NASA’s Lunar Reconnaissance Orbiter has captured the first images of the Chinese Chang’e 3 lander on the Moon.
Chang’e 3 landed on Mare Imbrium (Sea of Rains) just east of a 450 m (1,500 ft) diameter impact crater on 14 December 2013. Soon after landing, a small rover named Yutu (or Jade Rabbit in English) was deployed and took its first tentative drive onto the airless regolith. At the time of the landing, LRO’s orbit was far from the landing site so images of the landing were not possible. Ten days later on 24 December, LRO approached the landing site, and LROC was able to acquire a series of six LROC Narrow Angle Camera ( NAC ) image pairs during the next 36 hours (19 orbits). The highest resolution image was possible when LRO was nearly overhead on 25 December 03:52:49 UT (24 December 22:52:49 EST). At this time LRO was at an altitude of ~150 km (93 mi) above the site, and the pixel size was 150 cm (59 in).
The rover is only about 150 cm wide, yet it shows up in the NAC images for two reasons: the solar panels are very effective at reflecting light so the rover shows up as two bright pixels, and the Sun is setting thus the rover casts a distinct shadow (as does the lander). Since the rover is close to the size of a pixel, how can we be sure we are seeing the rover and not a comparably sized boulder? Fortuitously, the NAC acquired a “before” image (M1127248516R) of the landing site, with nearly identical lighting, on June 30, 2013. By comparing the before and after landing site images, the LROC team confirmed the position of the lander and rover, and derived accurate map coordinates for the lander (44.1214°N, 340.4884°E, 2640 meters elevation ).
The lander set down about 60 meters (200 feet) east of the rim of a 450-meter (1,500-foot) diameter impact crater (40 meters or 130 feet deep) on a thick deposit of volcanic materials. A large-scale wrinkle ridge (~100 km/62 mi long, 10 km/6.2 mi wide) cuts across the area and was formed as tectonic stress caused the volcanic layers to buckle and break along faults. Wrinkle ridges are common on the Moon, Mercury, and Mars.
Lunar mare basalts are divided into two main spectral (color) types: “red” and “blue” (blue is perhaps a misnomer, think “less red”). Basalts on the Moon (same on Earth) are composed mainly of two minerals, pyroxene, and plagioclase, though olivine and ilmenite can sometimes occur in significant amounts. The presence of ilmenite (FeTiO 3 ) results in lower reflectance and a “less red” color thus the blue basalts. The landing site is on a blue mare (higher titanium) thought to be about 3.0 billion years old. The boundary (black arrows in above WAC mosaic) with an older (3.5 billion years) red mare is only 10 km to the north.
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