Carbonaceous chondrites (CCs) exhibit profound non-systematic heterogeneity in their elemental and isotopic compositions, both within individual meteorite splits and among bulk samples of the same group, providing opportunities for a better understanding of early solar system processes. This variability also poses significant challenges for constraining bulk compositions of the parent bodies. We report new mass-independent Ti and Cr isotope data, integrated with major and trace element abundances for a suite of CC bulk rocks, to better understand the origin of this multiscale heterogeneity. Some bulk CCs (e.g., Yamato chondrites and Allende) exhibit elemental or isotopic compositions consistent with the literature, while others display significant differences.Simple binary or ternary mixtures, using ε50Ti, ε54Cr and chemical data from the present study and literature as constraints, cannot reproduce the full range of isotopic and elemental data. The data are best explained by a multi-component mixing model with a minimum of four endmembers, involving CI-like matrix, heterogeneous non-carbonaceous (NC) dust, and two distinct refractory inclusion populations. The latter are similar to the average composition of calcium-aluminium-rich inclusions (CAIs) and amoeboid olivine aggregates (AOAs) and a CAI-like component found in some chondrules. Crucially, the model constraints reveal that NC dust, which migrated into the CC region, contained chemically fractionated material, characterized by a significant depletion in siderophile elements. This result suggests that some NC dust in CC may represent silicate-rich debris derived from the collision of early differentiated planetesimals in the inner solar system. Thus, carbonaceous chondrites record a multi-stage history of early transport of variably 50Ti- and 54Cr-enriched CAIs and subsequent migration of chondritic and differentiated planetary debris into CI chondrite-like icy dust of the outer disk.

A multi‐element isotope (N, O, Ti, and Cr) study was conducted on C1 and CM‐like clasts hosted in achondrites and chondrite breccias to understand the genesis of these chondritic clasts. The mineralogy, O, and N isotopes confirm that CM‐like clasts in howardites and polymict eucrites closely resemble CM chondrite‐like material. The O and Cr isotope composition of C1 clasts in CR chondrites overlaps with those of CR chondrites, implying either formation in a similar nebular environment or resemblance to local CR material that underwent more extensive in situ alteration. Notably, these clasts are less enriched in 15 N than bulk CR chondrites. In contrast, C1 clasts in ureilites are enriched in 15 N relative to the Earth's atmosphere by ~100‰ setting them apart from any other known solar system material. They display elevated 17 O and 18 O values and lie along the CCAM line. In addition, a C1 clast from an ureilite represents the most 54 Cr‐enriched and 50 Ti‐depleted endmember among the carbonaceous chondrites. Altogether, these isotopic characteristics suggest that C1 clasts in ureilites represent material not sampled by any known meteorite group. Overall, this study highlights the presence of primitive, isotopically distinct materials in the early outer solar system, some of which were transported to the inner solar system to the accretion region of the host parent bodies.

In the last decade, several studies have reported enrichments of the heavy isotopes of moderately volatile elements in lunar mare basalts. However, the mechanisms controlling the isotope fractionation are still debated and may differ for elements with variable geochemical behaviour. Here, we present a new comprehensive dataset of mass-dependent copper isotope compositions (delta 65Cu) of 30 mare basalts sampled during the Apollo missions. The new delta 65Cu data range from +0.14 %o to +1.28 %o (with the exception of two samples at 0.01 %o and -1.42 %o), significantly heavier than chondrites and the bulk silicate Earth. A comparison with mass fractions of major and trace elements and thermodynamic constraints reveals that Cu isotopic variations within different mare basalt suites are mostly unrelated to fractional crystallisation of silicates or oxides and late-stage magmatic degassing. Instead, we propose that the delta 65Cu average of each suite is representative of the composition of its respective mantle source. The observed differences across geographically and temporally distinct mare basalt suites, suggest that this variation relates to large-scale processes that formed isotopically distinct mantle sources. Based on a Cu isotope fractionation model during metal melt saturation in crystal mush zones of the lunar magma ocean, we propose that distinct delta 65Cu compositions and Cu abundances of mare basalt mantle sources reflect local metal melt-silicate melt equilibration and trapping of metal in mantle cumulates during lunar magma ocean solidification. Differences in delta 65Cu and mass fractions and ratios of siderophile elements between low- and high-Ti mare basalt sources reflect the evolving compositions of both metal and silicate melt during the late cooling stages of the lunar magma ocean.

Moderately volatile trace elements (MVE) such as Cu are emitted in large quantities from volcanoes on Earth and are tracers and are important for volatility related processes on other planetary bodies such as the Moon. The evaporation of MVE from silicate melts is complex, as evaporation rates change with temperature, oxygen fugacity, and may also be influenced by the presence of ligand-forming elements such as S. While on Earth, MVE evaporation and their ligands can be evaluated by in situ sampling at volcanic vents and fumaroles, this is not possible on the Moon. Isotopic investigations of Apollo lunar picritic glasses provide evidence for evaporation and condensation processes on the lunar surface. Unlike Earth's oxidized volcanic activity, evidence suggests that ancient lunar volcanism was more reduced. To study the effect of temperature, oxygen fugacity, and the influence of S on the degassing of Cu from silicate melts, we conducted experiments at 1150-1500 degrees C and different oxygen fugacities (logfO2) ranging from strongly oxidizing conditions (i.e., in air) to reducing conditions that correspond to a fO2 that is 6 log units lower than the Fayalite-Magnetite-Quartz buffer (FMQ). Experimental results show an increase of Cu volatility associated with strong isotopic fractionation with increasing temperature, and with increasingly reducing conditions for all starting materials. We also observe that the temperature and redox conditions have a competing effect on Cu evaporation and isotopic fractionation. In S-bearing systems, Cu content decreases together with increasing isotopic composition as the conditions become more reducing. The isotopic fractionation becomes less pronounced as the temperature increases from 1200 to 1500 degrees C while the Cu content continues to drastically decrease. As such, we observe a lower depletion in Cu content but a stronger enrichment of 65Cu in the residue at 1200 and 1300 degrees C compared to 1400 and 1500 degrees C, and a negative correlation between Cu content and delta 65Cu under the most reducing conditions. We relate this to the behavior of Cu isotopes that are more fractionated in presence of S in the melt, and to Cu being more volatile than S under reducing conditions. We report alpha fractionation factors in the CuS system increasing from 0.9973 in oxidizing conditions to 0.9997 at high temperatures and reducing conditions (1400-1500 degrees C, Delta FMQ -2 to -6). These results suggest that the presence of the ligand-forming element S strongly influences Cu degassing at low temperatures and under oxidizing environments, such as terrestrial fumaroles. Its influence is more limited during degassing of hot magmas and under more reducing conditions, such as on the Moon. In agreement with these observations, we report lower Gibbs-free energies of formation for CuO compared to CuS, implying that less energy is required for Cu evaporation in the presence of S. Therefore, Cu evaporation and related isotopic fractionation under isothermal conditions is expected to be higher in S-dominated systems compared to S free experimental systems. This conclusion is in contrast with Heck et al. (2025) and highlights the significant role of Fe in stabilizing FeS molecules in the silicate melt.

Introduction: Because of early recurring impacts and later impact gardening, lunar crust surface turned into a layer of fragmented, variably shocked and occasionally melted impact breccias [Heiken et al., 199; White et al., 2020].One of the most severely affected group of rocks found on the lunar surface is the Mg-suite group. These are Mg-rich, primitive, plutonic to hypabyssal coarse-grained rocks which texture and bulk composition reflect magmatic accumulation of mineral phases [Heiken et al., 1991; White et al., 2020; Shearer et al., 2015; Černok et al., 2020].Whether the Mg-suite rocks formed by partial melting of the lunar mantle or they are impact-related is still debated [Taylor et al., 1993]. In the latter case, their origin could be related to the melting of early lunar crust and mantle caused by frequent hypervelocity impacts [Jolliff et al., 2006]. Some of their minerals, like Fe-Ni metals and sulfides, reflect mixing and melting of impactor(s) and target rocks and the proportion of impactor vs. target contributions [Tang et al., 2023; Day et al., 2020]. For example, a high Ni/Co ratio in Fe-Ni metal grains can be the consequence of the addition of either iron or chondritic impactors. Furthermore, those same minerals are extremely sensitive to processes that happened in Moon’s interior, such as fractional crystallization [Day et al., 2020]. For example, Ni/Co ratio decreases when mineral phases like pyroxene and plagioclase crystallize together because of the different compatibility of Ni and Co in both solid and melt.For these reasons, those minerals cannot only be considered important means to investigate lunar rocks origin, but also lunar evolution processes [Day et al., 2020]. In this study we concentrate on defining the mineral chemistry of Fe-Ni metal and sulfide grains in a set of variably shocked breccias from three different Apollo missions (15, 16 and 17). Figure 1. Fe-Ni metal grain in thin section 78235,38, BSE image Samples: Three different shocked breccia samples were selected from Apollo 15, 16 and 17 collections: shocked norite 78235 (thin sections 78235,38 and 78235,51), mainly consisting of glass veins and cumulus and partially fractured orthopyroxene and plagioclase, with much of the plagioclase converted into maskelynite [Meyer, 2010]; dimict breccia with shocked norite 15455 (thin sections 15455,27 and 15455,28), primarily made of fragmented orthopyroxene and plagioclase in a KREEP-rich, fine-grained igneous-textured groundmass containing plagioclase, olivine and pink spinel clasts [Meyer, 2010]; feldspathic polymict breccia 67915, showing two-main polymict lithologies, one white and one grey, containing heterogeneous lithic clasts cemented in shock-melted glass (thin sections 67915,76 and 67915,84) [Meyer, 2010].Methods: Non-destructive chemical analysis were performed at the Institute of Geological Sciences at the Freie Universität Berlin (Germany) using a JEOL JXA 8200 Superprobe on minerals selected with the help of QEMSCAN maps and BSE images. In both metals and sulfides we analyzed the concentration of siderophile (Fe, Ni, Co, Mn), chalcophile (S, Zn, Cu) and some lithophile elements (such as Ca, Mg, Si, Cr, P, used to evaluate possible interference by surrounding silicates). For all the elements detection limits lie between 100 and 200 ppm, while the beam size was usually 1 μm. Figure 2. Sulfide and Fe-Ni metal grains in thin section 78235,51, BSE image Initial results: In total, more than 150 grains were analyzed in four different thin sections, but most of them were very small (6700). Different is in 78235,38, where all metal grains plot within a small range of values (Ni/Co from ~0.7 to ~0.8, Fe/Ni from ~41.8 to ~48.7), while sulfide grains generally show a higher Ni/Co (from ~1.4 to ~3.1) and Fe/Ni (from ~1600 to >6800).In sample 15455 most of the selected grains were found in the impact melt, but are usually 4700 for pyroxenes, from ~9.3 to >4700 for plagioclase) compared to sulfides in 78235. In sample 67915 chemical analysis are yet to be performed.Preliminary conclusions: The calculated Ni/Co and Fe/Ni from the investigated Fe-Ni metals in differently shocked Apollo Mg-suite samples indicate that at least some are of possible impact-related origin. Fe-Ni metal grains within glass veins in sample 78235 and matrix in sample 15455 usually show Ni/Co ~20, compatible with possible iron meteorite contamination, as shown by Day et al (2020) and McCallum and Mathez (1975). FeNi metal grains belonging to other mineral assemblages have lower Ni/Co, usually ≤1, which is more compatible to an endogenous origin [Day et al., 2020]. This is also evident in sulfides, were a Ni/Co ratio that varies between ~0.3 and ~5 suggest a more endogenous origin. Fe/Ni values in Fe-Fe-Ni metals are mostly compatible with kamacite metal (>92% Fe,

Material that accreted after planetary core formation may have influenced the composition (e.g., availability of volatiles like H, C, S) and later evolution of the terrestrial planets. Central questions are: Was the accreted material similar to known solar system objects like the meteorites in our collections? Was it rich or poor in volatile components? When was the material accreted and can we relate impactite compositions to specific impact events and/or basins?Lunar impact basins and ancient impactites provide a valuable record of late accretion, starting from the formation of a solid crust until the onset of mare volcanism (~4.4 to ~3.6 Ga). However, the origin of variably fractionated HSE patterns in different impact breccia lithologies and at landing sites is still debated [1-10]. Here we discuss all available data on highly siderophile element (HSE) abundances and 187Os/188Os ratios in lunar impactites. The current dataset comprises a variety of impact lithologies from different Apollo landing sites and a few lunar meteorites. A compilation of all data reveals that impactites from different landing sites often form clusters that together define a broadly linear correlation of 187Os/188Os ratios (as a long-term measure of the Re/Os ratio) and HSE/Ir ratios, which range from sub- to suprachondritic. The compositional range was interpreted to either reflect signatures of compositionally distinct basin forming primitive impactors, some of them outside the range of known chondrites [1, 2, 4, 5] or to result from variable mixing of several ancient impactor compositions, including differentiated metal [3, 6, 7, 8]. In order to better constrain the composition of accreted material we will discuss the different impact lithologies and their HSE patterns with respect to their crustal provenance and constrain their redistribution due to impact gardening.The majority of HSE data was obtained on KREEP-rich mafic impact melt rocks and breccias. Samples from four different landing sites display variably fractionated HSE patterns with suprachondritic Re/Os and HSE/Ir ratios increasing towards moderately volatile HSE like Pd and Au. Collectively these impactites display suprachondritic Ru/Pt ratios, a feature which is observed only in a limited number of differentiated metal-bearing meteorites. The widespread occurrence of this rather uncommon composition was interpreted as the result of accretion of larger fragments of differentiated planetesimal core material to a KREEP-rich target region [6, 8]. Available data on nucleosynthetic isotope anomalies in Ru and Mo suggest that the differentiated signature might have originated from material of the inner solar system [10].Granulitic impactites are KREEP-poor feldspathic impactites which display metamorphic texture and equilibrated mineral compositions, indicative of sub-solidus recrystallization. Hence, their HSE inventory is interpreted to reflect early accretion of material to a KREEP-poor target region prior to formation of the younger impact basins, which apparently dominate the accessible ejecta deposits. The relative HSE abundances in Apollo 16 and 17 granulites are similar and strongly suggest accretion of volatile-depleted impactor material (possibly volatile depleted carbonaceous chondrite or primitive achondrite-like).Fragmental matrix breccias are dominant at the North Ray Crater of the Apollo 16 landing site and were interpreted as representative of the Descartes formation. The HSE inventory of these breccias is characterized by diverse impactite clasts, including KREEP-rich mafic melt breccias and granulitic impactites. In contrast to other impact lithologies, fragmental matrix breccias preserved an impactor signature different from known primitive meteorites. The HSE inventory is characterized by moderate depletions in Re and Os when compared to Ir, Ru and Pt, but chondritic Re/Os and a gradual depletion towards moderately volatile Pd and Au. The latter signature stems most likely from unknown primitive impactors with fractionations caused by nebular processes, like incomplete condensation or evaporation [7].HSE and lithophile element compositions of granulitic impactites and fragmental matrix breccias reveal that material similar to carbonaceous chondrites and acapulcoite-lodranite primitive achondrites was accreted early onto KREEP-poor highland regions. However, most studied KREEP-poor impactites follow a linear mixing trend from slightly subchondritic HSE ratios towards the composition of HSE-rich and fractionated KREEP-rich impactites. This, together with the presence of KREEP-rich impactite clasts, comprising characteristically fractionated HSE, in breccias of different landing sites constrains physical mixing processes ranging from the scale of g-sized samples to the area covered by the Apollo missions. In addition, comparison of Pd/Ir ratios (as measure of HSE fractionation) with abundances of incompatible trace elements like U (i.e., the fraction of KREEP component) reveal preservation of distinct compositional clusters in impactites at different landing sites. Such systematic differences between landing sites are best explained by early accretion of a core fragment onto the area of the Procellarum KREEP Terrane, variable mixing with KREEP-rich highland rocks and subsequent distribution of this combined signature and mixing with more primitive impactor material from KREEP poor sites. This interpretation is consistent with recent results from simulations of impact driven megaregolith evolution [11, 12].References: [1] Norman et al. (2002) EPSL 202, 217-218. [2] Puchtel et al. (2008) GCA 72, 3022-3042. [3] Fischer-Gödde and Becker (2012) GCA 77, 135-156. [4] Sharp et al. (2014) GCA 131, 62-80. [5] Liu et al. (2015) GCA 155, 122-153. [6] Gleißner and Becker (2017) GCA 200, 1-24. [7] Gleißner and Becker (2019) MAPS 54, 2006-2026. [8] Gleißner and Becker (2019) MAPS 55, 2044-2065. [9] McIntosh et al. (2020) GCA 274, 192-210. [10] Worsham and Kleine (2021) Sci. Adv. 7: eabh2837. [11] Liu et al. (2020) Icarus 113609. [12] Liu et al. (2022) EPSL 597, 117817.

Introduction: The TRR170-DB data repository (https://planetary-data-portal.org/) manages the research data from the collaborative research center ‘Late Accretion onto Terrestrial Planets’ (TRR 170). The published data are provided in open machine-readable formats to the planetary science community. They have been generated in various fields of planetology such as astromaterials science, experimental studies, remote sensing, and geophysical modeling. Our data policy and practices are aligned with the principles of Open Science [1] and the FAIR principles [2] fostering openness and transparency in scientific research. Since TRR170-DB is permanently hosted at Freie Universität Berlin (FUB) and interlinked with FUB’s Central Library System the data are on a long term scale preserved and accessible. The TRR170-DB is referenced by Re3data, a global registry of research data repositories [3].The TRR170-DB system: The repository is operated on the open source data management software Dataverse [4]. Users access the repository directly through its interface that connects to the storage environment of the datasets. Alternatively, a web portal allows for repository access while also guiding users how to use TRR170-DB.Data access, storage, and publication: While the TRR170-DB serves as a hub to exchange data for the TRR 170 user community through a password-guarded member area, published data are also accessible for other interested researchers. The repository interface provides search tools to allow users to conduct general searches or specify queries for published data via filters. Filters can direct searches to specific published data types (i.e., planetary materials/geophysics, planetary surface data, astronomy) via their metadata information. Specified searches result in compilations of data and metadata information available in the repository that can be directly viewed, saved, and downloaded via the advanced search tool Data Explorer (Fig.1). The Data Explorer complements the TRR170-DB and is an integrated part of the repository.Fig. 1: TRR170-DB Data Explorer query results. We support TRR 170 members and other users to meet journals’ and funding agencies’ requirements for FAIR data by providing storage for replication datasets (Fig. 2). Replication datasets make published data more easily findable and usable for other researchers. At present, most replication datasets were provided and used by TRR 170 authors of articles appearing in international journals since 2016. These replication datasets are freely available, and no special permission is required for reuse and verification of a study without having to contact the study's authors.Fig 2: Replication datasets in TRR170-DB linked to published research articles.Any data supplier receives a permanent archive and a digital object identifier (DOI, [5]) to make the dataset unique and findable. Data suppliers are requested to apply standardized ways to annotate, structure and organize data. This metadata information on the content, quality, origin, and other characteristics of the datasets ensure reliable data quality for future use in other research projects. In this way, data from different projects can be easier exchanged and be understood when used in different contexts. Metadata information links a dataset to its related published peer-reviewed paper.The metadata model: TRR170-DB has a flexible data-driven metadata system that uses tailored “metadata blocks” for specific data communities. The metadata blocks are based on standards that are compliant with several international metadata schemata (i.e. DDI, DataCite, Dublin Core, VOResource Schema, etc.) and controlled vocabularies. Once a dataset has been published, its metadata and files can be exported in various other open metadata standards and file formats (Fig. 3) to allow for easy data transfer among various international external databases and repositories. Fig. 3: Extract of TRR170-DB metadata and controlled vocabulary to metadata formats, upper right corner.TRR170-DB integration into the FUB Central Library System: FUB Central Library System houses the institutional open access repository, Refubium that contains research data collections. When TRR 170 members contribute datasets to the TRR 170-DB repository, the published version of this datasets gets automatically mirrored by the Refubium. This ensures a global visibility and accessibility through FUB's institutional repository.Within the TRR 170-DB repository, rigorous curation standards have been upheld to maintain the quality and integrity of the research data to ensure their reliability and suitability for scholarly use. To enhance data discovery and citability, published datasets are assigned an additional DOI through the FUB Refubium. The FUB Refubium is using the OAI-PMH (Open Archives Initiative Protocol for Metadata Harvesting) protocol [6] to harvest metadata in the TRR170-DB repository. The integration of the TRR170-DB repository with FUB's Central Library System extends its accessibility to users worldwide. Through Primo, FUB's discovery and access platform interested users gain seamless access to the diverse range of datasets available within Refubium.Future Work: When the TRR 170 research program closes at the end of 2024, all data stored in the TRR170-DB repository will be further accessible to the interested user through three different avenues: via (1) the TRR170-DB repository, (2) the FUB Refubium, and (3) the TRR 170 webpage. As a result, the TRR 170-DB repository facilitates the dissemination and discovery of valuable research data, fostering a culture of knowledge sharing and academic excellence.Acknowledgements: The TRR170-DB repository is managed by subproject TRR 170-INF (German Research Foundation (DFG), 263649064–TRR 170). Freie Universität Berlin provides server infrastructure and a web content management system for managing the TRR170-DB website. Dataverse software is maintained by the IQSS Dataverse team, Harvard University. We thank A. Balduin and archium® GmbH for technical support.References:[1] Open Science, https://www.dfg.de/en/research_funding/programmes/nfdi/index.html[2] FAIR principles, Wilkinson et al., https://doi.org/10.1038/sdata.2016.18[3] r3data, www.re3data.org.[4] Dataverse, dataverse.org.[5] DataCite, datacite.org.[6] Open Archives Initiative Protocol for Metadata Harvesting, https://www.openarchives.org/pmh

Introduction:Carbonaceous chondrites (CCs) are among the most primitive rock samples in our solar system. All CC groups are depleted in volatile elements (i.e., elements having 50% condensation temperature lower than ~1300 K) relative to CI chondrites [1]. This unique characteristic reveals mass-dependent enrichments of light isotopes by decreasing the mass fraction of moderately volatile element ([e.g., 2]; e.g., Zn, Rb, K, Cu, Te). The exact origin of this depletion is not fully understood with primary explanations including incomplete condensation from nebular gas [e.g., 2] or the varying mixing of volatile-rich and volatile-poor components [e.g., 3]. The recognition of light Zn and Te isotope enrichments in CV chondrules seems to suggest that the contribution of these depleted components is the main cause of the light isotope enrichments in the bulk rock CCs [4-6]. However, neither the impact on the chemical budget of bulk CCs nor the origin of the variation among them has been fully understood.In this study, we obtained Zn and Cu isotope data for 24 bulk rock CCs, along with isotope data of matrix and single chondrules in the CR2 chondrite MIL 15328, with the aim to better understand the origin of the volatile depletion in carbonaceous chondrites. Results/Discussion:Bulk rock CCs exhibit variable isotopic range from 0.05 to 0.43±0.02‰ and from -2.01±0.03‰ to -0.14±0.07‰ with an associated mass fraction range from 53 to 271μg/g and 55 to 170μg/g for Zn and Cu, respectively. In both isotopic systems, bulk rock CCs show mass-dependent light isotope enrichments with decreasing element mass fractions. The matrix-rich aliquot from the CR2 chondrite MIL 15328 has a lighter δ66/64Zn (0.20±0.04‰) but heavier δ65/63Cu (-1.51±0.04‰) compared to the respective bulk rock, which has value of 0.38±0.06‰ and -1.68±0.06‰ for Zn and Cu, respectively. The three analyzed single chondrules from MIL 15328 consistently display lighter compositions in both isotopic systems. Their δ66/64Zn and δ65/63Cu span a range from -3.17±0.17‰ to 0.28±0.06‰ and from -2.36 to -1.89±0.02‰, respectively, and correlate linearly with chondrule size. The data suggest that isotopically heavy Zn-Cu sulfide(±metal) was variably expelled during chondrule formation [e.g., 4]. Smaller chondrules, which contain fewer sulfides, are more strongly influenced by interaction with isotopically light gas under kinetic isotope fractionation during cooling of the local nebular domain. On the other hand, in larger chondrules, the expulsion of sulfide droplets from rotating silicate melt is less efficient, resulting in a composition that includes a mixture of isotopically heavy Zn and Cu sulfides in chondrule rims, while their cores remain sulfide-poor and isotopically lighter [5].Taken together, the observed mass-dependent light isotope enrichments in bulk CCs with decreasing element mass fractions result from nebular fractionation and mixing between volatile-rich and isotopically heavy CI-like matrix with volatile-poor, isotopically light chondrules. These findings suggest that chondrule size affects sulfide distribution and isotopic composition, shedding light on the processes contributing to volatile element depletion in carbonaceous chondrites.[1] Palme et al. (2014) Treat. on Geochem. 2 ed., 15-36.[2] Nie et al. (2021) Sci. Adv. 7(49).[3] Braukmüller et al. (2018) GCA 239, 17-48.[4] Pringle et al. (2017) EPSL 468, 62–71.[5] Van Kooten & Moynier (2019) GCA 261, 248-268.[6] Hellmann et al. (2020) EPSL 549, 116508.

Introduction: The Moon's impact basins and their deposits retain information about the timing, flux and composition of late accretion in the inner solar system. However, isotopic ages of particular basins have been difficult to determine reliably because reheating by later impacts have affected chronometers to variable extent and gardening of impact ejecta has led to additional complexity. Recently, in situ U-Pb geochronology of zirconium minerals and calcium phosphates coupled with petrographic, geological and geochemical studies have provided more evidence for the most likely ages of at least some lunar basins [1-8]. These data can be compared with advanced models of ejecta distribution and the contributions of impact melt from specific basins to the lunar landing sites [9] and with absolute model ages obtained by improved crater counting data (e.g. [10, 11]). It is important to expand the still limited database of reliable lunar impactite ages to better define basin ages. Because of the robustness of zircons, in situ U-Pb ages of these minerals in lunar impactites have the potential to provide clues for the early lunar bombardment history as they are more resistant to resetting than for instance K-Ar ages. The present study is focusing on Apollo 16 and 17 ancient regolith breccias, which contain a mixture of mineral and lithic clasts from different highland and other lithologies. The goal of the study was to test if they contain zircons that can be dated and if ages match those found in other lithologies at these landing sites. Ancient regolith breccias: Four thin sections were screened with SEM for zirconium phases (67035,13; 67115,29; 74115,18; 76565,8). The Apollo 16 samples were collected at the North Ray Crater rim. 67115,29 contains impact melt and some glass coated fragments. 67035,13 contains highly feldspatic matrix, pristine highland material, melt breccias and granulitic clasts. Most of the bigger clasts are anorthosites. 74115,18 is a compacted soil breccia, collected in the ‘light mantle’ area and contains fragments of orange glass spheres and shards, granulites and high-Ti mare basalts. 76565,8 is a dimict breccia rake sample from the North massif with a similar clast inventory. Zircon grains occur as individual mineral clasts in the matrix of the breccias, within larger lithic clasts or as coronas onilmenites.U-Pb age record in zircons: The new data show little to no common Pb in zircons and ancient 207Pb206Pb ages ranging from 3.92 to 4.37 Ga with uncertainties ranging from 9 to 29 Ma (2s). Breccia 67035,13 yields ages of 4.25 to 4.37 Ga, whereas 67115,29 shows an age of 4.21 Ga. Breccia 74115,18 shows age clusters at 3.92-3.93, 4.11-4.17 (most analyses) and 4.34 Ga, 76565,8 at 4.16-4.33 Ga. The oldest age of 4.33 Ga in 76565,8 belongs to a zircon grain attached to clinopyroxene in a evolved lithology. The oldest measured zircon (4.34 Ga) in 74115,18 is an individual grain in a clinopyroxene rich clast, the youngest ages at ~3.9 Ga belong to grains attached to ilmenite or noritic compositions. The 4.11-4.17 Ga cluster occurs in anorthositic clasts with granulitic texture and may reflect 2 or more discrete events or discordance from reheating of older zircon by the 3.92 Ga event. The youngest age of breccia 67035,13 (4.25 Ga) was found for an individual zircon grain associated with olivine and anorthite clasts in the matrix. 67115,29 yields an age of 4.21 Ga, obtained from two individual zircons, one being attached to a feldspar-spinel clast and the other associated with noritic composition. Fe-Ni metal inclusions were found in many of the host clasts or surrounding matrix of the analyzed zircons. Thus, a majority of the zircons in all thin sections can be associated with impact events. Discussion: The results agree with some of the ages and age clusters in lunar breccias obtained previously by in situ U-Pb analyses of zircon, baddeleyite and calcium phosphates [1-8]. In some of these studies, petrographic or microstructural evidence is pointing at the in situ crystallization or recrystallization of these minerals from impact melt or localized shock heating [3, 6, 12]. The presence of metal in dated lithic clasts and similar ages occurring at different landing sites relate these ages to basinforming impact events. Based on chemical and geological arguments, previously published ages at 3.92 and 4.20-4.22 Ga were linked to the formation of the Imbrium and Serenitatis basins, respectively [2, 5,7]. Ages ranging from 4.13 to 4.18 Ga may reflect two or more basin impacts as they are associated with granulite grade metamorphism [8]. Ages near 4.33-4.34 Ga may reflect the formation of one of the earliest preserved basins such as South Pole Aitken, consistent with crater counting ages [10, 11]. With few exceptions, the new ages from the Apollo 16 and 17 breccias confirm the age clusters from previous studies. The data also hint that there may be differences in the abundance of basin ages at the Apollo 16 and 17 landing sites and that ejecta from a few basins dominate the impactor age record at these landing sites [9].References: [1] Norman & Nemchin (2014) Earth and Planetary Science Letters(388):387-398. [2] Snape et al. (2016) Earth and Planetary Science Letters(451):149-158. [3] Crow et al. (2017) Geochimica et Cosmochimica Acta(202):264-284. [4] White et al. (2020) Nature Astronomy(4):974–978. [5] Cernok et al. (2021) Communications Earth & Environment(2):120. [6] Vanderliek et al. (2021) Earth and Planetary Science Letters(576):117216. [7] Nemchin et al. (2021) Geochemistry 81(1):125683. [8] Becker et al. (2023) GeoBerlin 2023. [9] Liu et al. (2020) Icarus(339):113609. [10] Evans et al. (2018) Journal of Geophysical Research: Planets(123):1596-1617. [11] Orgel et al. (2018) Journal of Geophysical Research: Planets(123):748–762. [12] Kusiak et al. (2022) Contributions to Mineralogy and Petrology(177):112.

The Moon’s mare volcanism predominantly occurs within the Procellarum KREEP Terrane (PKT), which is widely thought to be associated with KREEP components within the lunar interior. The Chang’e-5 (CE-5) mission sampled a young (2 Ga) mare basalt Em4/P58 unit of northern Oceanus Procellarum. The geochemistry of the CE-5 mare basalt enables assessment of mantle source compositions which are essential to understand the thermo-chemical mechanism for prolonged volcanism during secular cooling of the Moon. Geochemical compositions of the CE-5 bulk soil, breccias, and basalt clasts from various depths within the drill core consistently display high concentrations of incompatible trace elements (ITE: ∼ 0.3 × high-K KREEP; ∼ 5 μg/g Th) with KREEP-like inter-element ratios, for example for La/Sm, Nb/Ta, and Zr/Y. Exotic impact ejecta, extensive magma differentiation (<70 % fractional crystallization) and significant assimilation of KREEP materials during magma transit and eruption cannot account for the ITE contents and ratios or radiogenic isotope compositions (e.g., εNdinitial of + 8 to + 9 and εHfinitial of + 40 to + 46) of the CE-5 basalts; instead, partial melting of their mantle source played a dominant role. The Chang’e-5 basalt is a chemically evolved low-Ti mare basalt (Mg# of ∼ 34) with enriched KREEP-like ITE compositions but high long-term time-integrated Sm/Nd and Lu/Hf ratio, which represents a hitherto unsampled type of mare basalt. It formed by melting of an augite-rich mantle source (late-stage magma ocean cumulates containing > 30–60 % augite, and little or no ilmenite), with a small amount of late-stage interstitial melt that resembles KREEP (∼1–1.5 modal %, equivalent to 0.2–0.3 μg/g Th). The voluminous mare basalts making up the Em4/P58 unit (>1500 km3) provide compelling evidence for large-scale, ITE enriched young mare magmatism within Oceanus Procellarum. In combination with remote sensing data and with the unique Th-rich Apollo 12 basalt fragment 12032,366–18 (impact ejecta likely from Oceanus Procellarum), this implies that significant portions of the FeO- and Th-rich mare regions of the western PKT may also have formed in a similar way.

Introduction: One of the main characteristics of lunar rocks is their strong depletion in moderately volatile elements (MVE) compared to Earth [1], as well as a strong enrichment of heavy isotopes of the MVE, e.g. Cu, Zn, Rb, K, Ga [2-6]. These characteristics have been taken as major arguments in favor of catastrophic outgassing during the Moon forming impact [7], lunar magma ocean (LMO) evolution [8], and/or subsequent magmatic evolution [3]. Due to their ineffectiveness in producing a global MVE depletion and associated isotopic fractionation in the lunar mantle, the two last hypotheses have been questioned in the light of new cutting-edge ab initio calculations [9]. In addition, whereas some of the MVE, e.g. K, Rb, display relatively homogeneous mass-dependent isotopic composition in mare basalts (MB) there appears to be more isotopic heterogeneity for others, particularly Cu [2]. The exact reasons for this isotopic heterogeneity in MB are unknown and may lie in the siderophile/chalcophile behavior of Cu or local volatility-related processes. Here, we present new Cu isotope data for 30 MB and discuss whether their isotopic composition is related to processes during formation of their mantle sources, basalt formation or accompanying volatility-related processes.Samples and methods: 300 to 500 ng of Cu have been purified from 100 mg low-Ti and high-Ti MB from Apollo 11, 12, 15, and 17 following a chemistry specifically designed for Ti-Fe-rich samples. Copper isotopic ratios were obtained by a NEOMA MC-ICP-MS at Freie Universität Berlin and are reported as delta values (i.e. δ65Cu in ‰) relative to the ERM®-AE633 standard, with uncertainties at 95% confidence intervals.Results: Compared to low-Ti MB ([Cu]: 4.07 µg/g to 8.55 µg/g; δ65Cu: 0.22 ± 0.04 ‰ to 1.28 ± 0.06 ‰), high-Ti MB have a significantly lighter δ65Cu for a given [Cu] ([Cu]: 2.70 µg/g to 5.65 µg/g; δ65Cu: -1.42 ± 0.10 ‰ to 0.75 ± 0.01 ‰). In addition, most of the MB suites define a narrow range of [Cu]mean and δ65Cumean.Discussion: Copper content correlates between and within some suites with tracers of magmatic evolution (MgO, FeO, TiO2, Cr/Sm). In contrast, δ65Cu does not correlate with MgO, TiO2, and Cr/Sm and its variation within and between mare basalt suites cannot be explained by silicate fractionation. This strongly suggests that [Cu] changes in different MB suites is a collateral effect of silicate fractionation which agrees with the incompatible nature of Cu, whereas δ65Cu variations in a few suites may reflect mixing of magmas from isotopically different reservoirs and/or local volatility-related processes. However, considering the latter possibility, the range of δ65Cu compositions of MB can only be reproduced if unrealistic initial [Cu] are used, with isotopic fractionation factors very close to unity. Hence, we rule out evaporation during volcanic eruptions as the main process controlling δ65Cu heterogeneity in MB.Interestingly, MB with the heaviest δ65Cu and highest Mg# have also the lowest S/Cu, S/Se, S/Te, S/Ag and S/Pd ratios (Fig. 1). As S is less chalcophile and siderophile than Cu, Se, Te, Ag, and Pd, and Δ65Cumetal-sulfide > 0 [11], low S/Cu, S/Se, S/Te, S/Ag, S/Pd with heavy δ65Cu in MB should be characteristic of S-poor FeNi alloys while higher ratios generally match lighter δ65Cu expected for sulfides. Such systematics exist from low-Ti to high-Ti MB but not within most of the individual MB suites. Instead, most of the suites define clusters in variation diagrams of Cu and δ65Cu with mass fractions of incompatible elements. This clustering suggests limited fractionation of Cu isotopes, hence an evolution of most MB suites as individual systems, and points towards heterogeneous mantle sources. Thus, the δ65Cu differences between low-Ti and high-Ti MB likely reflect Cu isotope partitioning between silicates melt and alloys evolving from S-poor to S-rich at different stages of LMO crystallization. On the other hand, the more limited δ65Cu variation within MB suites relate to processes during parental melt evolution after melting of lunar mantle sources. Consequently, δ65Cu of lunar MB dominantly record processes prior and/or during solidification of mantle source and their bearing on volatility related processes is limited.References: 1. LPSE-Team° (1969). Sci 165:1211-1227. 2. G. F. Herzog et al.° (2009). GCA 73:5884-5904. 3. J. M. Day, F. Moynier° (2014). Philos Trans A Math Phys Eng Sci 372:20130259. 4. E. A. Pringle, F. Moynier° (2017). EPSL 473:62-70. 5. K. Wang, S. B. Jacobsen° (2016). GCA 178:223-232. 6. C. Kato, F. Moynier° (2017). Sci Adv 3:e1700571. 7. K. Pahlevan, D. J. Stevenson° (2007). EPSL 262:438-449. 8. C. Kato et al.° (2015). Nat Com 6:7617. 9. N. Dauphas et al.° (2022). Planet Sci Jour 3. 10. P. Gleißner et al.° (2022). EPSL 593. 11. H. M. Williams, C. Archer° (2011). GCA 75:3166-3178.

Introduction: Renewed interest in a human return to the Moon has revived the importance of past Apollo missions. Both manned and robotic missions to the Moon provided detailed information on locations of instruments, and locations of returned lunar samples. The upcoming lunar missions will produce a large amount of new data, including on samples returned from the Moon. Integration of such data with spatial data can aid in comprehending and analyzing the complexities of lunar data. Here we present a test version of the lunar version of the web-based browser Planet Explorer, which combines seamlessly lunar surface imageries with lunar landing site data without the need of handling file format details and data ingestion by the user.Data Visualization: Planet Explorer is a web browser based on the open software packages OpenLayers [1] and three.js [2] for combining planetary data sets and visualizing results. We have developed and implemented a test version that uses high-resolution images obtained with the Lunar Reconnaissance Orbiter Camera [LROC, 3] that are available in the open access LROC data archive [4]. The LROC narrow-angle camera [NAC, 3] has extensively imaged a substantial portion of the Moon's surface, achieving a resolution of 1 meter per pixel or better.Of particular interest are images that are matched with high-resolution digital elevation maps derived from stereo image pairs [5]. This LROC dataset includes all previous landing sites and many other locations of interest such as the Luna and Chang’e lunar landing sites. In Planet Explorer, the lunar maps can be supplemented with additional data sets from any location. Currently available data in Planet Explorer are • Layer and layer categories: geology, labels, structure (Fig. 1) • Epoch features: surface features of selected lunar epochs (pre-Nectarian to Copernican (Fig. 2a, b), color-coded areas indicate, for instance, geological units • Display of global and local lunar geological maps [6] • Location overlays with geological nomenclature and structural features • Analysis and map data from the TRR170-DB repository [7] of the DFG research program TRR 170 ‘Late Accretion onto Terrestrial Planets’ (Fig. 4.) • Other internet-based resources: i.e., lunar sample compendium [8]. Fig. 1: Menu view of Planet Explorer test case showing the nearside of the Moon's surface [9].Integration of External Data: Currently implemented test cases allow for combining LROC images matched with high-resolution digital elevation maps with sample data and other information. Sample data or other information can be linked or displayed on imageries from the LROC archives [4].Lunar sample data currently used by the Planet Explorer is retrieved from open access resources, e.g., the lunar sample compendium [8], and data from the curated and open access TRR170-DB repository of the TRR 170 research program ‘Late Accretion onto Terrestrial Planets’ [7], and from other internet-based resources. Fig. 2a: Geological map of the lunar farside (pre-Nectarian to Copernican) [10]. Fig. 2b: Geological map of the lunar nearside [11].The current test version of the Planet Explorer offers selected, curated sample data and related information from the Apollo 16 and 17 landing sites. These landing sites are represented as markers on the interface (Fig. 3). Users have the option to select specific locations, such as stations at these landing sites allowing the browser to present comprehensive data summaries for the selected locations. Fig 3. displays various layer categories and surface features of different epochs. Markers indicate Apollo 16 and 17 landing sites as examplesAfter choosing a point of interest (e.g., a landing site), the tool exhibits detailed historical and current information conveniently accessible through the left menu. This information informs on i.e., tracks, stations, instrumentation, and sample locations pertinent to that mission. Additionally, the visual representation of mission tracks and station locations is overlaid with integrated information on specific products such as i.e., sample analyses or comprehensive chemical or mineralogical maps (Fig. 4).Fig 4. Tracks and stations of the Apollo 16 landing site. The table associated with station EVA01 displays sources of related overview data [8, 12].Future Dataset Integration: Planet Explorer offers a digital framework that serves as a valuable resource for displaying compositional characteristics and various properties (such as geology, gravity, etc.) of the surface or near-surface of the Moon and other planetary bodies. Additionally, it is an effective tool for visualizing research data in a spatial data context. For forthcoming Lunar missions, the Planet Explorer may aid in the study of potential landing sites for future lunar exploration. We plan the release of an open access version of Planet Explorer in 2024.Acknowledgements: Funded by Deutsche Forschungsgemeinschaft DFG (Grant SFB-TRR 170, #263649064-INF).References (as retrieved on May 13, 2024):[1] OpenLayers, openlayers.org[2] three.js, https://threejs.org/[3] LRO Camera, https://www.lroc.asu.edu/about[4] LROC archive, https://www.lroc.asu.edu/archive[5] http://wms.lroc.asu.edu/lroc/search[6] Fortezzo et al. (2020), Release of the digital unified global geological map of the Moon at 1:5,000,000-scale, abstract #2760, LPSC[7] TRR170-DB Repository, (https://info.planetary-data-portal.org/)[8] Lunar Sample Compendium, https://curator.jsc.nasa.gov/lunar/lsc/[9] Spatial Reference, https://spatialreference.org/ref/iau2000/30101/[10] Geological map of the lunar farside, https:// www.hou.usra.edu/meetings/lpsc2020/pdf/2760.pdf[11] Geological map of the lunar nearside, https:// www.hou.usra.edu/meetings/lpsc2020/pdf/2760.pdf[12] Haase et al., https://doi.org/10.1029/2018EA000408

Meteorite recoveryAsteroid 2024 BX1 was discovered by astronomer K. Sárneczky at 21:48 UTC on 20 January 2024. NASA’s Scout and ESA’s Meerkat impact assessment systems soon identified it as a potential impactor and predicted that it would pass over Nennhausen, ~60 km W of Berlin, Germany, between 00:15 and 00:51 UTC on 21 January. At this time, a fireball was observed by eyewitnesses and recorded by allsky cameras of the European Fireball Network, IMO/All-Sky7, and FRIPON. Bolide analysis and strewn field calculations [1] indicated that strong winds blew the surviving meteorites to the SE, predicting a fall just south of Ribbeck. Starting on 22 January, a systematic search was carried out by scientists and students of MfN, DLR, FU Berlin, TU Berlin, the SETI Institute, and the Arbeitskreis Meteore. The first meteorite, totaling 171 g, was found by meteorite hunters on 25 January just west of Ribbeck. Two students from our team found two smaller meteorites (8.1 and 4.7 g) on 26 January, proving that the strewn field model was correct. Searching continued until 20 March and revealed about 200 reported finds with a total mass of >1770 g.Strewn fieldThe strewn field extends along a ~1 km wide and ~8 km long, WNW-ESW oriented corridor just south of Ribbeck (where meteorites of between 50 and 230 g were found) and Berge and Lietzow (where meteorites 5 km than predicted. The distribution of total mass per kilometer along the strewn field is approximately constant (~230 g/km) until the distribution of small (6 km due to sampling bias or a lack of small masses during fragmentation.Petrography of the Ribbeck aubritesPetrographic observations revealed that Ribbeck is an aubrite, which are rare enstatite achondrites [2–4]. The Ribbeck meteorites are fragmental breccias predominantly composed of up to 1.2-cm-sized, mostly angular, FeO-free, homogeneous enstatite (En99.2Fs0.0Wo0.8), less abundant (~1–11%), up to-1.5-cm sized, homogeneous forsterite (Fo99.9), and highly variable amounts (~1–17%) of sodic feldspar (An2.4Ab95.1Or2.5) set in a fine-grained, comminuted matrix of related material. Less abundant silicates include K-feldspar (An0.1Ab7.0Or92.2) and diopside (En53.5Fs0.1Wo46.4). Opaque phases include Ti-bearing troilite, exotic sulfides such as alabandite, keilite, djerfisherite, oldhamite, caswellsilverite, schöllhornite, and cronusite, Si-bearing (0.7–1.0 wt% Si) and Si-poor (

Most chondrites are depleted in moderately volatile elements (MVE) relative to the bulk solar system composition represented by CI chondrites. Here we present high-precision isotope dilution data for 11 moderately volatile elements (S, Cu, Zn, Ga, Se, Ag, Cd, In, Sn, Te and Tl) together with Cd and Zn stable isotope compositions for carbonaceous, ordinary, enstatite and Rumuruti chondrites complemented by a literature compilation of MVE stable isotope compositions. Together these data allow new insights into the processes that led to MVE depletion in chondrites and their redistribution within parent bodies.Moderately volatile element abundances in carbonaceous, ordinary and Rumuruti chondrites are best explained by two-component mixing between a chemically CI-like MVE-rich matrix and an MVE-poor refractory component dominated by chondrules. Chondrules are enriched in light MVE isotopes due to kinetic recondensation of a small vapor fraction initially lost from chondrules upon heating. Later, thermal metamorphism redistributed some MVE within chondrite parent bodies, which is evaluated here in a systematic way for different chondrite groups and plateau volatile elements based on related and comparatively large but unsystematic stable isotope fractionation. Compared to other chondrite classes, enstatite chondrites show less systematic MVE abundance patterns when the elements are plotted as a function of condensation temperatures. Type 3 and 4 enstatite chondrites are more MVE-rich than expected based on their low matrix fractions and are enriched in light Zn and Te isotopes relative to CI. The enrichment of light Zn and Te isotopes and high MVE abundances in type 3 and 4 enstatite chondrites relative to CI can be explained by recondensation of a larger MVE vapor fraction after chondrule formation than observed for other chondrite classes, which presumably occurred at comparatively high H2 pressures. Because MVE abundances and isotope compositions are fully consistent with chondrule formation, two-component mixing and MVE redistribution on parent bodies, we refute partial condensation from a hot solar nebula as the cause for MVE depletion in chondrite formation regions of the protoplanetary disk.