R. E. Arvidson,1*R. C. Anderson,2P. Bartlett,3J. F. Bell, III,4P. R. Christensen,5P. Chu,3K. Davis,3B. L. Ehlmann,1M. P. Golombek,2S. Gorevan,3E. A. Guinness,1A. F. C. Haldemann,2K. E. Herkenhoff,6G. Landis,7R. Li,8R. Lindemann,2D. W. Ming,9T. Myrick,3T. Parker,2L. Richter,10F. P. Seelos, IV,1L. A. Soderblom,6S. W. Squyres,4R. J. Sullivan,4J. Wilson3
1 Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA.
2 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
3 Honeybee Robotics, 204 Elizabeth Street, New York, NY 10012, USA.
4 Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA.
5 Department of Geological Sciences, Arizona State University, Tempe, AZ 85287, USA.
6 U.S. Geological Survey, Flagstaff, AZ 86001, USA.
7 NASA Glenn Research Center, Cleveland, OH 44135, USA.
8 Department of Civil and Environmental Engineering and Geodetic Science, The Ohio State University, Columbus, OH 43210, USA.
9 NASA Johnson Space Center, Houston, TX 77058, USA.
10 Deutsches Zentrum für Luft und Raumfahrt, Institut für Raumsimulation, Linder Höhe, Köln, D-51170, Germany.
* To whom correspondence should be addressed. E-mail: firstname.lastname@example.org
The location of the Opportunity landing site was determined to better than 10-m absolute accuracy from analyses of radio tracking data. We determined Rover locations during traverses with an error as small as several centimeters using engineering telemetry and overlapping images. Topographic profiles generated from rover data show that the plains are very smooth from meter- to centimeter-length scales, consistent with analyses of orbital observations. Solar cell output decreased because of the deposition of airborne dust on the panels. The lack of dust-covered surfaces on Meridiani Planum indicates that high velocity winds must remove this material on a continuing basis. The low mechanical strength of the evaporitic rocks as determined from grinding experiments, and the abundance of coarse-grained surface particles argue for differential erosion of Meridiani Planum.
The Mars Exploration Rover (MER) Mission required accurate tracking of the location of Opportunity to ensure efficient drives and to place measurements in proper geological context, e.g., associating a rock target with a particular terrain or geologic unit (1–3). The location of the lander in inertial coordinates was determined by fitting direct-to-Earth, two-way, X-band Doppler radio transmissions and two passes of two-way Ultra High Frequency (UHF) Doppler transmissions between Opportunity and the Mars Odyssey Orbiter. Based on analyses of these observations, the landed location is 1.9483’S (withan accuracy of 10 m) and 354.47417’E (with an accuracy of 10 cm), translated to International Astronomical Union (IAU) 2000 areocentric coordinates. The landed location was also tied to Mars Global Surveyor (MGS) Mars Orbital Camera and MER descent image data to within 10-m accuracy, by triangulation to three craters observed in the far field [through breaks in the local Eagle crater rim (4)] in Pancam images. These triangulation results, mapped to the cartographic network–derived MGS Mars Orbital Laser (MOLA) data (5), imply that the lander is located at 1.9462’S, 354.4734’E in IAU 2000 areocentric coordinates.
Opportunity stopped on the plains for a software upload on sols 75 to 78 (6), and its location (1.94752’S, 354.47716’E) was determined by analysis of two passes of UHF two-way Doppler tracking. The location was also determined by image-based triangulation to common features, with resultant values of 1.9453’S, 354.4766’E. For both landing and software-upload locations, the Doppler-based location was displaced 135 m at an azimuth of 176° clockwise from north from the location derived from image-based analyses. This displacement is consistent with expected offset errors between inertially derived locations and positions estimated from the MOLA-based global cartographic network (5). These offsets provide a quantitative description of map errors expected for Mars in the equatorial regions when the current cartographic framework is used.
The first 57 sols of operations were conducted within Eagle crater (6), taking advantage of extensive rock outcrops exposed on the northwestern side of the crater. Slopes from the crater floor to the outcrops ranged up to 20° from horizontal and were covered by soils (7). The soil-covered slopes caused wheel slip and forced the MER team to plan novel approaches to rock targets. To traverse from one portion of the outcrop to another, Opportunity traveled across the crater floor and then turned directly upslope to approach a given rock target. In some cases, the rover used visual odometry to update positional information by acquiring stereo image data during traverses and using the range information to update positional knowledge. Observed slippage during upslope traverses of soil slopes of in all cases, with more slip encountered at higher slopes. For example, 100% slip was encountered during the vehicle’s initial attempt on sol 56 to egress from the crater on soil-covered slopes tilted at 17°. The rover successfully completed egress on sol 57 by traversing at an oblique angle to the crater wall’s topographic contours. These slip values are similar to those found during experiments in which the MER test rover traversed over dry, loose, poorly sorted, sand-sized materials.
For localization in Cartesian coordinates, we used forward- and backward-looking overlapping images of the surface, images of the sun, on-board inertial measurement unit (IMU) observations of rover tilt vectors, and tracking wheel turns in a least squares bundle-adjustment procedure to derive detailed positional estimates (Fig. 1). The magnitude of wheel slip within Eagle crater is evident, in that use of the bundle-adjustment technique and comparisons to positional estimates based on wheel turns alone demonstrate an accumulated error of 20 m over a total traverse distance of 183 m. For typical traverses of several meters, the rover position was delineated with an accuracy of several centimeters with the bundle-adjustment techniques.
Measurements of suspension system angles, together with rover tilt as inferred from IMU data, were used to reconstruct the elevation of each wheel at a 2- to 8-Hz sampling rate, relative to the start of each traverse (Fig. 1). Profile data retrieved for the sol 82 traverse across the plains show a height standard deviation of only 3.2 cm over the first 55 m and 40.3 cm over the total traverse distance of 141 m. These values are comparable to the small height standard deviations ( scale) derived from pulse spreading observed in MOLA data (8), confirming the very smooth and flat nature of Meridiani Planum and the landing site. The smooth nature of the plains is occasionally interrupted by troughs and hollows that are typically several meters across or narrower, with depths less than several tens of centimeters (Fig. 1). Low-amplitude ripples (only several centimeters high) with wavelengths of less than a meter are ubiquitous on the plains.
Dust accumulation at the Meridiani Planum landing site is evident from analyses of Pancam data that show gradual reddening over 90 sols of the Pancam calibration target (9). Furthermore, analyses of short-circuit current-monitor solar cell data show a decrease in current of 0.29% per sol (corrected for seasonal variations in the Mars-sun distance and solar elevation angle) during the first 25 sols of operations, slowing to 0.13% per sol by sol 90. These values are comparable to those seen by Spirit at Gusev crater (10). Yet the MGS Thermal Emission Spectrometer–based bolometric albedo at the Meridiani site is only 0.15 (11), consistent with Opportunity’s observations that show that dust is a minor surface component in Eagle crater and on the plains (9, 12). High-velocity winds must periodically scour the surface and remove surface dust accumulations from Meridiani Planum on a frequent basis.
The soils exposed at the Meridiani Planum landing site are dominated by dark, sand-sized and finer grained ( materials overlain by sparsely to densely arrayed spherules and irregular particles with grain sizes that range up to a few millimeters across (13). Trenches excavated to 8- to 10-cm depths in soils on sols 23, 54 (both in Eagle crater), and 73 [adjacent to the Anatolia trough (Fig. 1)] show that these coarser grains are also found within the soils but at lower concentrations than on the surface (14). The spherules have a hematitic signature and have been found in outcrops observed by the rover (9, 12, 15, 16). The high concentration of spherules and irregular particles at the surface is interpreted to be due to differential aeolian erosion of the evaporitic sedimentary rocks found by Opportunity (16), leaving behind a lag or pavement of relatively large and thus immobile materials. In addition, coarse-grained sand deposits have been reworked by wind to cover the ripples that are ubiquitous on the plains. The cores of the ripples are dominated by sand-sized and finer grained basaltic materials (13) (Fig. 2).
The physical nature of the soils within Eagle crater and on the plains can be inferred from a number of lines of evidence. Examination of wheel tracks shows that these deposits form high-fidelity casts of outer wheel surfaces, including cleat impressions with slopes greater than the angles of repose expected for most cohesionless materials. Impressions made by the Mössbauer contact plate (switch-activated when 1-N force was applied to soil surfaces) (Fig. 2), together with airbag bounce marks, show that spherules and irregular particles have been pressed into and partially covered by the finer grained soils (13), indicating that the uppermost fine-grained particles are easily displaced. In other cases, the spherules and irregular particles pressed into soils displace and expose millimeter-thick surface crusts. Furthermore, airbag seams are preserved well in bounce marks, and drag marks show complex curvilinear shapes with little indication of surface crumbling. All of these observations suggest that soils are only weakly cohesive (cohesive strength, 1 to 3 kPa) and consist of sand-sized and smaller grain sizes, allowing the fine-grained component to fill voids between the larger grains during remolding of the soils.
With regard to standard soil mechanical properties, the estimated bearing strength of the Eagle crater floor soils, based on wheel track sinkage values (17) and on the depth of depressions made by the Mössbauer contact plate, average 80 kPa with 5 kPa of cohesive strength and an angle of internal friction of 20°. The soils on the crater walls adjacent to the outcrops have an estimated bearing strength of 8 kPa cohesion of 0.5 kPa, and an angle of internal friction of 20°. Motor currents associated with soil trenching operations show that soils are more easily excavated at Meridiani Planum, as opposed to the Spirit landing site in Gusev crater (10), and that excavation into a ripple on the floor of Eagle crater required the least amount of trenching energy. This result suggests that the soil deposits on the floor of the crater were modified relatively recently by winds and have not yet had the time to become cohesive.
Rock outcrops within Eagle crater ground by the Rock Abrasion Tool (RAT) (18, 19) are of sedimentary origins (13) and include McKittrick (sol 30), Guadalupe (sol 34), and Flatrock (sol 44). Pilbara, another sedimentary rock located on the rim of Fram crater (Fig. 1), was ground on sol 86. Bounce rock, an igneous rock located on the plains near Eagle crater (Fig. 1), was ground on sol 66. Grinding of the McKittrick outcrop is illustrative of the multicomponent nature of the rocks exposed in Meridiani Planum. Two spherules were encountered during grinding, and their high grinding resistance relative to the weaker rock matrix caused the RAT to stop operations (Plate 8). One spherule was slightly rotated during the grinding, and an irregular clast was plucked from the rock and thrown downhill during grinding. The estimated grinding energies for the rock targets at Meridiani Planum are relatively low, as compared to rocks at Gusev crater and most samples ground in the laboratory (Table 1). The grind energy correlates with the slope angles for the outcrop, in that the more resistant Guadalupe target ground by the RAT is located on a 36 ± 5° slope, whereas the less resistant McKittrick target is located on a 6.7 ± 2° slope. The higher slope for the Guadalupe outcrop is interpreted to be due to higher resistance to weathering than the McKittrick outcrop. Finally, even Bounce rock is weaker than rocks ground at Gusev crater, consistent with the densely fractured appearance of this rock (Plate 12). Bounce rock is an isolated target on the plains and was probably transported to its current location as impact ejecta (12). The fractures may have been introduced during ejection and impact of this rock.
The hematite-bearing plains that Opportunity landed on are at the top of a section of layered strata that is 300 m thick and that disconformably overlies the Noachian-aged cratered terrain (11). We interpret the smooth, flat nature of Meridiani Planum to be due to differential stripping of horizontally layered strata, combined with continuing diffusion-driven mobilization of loose material to fill local depressions; i.e., soil fills in the craters, hollows, and troughs. Spherules, irregular particles, coarse sand covers, and basaltic soils represent the net result of concentration of these particles as the spherules were eroded from the weak evaporitic rocks in former and current aeolian environments. The hematite signature observed from orbit (20) that led us to land Opportunity in Meridiani Planum is due to a concentration of hematite-rich spherules that occurred as they were eroded from the evaporitic rocks. The lack of evaporite deposits in the soils on Meridiani Planum is due to relatively rapid aeolian erosion and removal as dust in suspension of these mechanically weak deposits. The amount of erosion is not well constrained, but it could range from meters to many meters.
References and Notes
1. S. W. Squyres et al., J. Geophys. Res. 108, 8062 (2003).
2. R. E. Arvidson et al., J. Geophys. Res. 108, 8070 (2003).
3. R. Li et al., J. Geophys. Res. 107, 8005 (2002).
4. Names have been assigned to areographic features by the Mars Exploration Rover (MER) Team for planning and operations purposes. The names are not formally recognized by the International Astronomical Union.
5. M. P. Golombek et al., J. Geophys. Res. 108, 8072 (2003).
6. A martian solar day has a mean period of 24 hours 39 min 35.244 s and is referred to as a sol to distinguish this from a roughly 3% shorter solar day on Earth.
7. The term martian soil is used here to denote any unconsolidated materials that can be distinguished from rocks, bedrock, or strongly cohesive sediment. No implication of the presence or absence of organic materials or living matter is intended.
8. G. A. Neumann et al., Geophys. Res. Lett. 30, 1561 (2003).
9. J. F. Bell III et al., Science 306, 1703 (2004).
10. R. E. Arvidson et al., Science 305, 5685 (2004).
11. R. E. Arvidson et al., J. Geophys. Res. 108, 8073 (2003).
12. P. R. Christensen et al., Science 306, 1733 (2004).
13. L. A. Soderblom et al., Science 306, 1723 (2004).
14. K. E. Herkenhoff et al., Science 306, 1727 (2004).
15. G. Klingelhöfer et al., Science 306, 1740 (2004).
16. S. W. Squyres et al., Science 306, 1698 (2004).
17. L. Richter, P. Hamacher, paper presented at the 13th Conference of the International Society for Terrain-Vehicle Systems, Munich, 14 to 19 September 1999.
18. S. P. Gorevan et al., J. Geophys. Res. 108, 8068 (2003).
19. T. M. Mynck et al., paper 2004-6096 presented at the American Institute of Aeronautics and Astronautics (AIAA) Space 2004 Conference and Exhibit, San Diego, CA, 28 to 30 September 2004.
20. T. M. Christensen et al., J. Geophys. Res. 105, 9623 (2000).
21. We thank the MER Team and the scientists and engineers who made the landing, traverses, and science observations a reality. Work funded by NASA through the MER Project.