The chemical compositions of relatively young mare lava flows have implications for the late volcanism on the Moon. Here we report the composition of soil along the rim of a 450-m diameter fresh crater at the Chang′e-3 (CE-3) landing site, investigated by the Yutu rover with in situ APXS (Active Particle-induced X-ray Spectrometer) and VNIS (Visible and Near-infrared Imaging Spectrometer) measurements. Results indicate that this region's composition differs from other mare sample-return sites and is a new type of mare basalt not previously sampled, but consistent with remote sensing. The CE-3 regolith derived from olivine-normative basaltic rocks with high FeO/(FeO+MgO). Deconvolution of the VNIS data indicates abundant high-Ca ferropyroxene (augite and pigeonite) plus Fe-rich olivine. We infer from the regolith composition that the basaltic source rocks formed during late-stage magma-ocean differentiation when dense ferropyroxene-ilmenite cumulates sank and mixed with deeper, relatively ferroan olivine and orthopyroxene in a hybridized mantle source.
The combination of precise chemical and physical properties of Apollo and Luna samples with known locations provides ‘ground truth’ for lunar remote sensing studies1,2. After some 40 years since the Apollo and Luna missions, China’s Chang′e-3 (CE-3) landing and Yutu rover mission in December, 2013, provided the next robotic in situ measurements on the Moon3,4,5,6. The CE-3 landing site is in the northern part of the Imbrium basin (340.49°E, 44.12°N). Serial eruptions flooded the Imbrium basin from ∼3.5 Ga to ∼2 Ga (ref. 7), making this region of great scientific value for the detection of lava variations during extended volcanic activity6,7,8. The CE-3 landing site represents a relatively young (∼2.96 Ga) medium-Ti lunar basalt exposure7,8,9,10. The top Eratosthenian lava flows at the Mare Imbrium surface on which CE-3 landed are interpreted to be 10–60 m thick and up to 1,200 km in length7,8,9,10,11.
Here we combine the data from two payload elements of the Yutu rover, the Active Particle-induced X-ray Spectrometer (APXS) and Visible and Near-infrared Imaging Spectrometer (VNIS; see Methods section for the instrument descriptions), and report the composition and mineralogy of the region explored by the rover. Our analysis indicates that this young lunar mare region has unique compositional characteristics, and represents a new type of mare basalt that has not been sampled by previous Apollo and Luna missions and lunar meteorite collections. APXS data suggest that the regolith is extremely rich in FeO, high in CaO, intermediate in TiO2, modest in Al2O3 and poor in SiO2. We present the mineralogical information derived from APXS chemical data and VNIS spectral data, showing self-consistent and well-correlated results in mineral modes (for example, the proportions of high-Ca pyroxene, low-Ca pyroxene and olivine) and mineral chemistries (both data sets indicate an abundance of high-Ca ferropyroxene plus Fe-rich olivine). The more accurate in situ chemical and mineralogical measurements of the new basalt type provide ground-truth validation of remote sensing studies that also indicated the olivine-rich mineralogy of the basalt unit where CE-3 landed. Because the CE-3 landing site was on the ejecta of a fresh impact crater, we take the local regolith composition to be essentially that of the basalt excavated by the impact crater, and then consider the implications of the measured composition. Results suggest an origin from late-stage magma-ocean cumulates that crystallized after ilmenite saturation and hybridized with an olivine-rich cumulate. The CE-3 landing site and in situ analyses of the rocks and soils derived from the fresh crater near the landing site provide key new ground truth for some of the youngest volcanism on the Moon.
Landing site description and Yutu rover operations
The location of CE-3 from a global to a ground view is shown in Fig. 1. CE-3 landed on the rim of a young crater (∼27–80 Myr old6), initially informally named Purple Palace4 and now formally named Zi Wei (Fig. 1c). The diameter of the crater is ∼450 m, which would have excavated ∼40–50 m beneath the surface. The ejecta of the impact should cover the entire CE-3 landing site and the region explored by the Yutu rover, evidenced by the blocky surface seen by the landing camera (Fig. 1d) and big boulders encountered by Yutu during its traverse (Fig. 1d,e). The Panoramic Camera imaged two types of rocks; one is a mainly light-toned and coarse-grained rock and the other is a relatively darker, fine-grained rock (Supplementary Figs 1 and 2, Supplementary Note 1). During 32 days of surface operations, Yutu travelled 114 m in this region and made four sets of in situ and stand-off measurements at four locations (Fig. 1d)3,4,6. The APXS and VNIS aboard the Yutu rover acquired compositional and spectral measurements at four locations (CE3-0005, -0006, -0007 and -0008), as shown in Fig. 1d. A detailed description of the instruments, measurements and data processing are given in the Methods section and refs 12, 13, 14, 15, 16.
Chemical compositions and normative mineralogies from APXS
APXS spectra show peaks of Mg, Al, Si, K, Ca, Ti, Cr, Fe, Ni, Sr, Zr and Y from the CE-3 soils (Fig. 2a). We used the peak-area ratio of measured samples and the calibration target (Supplementary Table 1) to derive the chemical compositions of three measured soils (CE3-0006_2, -0006_3 and -0008, Table 1). In general, the major element concentrations of the three soils at the CE-3 landing site are similar to each other and represent a distinctive composition (Table 1, Fig. 2b–d). They are characterized by low SiO2 (∼41.2 wt.%), very high FeO (∼22.8 wt.%), high CaO (∼12.1 wt.%), intermediate TiO2 (∼5.0 wt.%) and modest Al2O3 (∼9.7 wt.%).
When compared with Apollo and Luna soils and basaltic rocks (Fig. 2b–d)2,17, the TiO2 versus FeO relation of the CE-3 soils bears some similarity with Apollo 12 ilmenite basalts, but CE-3 soils have higher FeO and TiO2 (Fig. 2b). The CE-3 soils have MgO concentrations in the range 6.3–11.0 wt.% (Table 1) with derived Mg# (=Mg/(Mg+Fe) × 100)<50 (Fig. 2c) at the low end, but a higher CaO compared with other mare samples (Fig. 2d), and deviating from the KREEP—feldspathic highlands—mare compositional triangle based on the returned lunar samples. These compositional features suggest that the CE-3 soils differ significantly from other known lunar basaltic materials.
On the basis of chemical composition (Table 1), we calculated the abundances of normative minerals of CE-3 soils using a CIPW (Cross, Iddings, Pirsson and Washington) norm. The major CIPW norm results are summarized in Table 1 and the detailed results are shown in Supplementary Tables 2,3. For CE3-0006_2 and CE3-0006_3 (sampling sites ∼10 cm apart), we calculated the mean value as ‘Mean_0006.’ For the norms summarized in Table 1, we combined the high-Ca pyroxene components as diopside (Di) and the Ca-poor components as hypersthene (Hy). Given the analytical uncertainties associated with the APXS data (Supplementary Table 4), the main difference is in MgO, which is significantly higher in CE3-0008 (11 wt.%) compared with CE3-0006 (6.7 wt.%). The difference in MgO translates to a difference in the relative abundance of olivine and pyroxene and in the ratio of Di to Hy (Table 1). The higher MgO concentration of the CE3-0008 soil results in a higher Mg# (46) compared with CE3-0006 (34) and a higher Fo (=Mg/(Mg+Fe) × 100) in olivine, that is, ∼Fo51 for the CE3-0008 soil and ∼Fo40 for the CE3-0006 soil. The CE3-0006 soil is also richer in the high-Fe endmember for both Di and Hy (Table 1) as a result of the difference in MgO. Considering analytical uncertainties for Al, Si, Ca, Fe and Ti, normative abundances of plagioclase and ilmenite are the same in -0006 and -0008, within analytical uncertainties.
In Table 1, the ‘Means_all’ column shows the average chemical composition and normative mineralogy summary of the CE-3 landing site soils. The soils have a high percentage of normative pyroxene (∼42 wt.%), with most being high-Ca pyroxene, Di (29 wt.%), that is, about two times the Hy (13 wt.%). The normative feldspar content (27 wt.%) is within the range of many lunar basaltic samples. The normative olivine content (20 wt.%, corresponding to 17 vol.%) of CE-3 is at the high end of the range for known lunar basalts (for example, Apollo 12 olivine basalt has ∼20 vol.% olivine2). In the CE-3 soils, olivine is Fe-rich with relatively low average Fo content (∼43). The normative ilmenite contents of the three CE-3 soils are similar, averaging ∼9 wt.%. The average Mg# of the soils is ∼38, indicating the exceptionally ferroan character of source rocks that make up the local surface soils.
Mineral chemistry and mineral modes based on VNIR spectra
The visible-NIR (near-infrared) spectra (Fig. 3a,b) of four VNIS observations show characteristic 1 and 2 μm absorption features owing to the electron transfer of Fe2+ in the M1 and M2 sites of lunar mafic silicates18. The spectra (Fig. 3a) have obvious absorption features and relatively flat profiles, indicating a low degree of space weathering, consistent with the fact that the CE-3 landing site sits on a relatively young Eratosthenian lava flow and the fresh ejecta of the young and fresh Zi Wei crater.
To estimate the average composition of minerals contributing to the spectra, we apply the modified Gaussian model (MGM)19,20 to deconvolve the spectral bands. We find that the spectra from CE3-0005 and CE3-0008 sites have wide and strong 1 μm absorption bands but shallow 2 μm band depths (Fig. 3a,b), thus they should have a higher 1–2μm band area ratio (BAR), which implies the presence of a significant amount of olivine in the soils of these two sites15,21,22,23. The absorption components of all four continuum-removed spectra (Fig. 3b) are calculated using MGM, as mixtures of three endmembers, high-Ca pyroxene (HCP), low-Ca pyroxene (LCP) and olivine (Supplementary Note 5, Table 2). This combination is the most complicated for this type of spectral deconvolution24,25,26. The results of the MGM deconvolution are shown in Table 2.
Extensive laboratory studies of terrestrial and synthetic pyroxenes provide the basis to correlate the 1- and 2-μm band positions with their chemical compositions27,28,29,30. We plot the central positions of deconvolved 1 and 2 μm bands from HCP and LCP components based on the data of Adams27 and Cloutis and Gaffey28 (Fig. 3c). Here we define the HCP as wollastonite (Wo)>30 and LCP as Wo<30, keeping with previous work by Sunshine et al.31 and Klima et al.30. By comparison, the compositional features of LCP of the four soils are similar (Fig. 3c) and very Fe-rich, relative to orthopyroxene examined by Adams27 and Cloutis and Gaffey28. However, the HCP compositions of CE-3 soils occur in two groups; CE3-0006 and CE3-0007 are slightly richer in Ca and in Fe than CE3-0005 and CE3-0008, consistent with APXS data (Table 1). The pyroxene chemistry of the CE-3 soils derived from VNIS data thus supports their general Fe-rich character, with CE3-0006 and CE3-0007 having even higher Fe contents, consistent with APXS results.
The volume percentage ratio of HCP and LCP (HCP/LCP) can be estimated using the band-strength ratios of 1 and 2 μm bands from MGM deconvolution of VNIS spectra19,24,29,30,32. The HCP/LCP vol.% ratios for four CE-3 soils were calculated using both the 1- and 2-μm band-strength ratios. The results for each soil using two ratios are consistent (Table 2), indicating an equivalent compositional effect on both 1 and 2 μm bands. Overall, the HCP/LCP ratios in four CE-3 soils are similar, with HCP about two times LCP in abundance.
The MGM-derived band positions of olivine shift as a function of Fo content, thus they can be used to estimate olivine chemistry20,25. We plot central positions of two deconvolved M1 component bands of CE-3 olivine (Fig. 3d) with trend lines determined on terrestrial samples by Sunshine and Pieters20. The central positions of the two olivine M1 bands occur at 870–884 nm and 1234–1261, nm for the four CE-3 soils, suggesting they are Fe-rich (30<Fo<55, Fig. 3d). Specifically, spectra indicate that CE3-0005 and CE3-0008 soils have higher olivine Fo values than the other two soils.
The precise location of the M2 band (∼1050, nm) of olivine in the VNIS spectrum is difficult to determine via MGM deconvolution20,33 (Supplementary Note 5). However, we plotted the central positions of olivine M2 bands of four CE-3 soils derived from MGM deconvolution in Fig. 3d, which also shows a trend along the trend line determined by Sunshine and Pieters20. Therefore, olivine chemistry of the CE-3 soils derived from VNIS data supports their general Fe-rich character, consistent with normative analysis of the APXS results (Fo ∼43 on average, Table 1). The band-strength ratios of the HCP 1-μm band to the olivine M1 band near 1.25 μm could also be used to estimate their volume percentage24. The four CE-3 soils can be divided into two groups (Table 2): the CE3-0005 and -0008 soils are richer in olivine on the basis of VNIS analysis (HCP/OL=2.0 and 2.3) than CE3-0006 and CE3-0007 (HCP/OL=3.0 and 3.3, respectively).
Refinement of mineral mode by correlated APXS and VNIS
A key result from both the APXS and VNIS data is the inferred abundance of olivine. The APXS data indicate relatively low SiO2 and high FeO+MgO, resulting in a significant proportion of olivine in the norm (10 vol.% in CE3-0006 and 30 vol.% in CE3-0008, Table 1). Our MGM analysis of the VNIS spectra also reflects high olivine contents (the HCP/OL ratio is 3.0 for CE3-0006 and 2.3 for CE3-0008, Table 2). A high olivine content coupled with intermediate to high TiO2 makes the CE-3 soil and the basalt from which it derives unique among the known lunar samples, similar to a basalt type that has been inferred from orbital data34, but not until the CE-3 mission verified by in situ or sample analysis.
Second, olivine chemistry derived from the norm analysis based on the APXS composition (Table 1) and from the central positions of the olivine M1 bands in VNIS spectra (Fig. 3d) both support the Fe-rich character of olivine in CE-3 soils. Fe-rich olivine was predicted on the basis of remote sensing of this area21, thus the Fe-rich olivine found by CE-3 indicates a relatively evolved magma from late-stage volcanic activity in the Imbrium basin35.
We also find similarity in pyroxene features inferred from normative analyses of the APXS composition (Table 1) and deconvolved VNIS spectra (Table 2). For example, both sets of analyses suggest CE-3 soils are rich in HCP. A good match was found between HCP/LCP ratios in CE3-0006 soil derived from VNIS (2.0, Table 2) and the Di/Hy components derived from APXS analysis (2.0, Table 1). The CIPW norm analysis based on APXS composition indicates a much higher Di/Hy ratio for CE3-0008 (8.7, Table 1) than the HCP/LCP derived from VNIS (2.3, Table 2). This large difference results in part from the effect of the normative pyroxene components in which the Hy component has no Ca. In reality the LCP pyroxene (in this case, pigeonite) does contain Ca. The effect is greatest in CE3-0008 because it contains so much olivine that there is little normative Hy and abundant Di. Moreover, the VNIS and APXS target areas were within a short distance of each other (<1 m), so we do not expect such a large variation in this less (space-) weathered basaltic regolith.
To provide a better comparison between APXS data and VNIS data, we use typical compositions of lunar mare minerals (that is, olivine, augite, pigeonite and plagioclase) as endmembers in a mixing-model calculation instead of the normative calculation results (Supplementary Table 7). The results of this mixing analysis are shown in Table 3.
From the mixing analysis, the refined mineral mode of CE3-0008 yields an Aug/Pig ratio of 2.4 (Table 3), which matches well with the VNIS HCP/LCP ratio (2.3, Table 2) based on VNIS spectral deconvolution. For CE3-0006, the Aug/Pig value in the refined mineral mode (2.0) and the HCP/LCP value in the VNIS-derived mode (2.0) are essentially the same. Considering these results, the APXS and VNIS mineral modal data are consistent.
The CE3-0008 soil may have a greater abundance of material contributed from deeper levels of the nearby Zi Wei crater (Fig. 1e), with a composition similar to the nearby light-toned rocks (Supplementary Figs 2 and 3) such as the ‘Outer Fence’ boulder. From an image-based mineral modal estimation of Outer Fence, we infer ∼20 vol.% in plagioclase phenocrysts (Supplementary Fig. 3, Supplementary Table 5, Supplementary Note 2), which is in general agreement with our estimations (∼33 vol.%) of nearby CE3-0008 soil. Moreover, the regolith reflectance differences observed by the Lunar Reconnaissance Orbiter Camera Narrow Angle Cameras (LROC NAC) are rather limited around the landing site (Supplementary Fig. 4, Supplementary Note 3). The Al2O3 content of CE-3 landing site based on experience of lunar samples is most likely in the range of 7–10 wt.% (Supplementary Fig. 5, Supplementary Note 4). The reflectance of the nearby rocks at the CE-3 landing site may result from texture-related human-eye brightness exaggeration (that is, some workers36 initially interpreted the rock as an aluminous basalt with a plagioclase content possibly exceeding 40 vol.% (see Supplementary Notes 2–4 for additional discussion).
Correspondence between the landing site and remote sensing
Lunar Prospector (LP) Gamma-Ray Spectrometer (GRS) results suggest that soils developed on north-central Imbrium mare basalts, including the CE-3 landing site, have high FeO (>20 wt.%, half-degree per pixel binning) and TiO2 (5.20 wt.%, 2° per pixel binning)6,37. Clementine data for areas near the CE-3 site indicate ∼19 wt.% FeO and 5–7 wt.% TiO2. The LP-GRS TiO2 data in this part of Imbrium are variable, however. Considering both the LP-GRS data and the Clementine ultraviolet–visible data, the values are broadly similar to those of some widespread western Procellarum mare regions (for example, centred ∼18° N and 303° E) where the surface is spectrally similar and where LP-GRS TiO2 values are similar (4–6 wt.%). TiO2 is normally used as the primary compositional criterion to classify remote sensing data for lunar basalts and indicates that many of the lunar basalts are actually intermediate in TiO2 content (for example, 4.5–7.5 wt.%)38. The CE-3 composition falls in this range, thus we regard them as intermediate Ti basalt (similar to Neal et al.36). The intermediate Ti content of CE-3 provides an important calibration point for the TiO2 estimation by spectral data (for example, Clementine UVVIS)38,39, which has been problematic (for example, Gillis et al.40 suggested about 50% uncertainty in the Imbrium basalts). The CE-3 TiO2 data provide ground truth for further revision or evaluation of TiO2 estimation methods for remote sensing studies. The high CaO content of the CE-3 soils (compared with other mare basalts, Fig. 2d) and the abundance of HCP inferred from the visible-NIR spectra support a high Ca content in the area of this flow unit. This result is consistent with the LP-GRS results (CaO of ∼11.1 wt.%, same region in north-central Imbrium at 2° per pixel37) and Clementine UVVIS mineral mapping (rich in clinopyroxene and olivine, but poor in orthopyroxene)2,41. LRO Diviner data42 show a Christiansen feature value near 8.55 μm, indicating a low SiO2 content in this region, which qualitatively agrees with the low SiO2 (41.2 wt.% average, Table 1) of the CE-3 APXS measurements. Moreover, the high olivine content and Ti enrichment in the late-stage volcanism of the Procellarum and Imbrium regions have been interpreted by many authors21,22,23,34,43,44 according to spectral data from telescopic observations, the UVVIS camera on Clementine, and the Moon Mineralogy Mapper (M3) on Chandrayaan-1, and these observations are supported in the Imbrium region by CE-3 results.
Given a basalt that is rich in TiO2 (5%) yet also rich in olivine (>10%), we consider its possible origin. The composition of CE-3 basalt, inferred from APXS analyses of immature soils at the site derived from the uppermost young basalt flow, is FeO-rich, with an Mg/(Mg+Fe) value of ∼0.4. This composition suggests derivation from late-stage magma-ocean cumulates that crystallized after ilmenite saturation and thus were rich in ferropyroxene and ilmenite, possibly hybridized with an intermediate to late-stage olivine-orthopyroxene cumulate. Such an origin may be common among late-stage basalts in the Procellarum-Imbrium region (Procellarum KREEP Terrane or ‘PKT’45,46), producing olivine-bearing, ilmenite-rich ferrobasalts such as those of the flow sampled by CE-3 in north-central Imbrium as well as the extensive Ti-rich, olivine-bearing basalts of Western Procellarum21,34. Extended magmatic activity in the PKT may have been driven by radioactive decay and heating of late-stage, incompatible-element-rich cumulates that were also rich in Ti. Olivine enrichment would not be expected with such cumulates because lunar magma ocean (LMO) residual melts at the stage of ilmenite saturation (>95% LMO crystallization) would most likely be saturated with pigeonite and augite47,48, thus requiring localized mixing or hybridization with an olivine-rich cumulate. In that case, the olivine-rich cumulate would, itself, be fairly iron-rich, for example, as might have been produced from the LMO after some 75% solidification. These would be late-stage LMO cumulates, likely enriched in incompatible trace elements (ITEs), including U and Th, consistent with prolonged mare basaltic activity in this part of the Moon49. An origin of such hybridized magmas, as formed by partial melting of upper mantle cumulates, is similar to the origin inferred by Snyder et al.47 for high-Ti basalts.
In conclusion, from a correlated analysis of the regolith derived from rocks at the CE-3 landing site, freshly excavated by Zi Wei crater, we recognize a new type of lunar basalt with a distinctive mineral assemblage compared with the samples from Apollo and Luna, and the lunar meteorites. The chemical and mineralogical information of the CE-3 landing site provides new ground truth for some of the youngest volcanism on the Moon.
Instruments and data descriptions
The APXS is designed to conduct in situ elemental measurements of lunar regolith, using 55Fe and 109Cd as the excitation sources. The APXS is installed on the arm of the Yutu rover with an effective detection area of ∼50 mm in diameter13. The VNIS employs the Acousto-Optic Tunable Filter (AOTF) technique to provide hyperspectral images in the 450–950-nm region and point spectral measurements in the 900–2,400-nm region14,15,16. The VNIS is installed on the front of the rover at a height of 0.69 m, observing the lunar surface at a fixed 45° view angle. The targeting area of the VNIS imager is ∼16 × 21 cm. The targeting area of the VNIS-point spectrometer is a circle of ∼7 cm diameter, inside of the targeting area (Fig. 3a) of the VNIS imager. The distance between the sampling areas of the APXS and VNIS at one location is within 1 m. The detailed descriptions of these two instruments and their calibration procedures can be found in refs 12, 13, 14, 15, 16.
This study is based on level 2C (APXS) and 2B (VNIS) data released by the Ground and Research Application System (GRAS) of the Chang′e-3 Project. The APXS conducted two calibration target measurements and four sets of lunar soil measurements at two locations (CE3-0006 and -0008). Measurement 0006_1 was a test measurement at ∼5 cm distance from the surface of the regolith, 0006_2 was at the same location as 0006_1 but at a distance of ∼2.5 cm above the surface and 0006_3 was at a lateral distance of about 10 cm from 0006_2. The VNIS acquired four hyperspectral images (450–950 nm) and four point NIR spectral measurements (900–2,400 nm) at four locations (CE3-0005, -0006, -0007 and -0008). The locations of the APXS and VNIS measurements are shown in Fig. 1d. The APXS data at CE3-0006_1-3 and CE3-0008 correspond to the VNIS spectra from CE3-0006 and CE3-0008.
APXS data processing and analysis
The APXS has a calibration target with known chemical composition (Fig. 2a). We employed the peak-area ratio of measured samples and calibration target (proportional to the elemental ratios of corresponding elements) to derive the chemical compositions of the CE-3 soils. Our APXS data processing began with level 2C data, which has undergone energy, dead-time and temperature corrections13. The four raw spectra were accumulated for 2657, s, 2778, s, 2050, s and 3627, s. We first normalized the spectral counts of all four APXS spectra to 103 seconds (Fig. 2a). The background was then removed from raw spectra to eliminate the effects of multiple scattering. The peak areas of individual elements were derived by spectral curve fitting using GRAMS software (Galactic Industries Corporation, NH, USA). A Gaussian function was used to fit the peak shape. Multiple iterations in curve fitting were conducted until convergence was reached. The resulting peak area for each element was then divided by that from the calibration target, and multiplied by the known concentration of that element in the calibration target, to obtain the nominal concentrations of elements. The concentrations of seven major elements (Mg, Al, Si, K, Ca, Ti and Fe) as oxides were then normalized to 99% to obtain the final concentration of each of these elements in a CE-3 surface sample, with the remaining 1% set for elements not measured but known to be present, including Cr2O3, MnO, Na2O and P2O5, to 0.3, 0.3, 0.3 and 0.1 wt.%, respectively (Table 1). This method has the advantage of normalization of different observation geometries and instrument effects (for example, the CE3-0006_1 test measurement also shows a relatively reasonable result compared with CE3-0006_2, although it was taken at a distance of ∼2.5 cm higher than the other three measurements). Neal et al.36 also reported derived chemical compositions of the CE-3 soils, but using instead a Fundamental Parameters Method. Their results are in general agreement with our derived composition, but differ in detail, especially for Al. A detailed analysis of the differences is in the Discussion section of this paper.
VNIS data processing and analysis
Our VNIS spectral data processing began with level 2B data, which has undergone dark current, flat-field, temperature corrections and radiometric and geometric calibration15. For each of the four locations, we averaged ∼9182 pixels spectra (450–950 nm) of the sampling area from VNIS in the image mode, then connected the averaged spectrum with a point spectrum (900–2400, nm) measured from a circular area within the imaged area (Fig. 3a). To correct the step artifacts between the two spectral ranges due to the response differences of the two detectors, a factor obtained from 900 nm of the point spectrum was used to multiply the averaged spectrum in the 450–900 nm region. We derived the single scattering albedo of the combined spectra, which is independent of the illumination geometry of the visible-NIR measurements. Based on the Hapke radiative transfer model50,51, the radiance factor was converted at the standard illumination geometry (i=30°, e=0° and α=30°) to facilitate comparison. The spectra were then smoothed using the Savitzky–Golay smoothing method52, which is a spectral smoothing algorithm that essentially performs a polynomial regression to the data points in a moving window (Fig. 3b). The spectral background (continuum) was removed using a straight line that connects the spectral points at 750 nm and 1700, nm. Mineral modes of four CE-3 soils were extracted by spectral deconvolution using the MGM (refs 19, 20, 24, 25, 26, 32; Supplementary Figs 6 and 7, Supplementary Table 6, Supplementary Note 5). The software was downloaded from the Reflectance Experiment Laboratory (http://www.planetary.brown.edu/mgm/).
How to cite this article: Ling, Z. et al. Correlated compositional and mineralogical investigations at the Chang′e-3 landing site. Nat. Commun. 6:8880 doi: 10.1038/ncomms9880 (2015).
This research was partly funded by the National Natural Science Foundation of China (U1231103, 41473065, 41373068 and 41490634), National Science and Technology Infrastructure Work Projects (2015FY210500), Natural Science Foundation of Shandong Province (JQ201511 and ZR2015DQ001) and Key Research Program of the Chinese Academy of Sciences (KGZD-EW-603). Support from the Department of Earth & Planetary Sciences and the McDonnell Center for the Space Sciences at Washington University in St Louis for B.L.J., A.W. and Z.L. is greatly appreciated. We thank Ryan Clegg-Watkins for assistance in processing the LROC NAC images, and Randy Korotev, Carle Pieters, Bin Liu and Xiaohui Fu for helpful discussions. The authors thank Mariek Schmidt and two anonymous reviewers for constructive comments, which led to significant improvements in the manuscript.
Supplementary Figures 1-7, Supplementary Tables 1-8, Supplementary Notes 1-5 and Supplementary References.
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