NanoSIMS and EPMA dating of lunar zirconolite

Abstract

Zirconolite is a common Zr-rich accessary mineral in mafic rocks. It is also an ideal U–Pb/Pb–Pb chronometer because it commonly contains high U content (mostly 0.1–10 wt%) and negligible initial Pb. However, zirconolite is usually very small (e.g., ~ 1 μm in width) in lunar rocks, requiring a high spatial resolution analysis. We analyzed a single, large (25 μm × 20 μm) grain of zirconolite in lunar meteorite NWA 4485 using Pb–Pb dating by NanoSIMS and U–Th–Pb dating by EPMA. The resultant U–Th–Pb age is 4540 ± 340 Ma (2σ) with a spatial resolution of 1.3 μm. The Pb–Pb age by NanoSIMS is 4348.5 ± 4.8 Ma (2σ) with a spatial resolution of ~ 2 μm, consistent with the age of 4352 ± 10 Ma and 4344 ± 14 Ma reported in the same meteorite and its paired meteorite NWA 4472. Although U–Th–Pb age is somewhat older, it still includes the NanoSIMS results within the analytical uncertainty. This work demonstrates the potential application of the combined EPMA dating and REE analysis of lunar zirconolite, with the benefits of high spatial resolution, non-destructive, and readily accessibility of the instrument. The precision of the EPMA dating (7.6%, 2σ) can be improved by increasing the counting time for Pb, U and Th. We expect to apply this EPMA technique for a quick and non-destructive age survey and geochemical study of zirconolite grains from the lunar mare basalts newly returned by Chang’E-5 mission which landed on a very young (1.2–2.0 Ga by crater-counting chronology) basalt unit in Procellarum KREEP Terrain.

1 Introduction

Zirconolite (CaZrTi₂O₇) has been recognized as a fairly common accessory mineral first in terrestrial rocks (Williams and Giere 1996) and then in lunar basaltic rocks from Apollo 11 and 12 (Lovering and Wark 1971; Wark et al. 1973). Zirconolite usually contains high U (mostly 0.1–10 wt%) with negligible common Pb (Williams and Giere 1996), making it a potential U–Pb chronometer. Since the work by Rasmussen and Fletcher (2004), it has been demonstrated as an ideal mineral for U–Pb geochronology using sensitive high-resolution ion microprobe (SHRIMP) and secondary ion mass spectrometry (SIMS) techniques with reliable age precision (Downes et al. 2016; Norman and Nemchin 2014; Rasmussen et al. 20082009; Wu et al. 2010; Zhang et al. 2010). Meanwhile, the in situ U–Pb geochronology of zirconolite has also demonstrated that it yields Pb–Pb ages that are more precise than those obtained from coexisting zircon and baddeleyite (Rasmussen and Fletcher 2004).

Lunar zirconolite was commonly reported as a ubiquitous trace mineral in the late stage mesostasis of lunar mare basalt (Day et al. 2006; Rasmussen et al. 2008; Wark et al. 1973; Zeigler et al. 2005). It usually contains lower U and Th contents than terrestrial zirconolite and therefore less degree of metamictization and Pb-loss caused by alpha-decay damage. However, most lunar zirconolite grains are always fine-grained or elongated “strings”, ranging in shapes from laths to tubular rods (Rasmussen et al. 2008; Seddio et al. 2013). They rarely grow up to 10 μm in size and frequently appear as needle-like strings with length up to tens of μm but width less than 2 μm (Rasmussen and Fletcher 2004; Seddio et al. 2013). This typical morphology of zirconolite makes most occurrences too small for traditional analyses like SIMS or SHRIMP dating. Therefore, higher lateral resolution secondary ion spectrometer like CAMECA NanoSIMS 50L is more appropriate for small size zirconolite dating, which can recently achieve the submicron spatial resolution for Pb–Pb dating but with significant depth effect after equipped with the new radio-frequency iron source (Hao et al. 2021).

For traditional ion microprobes, such as SIMS, SHRIMP, and NanoSIMS, their major disadvantage is that they are destructive for zirconolite grains when analyzing. In addition, only limited elements or isotopes concentrations can be acquired at once by ion microprobes due to their limited detectors. For precious lunar sample, such as the recently returned Chang’E-5 lunar soil, damage-free and more effective dating method like EPMA U–Th–Pb chemical dating coupled with REE measurements is very useful for a quick prelude dating survey before destructive analyses. Regarding EPMA chemical dating, it was first published in Bowles (1990) and used on uraninite (UO₂), and then developed for use on other U-bearing minerals, such as monazite, zircon, and xenotime in Suzuki and Adachi (1991a, b). Later, numerous publications have demonstrated its usage in both terrestrial and lunar rocks, and analytical techniques to obtain the best result were also presented in these studies (Bowles 2015; Chatterjee et al. 2017; Cocherie and Legendre 2007; Cross et al. 2011; Downes et al. 2016; Hazarika et al. 2017; Montel et al. 1996; Pyle et al. 2005; Seddio et al. 2014, 2013; Suzuki et al. 1994; Yonemura et al. 2013). Among these work, several studies have tried to apply EPMA chemical dating to zirconolite, such as: Rajesh et al. (2006) reported EPMA dating of zirconolite from terrestrial samples, assuming that all Pb analyzed are radiogenic; Seddio et al. (2013) used EPMA to date the zirconolite from Apollo 12,032 granite. Although the accuracy of the EPMA dating is considered poor compared to the isotopic ages, its potential superior spatial resolution up to 1 μm, good integrating of minor elements and age information, non-destructive, and easier access of the facility, make EPMA chemical dating a complementary technique to SIMS dating (Hazarika et al. 2017; Montel et al. 1996).

To verify the reliability of EPMA dating of lunar zirconolite, a KREEP-rich lunar meteorite NWA 4485 (Arai et al. 2009) was used for study, which is a polymict regolith breccia and paired with NWA 4472 (Joy et al. 2011). Consistent with its high KREEP contents, there are many Zr-rich minerals including zircon, baddeleyite, and zirconolite that are suitable for dating measurements in NWA 4485. A single, large (25 μm × 20 μm) grain of zirconolite was found and analyzed using Pb–Pb dating by NanoSIMS and U–Th–Pb dating by EPMA, and then the result of chemical age is compared with that of Pb–Pb isotope age.

2 Methods

A polished section (1.2 × 1 cm²) of NWA 4485 was prepared from a chip of the meteorite, and it was carbon coated. The section was observed in backscatter electron (BSE) images using a field emission scanning electron microscope NOVA NANOSEM450 equipped with a Gatan cathodoluminescence (CL) detector at Institute of Geology and Geophysics, Chinese Academy of Sciences (IGGCAS). The operating conditions were 15 kV accelerating voltage and 3.2 nA beam current. Quantitative analysis of zirconolite was determined using a Cameca SXFiveFE electron probe microanalyzer (EPMA) equipped with wavelength-dispersive X-ray spectrometers (WDS) at IGGCAS. The accelerating voltage of 20 kV and a beam current of 70 nA (~ 1 μm in diameter) were used. During data acquisition, peak counting time for each element is the same as their background counting time: Ca (K_α, 10 s), Ti (K_α, 10 s), Fe (K_α, 20 s), Y(L_α, 20 s), Zr (L_α, 20 s); Mg (K_α, 30 s), Al (K_α, 30 s), Si (K_α, 30 s), La (L_α, 30 s), Ce (L_α, 30 s), Nd (L_α, 30 s), Sm (L_β, 30 s), Gd (L_α, 30 s), Pb (M_α, 30 s), Th (M_α, 100 s), and U (M_β, 100 s). Additionally, Pb, Th, and U lines are all measured on LPET crystals. Overlapping correction method was used for interference correction according to the method reported by Pyle et al. (2005). Corrections for the interference of YL_γ2,3 on PbM_α, SmL_β7 on UM_β, and ThM_ζ1 on PbM_α were precisely carried out. Due to the small correction factor of PbM_α/ThM_ζ1 and low Th concentration in NWA 4485 zirconolite, the interference of ThM_ζ1 on PbM_α was too small to affect the Pb concentration and can be negligible. The full range WDS spectra acquired with TAP, LPEP, and LiF diffractors are shown in Additional file 1: Fig. S1. The standard materials used for U, Th were both synthesized glasses: 7.40 wt% Al, 27.25 wt% Si, 15.76 wt% Ca, 5.18 wt% Th, and 44.63 wt% O for Th; 7.42 wt% Al, 27.52 wt% Si, 16.07 wt% Ca, 3.85 wt% U, and 44.90 wt% O for U. Natural crocoite (PbCrO₄) was used as Pb standard material. Other synthetic and natural standards were periclase (MgO) for Mg, corundum (Al₂O₃) for Al, wollastonite (CaSiO₃) for Si and Ca, rutile (TiO₂) for Ti, hematite (Fe₂O₃) for Fe, yttrium aluminum garnet (Y₃Al₅O₁₂) for Y, and 10% REE Si–Al–Ca–O glasses for La, Ce, Nd, Sm and Gd, respectively. Detection limits are 30–50 ppm for Mg, Al, Si, Ca and Ti, 70–90 ppm for Fe, Th and U, 110–120 ppm for Y and Gd, 130 ppm for Pb, 220 ppm for Zr, 150–170 ppm for La, Ce and Nd, 300 ppm for Sm. The Phi-Rho-Z matrix correction were applied for all data (Merlet 1994). In addition, Monte Carlo simulation of electron scattering in zirconolite was generated using Casino (Drouin et al. 2007) at accelerating voltage of 20 kV. The density of zirconolite is defined as 4.8 g/cm³. 1 × 10⁴ electron trajectories were calculated and used for displaying images. The resultant spatial resolution for our EPMA analyses is shown in Additional file 1: Fig. S2. We acquired the smallest interaction volume of electrons and generation volume of X-rays of 1.3 μm diameter when the focused beam size is used. The corresponding YZ energy distribution shows 95% of energy are distributed less than 1.5 μm in depth.

Following the method of Montel et al. (1996) for monazite, we calculated the chemical age of zirconolite, assuming that all the Pb is radiogenic. This assumption is verified by the negligible Pb²⁰⁴/Pb²⁰⁶ ratio in our NanoSIMS analyses in Sect. 3.3. Given this assumption, the amount of Pb produced is the sum of the Pb from the decay of both U and Th:

$$\begin{aligned} {\text{Pb}} &= \frac{Th}{{232}}\left( {e^{{^{232} t}} - 1} \right)208 + 0.9928\frac{U}{238.04}\left( {e^{{^{238} t}} - 1} \right)206 \\ &\quad+ \,0.0072\frac{U}{238.04}\left( {e^{{^{235} t}} - 1} \right)207\end{aligned}$$

where Pb, Th, U are in ppm, and λ²³² (4.9475 × 10^–11 year⁻¹; Steiger and Jäger 1977), λ²³⁵ (9.8485 × 10^–10 year⁻¹; Steiger and Jäger 1977), and λ²³⁸ (1.55125 × 10^–10 year⁻¹; Steiger and Jäger 1977) are the radioactive decay constants for ²³²Th, ²³⁵U and ²³⁸U, respectively.

Because of the lack of zirconolite references, the fractionation between U and Pb during the SIMS analysis cannot be calibrated. Instead, since the instrumental mass fractionation (IMF) of Pb isotopes is negligible (Yang et al. 2012), Pb–Pb ages of the zirconolite can be measured without U–Pb calibration. Therefore, Pb–Pb dating was carried out on the same zirconolite grain by a CAMECA NanoSIMS 50L at IGGCAS, following the method for Pb–Pb dating (Yang et al. 2012). The O⁻ primary beam was accelerated at 16 kV with a current of ~ 500 pA and a beam size of ~ 1.7 μm in diameter. In order to achieve the maximum spatial resolution, the scanning off mode was used (Yang et al. 2012). Magnetic peak-switching mode was applied for the Pb–Pb dating, and four magnetic fields were used in the following sequence: B1 for Pb background (203.5), B2 for ²⁰⁴Pb, B3 for ⁹⁶Zr, ²⁰⁶Pb, ²³⁸U, ²³²Th¹⁶O, ²³⁸U¹⁶O₂, and B4 for ⁸⁹Y and ²⁰⁷Pb, among which lead background (203.5) and Pb isotopes (²⁰⁴Pb, ²⁰⁶Pb, ²⁰⁷Pb) were measured with the same EM#4 detector. Before data acquisition, the sample surface was pre-sputtered by rastering the beam over 3 × 3 μm² area for 3 min in order to remove the surface contamination of terrestrial common Pb. M257 zircon (²⁰⁶Pb/²³⁸U age = 561.3 Ma) and Phalaborwa baddeleyite (²⁰⁷Pb/²⁰⁶Pb age = 2059.6 Ma) references (Yang et al. 2012) were measured to assess the potential drift of the instrument during the analytical session. Measured ²⁰⁴Pb/²⁰⁶Pb ratios were used for the correction of common Pb based on the two-stage evolution model of Stacey and Kramers (1975). Uncertainties of individual analysis are reported at 1 sigma level. Weighted average Pb–Pb age was processed using Isoplot program (Ludwig 2003) and quoted at 2 sigma level.

3 Results

3.1 Occurrence of zirconolite

Zirconolite is an accessory mineral in NWA 4485. It appears as light gray and is less reflective than ilmenite and troilite, but more reflective than zircon under reflected light microscope. A relatively large grain of zirconolite (25 μm × 20 μm in size) was identified as a mineral fragment in the regolith matrix of NWA 4485 (Fig. 1), surrounded by pyroxene, plagioclase and silicate melts (Fig. 1a). SEM and CL images of the zirconolite grain (Fig. 1b, c) revealed no compositional zoning or other internal features.

Fig. 1

The occurrence of zirconolite grain from NWA 4485. a BSE image of the zirconolite grain, occurring as a mineral fragment in matrix of the lunar regolith breccia. This grain is surrounded by plagioclase (Pl), pyroxene (Px), and silicate melts (Melt). b Contrast-enhanced backscattered image of the grain, showing a homogeneous composition. c The grain is dark in CL image, showing no trace elements heterogeneity or dislocation

3.2 EPMA quantitative analysis of zirconolite

Major and minor composition of zirconolite Five EPMA analyses were carried out on the zirconolite grain. The quantitative analyses do not show significant variation from the core to the rim, confirming the homogeneous BSE and CL images. The EPMA results and the formulas of cations calculated based on 7 atoms of oxygen are given in Table 1. It contains 36.4 wt% ZrO₂, 35.0 wt% TiO₂, 7.90 wt% CaO, 5.80 wt% FeO, within the range of other zirconolite grains reported from lunar samples (Norman and Nemchin 2014; Rasmussen et al. 2008; Seddio et al. 2013) and terrestrial mafic igneous intrusions (Giere et al. 1998; Williams and Giere 1996). The U, Th, and Pb average concentrations of this grain were 0.21 ± 0.01 wt%, 0.56 ± 0.01 wt%, and 0.43 ± 0.02 wt%, respectively. In addition, the concentrations of five REEs (La, Ce, Nd, Sm, Gd) and Y in the zirconolite were measured. Europium was below the detection limit (0.02 wt%) in all analysis, which resulted in a negative Eu anomaly (Fig. 2). The CI-normalized REEs and Y pattern is plotted in Fig. 2, with Y locating between Ho and Er (Korotev 1996; Seddio et al. 2013). LREE concentrations are relatively lower than those of middle-REE, increasing from 3800 × CI for La to 33,000 × CI for Gd. The CI-normalized Y concentration (22,500 × CI) is slightly lower than that of Gd. The chondrite-normalized REE pattern of zirconolite in NWA 4485 is characteristically convex and parallel to those of Apollo lunar zirconolites (Fig. 2) which show strong enrichment of REE (La 3834 × CI, Y 22,500 × CI) in Apollo 10,047 (Rasmussen et al. 2008). The other minor elements are MgO (0.44 wt%), Al₂O₃ (0.52 wt%) and SiO₂ (0.16 wt%). Low analysis totals reflect the presence of other elements probably including Nb, Ta, and HREEs.

Table 1 EPMA analyses of the zirconolite grain from NWA 4485, in wt%

Fig. 2

Chondrite-normalized REE pattern of zirconolite from NWA 4485. It is compared with Apollo lunar zirconolites (Norman and Nemchin 2014; Rasmussen et al. 2008; Seddio et al. 2013) and terrestrial grains from tholeiites (Rasmussen et al. 2008) and carbonatites (Wu et al. 2010). The Eu composition in our grain is predicted to be lower than 100 × CI based on Apollo lunar zirconolite studies

EPMA Chemical dating of zirconolite Following the method of Montel et al. (1996), we calculated the chemical ages for the zirconolite EPMA analyses using their Th, U, and Pb concentrations listed in Table 1. Five analyses yield a weighted mean age of 4540 ± 340 Ma (2σ) with mean square weighted deviation (MSWD) = 0.17 and probability = 0.96 (Fig. 3).

Fig. 3

Weighted mean U–Th–Pb EPMA chemical ages of zirconolite in NWA 4485

3.3 NanoSIMS Pb–Pb dating

We carried out two NanoSIMS Pb–Pb analyses on the zirconolite grain and the results are listed in Table 2. It shows that the zirconolite contains minimal common Pb with measured ²⁰⁴Pb/²⁰⁶Pb ratios less than 10^–5 (f₂₀₆ < 10^–6). The analytical uncertainty is rather small (3.4 Ma, 1σ), and both analyses are the same within the analytical uncertainty. The weighted mean Pb–Pb age is 4348.5 ± 4.8 Ma (2σ) with a mean square weighted deviation (MSWD) = 0.70 and probability = 0.40.

Table 2 Pb isotopic data of zirconolite in NWA 4485 obtained by NanoSIMS

4 Discussion

4.1 Accuracy and uncertainty of EPMA dating

Zirconolite is a common accessary mineral phase, characterized by a large variation of chemical composition even for major elements (Zr, Ca, and Ti) due to extensive substitutions under different formation conditions (Giere et al. 1998; Hurai et al. 2018; Norman and Nemchin 2014; Rasmussen et al. 2008; Seddio et al. 2013; Williams et al. 2001; Williams and Giere 1996). For U and Th, they mainly substitute Zr to a concentration level which can be estimated by EPMA analyses. According to the U, Th, and Pb composition reported in previous literatures and our study, it is evidenced that zirconolite is a good candidate for EPMA chemical dating.

Generally, our EPMA chemical U–Th–Pb age of 4540 ± 340 Ma (2σ) is somewhat older than that of NanoSIMS Pb–Pb age of 4348.5 ± 4.8 Ma, but still includes the NanoSIMS result within the analytical uncertainty. The upper limit of chemical age is higher than the age of the Moon, making it meaningless. Its lower limit includes the Pb–Pb age result, making it an acceptable result but with poor accuracy. As for analytical uncertainty, the 2σ relative deviation of chemical age is 7.6%, which is consistent with 7.2% of Apollo zirconolite chemical age reported by Seddio et al. (2013), but significantly poor than 2.3% in Rajesh et al. (2006). This is mainly because the terrestrial zirconolites in Rajesh et al. (2006) contain extremely high contents of UO₂ (6.51–9.64 wt%), ThO₂ (3.43–4.05 wt%) and PbO (0.50–0.72 wt%), leading to low instrumental counting statistics error. Thus, in order to increase age precision for zirconolite with low UO₂, ThO₂, and PbO, extend of peak counting time to improve the statistics for these elements is of great significance. Regarding the poor accuracy of chemical age, an increase of 0.03 wt% in the U or a decrease of 0.03 wt% in the Pb would be enough to make the EPMA date correspond to the NanoSIMS date. However, both 0.03 wt% for U and 0.03 wt% for Pb are larger than the 2σ standard deviation for five analyses. This indicates that there is a small systematic deviation for our EPMA analyses compared with the NanoSIMS Pb–Pb dating, resulting the higher U–Th–Pb chemical age for zirconolite. In order to eliminate this systematic deviation, more elements selected for analyses such as HREEs, Hf, and Nb are necessary to make the total content closer to 100 wt%. More careful elements interference correction for these unselected elements with high concentration on U, Th and Pb, such as the potential interference of HoL₁ on ThM_α, HoL_α on UM_β, need to be considered and corrected in future lunar samples analyses. In addition, the possible effects of primary and secondary florescence of neighboring phases might also be a potential factor for the poor accuracy. In our work, the neighboring phases of zirconolite are all silicates or silicate melts with negligible K concentration. The 0.16 wt% SiO₂ contents of our analyses are low and within the range of SiO₂ composition for lunar zirconolite (up to 1.9 wt% but most less than 0.3 wt%; Williams and Giere 1996). Therefore, there are little florescence effects and negligible KK_α interference on UM_β from neighboring phases in our analyses.

For zirconolite with younger ages, their Pb concentration depends both on its U, Th concentrations and on their ages. Due to low initial content of Pb for zirconolite, most contribution of Pb comes from the decay of U and Th. Therefore, crystallizing from high U, Th concentration magma melts can also lead to high radiogenic Pb content even with younger ages. As zirconolite from Apollo 12 sample 12,032 granite fragment reported in Seddio et al. (2013), it contains higher U, Th, and Pb concentrations than our zirconolite from NWA 4485 even with younger age of 3.9 ± 0.3 Ga. Therefore, for lunar zirconolite with younger ages, crystallized from a U, Th -rich source region, such as PKT area, will also make it a potential candidate for EPMA chemical dating.

4.2 Accuracy and uncertainty of NanoSIMS Pb–Pb dating

In contrast, due to the high contents of Pb and U compared with zircon and baddeleyite, the NanoSIMS Pb–Pb age of zirconolite has a remarkable precision of 0.11%, showing that zirconolite is an ideal mineral phase for isotopic Pb–Pb dating. The weighted average age of 4348.5 ± 4.8 Ma (2σ) is consistent with the age of 4352 ± 10 Ma of NWA 4485 in Arai et al. (2010) and 4344 ± 14 Ma reported of its paired meteorite NWA 4472 in Joy et al. (2011). In addition, the negligible common Pb in zirconolite measured by NanoSIMS confirmed the assumption that all Pb is radiogenic in zirconolite. The NanoSIMS analysis on zirconolite demonstrated that it can be used to date ancient rocks using a very small ion beam with a high precision of few million years in ²⁰⁷Pb/²⁰⁶Pb ratios superior to that of the coexisting zircon and baddeleyite.

4.3 REE pattern of zirconolite

Lunar zirconolite crystallized at a late stage from interstitial in the lunar basalts (Busche et al. 1972) and is an accessory mineral able to accommodate many incompatible elements, such as REE, U, Th Zr, Hf, like zircon. As such, it has the potential for playing a significant role in the petrological/geochemical evolution of these rock-types in which it crystallized. For example, several studies have provided evidence that zirconolite can reflect changes in the composition of the fluid during its evolutionary history, both in metasomatic system (Williams and Giere 1988, 1996), and in magmatic fractional process (Platt et al. 1987). For our analyses, the REE pattern shown in Fig. 3 displays apparent negative Eu anomaly, which indicates that this zirconolite grain formed after plagioclase as plagioclase is the main sink of Eu due to Eu²⁺ substitution for Ca²⁺ during crystallization.

5 Implication

Our result demonstrates the reliability and potential of EPMA U–Th–Pb dating of lunar zirconolite, which is a non-destructive, quick, and high-spatial resolution technique. In addition, zirconolite contains high Pb, U and Th, and it was commonly reported as a ubiquitous trace mineral especially in lunar KREEPy basalts (Day et al. 2006; Lovering and Wark 1971; Rasmussen et al. 2008; Wark et al. 1973; Zeigler et al. 2005; Zhang et al. 2010). The recently returned Chang’E-5 samples are expected to be young mare basalt with the age of 1.2–2.2 Ga and rich in KREEP component (Hiesinger et al. 2010; Qian et al. 2018; Zhao et al. 2017). Therefore, the development of EPMA U–Th–Pb dating is appropriate for a quick prelude dating survey of the new lunar sample with no sample damage, and also for zirconolite grains less than 2 μm which are too small for SIMS. Besides, the simultaneously acquired REE data can also help to study the geochemical evolution of the Chang’E-5 rock in which it crystallized.