Arecibo Radar Mapping of the Lunar Poles: A Search for Ice Deposits

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Science  06 Jun 1997:
Vol. 276, Issue 5318, pp. 1527-1530
DOI: 10.1126/science.276.5318.1527


The Arecibo 12.6-centimeter wavelength radar system was used to image the polar regions of the moon at a resolution of 125 meters in a search for ice deposits in areas of possible permanent shadow from the sun. No areas greater than 1 square kilometer were found with high radar backscatter cross sections and high circular polarization ratios, properties suggestive of the presence of ice. A number of areas smaller than 1 square kilometer were found with these properties, but optical images from spacecraft missions have shown some of these features to be in sunlight. Arecibo radar images of Sinus Iridum at latitude 47°N also showed a number of small features with similar properties. The coincidence of some of these features with the radar-facing slopes of craters and their presence in sunlit areas suggests that very rough surfaces rather than ice deposits are responsible for their unusual radar properties.

Ground-based observations of the moon were conducted using the Arecibo Observatory, Puerto Rico, 2.38-GHz (12.6-cm wavelength) radar system to map regions of lunar surface radio-wave backscatter in two polarizations at high spatial resolution (1). Observations of the polar regions were further motivated by the ability of radar to image areas not illuminated by sunlight; such areas may provide an environment suitable for the preservation of ice deposits or other volatiles over geologic time scales (2). Here, we present ground-based radar images of the north and south lunar poles and analyze the polarization properties of the reflected signal in the context of the possible presence of ice.

It has been suggested that permanently shadowed regions of the lunar poles would have relatively constant surface and subsurface temperatures, possibly as low as 40 K, providing an environment suitable for the entrapment and storage of ices over geologic time scales (2). The discovery of anomalous radar backscatter from permanently shadowed crater floors near the poles of Mercury and the interpretation of these regions as areas of probable water ice deposits (3, 4) strengthened the possibility of finding similar deposits near the lunar poles. The interpretation that ice is responsible for the anomalous radar backscatter in the Mercury radar images rests primarily on the unusual radar backscatter characteristics of many icy surfaces in the solar system—that is, high backscatter cross section per unit surface area (σo) with a circular polarization ratio (CPR) greater than unity (5). Although ice, with a dielectric constant of 3.15, does not have an intrinsically high reflectivity, it has low loss and thus may serve as a weakly absorbing material containing a matrix of embedded scatterers; such a material could support volume-scattering mechanisms such as the coherent backscatter opposition effect (6). Recent bistatic radar observations of the lunar south pole by the Clementine spacecraft are reported to show a backscatter enhancement consistent with, but not unique to, the presence of ice deposits (7). In comparison, the backscatter characteristics of rock surfaces that are rough on the scale of the radar wavelength (such as lava flows) and are observed at high incidence angles generally include high backscatter cross sections and CPRs of ≤1 (8). However, CPRs greater than unity have been observed over rock surfaces. Areas of the blocky SP lava flow in northern Arizona observed at incidence angles of 42° to 52° have CPRs between 1 and 2.5 (9).

As viewed from the lunar poles, the Arecibo Observatory rises a maximum of ∼6° above the horizon [incidence angle of 84° (10)], but, given the 1.53° inclination of the moon’s equatorial plane to the ecliptic plane, the limb of the sun can be up to 1.82° above the horizon. Because we lack detailed knowledge of the lunar topography, these small angles mean that an unknown fraction of the area shadowed from the sun is also shadowed from Arecibo and, hence, is not observable (for example, the floors of the large impact craters). At the lunar south pole, about 60% of the area below latitude 85°S is observed in the radar image, including much of the south pole area shown to be in solar shadow in Lunar Orbiter IV (11) and Clementine optical images (7, 12). However, areas shadowed in these spacecraft optical images are not necessarily in permanent shadow because of the 18.6-year precessional period of the lunar spin axis. The lack of detailed topographic information for the polar regions makes it impossible to determine which areas are in permanent shadow.

Radar images of the north and south polar regions of the moon were acquired in May and August 1992, respectively (1). A circularly polarized wave was transmitted from the main Arecibo antenna, and both senses of circular polarization—opposite circular (OC) and same circular (SC) (13)—were received at a smaller auxiliary antenna located 11 km from the Arecibo telescope. This bistatic radar arrangement permitted a pulsed radar experiment that avoided ambiguities in range (range aliasing) while maintaining an average data rate appropriate for the data acquisition hardware (14). The transmit signal was encoded with a pseudorandom code, and 16,384 pulses acquired in ∼25 min were combined to form a range-Doppler image with a resolution of ∼125 m and three or four looks (independent measurements of the backscatter from a given surface area). The final processing stage resampled the range-Doppler image into selenographic coordinates and applied small offsets to align the position of the poles with published locations (11).

The OC image of the north pole was acquired on 8 May 1992 when Arecibo was ∼4.1° above the horizon at the pole, resulting in extensive radar shadows from topographic features so that only ∼40% of the area above 85°N (28,900 km2) was imaged (Fig.1A). The image shows a slight topographic high running from 85.5°N, 240°E to 85°N, 110°E, which appears to be caused by adjacent impact crater rims; this feature prevents the measurement of a radar echo from a large area in the lower half of the image. Most areas of enhanced backscatter are associated with surface slopes inclined toward the radar, such as the radar-facing slopes in highland areas and the radar-facing inner and outer walls of impact craters. Smooth plains such as the flooded floor of the impact crater Gioja (82.5°N, 1.2°W) and the adjacent impact basin centered at 84.5°N, 6°E are characterized by fairly uniform backscatter interrupted by numerous smaller impact craters. In comparison, the highland areas, such as the segment between 30°W and 55°W, 85°N to 90°N, have a hummocky appearance.

Figure 1

OC backscatter image of (A) north pole and (B) south pole regions in a stereographic map projection. The radar signal incidence angle (10) is 85.9° at the north pole and 83.9° at the south pole (4.1° and 6.1° above the local horizon, respectively). The incidence angle varies in proportion to latitude along approximately the 0° to 180° longitude line in these maps. The processed radar data were averaged to three looks with a resolution of 121 m in slant range (image top to bottom) for both images, 136 m in cross range (image left to right) for the north pole and 108 m in cross range for the south pole, before resampling to selenographic coordinates. The radar backscatter is shown in units of σo, in a logarithmic scale with an absolute error of ∼3 dB (a factor of 2) (19). The sides of the south pole map show ghost images that were located at Doppler offsets beyond the radar sampling frequency (pulse repetition frequency) and were aliased into the processed Doppler bandwidth.

The south pole area was imaged on 18 August 1992 (Fig. 1B) when Arecibo was ∼6.1° above the horizon at the pole, so that ∼60% of the area below 85°S (43,300 km2) was imaged. Smooth plains are less prevalent in the south pole area, occurring mainly in the floor of the crater Amundsen at 84.7°S, 82.2°E, in the area to the east of Amundsen around 85.7°S, 127.7°E, and in the region around 86.5°S, 75°W, which appears to be the floor of an impact feature centered at 85.5°S, 90°W in the Clementine optical image (7,12).

The CPR images for the north and south pole regions have very similar characteristics. There are no extensive areas with CPRs approaching or greater than unity. The average CPRs for areas that appear to have little topographic expression (and are not in the radar shadow) are ∼0.45 for the north pole and 0.37 for the south pole. If large craters and complex areas are included in these measurements, then the CPRs increase to 0.54 and 0.45, respectively. These latter values are comparable to the ratio of 0.54 estimated from previous scattering law measurements for the average lunar surface at high incidence angles at 23-cm wavelength (15). The images of both poles show areas of high CPR associated with the radar-bright inner walls of several craters with rim diameters of <30 km as well as smaller radar-bright features, most of which appear to be associated with small craters. For these features, high SC backscatter cross sections correlate with the high CPRs, as shown in Fig. 2 for the south pole. For example, the large impact craters labeled A and B have radar-bright, radar-facing rims with CPRs near unity, whereas craters C and D have less bright radar-facing rims with CPRs closer to the mean value. The relatively flat region around location E has a uniform CPR of 0.4. Backscatter values for the middle area of the radar-facing inner rim of the 20.5-km-diameter crater A, the south pole crater (σoc o = 0.036, CPR = 0.94 ± 0.04), are greater than the values for the left side (in the image) of the radar-facing inner rim of crater C (σoc o = 0.001, CPR = 0.38 ± 0.02). The top of the rim of crater A is illuminated by sunlight in the Lunar Orbiter IV and Clementine images (7, 11, 12), indicating that it is not in permanent shadow, which suggests that the presence of ice is not a viable explanation for the enhanced backscatter. Geometric effects such as double bounce may be responsible but hitherto have been clearly observed only when the surface geometry supports forward scatter into a second surface (1, 16). The most probable explanation is enhanced backscatter from increased wavelength-scale surface roughness in the rims of craters A and B. The enhanced backscatter areas are associated with steeper slopes; estimates of the inner rim slopes from the crater radar shadow are 37° above the horizontal for crater A and 20° for crater C.

Figure 2

Images of (A) the SC polarization backscatter and (B) the CPR of the south pole region. The SC image has three looks, and the ratio image was calculated from data averaged to 1-km resolution and ∼230 looks using a boxcar filter, masked by the regions of radar shadow. Small radar-bright features with CPRs greater than unity are indicated by arrows. One of these features with extreme backscatter values is the 840-m-diameter impact crater at 88.4°N, 110°E, labeled F. The single-look image with a resolution of 121 m in range by 36 m in cross range (inset in A) shows that the radar-bright area is associated with the crater rim.

Similar increases in the backscatter cross section and CPR for the radar-facing inner slopes of craters were measured in clearly sunlit areas of the moon away from the poles. Figure 3 shows the SC and CPR images for Sinus Iridum and the hummocky terrain to the northwest (centered on 47.2°N, 32.5°W). The two craters in the lower left of the images, with diameters of ∼10 km, have CPRs in the range of 0.72 to 0.94 for several areas on the radar-facing rims. Histograms of the entire CPR images in Figs. 2B and 3B have similar mean values of 0.48 and 0.49, respectively, and the high CPR tails of both distributions extend past a CPR of 1.

Figure 3

Images of (A) the SC polarization backscatter and (B) the CPR of Sinus Iridum and the area to the northwest (centered on 47.2°N, 32.5°W) in the radar delay-Doppler projection. The images are 360 km high by 340 km wide, are oriented with southeast to the top and northwest to the bottom, and have an incidence angle varying from 52.4° at the top to 64.0° at the bottom. The ratio image was calculated from data averaged to ∼1.5-km resolution with 256 looks. The inner slopes of the three craters at the lower left, the ejecta of the medium-size crater at the upper middle left, and many areas around the basin rim have CPRs around unity.

A more puzzling problem than the near-unity CPRs for the slopes of some of the larger craters is the problem of CPRs greater than unity for (i) a number of craters with diameters of <1 km, (ii) small features that are probably craters with sizes near or below the image resolution, and (iii) regions of <1 km2 on the radar-facing slopes of some of the larger craters. Twenty-six of the these features were identified in the region of the south pole shown in Fig. 2. The CPRs for these features varied from ∼1.2, a lower limit set by a selection requirement that the average CPR be ≥2 standard deviations above unity, to 2.6 (17, 18). Their SC backscatter cross sections varied from 0.022 to 0.002. If the same expression as in Harmonet al. (4) is used to correct for the incidence angle, these cross sections correspond to full-disk albedos in the range 0.7 to 0.06, with half the features having a value close to 0.1. This range is similar to that obtained by Harmon et al. for the possible polar ice deposits on Mercury, although the median value is somewhat lower and the sizes of the regions are much smaller than those found on Mercury. However, examination of a mosaic of the south pole region made from Clementine images (12) indicates that at least 9 of the 26 features, primarily those in the smooth plains area to the left of crater C in Fig. 2 (near 86.5°S, 75°W), are in sunlit areas. This estimate is probably low because the Clementine images were obtained in the lunar southern winter, when the lunar spin axis was tilted so that the south pole pointed away from the sun (7); more of these features are likely to be in sunlight during the course of the lunar year and during the 18.6-year precessional period of the lunar spin axis.

An examination of the north pole and Sinus Iridum regions found a comparable number of small regions with high cross sections and CPRs of 1.2 to 2.2. Many of the features in the Sinus Iridum area are associated with the steep impact basin walls, but some are also associated with small craters. Consequently, scattering mechanisms associated with a high degree of wavelength-scale surface roughness (9) seem the most probable explanation for the high σo’s and CPRs of these small features. These same properties may, of course, also be indicative of ice for those features in permanent shadow. Feature F in Fig. 2A has a CPR of 2.4 ± 0.14 and an SC cross section of 0.022 for an area of 0.42 km2, and is the best candidate in the Arecibo data for a reflection from ice. However, as can be seen from the subimage of feature F in Fig. 2A, the high SC backscatter is from the radar-facing outer and inner slopes of the crater’s walls. It is not clear why this would be the case if the high radar return were the result of volume scattering in ice on the crater floor. This association of the enhanced scatter with the crater walls again suggests that a rough-surface scattering mechanism may be responsible.

The similarities in the Arecibo and Clementine bistatic radar (7) experiments make them suitable for comparison. Both used a 2.38-GHz radar system and measured the scattered circular polarization signal. Although the transmitter positions were different, both used a ground-based receiver, and thus the collected signal was constrained by the Earth-moon geometry. The Arecibo image of the south pole area, acquired with the Arecibo telescope 6.1° above the horizon, imaged fractionally more features within the south pole region than did Clementine, where the receiving antenna was 4.5° to 5.5° above the horizon. Shadows evident in Fig. 2A clearly show that the geometry for both the Arecibo and Clementine experiments precluded measurement of radar scatter from the floors of the craters at the south pole. Maps of the Clementine south pole footprints (7) and our best understanding of the north pole footprint were used to crop the Arecibo data and calculate CPRs for comparison with the Clementine measurements. The Arecibo results, which show similar CPRs for the two poles, do not agree with the Clementine measurement that showed a significantly enhanced CPR for the south pole relative to the north pole and to a reference area near the south pole (Table1). The Clementine experiment measured the radar cross sections as a function of the bistatic angle β for a large area (per observation), whereas the Arecibo experiment measured the backscatter signal (β = 0) at high spatial resolution. The Clementine data show a CPR enhancement near β = 0, whereas the Arecibo data show only small (<1 km2) areas with CPR > 1. If the enhancement in the south pole CPR measured by Clementine around β = 0 is attributable to the high-CPR areas identified in the much finer resolution Arecibo data set, then, because these areas are typically associated with impact craters and some appear to be in sunlit areas, the observed phenomena may be attributable to rough-surface scattering.

Table 1

Arecibo and Clementine CPR measurements.

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Because of the association of the high CPR areas with impact features and the location of many of these areas in sunlit regions, there is no clear evidence from the Arecibo images for the presence of ice. Most high CPR areas appear to be the result of increased surface roughness or blocky areas associated with the steep inner rim slopes of impact craters.

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