Fig. 1. Nighttime bolometric thermal inertia map of Mars. Thermal inertia is mapped at a resolution of per pixel from TES orbits 1583–11254. Interpolation is used to fill missing data between TES ground tracks for latitudes 80° S to 80° N. See text for discussion.

Fig. 2. Coverage of data in Fig. 1 prior to filling by interpolation. Approximately 60% of the map contains TES-derived thermal inertia values between 80° S and 80° N latitudes. See text for discussion.

Fig. 3. Cross-plot of thermal inertia values derived from MGS-TES with those from Viking IRTM (Vasavada et al., 2000) for 60° S to 80° S. Both datasets are mapped at per pixel and binned at . Diagonal line is 1:1.

Fig. 4. Two-dimensional histogram showing global correlation between TES nighttime bolometric thermal inertia and visible bolometric albedo, from unfilled maps. Thermal inertia bin size is . Albedo bin size is 0.01. White areas represent no occurrences. Filled contour levels are 1, n/20, n/10, n/5, n/3, and n/2, where n=16691.6 is the maximum in a single bin wherein each occurrence is weighted by the cosine of its latitude to account for the represented surface area. Three modes of frequent correlation are assigned as Units A, B, and C, with outliers assigned to Units D, E, F, and G. Unit letters correspond to those in Fig. 5 and Table 1.

Fig. 5. Thermal inertia–albedo unit map of Mars. Units represent thermal inertia–albedo modes in Fig. 4. White areas correspond to regions between unit bounds in Fig. 4 and to no-data regions beyond 80° latitude. See Table 1 for interpretation and text for discussion. Lander locations and regions discussed in the text: VL-1, Viking Lander 1; VL-2, Viking Lander 2; MPF, Mars Pathfinder Lander; Ac, Acidalia; AF, Amenthes Fossae; Am, Amazonis; AP, Alba Patera; Ar, Argyre; AT, Arabia Terra; CP, Chryse Planitia; CM, Cydonia Mensae; EM, Elysium Mons; EP, Elysium Planitia; H, Hellas; I, Isidis; MP, Malea Planum; P, Promethei Terra; OM, Olympus Mons; OP, Olympia Planitia; S, Syrtis Major; T, Tharsis; U, Utopia Planitia; VB, Vastitas Borealis; VM, Valles Marineris; X, Xanthe Terra.

Fig. 6. Thermal inertia–albedo unit map in an orthographic projection of the southern hemisphere of Mars filled to 80° S. Unit letters correspond to those in Fig. 4 and Table 1. The northernmost latitude shown is 0° (the equator).

Fig. 7. Thermal inertia map of the southern hemisphere of Mars in the same projection as Fig. 6, filled to 80° S. Compare polar low thermal inertia region (blue) to Unit D in Fig. 6. The northernmost latitude shown is 0° (the equator).

Fig. 8. Variation of Lambert-equivalent albedo with incidence angle relative to (a) an empirically-derived photometric function based on Viking IRTM data (Kieffer et al., 1977), (b) a Minnaert surface with an exponent of 0.9 (Pleskot and Miner, 1981), (c) a Minnaert surface with an exponent of 0.75 (Pleskot and Miner, 1981), and (d) an isotropic Hapke surface with single-scattering albedo of 0.5 (Hapke and Wells, 1981). Symbols represent the ratios of the median albedo of Unit D to those of Unit A, Unit B, and Unit C. See text for discussion.

Fig. 9. Unprojected MOC images over (a) Unit B (MOC Image M19/00982, near 321° W, 62° S) and (b) Unit D (MOC Image M08/06534, near 326° W, 69° S). Mantled surfaces appear in both images and ‘cracked’ surface appears in (b). Both images are about 2.8 km wide.

Fig. 10. Two-dimensional histogram showing global correlation between TES nighttime bolometric thermal inertia and MOLA elevation, created using unfilled maps. Thermal inertia bin size is . Elevation bin size is 400 m. White areas represent no occurrences. Filled contour levels are 1, n/20, n/10, n/5, n/3, and n/2, where n=15336.5 is the maximum in a single bin wherein each occurrence is weighted by the cosine of its latitude to account for the represented surface area. Four modes of frequent correlation are assigned as Units 1, 2, 3, and 4, with outliers assigned to Units 5, 6, and 7. Unit numbers correspond to those in Fig. 11 and Table 2.

Fig. 11. Thermal inertia–elevation unit map of Mars. Units represent thermal inertia–elevation modes in Fig. 10. White areas correspond to regions between unit bounds in Fig. 10 and to no-data areas beyond 80° latitude. See Table 2 for correspondence to thermal inertia–albedo units and text for discussion. Lander locations and regions discussed in the text: VL-1, Viking Lander 1; VL-2, Viking Lander 2; MPF, Mars Pathfinder Lander; Ac, Acidalia; AF, Amenthes Fossae; Am, Amazonis; AP, Alba Patera; Ar, Argyre; AT, Arabia Terra; CP, Chryse Planitia; CM, Cydonia Mensae; EM, Elysium Mons; EP, Elysium Planitia; H, Hellas; I, Isidis; MP, Malea Planum; P, Promethei Terra; OM, Olympus Mons; OP, Olympia Planitia; S, Syrtis Major; T, Tharsis; U, Utopia Planitia; VB, Vastitas Borealis; VM, Valles Marineris; X, Xanthe Terra.

Fig. 12. Overlay of unfilled TES-based thermal inertia map (5°×5°) on a Viking MDIM 2.0 mosaic (left) and panorama from the lander showing a representative 100° of azimuth (right) for each landing site. (a) VL-1 relocated from small red to large black × per Zeitler and Oberst (1999). Lander mosaic 12F180-BB4. (b) VL-2 Lander mosaic 22A252-BB4. (c) Portion of MPF Lander “Presidential Panorama” mosaic PIA01466.

Mars thermal inertia–albedo units

Mars thermal inertia–elevation units

Past lander site data, mapped units, and rock abundances