PMC

a, Backscattered electron image of Chang’e-5 basalt clast 041GP, 001. Cpx, clinopyroxene; Ilm, ilmenite; Pig, pigeonite; Pl, plagioclase; Ol, olivine; Spl, Spinel; Tro, troilite. b, Mg# versus TiO₂ diagram of the Chang’e-5 basalt clasts. The Apollo and Luna data are from Clive Neal’s Mare Basalt Database (https://www3.nd.edu/~cneal/Lunar-L/). c, Quadrilateral diagram of pyroxene in the Chang’e-5 basalt clasts. Temperature contours calculated at 0.5 GPa are shown, where 0.5 GPa was chosen according to the possible pressure range for lunar low-Ti basalts. The Apollo 12 samples are plotted (grey area) for comparison. Di, diopside; En, enstatite; Fs, ferrosilite; Hd, hedenbergite. d, Comparison of olivine compositions in Chang’e-5 basalts with those within the Apollo 12 and Apollo 15 basalts. The data for pyroxene and olivine are provided in Supplementary Table .

(a) CI chondrite normalised HSE data for the lunar basalt La Paz 02225,13 () compared with data for Parana basalt KS624 from Brazil (). With the exception of Re, the patterns for these two basalts are quite similar for such low HSE abundance rocks, suggesting similar partitioning of HSE between mantle and basaltic melt for both the Earth and Moon. (b) Data for additional lunar (coloured symbols) and terrestrial basalts (black symbols) show both similarities and differences. Lunar basalts plot systematically lower than terrestrial basalts by more than a factor of 20. Green, orange and blue symbols are from Apollo 15 and 17 landing sites, and the La Paz meteorites, respectively. Lunar basalt data are from . Terrestrial basalt data are from .

UCS estimation data derived from the equation obtained by Yilmaz. & Goktan. BES Scoriaceous basalt, BAFV Vesicular aphanitic basalt, BOPM Massive pyrogenic olivine basalt, BPLM Massive plagioclassic basalt, FON Phonolite, IGNS Unwelded ignimbrite, TRQ Trachyte, IGS Welded ignimbrite, TRQB Trachybasalt (Modified from).

Light noble gas abundances and isotopic ratios measured in basalt 15016. Yellow stars refer to error‐weighted mean isotopic compositions of the crushing series. Letters in circles indicate the crushing steps reported in Tables and . Numbers correspond to the heating steps given in Table S3 and S5. a) Neon isotopic composition of lunar basalt 15016 gases extracted by crushing (sample LS, green circle) and by CO ₂ laser heating (red [2.629 mg] and light pink [5.909 mg] squares). Pure solar cosmic ray (SCR) range of values (blue area) based on basalt 15016 chemistry (Meyer ) and Trappitsch and Leya ( ) model: ²⁰Ne/²²Ne = (1.04–2.27), ²¹Ne/²²Ne = (0.61–0.72). ATM: Terrestrial atmosphere (Ozima and Podosek ), ²⁰Ne/²²Ne = 9.8, ²¹Ne/²²Ne = 0.029. GCR: Calculated pure galactic cosmic ray endmember (Leya et al. ) based on sample chemistry (Meyer ), ²⁰Ne/²²Ne = 0.83, ²¹Ne/²²Ne = 0.875. Error bars are 2σ. b) Argon isotopic composition of lunar basalt 15016 gases extracted by crushing (green circles for sample LS, diamonds and hexagons for sample LP and LR, respectively) and by CO ₂ laser heating (red [2.629 mg] and light pink [5.909 mg] squares). Pure solar cosmic ray (SCR) range of values (blue area) based on basalt 15016 chemistry (Meyer ) and Trappitsch and Leya ( ) model: ⁴⁰Ar/³⁶Ar = 0, ³⁸Ar/³⁶Ar = (0.91–2.24). ATM = terrestrial atmosphere (Lee et al. ), ⁴⁰Ar/³⁶Ar = 298.56, ³⁸Ar/³⁶Ar = 0.1885. GCR = pure galactic cosmic ray endmember (Hohenberg et al. ), ⁴⁰Ar/³⁶Ar = 0, ³⁸Ar/³⁶Ar = 1.52. Error bars are 2σ. c) Fraction of ²²Ne and ³⁶Ar gradually released over the crushing steps (in percentage). Values are given in Tables .