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Highlands rocks display a large spread in Hf and W concentrations, consistent with their variable cumulate mineralogy, the anorthosites being the most depleted (Table 1). Intense meteorite bombardment may result in brecciation and variable contamination of these samples (23). This alteration is a particular problem for the ferroan anorthosites, which have only a few parts per billion of W (Table 1). Average solar system debris is probably chondritic in terms of W isotopic composition, but the average may not be relevant to a particular sample. To minimize this problem, we selected samples with a high confidence class (cc) (40), which is an index of pristinity, with 9 being the most pristine. All four ferroan anorthosites studied have cc ≥ 8. Where possible, we have also used samples with reasonably well-preserved Sm-Nd and U-Pb systematics. Most ferroan anorthosites are thought to be early, but sample 60025 (47) is particularly important in this respect: With a Sm-Nd age of 4.44 ± 0.02 Ga (18) and a Pb-Pb age of 4.51 ± 0.01 Ga (17), it has the most reliable age of any early lunar rock. Although troctolite 76535 (cc = 9) yields a Rb-Sr age of 4.61 ± 0.07 Ga (16), some have argued that the Sm-Nd age of 4.26 ± 0.06 Ga (74) may be closer to the correct value. For the norites, we used 77215 (cc = 8), which yields a Sm-Nd age of 4.37 ± 0.07 Ga (15), and 78235 (cc = 8), with a Pb-Pb age of 4.43 ± 0.07 Ga (19); both of these norites have exceedingly high W concentrations (Table 1). The Mg-granulite 67955 is a cataclasized poikiloblastic noritic anorthosite; of all of the samples, it is the least pristine and the most likely to be contaminated with meteoritic siderophiles. Its exact age is unclear.
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1842296527
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184W = 0.927633 (43). The quoted 2σ standard errors all refer to the least significant figures. The isotope dilution measurements of Hf and W were determined simultaneously, and the reproducibility was typically 0.2% or better.
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1842331701
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note
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184W cannot be calculated.
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note
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We thank the Curation and Analysis Planning Team for Extraterrestrial Materials, NASA curatorial staff, and J. Gooding for supplying the Apollo lunar samples; H. Kojima, curator of the National Institute of Polar Research, Tokyo, for providing the lunar meteorite; and M. Garcia and C. Langmuir for supplying the terrestrial samples for this study. We thank J. N. Christensen, C. M. Hall, J. Jones, H. Palme, T. Pettke, M. Rehkämper, S. R. Taylor, and P. van Keken for comments; M. Johnson and Cetac Technologies for invaluable technical assistance; and R. M. Canup for a preprint. We acknowledge discussions with C. J. Allègre, A. G. W. Cameron, R. M. Canup, M. J. Drake, A. W. Hofmann, J. Jones, D. McKenzie, H. J. Melosh, R. K. O'Nions, D. A. Papanastassiou, D. Turcotte, G. J. Wasserburg, and B. J. Wood. This work was supported by the U.S. Department of Energy, NASA, NSF, and the University of Michigan.
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