SIZE ANALYSIS WITH PRETREATMENTS TO REMOVE ORGANIC MATTER AND DISPERSED 10% CALGON SOLUTION. VALUES ARE WEIGHT PERCENTS IN GIVEN SIZE CLASS. Hori- SAND SILT CLAY TEXTURAL zon 2.0- 0.05- <0.002mm CLASS SITE 0.05mm 0.002mm <2.0mm ----------------------------------------------------------------- Playa A 2.5 33.9 63.6 C Cobble A 18.8 45.8 35.4 SiCL Mantled Flow A 40.6 31.4 28.0 CL Mantled Flow B 33.1 39.1 27.8 CL 100 MORE DETAILED SIZE ANALYSIS FOR COARSE FRACTION. VALUES ARE WEIGHT PERCENTS. VERY VERY COARSE COARSE MEDIUM FINE FINE COARSE MEDIUM FINE SAND SAND SAND SAND SAND SILT SILT SILT 2.0- 1.0- 0.50- 0.25- 0.10- 0.05- 0.02- 0.005- SAMPLE 1.0mm 0.50mm 0.25mm 0.10mm 0.05mm 0.02mm 0.005mm 0.002mm ----------------------------------------------------------------------- Playa 0.0 0.0 0.1 2.3 0.1 0.2 9.6 24.1 Cobble 0.3 0.5 0.4 5.3 12.3 7.5 13.9 24.4 Mantled 0.2 0.8 1.7 36.6 1.3 9.5 12.8 9.1 Flow Mantled 0.5 0.7 1.4 13.5 17.0 9.1 19.2 10.8 Flow CHEMICAL RESULTS Pre-treated SAMPLE -- pH in 1:1-- CEC pH 7.0 Cith-Dith Ext. Oxalate Ext. H2O KCl CaCl2 (NH4OAc 1N) Fe Al Fe Al Si ----------------------------------------------------------------------- Playa 8.0 7.7 7.9 45.8 <0.0 0.1 0.1 0.3 0.2 Cobble 8.9 7.4 8.2 41.3 <0.0 0.1 0.1 0.2 0.2 Mantled 7.9 7.6 7.8 31.2 <0.0 0.1 0.2 0.2 0.2 Flow Mantled 8.3 7.8 8.1 39.6 <0.0 0.1 0.1 0.1 0.2 Flow SAMPLE CaCO3 Organic Carbon (CHN analyzer) ------------------------------------------------ Playa 4.7 0.2 Cobble 4.1 0.2 Mantled Flow 9.6 0.4 Mantled Flow 12.4 0.3 101 APPENDIX G - EPPLEY PYRANOMETER DATA ACQUIRED TO SUPPORT PARABOLA DATA ANALYSES IRRADIANCE MEASUREMENTS ARE IN WATTS PER METER SQUARED DATE TIME SKY GROUND-REFLECTED (PDT) IRRADIANCE IRRADIANCE JULY 17, 1989 8:50:01 586.4 100.1 8:55:01 600.7 103.7 9:00:01 615.8 107.1 9:05:01 629.2 110.4 9:10:01 643.0 114.0 9:15:01 656.3 117.0 9:20:01 671.2 119.7 9:25:01 685.2 122.9 9:30:01 697.8 125.7 9:35:01 712.1 128.8 9:40:01 722.4 131.6 9:45:01 735.7 134.2 9:50:01 749.0 136.2 9:55:01 760.7 138.7 10:00:01 772.1 141.3 10:05:01 783.5 143.6 10:10:01 793.6 146.8 10:15:01 806.2 149.0 10:20:01 820.3 152.3 10:25:01 829.1 154.1 10:30:01 838.8 156.4 10:35:01 849.4 160.0 10:40:01 856.8 161.0 10:45:01 866.9 163.1 10:50:01 868.4 165.3 10:55:01 884.5 165.8 11:00:01 893.2 168.4 11:05:01 897.3 169.8 11:10:01 903.5 171.7 11:15:01 905.5 172.3 11:20:01 914.4 174.6 11:25:01 917.3 176.6 11:30:01 921.8 177.9 11:35:01 934.5 179.2 11:40:01 939.1 180.2 11:45:01 948.5 181.9 11:50:01 947.3 182.7 11:55:01 959.9 184.0 12:00:01 954.1 184.3 12:05:01 962.4 185.2 12:10:01 966.3 186.7 12:15:01 975.6 187.9 12:20:01 971.9 188.4 12:25:01 971.7 189.2 12:30:01 970.2 189.4 12:35:01 976.1 189.0 102 12:40:01 980.9 189.4 12:45:01 964.3 185.5 12:50:01 978.0 189.7 12:55:01 978.9 189.9 13:00:01 977.3 190.4 13:05:01 983.8 189.7 13:10:01 978.6 189.0 13:15:01 973.6 188.4 13:20:01 978.6 187.9 13:25:01 983.9 187.7 13:30:01 974.6 185.9 13:35:01 964.3 184.9 13:40:01 960.0 185.0 13:45:01 956.5 184.5 13:50:01 958.9 183.0 13:55:01 951.0 181.7 14:00:01 942.2 181.0 14:05:01 941.3 180.3 14:10:01 932.8 178.8 14:15:01 926.6 176.6 14:20:01 925.0 176.1 14:25:01 913.5 174.2 14:30:01 908.5 173.3 14:35:01 897.1 171.5 14:40:01 889.8 169.8 14:45:01 883.5 168.7 14:50:01 874.1 166.7 14:55:01 866.3 164.9 15:10:01 844.1 517.9 15:15:01 836.4 513.2 15:20:01 821.5 508.8 15:25:01 821.8 502.1 15:30:01 811.1 496.7 15:35:01 801.7 492.7 15:40:01 794.8 487.1 15:45:01 783.6 478.9 15:50:01 769.9 471.9 15:55:01 758.7 465.9 16:00:01 746.0 460.8 16:05:01 736.7 452.6 16:10:01 725.4 445.4 16:15:01 713.4 438.5 16:20:01 699.8 431.5 16:25:01 684.6 422.6 16:30:01 669.1 413.9 16:35:01 655.4 405.9 16:40:01 635.2 398.1 16:45:01 618.0 388.8 16:50:01 608.8 380.5 16:55:01 595.9 370.2 17:00:01 582.9 359.2 17:05:01 559.1 350.2 17:10:01 549.2 342.1 103 17:15:01 540.3 333.7 17:20:01 523.7 325.4 17:25:01 509.4 314.3 17:30:01 495.5 305.3 17:35:01 478.6 296.9 17:40:01 460.2 287.0 17:45:01 444.0 277.6 17:50:01 428.1 266.5 17:55:01 413.8 255.6 18:00:01 395.7 245.9 18:05:01 374.0 235.5 18:10:01 360.7 225.0 18:15:01 344.5 215.6 18:20:01 328.0 205.3 18:25:01 310.8 196.4 18:30:01 293.0 187.9 18:35:01 275.1 179.8 18:40:01 258.6 171.8 18:45:01 241.2 163.9 18:50:01 224.0 157.9 JULY 18, 1989 8:10:01 454.4 76.9 8:15:01 471.7 80.2 8:20:01 487.4 83.6 8:25:01 503.7 87.2 8:30:01 518.4 91.0 8:35:01 534.3 94.5 8:40:01 547.5 98.1 8:45:01 567.5 100.9 8:50:01 581.9 104.3 8:55:01 598.3 107.3 9:00:01 614.2 110.0 9:05:01 631.2 113.5 9:10:01 644.6 116.6 9:15:01 657.7 120.0 9:20:01 671.7 123.0 9:25:01 686.9 126.5 9:30:01 701.2 129.4 9:35:01 714.0 132.4 9:40:01 726.6 135.6 9:45:01 739.3 139.2 9:50:01 753.0 141.8 9:55:01 765.7 145.2 10:00:01 776.6 147.8 10:05:01 789.8 150.7 10:10:01 802.3 152.7 10:15:01 812.0 155.1 10:20:01 824.3 158.9 10:25:01 834.0 159.4 10:30:01 836.8 162.9 10:35:01 854.4 164.0 10:40:01 865.2 166.3 10:45:01 872.6 168.0 104 10:50:01 881.6 170.6 10:55:01 888.4 172.5 11:00:01 897.7 173.3 11:05:01 905.8 175.6 11:10:01 916.2 177.9 11:15:01 917.5 179.7 11:20:01 927.9 180.0 11:25:01 937.5 182.3 11:30:01 944.1 183.6 11:35:01 949.1 185.8 11:40:01 949.0 186.1 11:45:01 953.4 187.8 11:50:01 961.1 188.6 11:55:01 956.4 189.4 12:00:01 969.5 191.4 12:05:01 966.7 192.3 12:10:01 975.2 193.1 12:15:01 978.1 194.6 12:20:01 988.1 194.2 INSTRUMENTATION MOVED TO NEW SITE 13:25:01 980.2 108.3 13:30:01 980.7 108.4 13:35:01 973.8 109.6 13:40:01 981.2 108.2 13:45:01 964.2 107.7 13:50:01 971.3 107.3 13:55:01 968.9 107.5 14:00:01 964.5 107.6 14:05:01 961.6 108.0 14:10:01 954.4 106.2 14:15:01 948.2 105.1 14:20:01 942.7 104.6 14:25:01 936.5 103.9 14:30:01 928.3 103.1 14:35:01 919.6 102.2 14:40:01 909.7 101.1 14:45:01 896.3 98.7 14:50:01 886.0 98.1 14:55:01 883.1 98.3 15:00:01 873.6 96.5 15:05:01 862.3 95.5 15:10:01 854.5 94.5 15:15:01 843.9 93.8 15:20:01 833.2 91.8 15:25:01 819.4 89.9 15:30:01 803.3 88.6 15:35:01 793.3 87.4 15:40:01 780.9 86.7 15:45:01 767.2 84.9 15:50:01 754.5 83.3 15:55:01 743.9 82.1 105 16:00:01 735.9 81.5 16:05:01 720.9 79.1 16:10:01 713.1 79.4 16:15:01 700.6 77.6 16:20:01 684.6 74.1 16:25:01 671.2 73.6 16:30:01 654.3 71.4 16:35:01 637.4 69.2 16:40:01 621.9 69.5 16:45:01 607.8 66.6 16:50:01 590.6 65.3 16:55:01 573.2 62.6 17:00:01 556.7 60.8 17:05:01 538.2 58.8 17:10:01 522.6 58.6 17:15:01 505.1 55.8 17:20:01 487.7 53.9 17:25:01 472.8 53.1 17:30:01 453.7 50.5 17:35:01 436.8 48.4 17:40:01 417.2 46.0 17:45:01 398.9 43.7 17:50:01 381.6 43.2 17:55:01 362.8 41.9 18:00:01 345.8 40.1 18:05:01 327.7 37.6 18:10:01 309.8 35.8 18:15:01 292.4 34.2 18:20:01 274.4 32.0 18:25:01 256.7 30.9 18:30:01 239.4 28.6 18:35:01 221.7 26.4 18:40:01 204.3 24.9 JULY 19, 1989 8:00:01 416.4 262.3 8:05:01 432.6 270.8 8:10:01 457.1 282.1 8:15:01 479.7 294.3 8:20:01 201.4 112.9 8:25:01 621.8 377.0 8:30:01 215.0 119.7 8:35:01 584.6 354.7 8:40:01 552.4 336.0 8:45:01 553.4 332.3 8:50:01 568.6 339.1 8:55:01 571.0 346.2 9:00:01 601.2 358.5 9:05:01 637.2 374.3 9:10:01 640.9 376.2 9:15:01 643.3 377.4 9:20:01 666.3 389.4 9:25:01 674.2 392.5 9:30:01 678.1 395.2 106 9:35:01 693.9 401.7 9:40:01 707.6 408.2 9:45:01 727.3 415.9 9:50:01 740.9 422.3 9:55:01 752.5 428.3 10:00:01 760.9 432.8 10:05:01 774.5 436.0 10:10:01 781.3 440.6 10:15:01 795.5 447.0 10:20:01 803.1 451.3 10:25:01 816.4 458.7 10:30:01 833.4 467.1 10:35:01 856.5 480.0 10:40:01 906.4 508.1 10:45:01 920.4 513.7 10:50:01 1002.3 561.3 10:55:01 1058.3 593.0 11:00:01 338.2 183.6 11:05:01 538.6 293.8 11:10:01 408.7 223.5 11:15:01 1111.4 618.0 11:20:01 329.8 182.0 11:25:01 312.8 174.3 11:30:01 1119.2 626.5 11:35:01 348.2 194.3 11:40:01 469.6 259.9 11:45:01 1060.1 591.4 11:50:01 1065.8 591.0 107 APPENDIX H GRSFE CD-ROM ARCHIVE VOLUME AND DIRECTORY STRUCTURE Directory names are shown in upper case; file names in lower case. An asterisk (*) in a file name indicates multiple files with similar names; e.g. airlv01*.imq indicates files airlv01c.imq, airlv01l.imq, and airlv01p.imq. VOLUME 1 aareadme.txt ASAS asall04*.img, asall04*.lbl, (* = a,b,c,d,e,f,g) asall05*.img, asall05*.lbl, asaub01*.img, asaub01*.lbl DAEDALUS daedwave.dat, daedwave.lbl dae*.dat, dae*.lbl DIREMISS rmtll001.txt, thmll001.txt DOCUMENT daedalus.txt, parabola.txt, volinfo.txt GPSMICRO gpsmh001.dat, gpsmh001.lbl HELPRFL elell*.dat, elell*.lbl HYGROMTR hygll001.dat, hygll001.lbl INDEX airindex.tab, airindex.lbl, asaindex.tab, asaindex.lbl, avrindex.tab, avrindex.lbl, daeindex.tab, daeindex.lbl, eleindex.tab, eleindex.lbl, pfsindex.tab, pfsindex.lbl, prbindex.tab, prbindex.lbl, sirindex.tab, sirindex.lbl, timindex.tab, timindex.lbl LABEL asas.fmt LOCATOR 108 airloc.img, airloc.lbl, asaloc.img, asaloc.lbl, avrloc.img, avrloc.lbl PARABOLA prbll*a.dat, prbll*a.lbl, prbll*f.dat, prbll*f.lbl PFES pfs*.dat, pfs*.lbl, REAG_RAD regll001.dat, regll001.lbl, regll002.dat, regll002.lbl SIRIS sir*.dat, sir*.lbl, SOFTWARE newheader.inc oldheader.inc synthesz.for voldesc.sfd WINDEXP wndll001.dat, wndll001.lbl, wndll002.dat, wndll002.lbl WHTRSTA wthll001.dat, wthll001.lbl, wthll002.dat, wthll002.lbl VOLUME 2 aareadme.txt AIRSAR airdd01*.img, airdd01*.lbl AVIRIS avrlv01*.img, avrlv01*.lbl, (* = a,b,c,d,e,f,g,h) avrlv02*.img, avrlv02*.lbl, avrlv14*.img, avrlv14*.lbl, avrlv34*.img, avrlv34*.lbl DOCUMENT airsar.txt vicar2.txt SAMPLER airsm*.img, airsm*.lbl, 109 asasm*.img, asasm*.lbl, timsm*.img, timsm*.lbl voldesc.sfd VOLUME 3 aareadme.txt AIRSAR airsw01*.img, airsw01*.lbl, (* = c,l,p) airsw02*.img, airsw02*.lbl AVIRIS avrlv07*.img, avrlv07*.lbl, (* = a,b,c,d,e,f,g,h) avrlv27*.img, avrlv27*.lbl, avrlv31*.img, avrlv31*.lbl, avrlv35*.img, avrlv35*.lbl DOCUMENT airsar.txt vicar2.txt voldesc.sfd VOLUME 4 aareadme.txt AIRSAR airub01*.img, airub01*.lbl, (* = c,l,p) airub02*.img, airub02*.lbl, AVIRIS avrlv06*.img, avrlv06*.lbl, (* = a,b,c,d,e,f,g,h) avrlv26*.img, avrlv26*.lbl, avrlv32*.img, avrlv32*.lbl, avrlv33*.img, avrlv33*.lbl DOCUMENT airsar.txt vicar2.txt voldesc.sfd VOLUME 5 aareadme.txt AIRSAR 110 airll01*.img, airll01*.lbl, (* = c,l,p) airll02*.img, airll02*.lbl, airll03*.img, airll03*.lbl, airll05*.img, airll05*.lbl, airll06*.img, airll06*.lbl AVIRIS avrkl38*.img, avrkl38*.lbl, (* = a,b,c,d,e,f,g,h) avrpv23*.img, avrpv23*.lbl, avrpv29*.img, avrpv29*.lbl DOCUMENT airsar.txt vicar2.txt TIMS timtc02a.img, timtc02a.lbl voldesc.sfd VOLUME 6 aareadme.txt AVIRIS avrdg04*.img, avrdg04*.lbl, (* = a,b,c,d,e,f,g,h) avrdg18*.img, avrdg18*.lbl, avrdg36*.img, avrdg36*.lbl, avrdg37*.img, avrdg36*.lbl DOCUMENT airsar.txt vicar2.txt TIMS timdg02a.img, timdg02a.lbl, timdd03a.img, timdd03a.lbl, timub01a.img, timub01a.lbl, timub02a.img, timub02a.lbl voldesc.sfd VOLUME 7 aareadme.txt AVIRIS avrtc15*.img, avrtc15*.lbl, (* = a,b,c,d,e,f,g,h) avrtc16*.img, avrtc16*.lbl, avrtc19*.img, avrtc19*.lbl, avrtc20*.img, avrtc20*.lbl 111 DOCUMENT vicar2.txt TIMS timlv02a.img, timlv02a.lbl, timlv03a.img, timlv03a.lbl, timlv04a.img, timlv04a.lbl, voldesc.sfd VOLUME 8 aareadme.txt AVIRIS avrcm05*.img, avrcm05*.lbl, (* = a,b,c,d,e,f,g,h) avrcm13*.img, avrcm13*.lbl, DOCUMENT vicar2.txt TIMS timcm01a.img, timcm01a.lbl, timkl02a.img, timkl02a.lbl, timlv06a.img, timlv06a.lbl, timlv07a.img, timlv07a.lbl, timlv08a.img, timlv08a.lbl, timlv09a.img, timlv09a.lbl, timll02a.img, timll02a.lbl, timll03a.img, timll03a.lbl, timll05a.img, timll05a.lbl, timll06a.img, timll06a.lbl, timll07a.img, timll07a.lbl, timll08a.img, timll08a.lbl, timll09a.img, timll09a.lbl, timpv01a.img, timpv01a.lbl voldesc.sfd VOLUME 9 aareadme.txt ASAS asalv01*.img, asalv01*.lbl, (* = a,b,c,d,e,f,g) asall01a.img, asall01a.lbl, asall02*.img, asall02*.lbl, asall03*.img, asall03*.lbl LABEL asas.fmt 112 voldesc.sfd