CHEMICAL CLASSIFICATION OF SPHERULES RECOVERED FROM THE PACIFIC OCEAN SITE OF THE CNEOS 2014-01-08 (IM1) BOLIDE. A. Loeb1,2, S.B. Jacobsen2,3, R. Tagle2, T. Adamson2, S. Bergstrom2, J. Cherston 1,2, R. Cloete1,2, S. Cohen2,7, L. Domine1,2, H. Fu2,3, C. Hoskinson2, E. Hyung2,3, M. Kelly2, E. Lard2, F. Laukien2,6, J. Lem2,5, R. McCallum2, R. Millsap2, C. Parendo2,3, C. Peddeti2,4, J. Pugh2, S. Samuha2,7, D.D. Sasselov1,2, M. Schlereth2, J. Siler2, A. Siraj1,2, P.M. Smith2, J. Taylor2, R. Weed2,4, A. Wright2, J. Wynn2. 1Dept. of Astronomy, Harvard Univ., Cambridge, 02138, MA ([email protected]). 2Interstellar Expedition of the Galileo Project, Cambridge, 02138, MA. 3Dept. of Earth and Planet. Sci., Harvard Univ., Cambridge, 02138, MA. 4Dept. of Nuclear Eng., Univ. of California Berkeley, Berkeley, 94720, CA. 5Dept. of Mining Eng., PNG Univ. of Technology, Lae, 411, Papua New Guinea. 6Dept. of Chemistry and Chemical Biology, Harvard Univ., Cambridge, 02138, MA. 7Dept. of Materials Eng., NRCN, P.O. Box 9001, Beer-Sheva, 84190, Israel. Abstract: We have conducted an extensive towed-magnetic-sled survey during the period of June 14-28, 2023, over the seafloor about 85 km north of Manus Island, Papua New Guinea, centered around the calculated path of the bolide CNEOS 2014-01-08 (IM1). We found about 850 spherules of diameter 0.1- 1.3 millimeters in our samples. The samples were analyzed by micro-XRF, Electron Probe Microanalyzer and ICP Mass spectrometry. Here we report major and trace element compositions of the samples and classify spherules based on that analysis. We identified 78% of the spherules as primitive, in that their compositions have not been affected by planetary differentiation. We divided these into four groups corresponding to previously described cosmic spherule types. The remaining 22% appear to all reflect planetary igneous differentiation and are all different from previously described spherules. We call them D-type spherules. A portion of the D-spherules show an excess of Be, La and U, by up to three orders of magnitude relative to the solar system standard of CI chondrites. Detailed mass spectroscopy of 12 of these “BeLaU”-type spherules, the population of which may constitute up to ~10% of our entire collected sample, suggests that they are derived from material formed by planetary igneous fractionation. Their chemical composition is unlike any known solar system material. We compare these compositions to known differentiated bodies in the solar system and find them similar to evolved planetary materials - with lunar KREEP the closest in terms of its trace element enrichment pattern, but unusual in terms of their elevated CI-normalized incompatible elements. The “BeLaU”-type spherules reflect a highly differentiated, extremely evolved composition of an unknown source. 1 Introduction The retrieval of cosmic spherules from meteor sites has a long history, with related morphology and composition analyses linking them to various components of the solar system (Brownlee et al., 1979; Maurette et al., 1991; Taylor and Brownlee, 1991; Xue et al., 1994; Brownlee et al., 1997; Herzog et al., 1999; Taylor et al., 2000; Engrand et al., 2005; Genge et al., 2008; Vondrak et al., 2008; Wittke et al., 2013; Folco et al., 2015; Rudraswami et al., 2015; Genge et al., 2017). The spherules range in diameter from a minimum recoverable size of 0.25 to 1.7 mm. They have been classified as I, S and G-types. Marvin and Einaudi (1967) and others (Folco and Cordier 2015; Blanchard et al. 1980; Brownlee et al. 1997) have listed possible extraterrestrial and terrestrial origins for magnetic spherules like those discussed in this paper. Extraterrestrial origins may be: (i) ablation of meteorites during flight in the atmosphere; (ii) disintegration of carbonaceous chondrites in flight through the atmosphere; (iii) vaporization of large meteorites during impact crater formation; and (iv) infall of particles containing iron or iron oxide, of either asteroid or comet origin (they may enter the atmosphere as spherules, resulting from collisions in space, or may become spherules in the atmosphere). The terrestrial origins proposed were: (i) volcanic; (ii) industrial combustion of coal, crude oil, or wood; (iii) smelting products; and (iv) others such as forest fires and lightning discharges. On 8 January 2014 US government satellite sensors detected three atmospheric detonations in rapid succession about 84 km north of Manus Island, outside the territorial waters of Papua New Guinea (20 km). Analysis of the trajectory suggested an interstellar origin of the causative object CNEOS 2014-01-08: an arrival velocity relative to Earth more than ~45 km s−1, and a vector tracked back to outside the plane of the ecliptic (Siraj and Loeb 2022a). In 2022 the US Space Command issued a formal letter to NASA certifying a 99.999% likelihood that the object was interstellar in origin. Along with this letter, the US Government released the fireball light curve as measured by satellites, which showed three flares separated by a tenth of a second from each other. The bolide broke apart at an unusually low altitude of ~17 km. The object was likely substantially stronger than any of the other 272 objects in the CNEOS catalog, including the ~5%-fraction of iron meteorites from the solar system (Siraj and Loeb 2022b). Calculations of the fireball light energy suggest that about 500 kg of material was ablated by the fireball and converted into ablation spherules with a small efficiency. The fireball path was localized also based on the delay in arrival time of the direct and reflected sound waves to a seismometer located on Manus Island (Siraj and Loeb 2023), but this inference has been debated (e.g., Brown and Borovicka 2023). In this paper, we characterize spherules retrieved in an expedition that surveyed the region identified by the US Government satellites as the meteor site without assuming their association with the IM1 bolide. Sampling Expedition The expedition was mounted from Port Moresby, Papua New Guinea (PNG), to search for remnants of the bolide, labeled hereafter IM1. It utilized a 40-meter catamaran workboat, the M/V Silver Star. A 200- kg sled (Fig. 1) was used with 300 neodymium magnets mounted on both of its sides and video cameras mounted on the tow-bridle. Approximately 0.06 km2 were sampled in the target area (Fig. 2). The fine material collected on the neodymium magnets was extracted and brought in a wet slurry up to a laboratory set up on the bridge of the vessel for further examination. There, an initial wet-magnetic separation took place. Subsequently, both magnetic and non-magnetic separations were processed through sieves and dried. Spherules were handpicked with tweezers using a binocular zoom microscope. They ranged in size from 100 microns to 2 mm. We obtained a total of ~850 fragments consisting of spherules and shards by this method. Spherule Samples and Location 2 The terminology and measurements will be explained in the upcoming subsections (see also Loeb et al. 2024a,b). Figure 2 shows the tracks of our expedition survey. Tracks 22 and 17 were located outside the Department of Defense error box for IM1’s fireball, but the full extent of IM1’s strewn field is unknown. Figure 1: Magnetic sled design. Left: Isometric view of the magnetic sled design, Right: Side view of the sled when placed on the ocean floor. The 250-kg, 1 by 2 meter sled was covered with an array of 300 neodymium magnets on both sides and equipped with video cameras in the metal tow-halter ahead of it, which was anchored by a synthetic cable to a winch on the ship, the M/V Silver Star. Figure 2: List of ship track numbers around the expected path of IM1 based on seismometer data (Siraj and Loeb, 2023) from Manus Island (orange strip). Left: Tracks within the Department of Defense error box (in red). Right: Full map including runs 22 and 17. Background colors indicate ocean depth (with scale on the right). Latitude and longitude are marked in degrees and decimal minutes. At one degree south latitude, one minute of latitude or longitude equals one nautical mile which is 1.852 km. The red box, measuring 11.112 km on a side, marks the uncertainty in the Department of Defense (DoD) localization of IM1’s fireball, and the green box marks twice that size. Analytical Methods Most samples (~802) were first analyzed by microXRF with a Bruker Tornado M4 for their bulk major element composition, followed by imaging (SEM and EDS chemical mapping) and spot chemical analyses of ~80 samples with a JEOL Model JXA 8230 Electron Probe Microanalyzer (EPMA). Measurements of elemental abundances for about 60 major and trace elements were performed for 68 samples with an iCAP TQ triple quadrupole ICP-MS (ThermoFisher Scientific). microXRF: The major and trace element compositions of separated spherule and shard samples was analyzed using the M4 TORNADO PLUS micro XRF instrument from Bruker, situated at the central application facility in Berlin, Germany. This instrument features a 30 W micro-focus X-ray tube and a rhodium anode, with X-rays focused through a polycapillary lens to achieve a spot size of 20 µm for the high-energy range above 20 keV. The measurements were conducted under specific conditions: 50 kV, 200 µA, and 2 mbar for a duration of 60 s. The pressure of 2 mbar was chosen to enhance the detection of light elements and minimize absorption caused by air between the sample and detector. Fluorescent signals were collected using two light element window silicon drift detectors, each with a 60 mm² active area, with 3 independently operating signal processing units, allowing a maximal throughput of 250 kcps each at a spectroscopic resolution lower than 145 eV for manganese Kα. The samples were analyzed using the single- spot approach, capitalizing on the benefits arising from the significant information depth of X-rays (e.g. Beckhoff, B. et al., 2006) and the beam divergence of the poly-capillary lenses (approximately 60 µm/mm). This combination ensured optimal coverage of the sample volume and yielded representative results. Sample quantification was attained through standard-less fundamental parameter quantification after instrument calibration, involving a mix of pure elements and the NIST 620 certified reference glass sample to describe lens transmission and element sensitivity. The quantification algorithm uses the forward calculation of the complete spectrum following the approach describe by Sherman (1955). To eliminate any potential for blank signals, spherules and shards were mounted on acrylic plates using double-sided tape. The results for major and trace elements were computed, presenting major elements as oxides and traces as individual elements. The primary advantage of micro XRF lies in the combination of speed, major and trace element sensitivity as well as its non-invasiveness, positioning it as a pre-screening tool for more time- consuming and invasive analytical procedures with uncertainties below tens of percent. EPMA: We used the JEOL JXA-8230 electron microprobe at the Harvard Electron Microprobe Laboratory to obtain high-resolution backscatter (BSE) and secondary (SEI) electron images, elemental X- ray maps, and chemical analyses, using focused beam of ~1 mm in diameter. Most objects were mounted on sticky tape, while several spherules were mounted in epoxy and polished. All samples were carbon- coated. The chemical compositions of intact objects were measured by energy dispersive spectroscopy (EDS) using factory calibration curves. The polished areas of several spherules were analyzed by wavelength dispersive spectroscopy (WDS) using common natural minerals and synthetic glasses as calibration standards (e.g., Petaev and Jacobsen, 2009). The EDS analyses and imaging we performed at accelerating voltage of 20 kV and beam currents of 5-10 nA and ~0.1 nA at low- (< 1000×) and high- resolution (> 2000×), respectively. In the WDS analyses we used accelerating voltage of 15 kV, beam current of 20 nA, and counting times of 30 sec and 15 sec on peak and background, respectively. TQ-ICP-MS (Triple Quad elemental analysis): Measurements of elemental abundances for major and trace elements were performed on the iCAP TQ quadrupole ICP-MS (ThermoFisher Scientific) in the Cosmochemistry Laboratory at Harvard University. USGS reference materials were thoroughly dissolved and diluted in a 2% HNO solution spiked with 10 ppb indium diluted to a factor of 5000 to be used as 3 standards. Spherules were prepared for mass spectrometry measurements by first individually digesting the samples in a mixture of concentrated HF-HNO -HCl at a 1:3:1 ratio at 120-140 oC overnight. The samples 3 were subsequently dried down and then redissolved in a second acid mixture involving an aqua regia solution mixed with H O at a 3:2 ratio and heated to 120-140 oC overnight. This dissolution was dried down 2 for the second time and redissolved in a high-purity 2% HNO solution. A small aliquot (3%) was drawn 3 from this solution and further diluted for elemental analysis. To account for and to correct instrumental drift, the 2% HNO solution used for dilution was spiked with 2 ppb indium as an internal standard, prepared 3 identically to the standard solutions. Measurements were performed in KED mode with He as a collision cell gas as recommended by the Reaction Finder function built in the iCAP TQ Qtegra software, with the exception of Cr, which was measured in TQ mode with O as a mass-shifted molecule. The prepared 2 spherule solutions were measured as an unknown against a four-point calibration line consisting of a blank and three USGS standards: BCR-2, BHVO-2, and AGV-2. Calibration curves for individual elements were checked for linear intensity to concentration correlations for accurate measurements. Routine measurements of AGV-2 as an unknown on the iCAP TQ suggest fractional errors to be within 6% using this method. Results: Imaging and morphology of the spherules Electron microprobe images of recovered spherules are shown in Figs. 3, 4 and 5. The spherules in Fig. 3 are what we call primitive spherules, identified as such by their chemical composition (see next section). The dendritic textures of these spherules suggest rapid cooling. The spherules in Fig. 4 and 5 are 4 all identified as differentiated spherules by their chemical compositions (see next section) and do not in general have as perfect a spherical shape as the primitive group, and some of them are clusters of coalesced spherules. The complete spherule dataset will be released in a future publication. The shapes of the BeLaU- type spherules in Fig. 4c and f have been seen before in spherules from airbursts (Tankersley et al. (2024); van Ginneken et al. (2021, 2024). In addition to electron microprobe images, low resolution photos were taken for 684 samples prior to micro-XRF analysis. Among these, ~64 were determined to be “shards” as opposed to “spherules,” which were discerned based on sharp angles resembling broken surfaces or evidence of fragmentation. Figure 3. BSE images of primitive spherules from the a) S-type (IS20M-1) b) G-type (IS20M-21) c) I-type, high Ni (IS8M2-20) and d) I-type, low Ni (IS16A-SPH1) groups. The scale bar is 100 microns. 5 Figure 4. BSE images of differentiated spherules from each of the differentiated (D-type) spherule classifications: a) D-type low Sr, high Si (IS11M2-2) b) D-type high Sr, high Si (IS19M-14) c) D-type, high Si (17NMAG-5) d) D-type, low Sr, low Si (IS21-4) e) D-type high Sr, low Si (IS14M-2) and f) D- type, low Si (S21 or IS14-SPH1) groups. The images c) and f) are also classified as “BeLaU”-type spherules. The scale bar is 100 microns. 6 Figure 5. Additional BSE images of D-type spherules: a) 19NMAG-52 (D-type, high Sr, low Si), b) 19MAG-50 (D-type, high Sr, low Si), c) 19MAGx-4 (BeLaU, low Si), d) 17MAG-2 (BeLaU, low Si), e) 17MAG-29 (BeLaU, low Si), and f) 17MAG-6 (D-type, high Sr, low Si). The scale bar is 100 microns. Classification of the spherules based on elemental compositions. Cosmic spherules are sub-divided into three compositional types (Blanchard et al., 1980). These are the silicate-rich spherules or S-type, the Fe-rich spherules or I-type and glassy spherules or G-types. There is strong evidence that S-type cosmic spherules with chondritic-like composition are related to carbonaceous chondrites and ordinary chondrites (Blanchard et al., 1980). It has been suggested that I-type spherules are metal grains released from carbonaceous chondrites disaggregated in space (Herzog et al. 1999). The glassy or G-type spherules are thought to be mixtures of S and I. Relatively rare spherules have been called differentiated as they have similarities to achondrite meteorites and have been treated as a subgroup of S-type spherules. Differentiated spherules have major-element compositions with higher Si/Mg and Al/Si ratios, and higher refractory lithophile trace element contents relative to chondritic spherules (cf. Folco and Cordier 2015). The major element, Sr and Ni compositions of 745 spherules from the IM1 site measured by micro- XRF are in Table S1 (supplement). The data are plotted in a Mg/Si histogram (Figure 6) and show a minimum at Mg/Si = 1/3. Spherules with Mg/Si > 1/3 are similar to chondritic meteorites and cosmic S- type spherules, while those with Mg/Si <1/3 are similar to igneous rocks from Earth and other planetary bodies. The data are also plotted in a Mg-Si-Fe ternary diagram (Figure 7), since such a diagram has been shown to effectively distinguish the S-, I- and G-type groups (cf. Folco and Cordier 2015). We note that there are two distinct groups of spherule compositions in this plot. About 78 % of the spherules fall along the trend of S, G and I-type spherules. These are referred to as primitive spherules as they are thought to be related to primitive chondritic meteorites and represent materials that have not gone through planetary differentiation. The remaining 22% of the spherules have low Mg and plot close to the Si-Fe side of the diagram. The high-Si part of this group plots within the range of terrestrial igneous rocks that are shown for comparison. These spherules are thus called differentiated, meaning they are likely derived from crustal rocks of a differentiated planet. Since they are clearly different from the differentiated subgroup of S-type spherules we give them a new name D-type spherules. The Mg/Si = 1/3 is used to distinguish primitive and differentiated spherules. The D-type spherules were discovered in 17 of the 24 tracks explored during this expedition. Figure 6. Histogram of the Mg/Si ratio measured with micro-XRF for 745 IM1 site spherules. This diagram shows a clear dividing line between primitive and differentiated spherules. 7 Si I-type, high Ni I-type, low Ni 0 S-type 100 G-type UCC D-type, high Sr high Si AGV-1 10 D-type, high Sr low Si 90 D-type, low Sr high Si Shale D-type, low Sr low Si 20 Reference values BCR-1 80 Most Common Terrestrial BHVO-1 Igneous Rocks 30 70 N-MORB 40 CI 60 Bulk Earth 50 50 BSE 60 40 70 30 80 20 90 10 100 0 Mg 0 10 20 30 40 50 60 70 80 90 100 Fe Figure 7. Atomic Mg-Si-Fe plot (atom %) of micro-XRF data for 745 IM1 site spherules and shards. The spherules are classified with the parameter values in Table 1. The spherule groups are compared to reference values of Earth materials (Bulk Earth, bulk silicate Earth [BSE], upper continental crust [UCC], shale, normal midocean ridge basalts [N-MORB], Hawaiian basalt [BHVO-1], Columbia River basalt [BCR-1], Guano Valley andesite [AGV-1]) and CI meteorites. Also shown is the range of chemical compositions of terrestrial igneous rocks. For the primitive spherules we use 100Fe/(Fe+Si+Mg) > 90 to distinguish I-types from S- and G-types. This group is supposed to be primarily made of iron compounds and is clearly distinct from the other primitive spherules in the 100Fe/(Fe+Si+Mg) histogram (Figure 8a). This I-group is further subdivided into high Ni (>4000 ppm) and low Ni (<4000 ppm) groups (Figure 8b), as high Ni spherules are most likely of cosmic origin and typically have Ni > 4000 ppm (Engrand et al. 2006). The S- and G-type dividing line is 100Si/(Fe+Si+Mg) = 50 (Figure 8a), relatively consistent with previous literature (cf. Brownlee et al. 1997; Taylor et al. 2000; Folco and Cordier 2015). The primitive spherule groups are compared to reference values of Bulk Earth, bulk silicate Earth (BSE) (McDonough and Sun 1995), and CI meteorites (Anders and Grevesse 1989) that are and should be on the primitive trend (Figure 7). 8 Figure 8. Left: Histogram of the 100Fe/(Fe+Si+Mg) measured with micro-XRF for 745 IM1 site spherules. This diagram shows the dividing lines selected between S-, G-, and I-types. Right: Plot of Ni(ppm) vs. 100Fe/(Fe+Si+Mg), showing the dividing line selected for high-Ni vs low-Ni spherules. Owing to the incompatible nature of Sr, the Sr content of differentiated spherules is a good indication of the enrichment of refractory lithophile elements in the spherules and thus the extent of differentiation. The differentiated spherules in this study are thus divided into high Sr (>450 ppm) and low Sr groups (<450 ppm). They are further subdivided on the Si-content. For high Sr spherules we use 100Si/(Fe+Si+Mg) = 60 as the dividing line and for low Sr spherules a value of 100Si/(Fe+Si+Mg) = 70. These dividing lines are shown in Figure 9. The spherule groups are compared to reference values for samples of the Earth’s crust in Figure 7. This includes average composition of normal midocean ridge basalts (N-MORB) (Gale et al. 2013), average upper continental crust (UCC) (Rudnick and Gao 2014) and shale (Ray and Paul 2021). Also plotted is the outline of the field of 37000 terrestrial igneous rocks as well as 3 USGS standards [Hawaiian basalt (BHVO-1), Columbia River basalt (BCR-1), Guano Valley andesite (AGV-1) (Jochum et al. 2007)]. We note that the high Si varieties of D-spherules plot close to or within the range of terrestrial igneous rocks, while the low Si groups do not. Thus, the D-type spherules and have been divided into four distinct groups. This results in eight distinct spherule groups that are all shown in Figure 7. The parameters used to subdivide the spherules are summarized in Table 1. The total number of spherules identified in each group are listed in Table 2. 0 20 40 60 80 100 100Si/(Mg+Si+Fe) 9 )mpp( rS 2000 D-types High Sr high Si High Sr low Si Low Sr high Si Low Sr low Si Reference values 1500 1000 AGV-1 500 BHVO-1 BCR-1 UCC N-MORB 0 Figure 9. Micro-XRF data for 745 IM1 site spherules. Plot of Sr(ppm) vs. 100Si/(Fe+Si+Mg). Table 1. Classification of the spherules with the Mg-Si-Fe diagram. Type 100Fe/ Ni Mg/Si Sr (ppm) 100Si/ (Fe+Si+Mg) (ppm) (Fe+Si+Mg) Primitive I-type, high Ni >90 >4000 spherules I-type, low Ni >90 <4000 S-type <50 >1/3 G-type >50 and >1/3 <90 Differentiat D-type, high Sr, high <1/3 >450 >60 ed Si spherules D-type, high Sr, low Si <1/3 >450 >60 D-type, low Sr, high Si <1/3 <450 >70 D-type, low Sr, low Si <1/3 <450 >70 Table 2. Comparison of the number of each spherule type identified by micro-XRF and by ICP-MS results. Type Micro-XRF Micro-XRF ICP-MS ICP-MS Number Percent Number Percent Primitive I-type, high Ni 18 2.4 5 7.4 spherules I-type, low Ni 212 28.5 18 26.5 S-type 275 36.9 19 27.9 G-type 78 10.5 0 0 Differentiated D-type, high Sr, high Si 20 2.7 6 8.8 spherules D-type, high Sr, low Si 23 3.1 5 7.4 D-type, low Sr, high Si 29 3.9 0 0 D-type, low Sr, low Si 90 12.1 3 4.4 D-type, BeLaU high Si 2 2.9 D-type, BeLaU low Si 10 14.7 Total 745 100 68 100 The major element and trace element compositions of 68 spherules from the IM1 site measured by ICP- MS are in Table S2 (supplement). ICP-MS data for the spherules include many more elements than the micro-XRF data but does not include measurement of Si. Thus, we also plot the micro-XRF data in a Mg- Al-Fe diagram (Figure 9a) and compare it to the same diagram with ICP-MS measurements (Figure 9b). The micro-XRF results show the same groups in the Mg-Al-Fe plot as for the Mg-Si-Fe plot in Figure 8. Note that the primitive and differentiated trends are even better separated in Figure 9a, and the fields of the primitive spherule groups are also well defined by this diagram. We conclude that this new diagram is a good alternative to the Mg-Si-Fe diagram, when Si data are missing. The Sr concentrations of the D-type spherules measured by micro-XRF are plotted versus the Al/Fe ratio in Figure 10a. While there is some overlap, this diagram gives a relatively good separation of the high Si and low Si groups after separating the differentiated spherules into high (>450 ppm) and low (<450 ppm) Sr groups and is thus also useful for data with missing Si measurements. Classification of the spherules with the parameters in Table 3 will thus yield a relatively equivalent classification of the spherules compared to that obtained with the Mg-Si-Fe diagram. The primitive spherules are identified by 100Al/(Fe+Al+Mg) <10 and the differentiated spherules by 100Al/(Fe+Al+Mg) >10. For the primitive spherules the I-types are identified by 100Fe/(Fe+Al+Mg) >90, the S-types by 100Fe/(Fe+Al+Mg) <65, and the G-types in between these two values. 10 I I S G D D D D R M - - t t - - - - - e - o y y t t t t t t y f y y y y p p s y e p p p p p p t e e r e e e e e e C e , , , , , , h l n o o h h l l c i o o m g w i i e g g w w h m N h h v N S S a o i S S r r i l n u r r h l o e T h l i o g w s e ig w h r h S r S S e i S s i i i trial AGV-1 20 10 0 Al 100 90 80 a S I I D D D D D M I - - g t t - - - - - - o n y y t t t t t t y y y y y y p p e s p p p p p p t e e o e e e e e e C , , u , , , , , , h l s o o c h h l B B i o m g w R h i i e e g g w h o o m L L N h h n c N S a a o i d k S S U U r i n r s , r r i , , t l l h T i o o h l c i o e w g w ig w r h r h S S e S S i i s S i i t i rial 20 10 0 Al 100 90 80 b Igneous Rocks 30 70 30 70 UCC Shale 40 60 40 60 BCR-1 BHVO-1 50 50 50 50 N-MORB 60 4 B 0 ulk Earth 60 40 CI 70 30 70 30 BSE 80 20 80 20 90 10 90 10 100 0 100 0 Mg 0 10 20 30 40 50 60 70 80 90 100 Fe Mg 0 10 20 30 40 50 60 70 80 90 100 Fe Figure 10. (Figure formatting, faint grey lines present as outlines) a) Atomic Mg-Al-Fe plot (atom %) of micro-XRF data for 745 IM1 site spherules. The spherules are classified with the parameter values in Table 1 and are the same spherules shown in Figure 7. b) ICP-MS data for 68 spherules, classified with the parameters in Table 3 as discussed in the text. Table 3. Classification of the spherules with the Mg-Al-Fe diagram. Type 100Fe/ Ni 100Al/ Sr Sr vs Al/Fe BeLaU (Fe+Al+Mg) (ppm) (Fe+Al+Mg) (ppm) Primitive I-type, high Ni >90 >4000 <10 spherules I-type, low Ni >90 <4000 <10 S-type <65 <10 G-type >65 and <90 <10 Differentiated D-type, high Sr, high Si >10 >450 See Figure 3a <80 spherules D-type, high Sr, low Si >10 >450 See Figure 3a <80 D-type, low Sr, high Si >10 <450 See Figure 3a <80 D-type, low Sr, low Si >10 <450 See Figure 3a <80 D-type, BeLaU, high Si >10 >80 D-type, BeLaU, low Si >10 >80 0.0 0.5 1.0 1.5 2.0 2.5 3.0 Al/Fe Figure 11. Sr (ppm) vs the Al/Fe weight ratio for D-type spherules from the IM1 site. a) Micro-XRF data, b) ICP-MS data. 11 )mpp( rS a b 10000 1000 100 High Sr high Si High Sr low Si low Sr high Si low Sr low Si 10 0.0 0.5 1.0 1.5 2.0 2.5 3.0 Al/Fe )mpp( rS 10000 1000 100 High Sr, high Si High Sr, low Si Low Sr, low Si BeLaU, low Si BeLaU, high Si 10 For differentiated spherules we first use the fields of the four different D-types shown in Figure 10a to identify the same types for the ICP-MS data. In addition, we use Figure 11 to identify spherules with particularly high contents of refractory lithophile elements, based on the enrichments of Be, La and U relative to Mg and Fe. First the concentrations of these elements are normalized to the same elements in CI chondrites. The CI-normalized values (Be , La , U , Mg and Fe ) are used to calculate the following CI CI CI CI CI plotting parameters for the ternary diagram in Figure 12: Be +La +U BeLaU = CI CI CI Be +La +U +Mg +Fe CI CI CI CI CI 1000(Mg ) M = CI Be +La +U +Mg +Fe CI CI CI CI CI 100(Fe ) F = CI Be +La +U +Mg +Fe CI CI CI CI CI The BeLaU parameter was divided by 100, while the M-parameter was multiplied by 10 to make use of the entire area inside the ternary diagram. We define a BeLaU-type spherule as having BeLaU > 80, and we define high and low Si varieties based on the Al/Fe ratio, as in Figure 11a. This procedure identifies 10 of D-type spherules as low Si BeLaU-type spherules and 2 as high Si BeLaU-type spherules as shown in Figure 12. These spherules are also shown in Figures 10b and 11b. BeLaU-type spherules can only be identified with ICP measurements. We found 12 BeLaU-type spherules out 26 D-type spherules identified with ICP measurements (Table 2). The BeLaU spherules were found in tracks 4, 13, 14, 17 and 19. With the micro-XRF measurements, we identified 162 D-type spherules out of a total of 745 spherules. This results in an estimate of 10 % of all spherules to be of BeLaU-type. Thus, out of the ~802 spherule identified as natural materials by our micro-XRF and ICPMS measurements we estimate that there should be up to 80 BeLaU-type spherules in our collection. BeLaU 0 100 10 S-type 90 I-type, high Ni AGV I-type, low Ni D-type, high Sr high Si 20 D-type, high Sr low Si UCC 80 D-type, low Sr low Si D-type, BeLaU low Si 30 D-type, BeLaU high Si 70 Reference values 40 60 BCR-1 50 50 60 40 70 BHVO-1 30 80 N-MORB 20 90 BSE 10 100 0 M 0 10 20 30 40 50 60 70 80 90 100 F 12 Figure 12. Ternary diagram for identifying the spherules that are most enriched in Be, La and U (BeLaU) relative to Mg (M) and Fe (F). The parameters are CI chondrite normalized (see text). Origins of the spherule groups In total we analyzed 850 magnetic particles by either micro-XRF (792) or ICP-MS (68) or both (11). We found that 48 have simple chemical compositions that likely make them derived from industrial products or terrestrial minerals. They were thus not included in this study and so we are left with 802 spherules for which we report data in this paper. Origin of Primitive spherules: The primitive spherules are in general characterized by high Cr, Co, and Ni and highly variable Mn. Cr is moderately volatile, similar to Mn, thus in a Cr/Fe vs Mn/Fe plot (Figure 13) there is an overall positive correlation as expected for these ratios. We note that S-type spherules have both Cr/Fe and Mn/Fe similar carbonaceous chondrites (CCs) and non-carbonaceous chondrites (NCs), and there is no major effect from volatile loss of Cr and Mn for this type of spherules. The Ni-rich I-type spherules have very low Mn/Fe showing substantial volatile loss of Mn and also some for Cr. Most of the low Ni I-type spherules have normal chondritic Mn/Fe and slightly lower, so these do not have evidence for substantial volatile loss for Mn. This suggests that their low Cr content is due to some other partitioning process. The primitive nature of S- and I-type spherules are supported by their chondrite- like Cr/Fe and Mn/Fe, distinctly different from the planetary values (Earth, Moon, Vesta, Mars) shown in Figure 13. In a plot of Co/Fe vs Mn/Fe (Figure 14a) when comparing S-type spherules similar CCs and NCs, there is no major effect from volatile loss. When comparing with planetary bodies we see an overall negative correlation that is likely due to core formation in the planets. Ni-rich I-type spherules have very low Mn/Fe showing substantial volatile loss. Low Ni I-type again have normal chondritic Mn/Fe and slightly lower, so these do not have evidence for substantial volatile loss. The primitive nature of S- and I- type spherules are supported by their chondrite-like Co/Fe and Mn/Fe, distinctly different from planetary values. In a plot of Ni/Fe vs Mn/Fe (Figure 14b) we also see an overall negative correlation. Here the S- type spherules have lower Ni/Fe compared to CCs and NCs. Ni is more strongly partitioned into metal compared to Co, so some Ni rich metal must have been lost in producing the S-type Spherules. Thus, overall Mn, Cr, Co and Ni relative to Fe in S- and I-type spherules supports their origin from primitive chondritic meteorites but do show evidence of volatile loss as well as metal-silicate separation due the processing into spherules. Primitive Spherules 0.00 0.01 0.02 0.03 Mn/Fe Figure 13. A plot of Cr/Fe vs Mn/Fe for primitive spherules compared to carbonaceous (CC) and non- carbonaceous (NC) chondrites, Earth, Mars, Vesta and the Moon. Sources: CCs and NCs from Alexander 13 eF/rC 0.06 0.05 Mars Vesta Earth 0.04 0.03 Moon 0.02 S-type I-type high Ni I-type low Ni CCs 0.01 NCs Planets 0.00 2019ab. Mars: Yoshizaki and McDonough (2020), Vesta: Dreibus and Wänke (1980), Moon: Hauri et al. (2015). Primitive Spherules 0.00 0.01 0.02 0.03 Mn/Fe Figure 14. A plot of Co/Fe (a) and Ni/Fe (b) vs Mn/Fe for primitive spherules compared to carbonaceous (CC) and non-carbonaceous (NC) chondrites, Earth, Mars, Vesta and the Moon. Sources: CCs and NCs from Alexander 2019ab. Mars: Yoshizaki and McDonough (2020), Vesta: Dreibus and Wänke (1980), Moon: Hauri et al. (2015). Origin of D-type spherules: The Mg-Al-Fe plot in Figure 10 has also been used for classifying terrestrial komatiites, ultramafic lavas that are primarily found in the Archean (cf. Rickwood 1989). The only modification is that Fe is replaced with Fe+Ti. Such a plot is used in Figure 15 to further understand the origin of D-type spherules. The importance of this diagram is that it shows komatiites as separate fields from tholeiitic basalts and calc-alkaline and tholeiitic magma series. The blue outline shows the field of common terrestrial rock while the red outline includes all terrestrial igneous rocks. The importance for interpreting the D-type spherules is that all except some of the Si-rich D-type spherules are outside the field of common terrestrial igneous rocks and most of them are outside the red outline where there are no terrestrial igneous rocks. In particular, the low-Si BeLaU spherules are all close to the expected meteor path, except for two outside this field. The BeLaU spherules are also clearly different from the lunar high- K KREEP composition, which is the magmatic composition on the Moon with the highest concentration of Be, La and U. Martian SNC meteorites reflect the Fe-rich composition of the martian mantle and are the only known solar system igneous rocks that plot in the triangle between the red line and the Fe+Ti apex of the diagram. However, there are no Martian igneous rock that get as close to the Al-(Fe+Ti) side of the diagram as the BeLaU-type spherules. The BeLaU-type spherules composition could probably be produced by extreme differentiation of an iron-rich Martian-like magma that produced the igneous rocks among the Martian SNC meteorite. BeLaU spherules are observed to be depleted in volatile elements such as Zn, Mn, K, and Pb. In addition, potassium and Mn are both volatile during planet formation while U and Fe are more refractory, so planets end up with different K/U and Mn/Fe ratios. The data for the D-type spherules are shown in a K/U vs Mn/Fe diagram (Figure 16). The reason for using these elemental ratios is that they both have for a long time been used to distinguish materials from different bodies in the solar system (cf. Papike et al. 2017; Halliday and Porcelli 2001). This works because K and U are both highly enriched in melts, so their ratio does not change much during igneous processes. Therefore, unaltered igneous rocks typically directly reflect a ratio close to the planetary value. In contrast Fe and Mn are both roughly equally distributed between melts and solids, so their ratio also does not change during igneous processes. Since K and Mn are both volatile one would expect both to be lost from the spherules during their flight through the atmosphere. The D-type spherules are compared with primitive chondritic meteorite and planetary values in Figure 16. There are three distinct groups. The group A spherules are similar to the Earth values and could by this comparison represent some terrestrial volcanic material. We note that these are all Si-rich spherules which 14 eF/oC Primitive Spherules S-type 0.006 I-type high Ni I-type low Ni CCs NCs Planets 0.004 0.002 Earth Moon Mars Vesta 0.000 0.00 0.01 0.02 0.03 Mn/Fe eF/iN 0.10 0.08 S-type I-type high Ni I-type low Ni CCs NCs 0.06 Planets 0.04 Earth 0.02 Moon Mars Vesta 0.00 also make them similar in composition to terrestrial igneous rocks. Group B is strongly depleted in K relative to the Earth. Group C is strongly depleted in both K and Mn relative to the Earth. Most of the BeLaU spherules are in the group C field and none are in the Earth-like group A field. This shows that all the BeLaU spherules have exceptionally high volatile element loss, suggestive of extraterrestrial origin. Al Atom % 0 D-type, high Sr high Si 100 D-type, high Sr low Si D-type, low Sr high Si D-type, low Sr low Si 10 D-type, BeLaU low Si 90 D-type, BeLaU high Si Mars SNC meteorites Moon High-K KREEP 20 Reference values 80 Rock Type Dividing Lines Field of Terrestrial Igneous Rocks Most Common Terrestrial Igneous Rocks 30 AGV1 UCC 70 40 60 50 Calc-alkaline Tholeiitic 50 Mg-rich BCR1 60 N M - ORB Tholeiite BHVO1 F T e h - o r l i e c i h ite 40 70 30 Basaltic 80 Komatiite 20 90 Komatiite 10 BSE CI 100 0 Mg 0 10 20 30 40 50 60 70 80 90 100 Fe+Ti Figure 15. Atomic Mg-Al-Fe plot (atom %) Comparison of IM1 site spherules to differentiated materials from Earth (same references as for Figure 7), Moon (High-K KREEP; Warren (1989)) and Mars (SNC meteorites; Lodders (1998)). D-type Spherules 102 103 104 105 K/U 15 eF/nM 10-1 Vesta Mars CI 10-2 B Moon Earth A 10-3 C High Sr high Si High Sr low Si Low Sr low Si BeLaU low Si BeLaU high Si Planets 10-4 CI Chondrite Figure 16. A plot of Mn/Fe vs K/U for D-type spherules compared to CI chondrites, Earth, Mars, Vesta and the Moon. Sources: Anders and Grevesse 1989; McDonough and Sun 1995 Mars: Yoshizaki and McDonough (2020), Vesta: Dreibus and Wänke (1980), Moon: Hauri et al. (2015). Origin of the novel BeLaU-type spherules: The spherules with enrichment of beryllium (Be), lanthanum (La) and uranium (U), labeled “BeLaU”, appear to have an exotic composition different from other Solar System materials. The results for the “BeLaU” spherule S21 are displayed in Figures 17a and 17b. We use this spherule to point out some of the unique feature of the “BeLaU” elemental composition. A plot of the elemental abundances of the spherule S21 (normalized to CI chondrites) as a function of atomic number for 56 elements is shown in Figure 17a. Across the diagram the peak abundances are for Be, La and U, hence the name “BeLaU.” The abundance pattern of S21 implies derivation from a planetary crust, highly enriched in refractory lithophile elements (red dots). The volatile element abundances (green dots) are very low, suggesting either derivation from an extremely volatile-depleted planet or evaporative loss during passage through the Earth’s atmosphere. The very low content of refractory siderophile elements with affinity to iron (Re) suggest a source planet with an Fe core. Since there are strong indications that the spherules are derived from a differentiated planet, the data are also plotted in Figure 17b as a function of an igneous compatibility sequence. Compatibility is a geochemical parameter measuring how readily a particular element substitutes for a major element in mantle source minerals during melting to produce magma. It also roughly represents the sequence of enrichments of elements in a crystallizing magma. The abundances of elements as function of their compatibility for all 12 “BeLaU”-type spherules are shown in Figure 18. The “BeLaU” spherules’ variations in the abundances of trace elements relative to CI chondrites are higher by 1-3 orders of magnitude compared to cosmic spherules from the solar system reviewed by Folco et al. (2015). The “BeLaU” element patterns are compared in Figure 19 with the highly enriched sources of differentiated bodies in the solar system, including Earth’s upper continental crust (Rudnick and Gao, 2014) and kimberlites (Giuliani et al., 2020), lunar magma ocean residual liquid (KREEP) (Warren, 1989), Shergottites from Mars (Lodders, 1998; Jambon et al., 2002) and eucrites from Vesta (Kitts and Lodders, 1998). Figure 19 presents the comparison of refractory lithophiles that are not easily lost by evaporation or altered by fluids. Shergottites and eucrites are markedly distinct from the “BeLaU” samples due to the systematically lower incompatible element enrichments. The upper continental crust is also overall depleted in incompatible elements compared to “BeLaU.” Additionally, “BeLaU” samples have prominent negative anomalies of Ti, Li, higher Lu/Al, and variable Be and Sr enrichments that do not match the smooth pattern of the upper continental crust. Kimberlite is also remarkably distinguished from the “BeLaU” pattern in their Ta and Nb positive anomalies and the strong heavy rare earth element depletion. Lastly, despite the resembling overall element enrichments, the lunar KREEP displays pronounced differences in light rare earth element enrichment and strong Sr, Eu, and Cr negative anomalies from “BeLaU” that distinguish the two groups. Figure 20 compares the BeLaU elemental pattern with the average upper continental crust composition. This shows that BeLaU-type spherules are depleted by a factor of 2 to more than 10 for all volatile elements (Na, K, Mn, Zn, Rb, Cs, Tl, Pb and Bi), while refractory lithophile elements are enriched by a factor of 3- 20 compared to the average continental crust. Also, the rare earth element pattern is substantially fractionated when compared to the average upper continental crust. We must conclude that the elemental pattern of the BeLaU spherules is very different from the upper continental crust composition. The volatile elements (such as K, Mn, Zn and Pb) were most likely lost by evaporation during the passage of a bolide like IM1 through the Earth’s lower atmosphere. We pointed out earlier the difference of the BeLaU signature from KREEP in major elements (Figure 15). In spite of some distinct differences from KREEP there are enough similarities in the elemental composition to consider a similar type of origin for both patterns. The lunar KREEP composition is widely believed to be the result of crystallization of an early lunar magma ocean (Snyder et al., 1992; Rapp and Draper, 2018; Charlier et al., 2018). We conclude that the “BeLaU” samples possibly reflect a highly differentiated and extremely evolved composition, but from an unknown source. 16 Figure 17: a) The “BeLaU” elemental abundances of the spherule S21 (normalized to CI chondrites) versus atomic number for 56 elements. The solar system standard of CI chondrites is represented by a value of unity on the plot. b) Abundances versus compatibility (see text) for S21. Elements ordered with increasing compatibility towards the right. BeLaU-type Spherules U BeThBaLaCePrNdTaNb Zr Hf SrSmEuGd Ti TbDyHo Y ErTm Li YbLu Al CaSc V FeCoMgNi Cr Figure 18. Abundances of refractory lithophile elements as function of their compatibility for all 12 “BeLaU”-type spherules. 17 IC/lpmaS 10000 1000 100 10 S10 IS4B SPH1 1 S21 IS14 SPH1 (6) IS14 SPH4 (19) IS4 SPH8 IS14 SPH3 0.1 17NMAG_35 17NMAG_33 17NMAG_2 19MAGx_4 0.01 17NMAG_29 (25) IS13 SPH5 17NMAG_5 Compatibility 0.001 U BeThBaLaCePrNdTaNbZr HfSrSmEuGdTiTbDyHo Y ErTmLiYbLuAlCaSc V FeCoMgNiCr Figure 19. The “BeLaU” element abundance and pattern distinguish from the enriched sources from the solar system bodies. Elements are ordered with increasing compatibility. Data source: Earth’s upper continental crust (Rudnick and Gao, 2014); kimberlites (Giuliani et al., 2020); lunar KREEP (Warren, 1989); shergottites (Shergotty, Zagami, and Los Angeles) (Lodders, 1998; Jambon et al, 2002); eucrites (Bouvante, Pomozdino, and Stannern) (Kitts and Lodders, 1998). Figure 20. Comparison of average BeLaU-type spherules with average upper continental crust. 18 IC/elpmaS 1000 100 10 1 0.1 UCC Kimberlite Shergotty (Mars) Zagami (Mars) 0.01 Los Angeles (Mars) Bouvante (Vesta) Pomozdino (Vesta) Stannern (Vesta) 0.001 KREEP (Moon) Average BeLaU Compatibility 0.0001 Comparison of Upper Continental Crust (UCC) and BeLaU spherules LiBeNaMgAlP KCaScTi VCrMnFeCoNiCuZnGaGeAsSeRbSrYZrNbMoAgCdSbCsBaLaCePrNdSmEuGdTbDyHoErTmYbLuHfTaWTlPbBiThU CCU/UaLeB 100 Av BeLaU Mo Average UCC Cr Be Fe Lu Y 10 W Ge Se La Sc U 1 Na Mg Zn Cs Pb Mn K Rb 0.1 Tl Bi Conclusions The magnetic sled survey around IM1’s path during 14–28 June 2023 resulted in 850 magnet particles (consisting mostly of spherules) of diameters within the range of 0.1-1.3 millimeters through 26 runs surveying 0.06 km2. It is not yet clear as to whether any of these specimens are associated with the IM1 bolide. We identified four distinct groups of primitive spherules (S-type, G-type, I-type high Ni, I-type low- Ni). We also identified a substantial fraction (22%) of the spherules as being derived from igneous precursors. As these are clearly not related to typical achondrite meteorites as for previously discussed differentiated spherules we denote these new types of differentiated spherules as D-type spherules. The D- type spherules were classified into four distinct groups. The chemical compositions of 10 % of the spherules show extremely strong enrichment of refractory lithophile elements such as Be, La and U (BeLaU-type spherule), but very low refractory siderophile elements such as Re. Volatile elements, such as K, Mn, Zn and Pb are very low in the BeLaU-type spherules and were most likely lost by evaporation during passage through the Earth’s lower atmosphere. While the BeLaU-type spherules clearly appear to be derived from material formed by igneous fractionation, their chemical composition is novel in that there it is different from known existing solar system materials that have been analyzed thus far, with the KREEP component of the lunar crust being closest. The “BeLaU” samples reflect a highly differentiated, extremely evolved composition, of an unknown origin. These interpretations will be considered critically along with additional results from spherule analysis in future publications. Recovering larger pieces of similar composition from the search area and comparing the findings to distant control regions would certainly help in the interpretation. Author contributions. A. Loeb served as the chief scientist of the expedition, which was coordinated by R. McCallum and funded by C. Hoskinson. All other co-authors were involved in the retrieval and analysis of the spherules sample. The analysis was performed in the laboratories of S. 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(2024) The identification of airbursts in the past: Insights from the BIT-58 layer, Earth Planet. Sci. Lett. 627, 118562. https://doi.org/10.1016/j.epsl.2023.118562 Warren, P.H. (1989) KREEP: major-element diversity, trace-element uniformity (almost)., in: Moon in transition: Apollo 14, KREEP, and evolved lunar rocks, pp. 149–153. https://ui.adsabs.harvard.edu/abs/1989mtak.conf..149W Yoshizaki, T., McDonough, W.F. (2020). The composition of Mars. Geochim. Cosmochim. Acta 273, 137162. https://doi.org/10.1016/j.gca.2020.01.011 21 Supplementary Material. Data tables in Excel spreadsheets: Table S1. Major and trace elements concentrations (ppm) measured by micro-XRF for 745 samples (data plotted in Figures 5, 6, 7, 8, 9a, 10a). Table S2. Major elements, Be, Cr, Co, Ni, Sr, La and U concentrations (ppm) measured by ICP-MS for 68 samples (data plotted in Figures 9b, 10b, 11, 12, 13, 14, 15). Table S3. Elemental data (ppm) measured by ICP-MS for 12 BeLaU-type spherules and the CI normalizing values of Anders and Grevesse (1989). Table S4. Electron microprobe data on the chemical composition in the different region on the surface of the spherule S21, as labeled in Figure S1. Element Pt#1 Pt#2 Pt#3 Pt#4 Pt#5 Pt#6 Pt#7 (weight %) (weight %) (weight %) (weight %) (weight %) (weight %) (weight %) C 0.64 0.7 1.5 2.1 5.48 2.66 O 13.95 28.9 32.35 29.18 18.66 34.19 Na 0.63 0.73 0.7 0.72 Mg 0.28 0.42 0.15 Al 2.93 3.48 1.15 2.45 1.44 1.18 Si 6.4 10.85 2.92 4.2 0.97 P 0.31 Cl 0.26 0.4 0.51 1.28 K 0.39 Ca 3.88 4.55 1.73 1.85 0.23 Cr 0.31 Fe 70.65 50.78 99.3 65.01 59.69 66.22 60.77 Total 100 100 100 100 100 100 100 22 Figure S1. An example of a large (1.3 mm in maximum diameter, 0.9 mm average) spherule in the region along IM1's path is S21 (IS14-SPH1) from run 14. An example of a large (1.3 mm in maximum diameter, 0.9 mm average) spherule in the region along IM1’s likely path is S21 (IS14-SPH1) from run 14. This lopsided spherule, shown in Fig. S1, is a composite of three spherules that solidified shortly after merger but too late for the merger product to become spherical. The mass of S21 (1.7 mg) is about twice that of IS16A SPH1 (0.84 mg). The existence of a triple-merger like S21 can potentially be explained as a product of a meteoric airburst. The total mass collected by S21- like spherules in all our runs is of order ~0.1g. Given the sled’s width of 1m, the total surveyed area, ~0.06 km2, constitutes a fraction of ~10-3 of IM1’s strewn field. This implies a total mass in S21-like spherules in our estimated strewn field of order ~100g, as expected given that most of IM1’s mass evaporated to undetectable particles (well below tens of µm in size) or gas (Tillinghast-Raby et al., 2022). Assigning a mass of ~10-3 g per spherule implies a total number of ~105 such spherules. Based on IM1’s speed and fireball energy, the total mass ablated by IM1’s fireball is ~5x105 g corresponding to an object radius of R ~50 cm (Siraj and Loeb, 2022b). The total number of spherules divided by the initial volume associated with R yields an initial spherule number density of n ~0.2 cm-3 which gets diluted as the material expands. For the characteristic diameter of a spherule, ~1mm, the geometric cross-section for spherule-spherule collisions is σ ~ 4x10-2 cm2. The resulting collision probability is τ ~ nσ(2R) ~ (0.2 cm-3) x (4x10-2 cm2) x (100 cm) ~0.8, implying a likelihood of τ2 ~0.6 for triple-spherule mergers such as S21. Mergers that occur inside a liquid envelope would result in a spherical shell with embedded sub-spherules inside of it. Additional images of spherules are shown in Figure S2. 23 Figure S2. BSE images displaying varied morphologies of the samples in this study: a) IS8M2-1 (I-type, low Ni), b) IS13M1-19 (D-type, low Sr, low Si), c) IS20M-18 (S-type spherule displaying a polyhedral or “turtle-back” morphology), d) IS22M-16 (D- type, high Sr, low Si), e) IS14M(A)-7 (S-type spherule), and f) IS22M1-18 (identified as “shard,” no compositional classification). The scale bars indicate 100 microns. Comparison to Coal Fly Ash and Spherule Data Reported by Rudraswami et al. (2016) Comparison of Fly Ash and BeLaU spherules LiBeNaMgAlPKCaScTiVCrMnFeCoNiCuZnGaGeAsSeRbSrYZrNbMoAgCdSbCsBaLaCePrNdSmEuGdTbDyHoErTmYbLuHfTaWTlPbBiThU Figure S3. Comparison BeLaU with the NIST coal fly ash standard SRM1633a for 55 elements. It has been claimed that the compositions of BelaU spherules are consistent with coal ash (Gallardo 2023). The National Institute of Standards and Technology (NIST) has provided standards of coal fly ash. The best documented standard for many elements is SRM 1633a (Jochum et al. 2005). We compare the 24 UaLeB/a3361MRS 100 Tl Bi Fly Ash (NIST SRM1633a) As Average BeLaU Se Cd Pb 10 Zn Sb Rb Cs K P Ge 1 Na 0.1 Cr average composition of BeLaU spherules for 55 elements with the SRM1633a coal fly ash standard in Figure S3. Many volatile elements (Zn, As, Se, Cd, Tl, Pb and Bi) are enriched in the coal fly ash by factors of about 10 to 100 compared to the BeLaU spherules. Some refractory elements (Be, Ca, Cr, Fe, Y, Tm, Yb, Lu W) are depleted by factors of 3 to 10 in coal fly ash when compared to BeLaU spherules. Thus, BeLaU spherules do not have the composition of coal fly ash, making the claim of Gallardo (2023) invalid (Loeb et al. 2024a). The BeLaU composition shows an excess of Be, La and U, and other elements by up to three orders of magnitude relative to the solar system standard of CI chondrites. Many of these elements are 1–2 orders of magnitude more abundant than for the spherules reported by Rudraswami et al. (2016) (their Figure 2). All spherules, except for one, reported by Rudraswami et al. (2016) are S-type spherules (Figure S4), and the one exception does not have trace element enrichments like our BeLaU spherules. Figure S4 Ternary Mg-Si-Fe plot (atom %) of spherules from Rudraswami et al. (2016) normalized to (Mg + Fe + Si) and plotted in elemental proportions. The spherules in this study have been characterized to be S-type spherules. 25 Table S1. Major and trace elements concentrations (ppm) measured by micro-XRF for 745 samples (data plotted in Figures 5, 6, 7, 8, 9a, 10a). Type Sub-type Track Sample name O Na Mg I-type High Ni 15 IS 15 MAG-1__5_2 274729 15459 340 I-type High Ni 6 IS 6_1 304404 0 1663 I-type High Ni 19 19MAGx_25 291485 0 576 I-type High Ni 8 IS 8-MAG-2__20_1 297798 1999 2288 I-type High Ni 12 IS 12-MAG-2__24_2 303632 15843 6400 I-type High Ni 12 IS 12-MAG-2__25_1 303632 15843 6400 I-type High Ni 12 IS 12 -MAG 1__32_1 297950 0 43 I-type High Ni 13 IS 13M UNSIFTED 1 s__14_1 301568 0 0 I-type High Ni 13 IS 13M UNSIFTED 60 s__14_1 302748 3873 1165 I-type High Ni 12 IS 12 -MAG 1__15_1 298838 0 374 I-type High Ni 14 IS 14M Unsifted__22_1 301799 0 7305 I-type High Ni 22 IS 22-MAG -1__12_1 302124 3920 900 I-type High Ni 12 IS 12-MAG-2__8_1 305536 9908 1127 I-type High Ni 14 IS 14M Unsifted__42_1 302032 2072 195 I-type High Ni 22 IS 22-MAG-3__8_1 300689 15033 4190 I-type High Ni 24 IS 24 -MAG__4_1 300929 4216 0 I-type High Ni 12 IS 12 -MAG 1__10_1 302259 0 201 I-type High Ni 12 IS 12-MAG-2__10_1 334652 23474 475 I-type Low Ni 17 17MAG_37 300569 1247 1270 I-type Low Ni 15 IS 15 MAG-1__3_1 304121 23761 0 I-type Low Ni 10 IS 10 -MAG__3_1 307534 8489 8556 I-type Low Ni 13 IS 13-M-1__11_1 303294 689 38 I-type Low Ni 16 IS 16 MAG_2__13_2 306420 3088 3762 I-type Low Ni 11 IS 11-MAG__13_1 303069 0 0 I-type Low Ni 12 IS 12 -MAG 1__33_1 306796 1290 1315 I-type Low Ni 20 IS 20 MAG__22_1 303053 721 508 I-type Low Ni 12 IS 12-MAG-2__26_1 307734 9472 0 I-type Low Ni 14 IS 14M Unsifted__38_1 304500 2098 608 I-type Low Ni 20 IS 20 MAG__33_2 317672 8769 107 I-type Low Ni 16 IS 16 MAG_2__2_2 305332 11039 589 I-type Low Ni 17 17MAG_42 306544 2546 3681 I-type Low Ni 19 19NMAG_3 304372 753 1487 I-type Low Ni 24 IS 24 -MAG__14_1 303837 1307 1283 I-type Low Ni 19 IS 19 M__23_1 305791 7426 359 I-type Low Ni 19 IS 19 M__24_1 301555 17591 3086 I-type Low Ni 12 IS 12-MAG-2__23_1 316414 13455 1868 I-type Low Ni 12 IS 12 -MAG 1__9_2 303406 0 551 I-type Low Ni 24 IS 24 -MAG__1_1 304920 660 1258 I-type Low Ni 16 IS 16 MAG_2__17_1 313828 2688 5057 I-type Low Ni 14 IS 14M UNSIFTED B 60 s_5_1 309689 7552 7565 I-type Low Ni 13 IS 13M UNSIFTED 60 s__27_1 306750 1912 2991 I-type Low Ni 19 19NMAG_46 305305 0 1566 I-type Low Ni 15 IS 15 MAG-1__4_1 317903 8047 3985 I-type Low Ni 13 IS 13M UNSIFTED 60 s__40_1 305544 709 319 I-type Low Ni 20 IS 20 MAG__32_1 310137 3592 3198 I-type Low Ni 13 IS 13M UNSIFTED 1 s__37_1 316618 629 6424 I-type Low Ni 8 IS 8-MAG-2__6_2 301860 4121 109 I-type Low Ni 24 IS 24 -MAG__7_1 306571 3804 0 I-type Low Ni 12 IS 12-MAG-2__2_2 303385 6386 44 I-type Low Ni 17 IS 17-MAG__4_1 308712 522 1698 I-type Low Ni 17 17NMAG_30 300436 25 1427 I-type Low Ni 22 IS 22-MAG-3__9_2 308601 1625 649 I-type Low Ni 19 IS 19 M__8_1 301286 598 0 I-type Low Ni 19 IS 19 M 24 Small 302242 22600 3702 I-type Low Ni 12 IS 12 -MAG 1__5_1 306791 2481 1814 I-type Low Ni 13 IS 13M UNSIFTED 60 s__37_1 317105 5035 11639 I-type Low Ni 13 IS 13-M-1__1_1 302524 12630 203 I-type Low Ni 13 IS 13M UNSIFTED 60 s__12_1 311555 3571 6895 I-type Low Ni 13 IS 13M UNSIFTED 60 s__24_1 304994 2598 600 I-type Low Ni 13 IS 13M UNSIFTED 1 s__27_1 306739 12459 3969 I-type Low Ni 14 IS 14M Unsifted__15_1 304205 10353 734 I-type Low Ni 13 IS 13M UNSIFTED 1 s__12_1 312012 0 6130 I-type Low Ni 9 IS 9C S18 303107 413 343 I-type Low Ni 20 IS 20 MAG__31_1 302571 71764 1066 I-type Low Ni 19 IS 19 M__15_1 316972 44498 12078 I-type Low Ni 13 IS 13M UNSIFTED 60 s__25_1 325212 83 6902 I-type Low Ni 8 IS 8-MAG-2__29_2 317850 83137 4147 I-type Low Ni 8 IS 8-MAG-2__14_1 304988 1289 1685 I-type Low Ni 19 IS 19 M__11_1 308426 1331 1121 I-type Low Ni 12 IS 12 -MAG 1__1_1 305523 0 953 I-type Low Ni 12 IS 12-MAG-3__8_1 302331 3397 0 I-type Low Ni 13 IS 13M UNSIFTED 60 s__61_1 308334 5484 2485 I-type Low Ni 13 IS 13M UNSIFTED 60 s__54_1 306127 16085 3746 I-type Low Ni 19 19MAG_3 305049 0 2051 I-type Low Ni 17 17MAG_44 304852 1048 1630 I-type Low Ni 13 IS 13M UNSIFTED 1 s__40_1 305830 0 0 I-type Low Ni 15 IS 15 M 2__1_1 307071 26682 192 I-type Low Ni 20 IS 20 MAG__19_2 308853 3007 4221 I-type Low Ni 12 IS 12 -MAG 1__39_2 303983 0 2389 I-type Low Ni 15 IS 15 MAG-1__7_2 300615 68362 0 I-type Low Ni 10 IS 10 -MAG__1_1 310690 25911 2354 I-type Low Ni 13 IS 13M UNSIFTED 60 s__56_1 304021 3135 488 I-type Low Ni 22 IS 22 MAG-2__2_1 311239 6443 1115 I-type Low Ni 19 IS 19 M__10_1 313124 26606 3863 I-type Low Ni 12 IS 12-MAG-3__3_1 311601 30776 1513 I-type Low Ni 24 IS 24 -MAG__6_1 304628 3489 109 I-type Low Ni 13 IS 13M UNSIFTED 60 s__41_1 304452 786 627 I-type Low Ni 12 IS 12 -MAG 1__36_1 310819 2860 0 I-type Low Ni 12 IS 12 -MAG 1__41_1 303105 2134 505 I-type Low Ni 9 IS 9-MAG__2_1 321539 0 10430 I-type Low Ni 19 IS 19 M__5_1 304980 7650 415 I-type Low Ni 15 IS 15 C_1 303211 0 0 I-type Low Ni 22 IS 22 MAG-2__4_1 311591 25815 833 I-type Low Ni 9 IS 9-MAG__13_1 322906 1351 8302 I-type Low Ni 11 IS 11-MAG__6_1 307017 22785 1929 I-type Low Ni 12 IS 12 -MAG 1__11_2 304108 0 386 I-type Low Ni 17 17NMAG_10 303211 0 359 I-type Low Ni 11 IS 11-MAG__16_1 306152 4015 1130 I-type Low Ni 13 IS 13-MAG B__1_1 318856 9258 1787 I-type Low Ni 9 IS 9-MAG__12_1 305239 11302 259 I-type Low Ni 19 IS 19 M__20_1 307664 14294 1205 I-type Low Ni 14 IS 14M Unsifted__26_1 304683 1675 141 I-type Low Ni 8 IS 8-MAG-2__15_2 312871 11036 2424 I-type Low Ni 12 IS 12 -MAG 1__22_1 304282 943 0 I-type Low Ni 12 IS 12 -MAG 1__23_1 304282 943 0 I-type Low Ni 17 IS 17-MAG__2_1 305218 13267 1465 I-type Low Ni 24 IS 24 -MAG__3_1 303392 1129 0 I-type Low Ni 16 IS 16 MAG_2__16_1 301584 62995 0 I-type Low Ni 13 IS 13M UNSIFTED 60 s__15_1 307017 3900 1068 I-type Low Ni 8 IS 8-MAG-2__32_2 299878 6331 241 I-type Low Ni 8 IS 8-MAG-2__24_1 321588 5077 1095 I-type Low Ni 13 IS 13M UNSIFTED 60 s__58_1 304529 0 898 I-type Low Ni 20 IS 20 MAG__24_2 307420 4875 614 I-type Low Ni 8 IS 8-MAG-2__10_2 306838 16907 1744 I-type Low Ni 20 IS 20 MAG__23_1 303529 578 0 I-type Low Ni 8 IS 8-MAG-2__13_2 304694 6798 271 I-type Low Ni 19 IS 19__2_1 306343 2948 1441 I-type Low Ni 9 IS 9-MAG__8_1 309129 8807 520 I-type Low Ni 17 IS 17-MAG__13_1 319034 28867 4116 I-type Low Ni 19 IS 19 M__9_1 302780 4699 62 I-type Low Ni 7 IS 7 MAG__1_1 309721 14287 799 I-type Low Ni 20 IS 20 MAG__17_2 302407 0 327 I-type Low Ni 16 IS 16 MAG_2__6_2 302723 0 0 I-type Low Ni 12 IS 12-MAG-2__22_1 302679 311 0 I-type Low Ni 19 19NMAG_66 303100 1518 628 I-type Low Ni 8 IS 8-MAG-2__12_2 303698 545 398 I-type Low Ni 13 IS 13M UNSIFTED 1 s__24_1 305375 0 0 I-type Low Ni 20 IS 20 MAG__26_2 307435 2168 2340 I-type Low Ni 19 IS 19 M__26_1 303824 547 0 I-type Low Ni 13 IS 13M UNSIFTED 60 s__21_1 314461 4386 3424 I-type Low Ni 16 IS 16 MAG_2__19_1 302695 26223 0 I-type Low Ni 11 IS 11-MAG__3_1 302476 5357 0 I-type Low Ni 13 IS 13M UNSIFTED 60 s__45_1 304274 3406 292 I-type Low Ni 8 IS 8-MAG-2__16_1 303874 0 0 I-type Low Ni 12 IS 12 -MAG 1__30_1 304146 484 551 I-type Low Ni 13 IS 13-M-1__20_1 309800 2260 709 I-type Low Ni 12 IS 12 -MAG 1__27_1 315155 6798 9696 I-type Low Ni 21 IS 21__2_1 305416 532 0 I-type Low Ni 13 IS 13M UNSIFTED 1 s__25_1 321377 0 6183 I-type Low Ni 12 IS 12-MAG-2__21_2 303142 4282 0 I-type Low Ni 13 IS 13M UNSIFTED 60 s__63_1 309629 0 849 I-type Low Ni 22 IS 22-MAG -1_right__3_1 302585 0 0 I-type Low Ni 12 IS 12-MAG-2__17_2 304442 3901 502 I-type Low Ni 13 IS 13-M-1__17_1 307994 1208 2065 I-type Low Ni 8 IS 8-MAG-2__27_1 301094 0 635 I-type Low Ni 22 IS 22-MAG-3__7_1 305239 143 3790 I-type Low Ni 11 IS 11-MAG__9_1 303248 3760 0 I-type Low Ni 14 IS 14M Unsifted__9_1 306804 1849 894 I-type Low Ni 12 IS 12-MAG-2__14_2 308090 9670 757 I-type Low Ni 14 IS 14M Unsifted__19_1 303889 3449 117 I-type Low Ni 12 IS 12 -MAG 1__21_2 323199 0 0 I-type Low Ni 8 IS 8-MAG-2__1_1 302148 2528 0 I-type Low Ni 4 IS 4-MAG-A__6_2 299707 4128 0 I-type Low Ni 19 19MAGx_13 301177 0 0 I-type Low Ni 19 19NMAG_62 301190 0 0 I-type Low Ni 8 IS 8-MAG-2__26_1 302948 2292 0 I-type Low Ni 15 IS 15 B_1 302555 0 0 I-type Low Ni 19 19NMAG_64 300566 2187 454 I-type Low Ni 4 IS 4-MAG-A__2_2 301636 4612 276 I-type Low Ni 16 IS 16 MAG_2__5_2 301914 0 0 I-type Low Ni 19 19NMAG_59 300764 0 59 I-type Low Ni 19 19MAGx_17 301508 0 0 I-type Low Ni 19 19NMAG_72 291486 0 0 I-type Low Ni 19 19MAGx_16 299706 0 0 I-type Low Ni 8 IS 8-MAG-2__4_2 303195 1078 26 I-type Low Ni 19 19NMAG_63 301288 558 181 I-type Low Ni 24 IS 24 -MAG__2_1 302160 8166 0 I-type Low Ni 12 IS 12 -MAG 1__26_1 301734 0 0 I-type Low Ni 19 19MAGN_61 301094 0 0 I-type Low Ni 19 19NMAG_56 301816 0 232 I-type Low Ni 17 IS 17-MAG__16_1 299372 1412 566 I-type Low Ni 12 IS 12 -MAG 1__29_1 302833 0 0 I-type Low Ni 21 IS 21__3_1 302564 0 351 I-type Low Ni 19 IS 19 M__22_1 303896 7406 0 I-type Low Ni 19 19MAG_4 part2 301434 0 859 I-type Low Ni 17 17NMAG_13 302636 0 277 I-type Low Ni 12 IS 12-MAG-2__15_1 303075 3030 0 I-type Low Ni 13 IS 13M UNSIFTED 1 s__45_1 304219 0 0 I-type Low Ni 13 IS 13M UNSIFTED 1 s__58_1 303600 0 0 I-type Low Ni 13 IS 13-M-1__4_1 302291 28908 22 I-type Low Ni 19 19MAG_2 302995 0 1010 I-type Low Ni 13 IS 13M UNSIFTED 1 s__41_1 302236 11252 2706 I-type Low Ni 19 19NMAG_55 300711 0 784 I-type Low Ni 17 17NMAG_33 303534 0 0 I-type Low Ni 12 IS 12 S3_1 308739 109 0 I-type Low Ni 13 IS 13M UNSIFTED 1 s__50_1 306017 0 0 I-type Low Ni 13 IS 13M UNSIFTED 1 s__56_1 304250 0 0 I-type Low Ni 17 17MAG_22 302679 0 148 I-type Low Ni 13 IS 13M UNSIFTED 60 s__50_1 306219 2032 593 I-type Low Ni 13 IS 13M UNSIFTED 60 s__19_1 304622 13 0 I-type Low Ni 13 IS 13M UNSIFTED 1 s__19_1 305194 0 0 I-type Low Ni 13 IS 13M UNSIFTED 1 s__15_1 304430 8872 0 I-type Low Ni 19 19NMAG_1 302643 0 1387 I-type Low Ni 13 IS 13M UNSIFTED 1 s__63_1 307685 3607 0 I-type Low Ni 13 IS 13M UNSIFTED 1 s__17_1 302515 6464 0 I-type Low Ni 19 19NMAG_45 304570 1049 1697 I-type Low Ni 13 IS 13M UNSIFTED 60 s__17_1 302010 7842 389 I-type Low Ni 17 17NMAG_1 304293 831 1338 I-type Low Ni 15 IS 15 M 2__6_2 303118 45031 0 I-type Low Ni 19 IS 19 M__25_1 302451 57807 422 I-type Low Ni 17 17MAG_31 304884 0 808 I-type Low Ni 17 17MAG_21 307583 0 554 I-type Low Ni 24 IS 24 -MAG__13_1 307228 664 1791 I-type Low Ni 17 17MAG_17 314489 332 3192 I-type Low Ni 17 17MAG_7 314790 431 3272 I-type Low Ni 9 IS 9-MAG__14_1 306549 6991 915 I-type Low Ni 15 IS 15 M 2__7_1 307075 18239 721 I-type Low Ni 13 IS 13M UNSIFTED 1 s__54_1 306314 3743 289 I-type Low Ni 13 IS 13M UNSIFTED 1 s__61_1 307945 0 0 I-type Low Ni 17 17MAG_13 306549 842 1335 I-type Low Ni 17 17MAG_3 306743 1051 1360 I-type Low Ni 19 19NMAG_60 306014 7436 1930 I-type Low Ni 17 17NMAG_16 306426 1572 2501 I-type Low Ni 8 IS 8-MAG-2__7_1 313229 12079 3769 I-type Low Ni 17 17MAG_4 307099 6483 2845 I-type Low Ni 17 17MAG_14 307282 6613 2814 I-type Low Ni 19 19MAG_1 308981 383 2004 I-type Low Ni 17 17NMAG_3 309058 0 740 I-type Low Ni 8 IS 8-MAG-2__23_1 314708 4997 1727 I-type Low Ni 15 IS 15 MAG-1__8_2 305036 23560 799 I-type Low Ni 19 19MAG_4 part1 308221 0 1102 I-type Low Ni 17 17NMAG_33 TI 313464 0 0 I-type Low Ni 16 IS 16 MAG_2__15_1 320752 8234 0 I-type Low Ni 17 17MAG_45 319207 1275 3687 I-type Low Ni 14 IS 14M Unsifted__37_1 307241 15108 516 I-type Low Ni 4 IS 4-MAG-A__14_2 306685 37256 1523 I-type Low Ni 17 17NMAG_14 315012 0 6850 I-type Low Ni 13 IS 13M UNSIFTED 1 s__21_1 311553 762 1386 I-type Low Ni 17 IS 17-MAG__5_2 302101 41437 10841 I-type Low Ni 8 IS 8-MAG-2__5_1 318119 4581 1624 S-type 13 IS 13M UNSIFTED 60 s__39_1 424509 6207 300999 S-type 13 IS 13M UNSIFTED 1 s__39_1 426929 0 297282 S-type 19 IS 19 M__4_1 423368 7216 284811 S-type 13 IS 13-M-1__15_1 423460 11655 207412 S-type 14 IS 14M Unsifted__16_1 429669 1838 189171 S-type 13 IS 13 NM-1_1 409190 19531 238724 S-type 24 IS 24 -MAG__10_1 414197 5606 231467 S-type 12 IS 12 -MAG 1__4_2 426257 1196 174517 S-type 12 IS 12 -MAG 1__17_1 416818 1655 208220 S-type 13 IS 13M UNSIFTED 1 s__18_1 419059 0 210453 S-type 14 IS 14M Unsifted__17_1 420644 8407 172138 S-type 17 17MAG_25 430676 1001 123697 S-type 13 IS 13M UNSIFTED 1 s__22_1 413807 0 209210 S-type 13 IS 13M UNSIFTED 60 s__18_1 415868 5982 195664 S-type 13 IS 13M UNSIFTED 60 s__22_1 412143 3971 206779 S-type 22 IS 22-MAG -1__6_1 410058 6150 212022 S-type 13 IS 13M UNSIFTED 60 s__60_1 414126 30071 155147 S-type 12 IS 12-MAG-3__1_1 405851 5743 219176 S-type 17 IS 17-MAG__6_1 409178 1878 200909 S-type 19 19NMAG_6 429362 0 119911 S-type 13 IS 13M UNSIFTED 1 s__60_1 415101 18949 153922 S-type 19 19MAGx_9 403826 3268 215969 S-type 13 IS 13M UNSIFTED 1 s__30_1 411375 3511 158050 S-type 13 IS 13M UNSIFTED 60 s__30_1 411003 4453 155165 S-type 13 IS 13-M-1__10_1 409782 8888 162241 S-type 11 IS 11-MAG__2_1 400244 8028 213773 S-type 4 IS 4-MAG-A__13_2 404890 2454 198300 S-type 13 IS 13M UNSIFTED 1 s__2_1 404979 3124 165528 S-type 15 IS 15 MAG-1__9_1 403869 2570 188538 S-type 20 IS 20 MAG__16_1 401715 14025 176990 S-type 19 IS 19 M__2_1 405519 1672 184568 S-type 13 IS 13M UNSIFTED 1 s__33_1 397646 0 221201 S-type 17 17NMAG_7 404935 576 179978 S-type 13 IS 13M UNSIFTED 60 s__33_1 396531 4933 215750 S-type 22 IS 22-MAG -1_right__1_1 402847 1438 170453 S-type 17 17MAG_12 403453 732 173962 S-type 19 IS 19 M__6_1 397711 17093 180988 S-type 12 IS 12 -MAG 1__8_1 396431 2567 196626 S-type 20 IS 20 MAG__14_1 403281 4473 163112 S-type 12 IS 12 -MAG 1__28_1 391487 3917 198416 S-type 24 IS 24 -MAG__8_1 399426 9243 182589 S-type 11 IS 11-MAG-3__3_1 400735 13804 144242 S-type 11 IS 11-MAG__8_1 395308 837 188612 S-type 17 17MAG_2 402816 807 171423 S-type 8 IS 8-MAG-2__2_2 398296 11618 164366 S-type 13 IS 13M UNSIFTED 60 s__64_1 395157 2719 168690 S-type 13 IS 13M UNSIFTED 1 s__64_1 395504 0 171417 S-type 19 IS 19 M__7_1 409863 21459 116216 S-type 22 IS 22-MAG -1__15_1 410799 4097 130001 S-type 12 IS 12-MAG-2__12_2 398339 27823 147629 S-type 13 IS 13M UNSIFTED 60 s__20_1 403221 7352 147499 S-type 13 IS 13M UNSIFTED 1 s__20_1 402884 7077 148604 S-type 13 IS 13-M-1__7_1 393705 5416 194176 S-type 13 IS 13-M-1__13_1 392377 23543 176165 S-type 17 17MAG_1 387780 1159 200283 S-type 17 17MAG_11 387676 787 200340 S-type 16 IS 16 M 1__1_1 397982 23047 147977 S-type 19 19MAGx_10 390505 524 189744 S-type 17 IS 17-MAG__10_1 401322 5121 135113 S-type 19 19NMAG_68 NI 379679 0 162195 S-type 13 IS 13-M-1__2_1 392930 11271 160558 S-type 16 IS 16 MAG_2__11_1 392585 10715 152189 S-type 22 IS 22-MAG -1__4_2 384194 3258 186056 S-type 13 IS 13M UNSIFTED 60 s__10_1 410549 2802 117792 S-type 12 IS 12 -MAG 1__43_1 386998 2951 178097 S-type 12 IS 12 -MAG 1__13_1 391942 1973 181966 S-type 16 IS 16 MAG_2__1_1 390265 6364 186370 S-type 17 IS 17-MAG__14_1 393716 5683 172129 S-type 19 19NMAG_71 390771 0 172736 S-type 18 IS 18-MAG__2_1 387182 709 180884 S-type 13 IS 13M UNSIFTED 60 s__55_1 389798 5660 164231 S-type 14 IS 14M Unsifted__23_1 393024 2170 156739 S-type 19 19MAGx_5 393166 857 164627 S-type 13 IS 13M UNSIFTED 60 s__43_1 402816 12228 127159 S-type 17 17MAG_39 393964 758 157239 S-type 13 IS 13M UNSIFTED 1 s__65_1 393835 0 168839 S-type 12 IS 12 -MAG 1__2_1 390055 3486 185381 S-type 19 19MAGx_18 392870 0 157287 S-type 13 IS 13M UNSIFTED 60 s__34_1 386499 1873 174983 S-type 13 IS 13M UNSIFTED 60 s__65_1 394167 1888 162827 S-type 12 IS 12 -MAG 1__12_2 390458 397 165424 S-type 12 IS 12-MAG-2__1_1 391764 34887 135656 S-type 13 IS 13M UNSIFTED 1 s__34_1 386189 0 174984 S-type 4 IS 4-MAG-A__10_2 387464 18196 153478 S-type 13 IS 13M UNSIFTED 60 s__36_1 386733 4422 170722 S-type 13 IS 13M UNSIFTED 60 s__8_1 396434 129 139751 S-type 13 IS 13M UNSIFTED 1 s__43_1 401711 1298 131719 S-type 13 IS 13M UNSIFTED 60 s__2_1 393091 5716 149331 S-type 17 17NMAG_11 NI 373299 0 164624 S-type 13 IS 13M UNSIFTED 60 s__62_1 392909 8642 154631 S-type 20 IS 20 MAG__18_1 390754 3698 165615 S-type 4 IS 4-MAG-A__1_1 391862 3167 155502 S-type 13 IS 13M UNSIFTED 1 s__55_1 387716 248 156768 S-type 13 IS 13M UNSIFTED 1 s__10_1 408362 3768 101879 S-type 13 IS 13M UNSIFTED 1 s__36_1 386336 9433 162852 S-type 14 IS 14M Unsifted__18_1 378760 15774 176632 S-type 13 IS 13M UNSIFTED 1 s__62_1 394483 0 152458 S-type 13 IS 13M UNSIFTED 60 s__59_1 382106 2619 171259 S-type 22 IS 22-MAG -1__5_1 387769 2100 162890 S-type 13 IS 13M UNSIFTED 1 s__59_1 382423 152 172103 S-type 20 IS 20 MAG__10_2 385922 5603 175092 S-type 13 IS 13M UNSIFTED 1 s__8_1 394525 0 134670 S-type 17 17MAG_5 384722 4435 142980 S-type 17 17NMAG_9 387752 590 159571 S-type 12 IS 12 -MAG 1__16_2 392582 1569 141980 S-type 13 IS 13M UNSIFTED 1 s__57_1 387559 0 161666 S-type 24 IS 24_1 382774 832 166896 S-type 12 IS 12 -MAG 1__18_2 383750 1747 165346 S-type 16 IS 16 MAG_2__18_1 382297 35250 154487 S-type 8 IS 8-MAG-2__8_1 383587 444 163208 S-type 18 IS 18-MAG__4_1 378493 61459 144134 S-type 19 IS 19 M__21_1 380702 8096 165854 S-type 17 17NMAG_23 385013 854 161215 S-type 19 19NMAG_48 382990 1928 173897 S-type 8 IS 8-MAG-2__18_2 380087 20667 159243 S-type 13 IS 13M UNSIFTED 60 s__29_1 387367 0 148170 S-type 22 IS 22-MAG -1__22_2 377266 40443 151334 S-type 13 IS 13-M-1__6_1 378577 6524 171987 S-type 13 IS 13M UNSIFTED 60 s__57_1 384275 8322 154590 S-type 17 17MAG_15 383527 4391 137149 S-type 20 IS 20 MAG__11_1 382461 2744 170687 S-type 11 IS 11-MAG-3__2_2 387805 6333 153330 S-type 17 17NMAG_26 379501 1417 157207 S-type 19 19MAGx_1 380843 2513 163734 S-type 4 IS 4-MAG-A__12_1 381232 3839 157362 S-type 17 17MAG_10 385272 629 161503 S-type 13 IS 13M UNSIFTED 1 s__29_1 386587 0 141851 S-type 16 IS 16 MAG_2__3_1 381647 6672 153113 S-type 17 IS 17-MAG__1_1 387221 3741 148440 S-type 19 19MAGx_2 386114 0 142145 S-type 11 IS 11-MAG__7_1 379822 21810 160793 S-type 17 17MAG_20 384258 551 160477 S-type 13 IS 13M UNSIFTED 60 s__49_1 377028 4001 159079 S-type 24 IS 24 -MAG__9_1 379892 9425 164621 S-type 22 IS 22-MAG-3__5_1 377493 13803 158316 S-type 9 IS 9-MAG__9_1 385431 6131 149577 S-type 16 IS 16 M 1__3_1 379262 18258 146619 S-type 14 IS 14M Unsifted__3_1 374306 13713 157095 S-type 14 IS 14M Unsifted__43_1 374425 15367 159829 S-type 13 IS 13M UNSIFTED 1 s__49_1 377159 677 156463 S-type 17 17NMAG_11 375072 203 159579 S-type 14 IS 14M Unsifted__7_1 385942 3437 140193 S-type 15 IS 15 M 2__5_1 375263 34029 154842 S-type 13 IS 13M UNSIFTED 1 s__13_1 382128 0 158458 S-type 13 IS 13M UNSIFTED 60 s__13_1 381418 4902 153600 S-type 13 IS 13M UNSIFTED 60 s__47_1 377747 1790 151576 S-type 19 19NMAG_47 383577 1718 130369 S-type 17 17MAG_19 378881 141 142437 S-type 19 19MAGx_3 378285 0 146778 S-type 14 IS 14M Unsifted__21_1 378985 775 152943 S-type 22 IS 22-MAG-3__1_1 379542 8372 154466 S-type 13 IS 13M UNSIFTED 60 s__66_1 376510 5122 132240 S-type 22 IS 22-MAG -1__10_1 375415 4217 153202 S-type 12 IS 12-MAG-3__9_2 377946 13580 149391 S-type 22 IS 22-MAG -1__9_1 375055 2969 153340 S-type 19 19NMAG_53 376505 261 152475 S-type 13 IS 13M UNSIFTED 60 s__32_1 379317 11345 131291 S-type 13 IS 13M UNSIFTED 1 s__47_1 376041 0 150669 S-type 4 IS 4-MAG-A__16_1 378887 23471 127728 S-type 12 IS 12-MAG-2__19_2 377050 21534 134525 S-type 17 17NMAG_21 371953 145 148820 S-type 21 IS 21__1_1 373203 1147 150366 S-type 17 17MAG_18 371257 356 149113 S-type 17 17MAG_6 Ni 377094 0 145479 S-type 17 17MAG_9 377741 393 136845 S-type 9 IS 9-MAG__11_1 369549 22070 132957 S-type 13 IS 13M UNSIFTED 60 s__48_1 375086 2004 147777 S-type 24 IS 24 -MAG__12_1 374476 3459 140133 S-type 12 IS 12-MAG-3__2_2 371375 34685 117133 S-type 13 IS 13M UNSIFTED 1 s__48_1 375017 0 148109 S-type 13 IS 13M UNSIFTED 1 s__32_1 379746 1035 130212 S-type 17 17MAG_16 375990 519 142592 S-type 12 IS 12 -MAG 1__35_1 373818 7830 146280 S-type 9 IS 9-MAG__7_1 379971 8114 132614 S-type 17 17MAG_9 Ni 374902 0 138677 S-type 13 IS 13-M-1__3_1 378001 3156 151612 S-type 17 17MAG_6 375637 70 141349 S-type 17 17MAG_43 375030 2547 146452 S-type 4 IS 4-MAG-A__7_2 371096 5212 145881 S-type 14 IS 14M Unsifted__10_1 375986 0 128374 S-type 12 IS 12 -MAG 1__42_1 371517 2773 141660 S-type 13 IS 13-M-1__14_2 377496 23144 122658 S-type 12 IS 12-MAG-2__9_2 368173 20237 141666 S-type 13 IS 13M UNSIFTED 60 s__51_1 373830 8156 136496 S-type 20 IS 20 MAG__1_1 372851 5716 144065 S-type 17 17MAG_8 368718 617 146044 S-type 8 IS 8-MAG-2__30_1 371528 9795 137218 S-type 17 17MAG_19 Ni 373679 0 135439 S-type 19 19MAG_6 378722 0 131988 S-type 13 IS 13M UNSIFTED 1 s__66_1 374396 0 121926 S-type 12 IS 12 -MAG 1__31_1 379710 4441 125749 S-type 12 IS 12-MAG-2__5_2 376986 29016 111321 S-type 11 IS 11-MAG__1_1 373217 11194 131566 S-type 20 IS 20 MAG__4_1 369318 1780 144201 S-type 15 IS 15 MAG-1__2_1 370937 20285 123835 S-type 10 IS 10 -MAG__2_1 372166 39812 102606 S-type 9 IS 9-MAG__5_1 374237 9655 141036 S-type 11 IS 11-MAG__14_1 371673 4709 134151 S-type 8 IS 8-MAG-2__3_2 359089 107679 118941 S-type 8 IS 8-MAG-2__19_2 365953 22196 127730 S-type 12 IS 12 -MAG 1__38_1 366392 7667 128870 S-type 19 19MAGx_14 368669 1372 141865 S-type 17 17MAG_5 Fe 383950 2433 90895 S-type 12 IS 12 -MAG 1__40_1 370727 1653 142155 S-type 14 IS 14M Unsifted__13_1 367134 8334 146020 S-type 19 19NMAG_74 365689 0 128389 S-type 19 19MAGx_6 372389 813 119533 S-type 17 17NMAG_20 370520 286 138816 S-type 17 17MAG_40 403234 3473 54414 S-type 13 IS 13M UNSIFTED 60 s__16_1 381318 3144 104806 S-type 19 19NMAG_49 370319 0 128549 S-type 17 17MAG_26 371036 1648 131322 S-type 12 IS 12-MAG-3__11_1 356946 134119 98393 S-type 13 IS 13M UNSIFTED 1 s__51_1 371212 0 128067 S-type 17 17NMAG_25 367762 882 138793 S-type 15 IS 15 M 2__2_1 365517 27091 123832 S-type 13 IS 13M UNSIFTED 60 s__53_1 371443 9469 114131 S-type 13 IS 13M UNSIFTED 1 s__44_1 368900 0 126508 S-type 13 IS 13M UNSIFTED 1 s__23_1 371047 0 131794 S-type 4 IS 4-MAG-A__9_1 372479 7930 125426 S-type 13 IS 13-M-1__18_1 365438 35118 128515 S-type 13 IS 13M UNSIFTED 60 s__44_1 366644 3114 128126 S-type 12 IS 12-MAG-3__4_1 365468 11868 128423 S-type 19 19NMAG_54 363051 0 132898 S-type 13 IS 13M UNSIFTED 1 s__16_1 378318 0 103359 S-type 13 IS 13M UNSIFTED 60 s__53_1 1 370494 7575 111679 S-type 13 IS 13M UNSIFTED 60 s__53_1 B 370494 7575 111679 S-type 17 17NMAG_19 367483 0 119257 S-type 4 IS 4-MAG-A__11_2 367087 4979 129976 S-type 12 IS 12-MAG-3__7_2 370150 13965 115803 S-type 17 17MAG_5 Cr 350790 0 116990 S-type 4 IS 4-MAG-A__5_2 364901 6516 127519 S-type 13 IS 13M UNSIFTED 60 s__23_1 369828 1289 124191 S-type 15 IS 15 M 2__3_2 377178 0 104067 S-type 4 IS 4-MAG-A__8_2 363858 19925 122336 S-type 15 IS 15 MAG-1__12_2 365983 33703 99723 S-type 19 19NMAG_68 367180 0 104984 S-type 19 IS 19 M__1_1 360764 18503 118894 S-type 19 19NMAG_47-Ni 347055 0 82940 S-type 14 IS 14M Unsifted__45_1 365768 8030 126943 S-type 12 IS 12-MAG-2__7_2 362026 12355 127929 S-type 14 IS 14M Unsifted__34_1 361564 18690 124140 S-type 13 IS 13M UNSIFTED 1 s__53_1 372980 2239 96437 S-type 17 IS 17-MAG__7_2 363980 8002 121013 S-type 12 IS 12 -MAG 1__19_1 365921 0 121278 S-type 17 17NMAG_22 360451 0 116136 S-type 14 IS 14M Unsifted__8_1 366701 812 116550 S-type 4 IS 4-MAG-A__3_2 365103 6435 107461 S-type 17 17NMAG_12 361089 0 117706 S-type 19 IS 19 M 24 Large 364540 49495 99600 S-type 11 IS 11-MAG__12_1 368234 8172 118065 S-type 14 IS 14M Unsifted__5_1 366293 2782 115064 S-type 19 19MAGx_15 370226 520 102140 S-type 14 IS 14M Unsifted__44_1 361730 6849 117624 S-type 17 17NMAG_18 NI 357564 0 113415 S-type 19 19MAGx_12 361581 0 120731 S-type 14 IS 14M Unsifted__39_1 367746 1259 91307 S-type 13 IS 13-M-1__12_1 366626 3604 114981 S-type 17 17NMAG_26 NI 286392 0 89431 S-type 13 IS 13M UNSIFTED 1 s__5_1 360880 11082 112295 S-type 13 IS 13M UNSIFTED 60 s__5_1 362338 1554 113247 S-type 9 IS 9-MAG__10_1 370136 17673 58171 S-type 19 IS 19 M__17_1 360662 28557 90148 S-type 11 IS 11-MAG__5_1 366136 7504 103076 S-type 15 IS 15 MAG-1__6_1 363257 26980 91305 S-type 13 IS 13M UNSIFTED 1 s__31_1 357287 0 100716 S-type 12 IS 12 -MAG 1__6_2 363394 0 97661 S-type 17 IS 17-MAG__11_1 355538 38881 102306 S-type 12 IS 12 -MAG 1__37_1 363015 10870 99312 S-type 14 IS 14M Unsifted__12_1 356571 3799 113531 S-type 14 IS 14M Unsifted__41_1 357084 14762 113940 S-type 12 IS 12 -MAG 1__24_1 378208 3 57538 S-type 9 IS 9B S15 354458 805 113525 S-type 12 IS 12-MAG-2__13_1 349418 44344 102832 S-type 22 IS 22 MAG-2__1_1 357572 21747 92802 G-type 13 IS 13M UNSIFTED 60 s__31_1 355351 554 90465 G-type 8 IS 8-MAG-2__11_1 357208 8474 93016 G-type 19 IS 19 M__3_1 360493 30864 77353 G-type 19 19MAGx_22 344059 0 109472 G-type 15 IS 15 M 2__4_1 353694 55476 78226 G-type 12 IS 12 B_1 368411 823 63222 G-type 16 IS 16 MAG_2__12_1 357962 28965 81501 G-type 11 IS 11-MAG__11_1 364730 8567 73700 G-type 12 IS 12-MAG-2__20_1 350310 21238 99386 G-type 17 17NMAG_22 NI 336269 0 89668 G-type 23 IS 23 M__1_1 352447 9314 74961 G-type 17 17NMAG_18 354958 0 96309 G-type 14 IS 14M Unsifted__31_1 357474 11227 87198 G-type 16 IS 16 M 1__4_2 353641 4336 95788 G-type 13 IS 13M UNSIFTED 1 s__52_1 343901 0 96053 G-type 12 IS 12-MAG-2__16_1 348245 8453 92979 G-type 22 IS 22-MAG -1__21_2 358786 5275 72340 G-type 15 IS 15 MAG-1__1_1 355498 20718 89431 G-type 13 IS 13M UNSIFTED 60 s__11_1 350645 558 79357 G-type 17 IS 17-MAG__8_2 361608 47022 42746 G-type 13 IS 13M UNSIFTED 1 s__11_1 353094 0 72131 G-type 22 IS 22-MAG -1_right__2_1 353619 0 82844 G-type 20 IS 20 MAG__20_1 350246 5790 85655 G-type 13 IS 13M UNSIFTED 60 s__52_1 341358 0 88820 G-type 12 IS 12-MAG-2__11_1 346400 19129 86667 G-type 17 17NMAG_27 348925 0 76819 G-type 19 IS 19 M__19_1 362724 4658 47359 G-type 14 IS 14M Unsifted__28_1 349334 3676 78842 G-type 12 IS 12 -MAG 1__34_1 352140 15203 71386 G-type 20 IS 20 MAG__21_1 354097 967 67521 G-type 14 IS 14M Unsifted__20_1 358630 0 63086 G-type 19 19MAGx_11 359099 0 49463 G-type 9 IS 9-MAG__4_1 339786 4022 78928 G-type 16 IS 16 M 1__2_1 354153 21570 59244 G-type 14 IS 14M Unsifted__14_1 352159 88 83659 G-type 13 IS 13-MAG B__4_1 345516 18886 63884 G-type 11 IS 11-MAG__15_1 336416 6496 95302 G-type 12 IS 12-MAG-2__18_2 342171 24157 88719 G-type 19 19MAGx_8 345873 0 58888 G-type 14 IS 14M UNSIFTED B 60 s_8_1 336664 28680 74511 G-type 17 IS 17-MAG__3_1 351304 0 52913 G-type 12 IS 12-MAG-3__10_1 343264 15493 54634 G-type 19 19NMAG_51 345182 0 49683 G-type 24 IS 24_2 351608 762 56158 G-type 12 IS 12-MAG-2__4_2 355387 23962 38717 G-type 19 19MAGx_19 344882 0 46529 G-type 17 17MAG_40 Cu 357525 0 31244 G-type 13 IS 13M UNSIFTED 1 s__42_1 327446 0 67877 G-type 13 IS 13M UNSIFTED 60 s__42_1 326083 145 68734 G-type 14 IS 14M Unsifted__35_1 335228 1216 51206 G-type 17 17MAG_29 342864 249 48349 G-type 24 IS 24 -MAG__5_1 340260 10581 35862 G-type 13 IS 13-M-1__5_1 337168 4734 57868 G-type 14 IS 14M Unsifted__46_1 338658 0 41353 G-type 17 17MAG_38 Ni 2 323440 0 42638 G-type 17 17MAG_38 Ni 1 323342 0 36850 G-type 19 19MAGx_23 322806 0 43618 G-type 12 IS 12-MAG-2__3_1 328044 28748 34990 G-type 8 IS 8-MAG-2__17_2 335003 6231 27975 G-type 9 IS 9-MAG__6_1 322387 12044 25626 G-type 8 IS 8-MAG-2__31_2 338208 11794 14422 G-type 13 IS 13-MAG B__6_2 320600 9724 31562 G-type 17 IS 17-MAG__12_2 326308 4669 23151 G-type 14 IS 14M Unsifted__40_1 316210 0 29934 G-type 17 17MAG_38 318704 0 24428 G-type 23 IS 23 M__2_1 315572 0 27717 G-type 19 19MAGx_26 313495 0 25064 G-type 8 IS 8-MAG-2__25_1 314169 2042 26197 G-type 12 IS 12 -MAG 1__25_2 316372 0 18807 G-type 17 17MAG_30 332538 2223 15316 G-type 8 IS 8-MAG-2__28_1 313121 4155 19557 G-type 15 IS 15 MAG-1__11_1 326571 12153 12512 G-type 13 IS 13-MAG B__7_1 313702 1119 22777 G-type 22 IS 22-MAG -1__17_1 321809 3568 14547 G-type 19 IS 19__1_1 316606 6058 9016 G-type 20 IS 20 MAG__3_1 302106 0 19229 G-type 12 IS 12 -MAG 1__20_1 310861 1587 16986 G-type 13 IS 13M UNSIFTED 1 s__9_1 320215 0 7847 D-type High Sr, high Si 17 IS 17-MAG__17_2 433886 9357 8953 D-type High Sr, high Si 13 IS 13M UNSIFTED 1 s__3_1 465744 14498 5220 D-type High Sr, high Si 15 IS 15 MAG-1__10_1 438607 33752 3585 D-type High Sr, high Si 22 IS 22-MAG -1__3_2 452383 19390 4328 D-type High Sr, high Si 22 IS 22 MAG-2__8_1 426804 25964 6328 D-type High Sr, high Si 13 IS 13M UNSIFTED 60 s__3_1 463100 18292 10580 D-type High Sr, high Si 13 IS 13M UNSIFTED 1 s__1_1 433442 12348 7057 D-type High Sr, high Si 13 IS 13M UNSIFTED 60 s__1_1 432651 22002 12455 D-type High Sr, high Si 11 IS 11-MAG 2__1_1 437156 24059 10306 D-type High Sr, high Si 17 17MAG_33 Ni 457285 14467 8073 D-type High Sr, high Si 19 IS 19 M__14_1 451431 35573 3000 D-type High Sr, high Si 17 17MAG_36 424408 22240 12236 D-type High Sr, high Si 20 IS 20 MAG__7_2 412896 33192 10642 D-type High Sr, high Si 22 IS 22-MAG -1__7_1 419925 27766 11242 D-type High Sr, high Si 22 IS 22-MAG -1__8_1 419925 27766 11242 D-type High Sr, high Si 11 IS 11-MAG 2__3_1 443060 21195 10888 D-type High Sr, high Si 17 17NMAG_29 428520 22656 14645 D-type High Sr, high Si 17 17NMAG_5 449883 17085 5571 D-type High Sr, high Si 16 IS 16 MAG_2__4_1 438108 15952 67785 D-type High Sr, high Si 22 IS 22 MAG-2__6_1 436079 11419 27254 D-type High Sr, low Si 8 IS 8-MAG-2__9_2 421225 3465 2355 D-type High Sr, low Si 19 IS 19 M__16_1 408695 1778 8536 D-type High Sr, low Si 22 IS 22-MAG -1__20_1 397243 7029 9384 D-type High Sr, low Si 17 17MAG_35 Ni 1 403346 0 714 D-type High Sr, low Si 17 IS 17-MAG__15_1 391021 39726 5580 D-type High Sr, low Si 24 IS 24 -MAG__11_1 392147 15882 12288 D-type High Sr, low Si 17 17MAG_35 Ni 2 391872 0 838 D-type High Sr, low Si 19 19NMAG_50 378417 2222 12512 D-type High Sr, low Si 17 17MAG_35 372911 2299 4300 D-type High Sr, low Si 19 IS 19 M__18_1 369510 2982 8808 D-type High Sr, low Si 22 IS 22-MAG-3__4_2 362544 97144 14232 D-type High Sr, low Si 17 17MAG_33 350941 0 9317 D-type High Sr, low Si 17 17NMAG_6 353270 2353 7556 D-type High Sr, low Si 9 IS 9-MAG__3_1 345775 21453 16793 D-type High Sr, low Si 19 19MAGx_4 347850 9926 4935 D-type High Sr, low Si 14 IS 14M UNSIFTED B 60 s_2_1 333734 60742 5309 D-type High Sr, low Si 14 IS 14M Unsifted__48_1 344885 7822 11025 D-type High Sr, low Si 17 17NMAG_2 342753 1226 10054 D-type High Sr, low Si 15 IS 15 M 2__8_1 328989 73345 2554 D-type High Sr, low Si 13 IS 13-MAG B__3_2 314504 139827 1078 D-type High Sr, low Si 17 17NMAG_28 329648 0 628 D-type High Sr, low Si 22 IS 22-MAG -1__16_1 326467 4293 0 D-type High Sr, low Si 14 IS 14M Unsifted__47_1 329013 5190 2721 D-type Low Sr, high Si 13 IS 13 NM-2_1 452594 32227 4936 D-type Low Sr, high Si 14 IS 14 NM__1_1 470732 32625 1735 D-type Low Sr, high Si 17 IS 17-MAG__19_1 463670 32183 2658 D-type Low Sr, high Si 9 IS 9-NM_1 466003 31583 8480 D-type Low Sr, high Si 16 IS 16 MAG_2__14_1 447115 60422 1522 D-type Low Sr, high Si 17 17NMAG_4 460671 26930 9084 D-type Low Sr, high Si 20 IS 20 MAG__8_2 467580 28765 806 D-type Low Sr, high Si 12 IS 12 M4_1 461701 40861 16899 D-type Low Sr, high Si 13 IS 13 NM-1_2 447871 50816 9366 D-type Low Sr, high Si 22 IS 22 MAG-2__7_1 444757 65937 8190 D-type Low Sr, high Si 14 IS 14M Unsifted__4_1 464441 27797 10371 D-type Low Sr, high Si 12 IS 12-MAG-3__6_1 446815 59013 5124 D-type Low Sr, high Si 19 19MAG_10Fe 449248 27457 19308 D-type Low Sr, high Si 17 17MAG_28 Particle 2 449969 27637 9556 D-type Low Sr, high Si 17 17MAG_23 453317 29122 1411 D-type Low Sr, high Si 14 IS 14M UNSIFTED B 60 s_3_1 446133 30597 11779 D-type Low Sr, high Si 11 IS 11-MAG 2__2_2 445398 30319 12256 D-type Low Sr, high Si 12 IS 12-MAG-3__12_1 435658 48719 8952 D-type Low Sr, high Si 19 19NMAG_7 445505 26015 1709 D-type Low Sr, high Si 19 19NMAG_8 443276 14831 40910 D-type Low Sr, high Si 22 IS 22-MAG -1__2_2 440110 34934 923 D-type Low Sr, high Si 17 IS 17-MAG__18_2 447091 7253 2861 D-type Low Sr, high Si 20 IS 20 MAG__9_1 438556 28914 15167 D-type Low Sr, high Si 17 17MAG_27 439219 24942 4035 D-type Low Sr, high Si 19 IS 19__3_1 438905 34504 3011 D-type Low Sr, high Si 15 IS 15 M_1 435337 20077 39668 D-type Low Sr, high Si 14 IS 14M UNSIFTED B 60 s_4_1 432868 42545 10262 D-type Low Sr, high Si 19 19MAG_5 447848 26489 33684 D-type Low Sr, high Si 14 IS 14 NM__4_1 425715 33699 23071 D-type Low Sr, high Si 22 IS 22-MAG -1__19_1 427420 25527 1653 D-type Low Sr, high Si 14 IS 14M UNSIFTED B 60 s_6_1 424739 27994 2604 D-type Low Sr, high Si 19 19NMAG_5 437566 9007 3059 D-type Low Sr, high Si 19 19NMAG_8 Ti 430215 4446 0 D-type Low Sr, high Si 17 17NMAG_32 439629 3206 1869 D-type Low Sr, high Si 19 19NMAG_57 424905 20028 2145 D-type Low Sr, high Si 19 19NMAG_4 422780 17768 0 D-type Low Sr, high Si 19 19NMAG_7 Ti 418183 26951 0 D-type Low Sr, high Si 22 IS 22-MAG-3__10_1 411095 50410 2493 D-type Low Sr, high Si 13 IS 13M UNSIFTED 60 s__38_1 414005 21392 1305 D-type Low Sr, high Si 20 IS 20 MAG__5_1 419252 22982 39 D-type Low Sr, high Si 18 IS 18-MAG__1_1 402636 69149 485 D-type Low Sr, high Si 20 IS 20 MAG__28_2 415320 35576 852 D-type Low Sr, high Si 13 IS 13M UNSIFTED 60 s__28_1 417000 24028 1690 D-type Low Sr, high Si 16 IS 16 MAG_2__10_2 415191 36571 8497 D-type Low Sr, low Si 13 IS 13M UNSIFTED 1 s__28_1 416861 14098 0 D-type Low Sr, low Si 17 17MAG_28 Particle 1 412894 24553 1444 D-type Low Sr, low Si 17 17NMAG_31 414250 19824 3142 D-type Low Sr, low Si 19 19MAGx_7 412082 20789 2813 D-type Low Sr, low Si 22 IS 22-MAG -1__13_1 411523 23792 886 D-type Low Sr, low Si 17 17NMAG_8 406689 18030 1417 D-type Low Sr, low Si 13 IS 13M UNSIFTED 1 s__7_1 419069 2084 14009 D-type Low Sr, low Si 19 19MAGx_21 408206 26557 5491 D-type Low Sr, low Si 22 IS 22 MAG-2__3_1 399739 57659 3157 D-type Low Sr, low Si 13 IS 13M UNSIFTED 60 s__7_1 419916 5911 21699 D-type Low Sr, low Si 14 IS 14M UNSIFTED B 60 s_7_1 403493 41715 1954 D-type Low Sr, low Si 12 IS 12 -MAG 1__7_1 406772 20366 1614 D-type Low Sr, low Si 20 IS 20 MAG__25_2 404791 20375 2106 D-type Low Sr, low Si 11 IS 11-MAG__10_1 406264 25269 2098 D-type Low Sr, low Si 11 IS 11-MAG__4_1 405621 21909 1313 D-type Low Sr, low Si 19 IS 19 M__12_1 405510 40967 1214 D-type Low Sr, low Si 19 19NMAG_58 399114 20565 2051 D-type Low Sr, low Si 19 19NMAG_73 400576 18561 0 D-type Low Sr, low Si 13 IS 13M UNSIFTED 1 s__6_1 398404 22678 0 D-type Low Sr, low Si 4 IS 4-MAG-A__4_2 394778 56956 3457 D-type Low Sr, low Si 19 19NMAG_70 399980 14959 0 D-type Low Sr, low Si 17 17MAG_32 397453 23316 3580 D-type Low Sr, low Si 13 IS 13-M-1__16_2 398270 22080 521 D-type Low Sr, low Si 22 IS 22-MAG -1__8_2 401027 21054 3138 D-type Low Sr, low Si 17 17MAG_25 Ti 400172 14789 9836 D-type Low Sr, low Si 14 IS 14M Unsifted__36_1 400206 22343 2486 D-type Low Sr, low Si 20 IS 20 MAG__27_1 392043 39113 1648 D-type Low Sr, low Si 14 IS 14 NM__2_1 395909 8327 12663 D-type Low Sr, low Si 9 IS 9-MAG__1_1 404750 18563 13320 D-type Low Sr, low Si 13 IS 13M UNSIFTED 60 s__6_1 396008 22957 3744 D-type Low Sr, low Si 17 17MAG_24 393962 15312 2811 D-type Low Sr, low Si 18 IS 18-MAG__3_1 382774 78154 1176 D-type Low Sr, low Si 8 IS 8-MAG-2__21_2 392537 29683 1718 D-type Low Sr, low Si 19 19MAGx_20 393339 18436 2908 D-type Low Sr, low Si 12 IS 12-MAG-2__6_1 383553 61479 1001 D-type Low Sr, low Si 14 IS 14M Unsifted__24_1 393662 15875 8515 D-type Low Sr, low Si 19 19MAGx_29 388524 27767 5394 D-type Low Sr, low Si 19 19MAGx_27 386662 10765 7706 D-type Low Sr, low Si 17 IS 17-MAG__9_2 386894 4312 338 D-type Low Sr, low Si 19 19MAGx_24 383297 11477 3843 D-type Low Sr, low Si 18 IS 18-MAG__6_1 389336 13246 14783 D-type Low Sr, low Si 21 IS 21__4_1 385227 10297 5105 D-type Low Sr, low Si 12 IS 12-MAG-3__5_1 388345 14847 21257 D-type Low Sr, low Si 14 IS 14M UNSIFTED B 60 s_1_1 376127 2570 11873 D-type Low Sr, low Si 14 IS 14M Unsifted__30_1 380882 7679 4580 D-type Low Sr, low Si 19 IS 19 M__12_map 372836 27122 355 D-type Low Sr, low Si 17 17MAG_34 366157 13289 2511 D-type Low Sr, low Si 19 19MAG_10Ti 366554 7538 15633 D-type Low Sr, low Si 19 19MAG_67 370964 10404 1620 D-type Low Sr, low Si 16 IS 16 MAG_2__21_2 360940 6541 121 D-type Low Sr, low Si 19 19NMAG_67 364132 6792 1173 D-type Low Sr, low Si 14 IS 14M Unsifted__2_1 349902 38779 9163 D-type Low Sr, low Si 13 IS 13-M-1__19_1 355786 14855 1615 D-type Low Sr, low Si 11 IS 11-MAG-3__4_1 348510 860 1573 D-type Low Sr, low Si 22 IS 22-MAG-3__3_1 344368 59112 19033 D-type Low Sr, low Si 7 IS 7 MAG__3_1 340175 23496 612 D-type Low Sr, low Si 19 19MAG_9 339764 8018 7261 D-type Low Sr, low Si 13 IS 13M UNSIFTED 60 s__46_1 348450 19765 11880 D-type Low Sr, low Si 19 19NMAG_52 338553 3423 3769 D-type Low Sr, low Si 19 19MAG_7 336641 4860 1610 D-type Low Sr, low Si 19 19NMAG_9 338218 5487 4981 D-type Low Sr, low Si 16 IS 16 MAG_2__20_1 334096 2340 1069 D-type Low Sr, low Si 7 IS 7 MAG__2_1 333451 7381 1075 D-type Low Sr, low Si 19 19MAGx_28 328460 2624 1811 D-type Low Sr, low Si 19 19NMAG_11 FeTi 331773 0 9939 D-type Low Sr, low Si 13 IS 13M UNSIFTED 60 s__9_1 328940 3775 5641 D-type Low Sr, low Si 22 IS 22-MAG-3__2_2 331799 16683 4961 D-type Low Sr, low Si 20 IS 20 MAG__15_2 326975 5818 4681 D-type Low Sr, low Si 13 IS 13-M-1__8_1 318026 29002 2396 D-type Low Sr, low Si 8 IS 8-MAG-2__22_1 327176 10512 6195 D-type Low Sr, low Si 19 19MAG_8 329135 2548 4839 D-type Low Sr, low Si 13 IS 13M UNSIFTED 60 s__4_1 318945 25125 1849 D-type Low Sr, low Si 13 IS 13M UNSIFTED 1 s__4_1 319143 14591 545 D-type Low Sr, low Si 17 17MAG_41 321451 0 4572 D-type Low Sr, low Si 19 19NMAG_69 310790 5541 4129 s (data plotted in Figures 5, 6, 7, 8, 9a, 10a). . Major and trace elements concentrations (ppm) measured by micro-XRF for 745 sample Al Si K Ca Ti Cr Mn Fe Ni 1792 9531 292 393 2550 99 0 590334 102811 2877 16985 87 999 652 3726 561 601403 51004 1926 6383 0 496 137 36 0 655832 33693 1185 6420 804 374 265 598 0 666758 20804 2637 15437 673 1003 445 718 240 634589 17641 2637 15437 673 1003 445 718 240 634589 17641 624 5442 0 213 0 563 0 677360 16948 1847 10361 186 856 1666 759 0 666997 15516 3719 11186 221 1102 1670 837 0 658125 14888 410 5186 0 177 68 273 0 679923 13882 951 7967 160 2503 184 1431 0 665329 11949 1473 9777 0 365 222 231 122 668334 11938 2839 16898 992 3239 623 2567 1494 642196 10364 2155 8349 128 158 616 1133 0 672229 10233 2555 10085 526 620 884 12623 0 646029 6125 508 5420 0 65 92 708 77 681217 6106 1024 6685 27 188 209 1546 5 682446 4887 7120 30379 1805 11687 1838 205 1489 554693 4058 978 7511 0 1732 139 4068 4394 662231 2418 2079 10805 2401 919 142 331 0 653294 1796 1606 13656 246 411 138 2252 0 654595 1687 1706 6549 38 325 226 1638 0 683447 1589 1791 14091 57 2569 192 90 6366 658832 1320 1120 5503 0 328 104 158 0 687880 1316 1843 11967 129 803 173 317 0 673627 1137 1415 6493 138 190 76 233 2426 682891 1081 794 17454 306 545 227 891 1192 659518 915 2498 8245 145 1542 351 1298 0 676592 816 6329 32498 632 2945 975 483 140 627455 816 3262 11958 226 12819 2885 761 5688 643343 732 2341 16223 2 1302 112 558 1122 649351 605 3793 10237 50 1058 220 210 2901 665113 568 847 7377 11 234 4441 112 2292 674951 547 1395 12584 55 428 93 969 1547 667970 540 915 7942 98 60 128 95 4568 659311 537 7707 19996 938 1208 31811 282 2844 600114 534 518 5748 267 347 39 323 0 687970 510 1539 8808 27 335 289 264 593 679787 505 9970 14269 263 504 25087 1372 3230 621845 494 1808 15759 354 672 279 631 66 654249 472 1890 12763 217 1033 629 816 3017 665313 468 1383 12377 72 1087 3733 276 4022 660153 465 9817 24537 517 2608 22454 966 4609 602164 446 3793 7391 93 1481 1191 156 0 678054 427 726 20042 608 5017 2508 47 608 647100 424 18058 11114 0 874 25932 578 802 618061 420 447 6905 0 34 238 1328 4497 678371 410 3489 10338 342 1457 13804 501 5019 652710 376 1073 7715 281 182 41 436 846 676957 350 871 14497 46 3685 238 172 119 666231 323 1604 18664 174 972 2280 21705 20006 624080 307 3382 16071 71 2268 3737 220 2332 658105 305 426 6361 136 63 13 4111 1533 682733 296 1206 9732 240 213 249 85 4593 649902 296 3659 12586 162 1006 1110 543 3848 665451 288 17933 11456 121 1263 25461 673 943 607251 270 1144 11636 90 214 59 395 9468 659813 262 10306 9058 128 564 24292 2376 2137 627596 256 1451 10614 158 503 305 354 2671 673899 253 1156 13236 0 820 676 624 2692 655970 251 939 11547 399 393 455 1298 3994 663502 248 11203 8818 63 473 24846 2133 1966 631000 231 579 8202 0 96 87 393 3800 681061 230 2853 13103 441 992 182 1511 2762 598971 203 17236 13920 440 746 31216 664 1168 559293 201 35563 19244 421 1397 25826 1540 2538 579229 185 14759 20634 521 281 47202 470 2188 506477 183 2082 10715 37 681 486 750 2245 671971 182 4573 14728 242 5982 375 525 1391 660158 182 1547 8584 41 926 6541 287 3759 670251 174 448 6019 625 65 59 292 2588 683452 172 2955 15408 117 1320 216 262 2767 658666 170 2246 13974 665 2511 735 277 3281 647184 169 1633 12669 864 732 579 763 5958 663118 167 2171 10735 0 1611 167 647 1701 664564 166 3744 8017 0 1384 992 169 0 679519 164 3358 11046 160 5980 43397 492 17063 581721 163 389 15658 559 853 1909 233 1225 661739 152 1928 7710 26 695 125 839 2507 678439 151 1061 7989 429 462 666 319 1666 617017 150 1356 23619 2505 541 1526 197 2658 627321 150 893 9185 43 525 239 535 2702 676979 147 5863 18387 274 4105 1473 468 995 648559 146 2836 19999 372 967 21748 107 1124 607403 144 7472 21961 360 1179 134 146 1791 622053 136 1126 8652 105 431 1401 209 1661 677453 123 1864 8732 0 548 99 800 1695 679202 116 1058 29584 98 195 126 3057 10556 639157 110 695 6873 0 248 155 666 1911 682707 110 16760 15850 215 2421 43758 974 3276 583099 102 2012 12355 150 1126 68 461 5715 663986 99 637 9080 39 121 16 345 5841 680038 90 6181 20114 427 4154 2893 322 1618 623870 86 24939 17941 485 581 36155 1794 3198 580670 83 2072 12991 324 773 1502 371 2133 644995 82 576 8148 35 80 172 390 1258 683475 77 1593 8148 0 538 509 398 32 678019 76 2846 10729 67 953 1008 196 2909 668977 75 16337 26660 1760 3601 2757 124 114 616282 74 819 10364 67 353 4502 225 2173 663014 73 2653 12145 120 4332 21034 315 6731 627591 70 994 9718 133 486 1332 225 2781 676215 69 1678 21771 514 4753 10236 159 1775 630604 63 455 6684 0 100 3446 371 1366 679378 62 455 6684 0 100 3446 371 1366 679378 62 3934 13544 67 1685 249 273 8964 649995 61 546 6242 167 102 1199 143 297 685373 60 1292 9195 243 336 908 208 1606 620845 60 2225 13887 0 634 402 175 3346 665241 60 505 6401 35 451 379 1511 8767 673062 58 8355 29941 304 23094 25926 1537 42 581005 49 1172 8915 115 688 395 138 2759 679760 49 5991 14131 745 1302 1213 587 4733 656121 49 1463 14313 7 1211 112 332 2014 653961 49 621 6059 28 132 1466 336 756 686090 46 1312 9126 93 151 4 178 305 676015 42 1018 10910 51 591 994 264 367 674720 41 2549 19337 166 351 0 308 3508 654479 41 30186 23736 1118 7614 2295 221 5716 573767 39 815 7618 35 170 1810 4210 2125 673832 38 4927 17390 597 769 189 292 2638 646248 37 634 5789 0 80 48 371 3279 686243 37 632 6816 42 62 536 471 3465 684160 36 498 5804 85 190 16 1274 1431 686869 35 1248 8458 0 418 310 602 1041 675676 35 1587 7934 0 438 89 129 1979 680803 34 648 10683 110 417 351 272 2207 678637 34 6822 7171 111 55 15218 1564 3232 652721 32 1241 6737 223 423 630 327 1288 684020 30 6140 24995 620 1271 273 500 359 641647 27 1029 8508 39 431 215 190 1767 657558 24 530 6283 43 42 179 494 2473 681446 24 1137 8254 95 598 461 410 557 679250 24 1321 6932 0 175 39 264 477 685561 23 1124 7520 0 243 444 694 1327 682752 23 1947 17302 70 288 12939 83 5804 647669 22 10101 8014 689 475 47023 513 3908 596155 20 1707 7160 0 3427 5962 262 2302 671776 19 28534 15298 253 1442 26974 1454 2083 595358 19 803 7693 172 68 563 603 3371 678238 17 12048 12007 650 8808 1245 56 0 651924 16 332 5130 0 48 48 332 1032 689548 15 1166 8056 151 539 39 275 1239 678651 12 3827 19150 479 1803 1543 195 11289 649227 11 1164 7610 148 157 876 6318 4929 675285 10 3735 10313 66 1876 20534 1512 9055 634789 8 456 7091 93 59 277 192 2009 681908 7 1792 12801 379 1466 848 204 3333 668142 6 3046 12585 695 2030 11660 263 2560 646063 5 510 6981 0 259 333 74 575 683382 4 17736 34372 407 1020 968 93 0 621008 4 587 5881 32 417 58 578 3604 683766 2 832 2154 44 68 94 274 5670 686426 0 303 5222 0 100 163 149 4794 682784 0 412 5287 0 85 86 232 1655 684679 0 302 5374 0 23 65 107 487 688122 0 360 5577 17 151 311 640 562 687897 0 756 5037 0 31 54 367 7242 677025 0 1778 5288 113 1084 116 117 5321 677961 0 511 5715 0 259 122 260 466 685789 0 822 5736 0 133 62 326 4026 679943 0 544 5839 0 111 97 277 1171 683736 0 410 5825 55 2356 515 452 1687 657286 0 667 6147 0 200 852 317 3802 675663 0 1088 6398 481 102 55 207 1732 685013 0 1139 6254 30 241 191 294 4621 677750 0 603 6559 85 161 1079 1075 3412 675492 0 1094 6641 89 203 820 758 7593 680774 0 1046 6797 2 365 377 263 4233 676586 0 1421 6674 121 1308 836 203 3330 676061 0 1609 6262 0 392 645 665 14924 672826 0 1019 7173 127 224 81 497 5377 681084 0 864 6991 106 670 1073 449 5729 680877 0 689 7403 101 188 1148 205 449 677951 0 724 6490 99 875 785 225 2594 677459 0 1842 7446 139 810 3638 877 3032 671341 0 579 7897 175 95 76 1234 2519 680391 0 0 8012 24 478 705 245 394 685138 0 0 8213 0 751 552 111 2777 683160 0 899 8001 464 241 0 129 1489 656484 0 1191 7023 0 745 6150 328 4109 669292 0 0 5409 0 293 71 690 1511 675338 0 1533 7573 0 436 146 324 6117 663075 0 3663 8772 0 329 600 223 186 674133 0 12488 9050 102 330 257 197 71 667749 0 3351 9438 0 1660 61 33 0 678520 0 0 9546 0 400 235 356 2622 681957 0 1351 9607 84 563 280 380 9066 668314 0 3687 9708 110 1698 119 62 63 674635 0 1406 10459 425 2652 464 850 3110 673150 0 1729 10693 572 3262 469 843 2723 673585 0 301 10667 0 569 382 141 2812 671212 0 2170 9382 0 1127 475 215 2861 669035 0 9258 10809 387 8483 1088 0 0 655500 0 747 11194 3022 221 428 459 9997 663497 0 618 9420 0 537 1786 304 1766 669164 0 1090 10814 3436 281 270 581 10258 661586 0 2682 10031 42 1117 179 315 3372 668390 0 610 11441 285 261 941 428 1961 635470 0 914 11254 1505 599 210 229 1595 621800 0 2461 11689 154 5872 306 137 3961 661804 0 9351 12610 243 1145 637 140 175 659314 0 2794 11602 119 1578 804 246 611 671880 0 29755 9147 0 2042 7344 153 1879 624304 0 30307 9236 0 2069 7403 156 1881 623301 0 3218 12905 507 3187 940 160 3359 660162 0 2550 13602 554 1113 669 107 0 653659 0 590 14375 459 2384 666 234 2932 665263 0 1476 15418 0 1172 230 204 2561 669494 0 3719 14620 181 1894 1294 831 4859 655755 0 3780 14721 185 1919 1277 818 4833 655583 0 3173 14109 36 1048 196 343 1075 653524 0 1522 13976 0 846 3223 452 7013 657058 0 7545 11760 275 694 36447 455 3042 609091 0 1909 13819 137 2322 530 621 2638 642485 0 1901 13915 136 2381 534 617 2643 641916 0 1063 15708 139 2185 1560 413 4011 650237 0 5598 17558 346 2224 715 126 475 654396 0 7375 15096 9292 274 42248 775 1768 599976 0 3225 17895 460 3959 392 95 13979 629864 0 4494 18156 832 5638 4311 605 3842 642990 0 12557 19043 270 345 14377 174 235 629710 0 4608 19217 2712 3189 217 103 9 621166 0 4420 15325 341 4539 928 147 3497 621137 0 1021 20290 77 403 29 287 8800 645085 0 3475 18506 981 501 195 250 7842 620212 0 16658 11661 73 1745 35620 404 2543 597220 0 3334 21221 240 902 426 532 0 657480 0 1880 13553 88 1272 4151 454 3332 604717 0 10272 31428 499 9988 5455 305 6648 610067 0 1443 157117 159 1830 379 2120 1399 99546 3469 0 163338 186 1806 363 2205 1300 102707 3445 909 159443 35 5289 171 1585 3636 112675 24 4853 182840 615 8055 701 1120 3372 154170 1349 4257 202034 93 2078 732 5193 2891 160262 1145 3332 144705 230 7798 604 2798 1319 170679 384 5696 156555 104 1936 995 3006 3213 173722 2354 5311 199942 201 7800 655 7923 2324 173056 60 7038 168159 368 10828 819 4406 2311 177471 1406 2247 172515 700 5259 1860 1513 3532 180966 808 6296 187520 78 14743 590 755 3573 182846 1765 8526 224897 1549 13902 1265 457 9743 174142 0 2649 163176 37 11284 666 2266 3776 192826 0 5880 169623 801 6937 2258 1690 3548 189594 944 6204 158633 20 11494 777 2263 3718 193296 7 4949 154447 966 5269 464 734 4777 198009 712 10106 181262 472 10906 1037 3611 5531 186566 174 2727 143724 29 4869 415 1773 3532 210399 671 3804 157824 0 9421 351 745 3147 207109 5280 13347 210921 0 19571 1375 0 10042 188123 0 6533 185438 262 11135 932 3663 5975 197221 52 2806 139194 0 7563 2093 103 1840 219441 0 5066 181675 0 10994 663 1947 3691 208934 13842 6494 181123 0 11204 671 2102 3774 209775 13556 11055 166094 1813 18734 6113 3441 3172 206413 1474 2037 134045 140 6593 777 874 3075 228858 628 2800 147229 28 1317 135 133 3889 238443 0 5617 155518 2495 26497 789 1929 2512 221428 4531 3982 150098 57 6292 792 3713 1655 235635 1766 7858 148543 554 12051 1068 4269 1346 227086 3297 6916 151291 0 7604 577 1226 1967 236149 2040 0 125905 502 2469 394 205 1441 249543 489 9815 149256 0 13363 918 188 2034 234326 592 829 125668 678 2591 355 307 1595 249524 483 10185 151410 0 15979 906 367 1967 236002 7834 6089 152505 0 6022 304 277 3778 245832 3693 1680 142330 489 7813 723 3036 2760 244522 393 1801 134398 67 1899 1481 4349 3944 253991 1101 7010 157212 124 9788 747 397 5302 243120 4823 3420 127853 121 5719 442 3840 2112 251358 10354 821 146315 0 1083 54 3148 4789 251509 565 17226 156044 2521 17399 1849 1204 3125 228494 11978 8956 131091 130 16005 1043 3934 2369 247133 3878 6068 151908 0 5941 314 270 3791 249870 3634 6517 149723 71 8357 689 1475 1888 246226 10262 5745 146564 163 8492 931 3874 1542 248745 16540 2176 147565 177 9341 757 3914 1284 252094 15364 13198 181008 187 14821 799 1491 3599 235421 1345 8549 180246 0 7513 482 1546 3869 248814 2991 4461 155579 784 3754 515 5529 4412 249091 309 10278 158420 0 13452 775 2686 4140 251190 246 10076 156961 0 13549 848 2538 3700 253156 145 1582 127148 264 1999 0 656 1444 271545 612 4078 130347 16 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1997 266475 0 63526 191512 10264 23683 14750 272 1420 233523 80 44221 204674 5285 11569 19816 136 1857 280377 0 44482 198379 5154 12590 19467 273 2495 272117 0 45383 198062 4459 12611 23348 41 2261 270744 0 45216 195019 4827 20496 20549 0 1855 269794 0 42933 194985 4580 18916 21313 152 2119 278143 0 40429 190852 6902 28424 13603 9 3230 283257 0 88132 183506 4086 27495 2857 29 6733 250995 0 58241 179728 7763 13474 22245 0 2824 270025 0 48754 172164 12715 19128 18787 316 1576 264350 36 90949 181720 4172 27066 2709 108 6607 237687 18 40373 181791 4991 12933 17386 445 2744 289289 84 41967 184723 4195 13932 22610 189 2315 300236 0 41170 182391 5437 24295 20233 129 2087 295874 124 51778 178859 9053 5789 21245 226 1884 296926 0 41484 182386 3657 8944 23705 365 2282 307089 346 101080 153201 6246 19706 3963 56 0 265154 72 41642 164699 4336 40260 22803 0 2553 289160 0 39994 174556 3680 15354 22770 0 2233 316353 0 31743 176482 4050 20305 20085 257 3511 320129 95 42918 165292 4376 16790 13596 211 1343 299194 0 39874 175652 3336 9322 16657 0 1980 332878 0 41330 166996 11078 7313 29484 0 4179 309557 0 34485 174726 5294 9838 19334 161 2876 331387 0 41718 174138 2937 8968 17921 772 1592 325160 0 33408 175998 4834 7601 23796 127 3292 318580 0 39800 174594 3438 6602 13752 882 844 334319 3 38632 162222 10478 9351 24602 167 5812 314350 145 11854 189830 23647 7920 1755 113 1380 345231 35 57906 167028 1457 18939 16389 352 1119 299179 208 31560 169386 3418 18028 22259 265 3022 326049 322 37749 158095 5126 31627 31419 0 2960 312412 0 31274 148816 5320 4396 24456 186 2485 318735 536 37250 157924 2149 5815 25790 95 3033 342598 0 37260 160047 2572 4532 26132 22 2879 346159 0 31965 151623 4688 7803 10945 321 1210 344272 0 75475 143183 20686 4583 12706 374 2439 320136 1665 61521 122283 1920 20564 70626 0 2045 289992 0 43740 144475 1657 11018 17624 247 1782 365691 40 58987 142854 2256 14001 926 40 8202 379708 0 37838 142784 2454 3919 18717 143 1389 384339 632 48686 140699 1004 16485 15055 904 953 357031 557 70453 128276 8398 32305 4575 96 227 352016 0 54387 137222 2712 18796 5083 805 1022 354438 166 21149 140159 18724 3648 1785 175 14 421431 361 86866 104082 502 43067 11828 354 1413 357177 15 75985 101800 4663 16356 3650 58 0 393682 619 29095 105930 1937 7938 31575 0 3522 429155 0 24401 106790 3111 24402 33534 8 4059 405538 0 39558 91492 741 43278 23184 19 2459 390142 0 16694 113122 2873 1703 627 90 499 495276 95 35569 85038 611 30604 23546 16 2590 428432 0 8457 96270 12888 1656 712 152 276 476116 1265 56223 77290 3891 10624 1720 135 0 477030 21 24357 81785 647 20319 2569 128 0 517191 279 16552 74087 616 9119 22114 296 3932 448719 159 11922 75767 3074 8433 2385 63 338 532246 13 30285 63886 1341 4605 38970 414 2640 470627 232 25954 63658 1247 5984 50794 533 1276 467243 2049 25506 64229 5254 4846 3461 164 572 543262 0 18972 64633 507 10262 378 151 0 555198 0 16729 57160 485 1624 34034 97 4152 531319 0 18228 56791 2129 3506 2989 202 263 576705 3 19079 55067 829 16873 4211 212 460 559553 0 7433 51561 1568 3824 13473 1088 3106 570256 271 12304 44545 434 8862 38000 14 3717 542751 0 12791 39672 583 51116 40899 506 3917 510734 0 22306 36520 1777 1242 55677 425 3298 519419 0 12584 34937 477 9260 39561 282 3852 559530 100 8589 33478 1594 41569 11815 750 3514 547862 78 13696 34282 852 9727 36107 702 1428 558088 179 12672 33441 461 9969 38613 7 4294 549224 0 6184 35243 561 7655 7140 280 101 593104 224 5717 35292 357 7546 7032 255 0 606427 0 21634 32544 121 13118 372 157 4317 593931 0 7771 29430 370 6763 1158 318 3738 594769 4424 Sr 9 17 179 2 0 0 9 79 2 24 0 0 115 0 17 0 48 45 196 0 21 0 73 0 5 5 0 53 52 9 151 21 30 9 1702 0 0 27 89 5 66 114 0 46 351 4 0 0 50 48 74 123 93 2067 33 13 32 30 74 0 0 66 0 30 34 86 0 72 16 20 44 4 25 89 261 0 9 4 30 33 6 38 0 0 0 93 92 49 38 31 27 0 41 48 0 50 72 0 155 14 18 65 24 39 39 26 0 6 44 39 55 18 68 23 7 19 18 27 307 55 26 0 109 108 127 54 76 0 0 16 67 10 54 5 10 1 70 66 0 4 442 44 4 12 66 336 20 45 63 0 34 91 0 134 105 0 6 129 52 0 155 114 173 143 28 81 0 0 65 63 35 4 0 44 30 106 52 0 32 72 103 0 124 233 43 160 21 111 92 115 0 32 57 373 66 113 46 99 28 4 94 290 26 76 77 120 418 0 0 192 186 156 107 24 145 151 98 357 7 0 215 329 0 189 29 0 123 48 25 57 48 21 32 26 0 7 44 27 56 46 69 139 0 42 51 12 37 5 31 62 46 93 37 38 63 27 9 0 54 13 9 15 156 25 23 215 21 21 51 23 5 68 52 122 14 32 0 25 54 109 27 0 4 23 124 115 13 86 55 149 23 45 37 26 41 20 5 26 139 28 47 62 167 26 119 0 0 185 35 32 31 52 36 51 66 42 0 57 185 48 30 100 0 12 0 81 27 52 27 0 0 0 168 157 16 0 7 79 32 6 25 33 108 63 32 36 14 18 49 130 47 8 121 89 34 132 12 63 0 79 6 137 48 14 6 43 24 25 35 0 88 37 37 0 65 55 156 83 96 34 20 66 38 0 47 143 57 0 0 151 93 17 99 60 75 30 29 6 33 0 0 146 23 27 102 32 152 97 17 11 26 28 32 71 0 142 50 94 132 102 26 150 21 18 47 43 9 0 0 13 26 207 133 25 77 103 66 278 186 27 97 107 1 0 129 51 86 0 0 37 40 68 38 134 15 87 87 101 36 42 500 21 37 55 78 32 123 39 145 90 27 66 0 0 2 85 31 29 121 62 67 20 90 29 378 118 38 49 296 129 103 36 18 19 28 118 85 33 31 41 35 69 61 31 77 81 25 50 166 42 82 38 54 69 253 47 191 72 11 0 139 44 3 247 29 235 49 69 84 16 100 53 6 57 68 16 106 79 54 0 152 121 179 207 34 32 42 135 5 95 135 384 163 64 71 820 0 17 2 296 447 98 71 0 552 57 55 384 13 325 0 308 0 7 37 19 55 84 822 76 49 5 77 2340 1006 1345 578 787 1142 552 906 777 1063 2091 988 1293 1841 1841 1455 687 2804 473 859 634 927 1131 504 2920 1325 687 549 1336 845 8759 696 1299 537 839 1971 3250 2116 1620 1120 490 3204 842 211 289 203 155 145 352 41 134 167 391 45 191 79 425 229 107 276 275 65 86 23 319 428 179 154 153 24 137 146 55 108 372 106 126 51 89 89 62 53 60 51 26 87 46 25 99 72 59 52 118 158 54 29 177 75 75 22 47 30 397 119 43 116 62 52 39 42 75 61 23 41 128 44 165 122 33 22 55 31 86 114 37 88 122 25 232 28 120 195 437 104 124 138 81 92 36 58 274 85 177 34 56 382 261 33 404 409 325 111 155 57 160 75 21 183 172 66 330 166 Table S2. Major elements, Be, Cr, Co, Ni, Sr, La and U concentrations (ppm) measured by ICP-MS for 68 samples (data plotted in Figures 9b, 10b, 11, 12, 13, 14, 15). Type Sub-type Track Sample name Be Na Mg Al S-type Chondritic 4 IS4 SPH4 9542 177567 4157 S-type Chondritic 4 IS4 SPH5 4832 172742 16224 S-type Chondritic 13 IS13 SPH4 0.156 6421 166184 9791 S-type Chondritic 17 IS17 SPH2 178 133511 15097 S-type Chondritic 19 S25 IS19 SPH2 1919 140779 7730 S-type Chondritic 4 S12 IS4D SPH3 184 146583 15371 S-type Chondritic 4 S9 IS4A SPHS 155 161306 15441 S-type Chondritic 22 IS22 SPH2 642 155559 11244 S-type Chondritic 22 IS22 SPH3 3.318 763 164573 9706 S-type Chondritic 13 (4) IS13 SPH11 0.008 759 177936 5736 S-type Chondritic 14 (8) IS14 SPH8 0.019 656 155222 14846 S-type Chondritic 22 (16) IS22 SPH5 0.0004 1163 152596 13280 S-type Chondritic 4 (20) IS4 SPH9 2195 145125 15516 S-type Chondritic 8 (23) IS8 SPH5 640 157212 11706 S-type Chondritic 13 (27) IS13 SPH7 181 139668 17950 S-type Chondritic 13 (29) IS13 SPH10 348 183043 4311 S-type non-Chondritic 14 (7) IS14 SPH7 44 216146 412 S-type Chondritic 14 (9) IS14 SPH9 0.004 376 137838 8850 S-type Chondritic 22 (1) IS22 SPH1 0.426 8168 104355 22530 I-type Ni-rich 13 IS13 SPH3 749 235 1748 I-type Ni-rich 4 S11 IS4C SPH2 176 19263 2512 I-type Ni-rich 14 (12) IS14 SPH14 664 628 2047 I-type Ni-rich 8 (24) IS8 SPH6 183 85 927 I-type Ni-rich 17 17NMAG_37 2680 3197 521 I-type Ni-poor 8 IS8 SPH1 0.019 1578 964 875 I-type Ni-poor 8 IS8 SPH2 330 798 1531 I-type Ni-poor 16 S7 IS16A SPH1 850 166 348 I-type Ni-poor 12 S16 IS12C SPH1 0.629 623 345 7764 I-type Ni-poor 19 S23 IS19 SPH1 536 573 404 I-type Ni-poor 19 S29 IS19 SPH7 822 725 1603 I-type Ni-poor 8 S5 IS8 SPHR 0.199 384 401 856 I-type Ni-poor 13 S19 IS13B SPH2 203 295 188 I-type Ni-poor 22 (2) IS22 SPH4 0.012 387 100 109 I-type Ni-poor 13 (5) IS13 SPH9 0.008 154 339 151 I-type Ni-poor 14 (10) IS14 SPH10 514 327 570 I-type Ni-poor 8 (22) IS8 SPH4 1765 10533 17786 I-type Ni-poor 13 (26) IS13 SPH6 320 87 367 I-type Ni-poor 17 17NMAG_15 0.465 5316 6178 10622 I-type Ni-poor 4 (18) IS4 SPH7 0.010 3943 7496 15125 I-type Ni-poor 13 (30) IS13 SPH12 0.030 2069 11399 14476 I-type Ni-poor 14 (31) IS14 SPH5 0.006 2101 8362 13894 I-type Ni-poor 4 (17) IS4 SPH6 2.62 979 9470 10844 D-type High Sr, high Si 17 IS17 SPH1 1.46 61972 32998 210325 D-type High Sr, high Si 17 (14) IS17 SPH4 1.42 61916 28451 209998 D-type High Sr, high Si 13 (28) IS13 SPH8b 2.03 49383 33244 195530 D-type High Sr, high Si 17 (13) IS17 SPH3 1.53 49431 27214 122313 D-type High Sr, high Si 17 (15) IS17 SPH5 1.22 41987 24935 124433 D-type High Sr, high Si 17 17NMAG_36 0.83 18354 12657 59920 D-type High Sr, low Si 17 17NMAG_6 2.87 11147 37615 124736 D-type High Sr, low Si 14 (32) IS14 SPH6 5.05 1712 6220 94992 D-type High Sr, low Si 14 IS14 SPH2 1.51 13933 7114 57204 D-type High Sr, low Si 19 19NMAG_50 2.37 910 6387 53827 D-type High Sr, low Si 19 19NMAG_52 3.13 7914 10729 46119 D-type Low Sr, low Si 14 (11) IS14 SPH11 6.31 6653 10818 43731 D-type Low Sr, low Si 8 (21) IS8 SPH3 2.01 1539 20310 35301 D-type Low Sr, low Si 19 S31 IS19 SPH8 211 3912 84288 D-type BeLaU low Si 4 S10 IS4B SPH1 14.7 13864 2907 88610 D-type BeLaU low Si 14 S21 IS14 SPH1 7.8 2618 2231 53878 D-type BeLaU low Si 14 (6) IS14 SPH4 10.0 7902 4911 90915 D-type BeLaU low Si 4 (19) IS4 SPH8 32.4 3977 2704 115941 D-type BeLaU low Si 14 IS14 SPH3 11.4 9001 3336 49658 D-type BeLaU low Si 17 17NMAG_35 34.6 13854 8615 137992 D-type BeLaU low Si 17 17NMAG_33 17.6 4740 8348 136612 D-type BeLaU low Si 17 17NMAG_2 15.0 11780 14941 132262 D-type BeLaU low Si 19 19MAGx_4 13.5 6623 10360 126494 D-type BeLaU low Si 17 17NMAG_29 13.4 13895 7152 118488 D-type BeLaU high Si 13 (25) IS13 SPH5 114.7 13169 8884 236886 D-type BeLaU high Si 17 17NMAG_5 19.1 17227 9240 148150 for 68 samples (data plotted in Figures 9b, 10b, 11, 12, 13, 14, 15). . Major elements, Be, Cr, Co, Ni, Sr, La and U concentrations (ppm) measured by ICP-MS P K Ca Ti Cr Mn Fe Co Ni 546 702 14512 486 2755 1651 201084 326 1484 578 1667 42093 689 762 1838 174601 124 421 569 1310 10107 321 8850 2858 222319 159 6262 1782 581 62464 1139 6359 1359 254052 699 12225 2234 3786 32720 509 6493 1911 271410 578 10610 473 1146 14659 703 4430 2098 269312 699 10253 220 808 19190 678 2109 1946 231199 368 3727 443 3925 21412 934 2742 1953 245727 401 5558 1007 3428 18623 214 3817 1983 221658 630 10550 635 412 3871 479 4363 2098 207312 465 10511 535 343 14309 759 2640 2275 246444 887 12302 1469 75 15121 803 5394 2203 257609 881 4653 126 304 7850 612 4171 2009 280680 462 9650 316 829 3515 1938 265567 534 7504 742 24680 682 4647 2272 278641 652 5677 312 187 343 5819 1459 207997 567 6954 18 53 936 54 49 3043 124011 1.22 370 220 17121 377 3291 1898 304464 477 6812 7908 3340 174568 14586 6 6351 197902 63 12 88 632 8396 405 5174 4 696801 2486 12023 126 567 3019 92 500 212 618980 4145 56989 981 189 6455 10 695233 3114 24436 68 43 12 237 14 711965 2828 16474 447 872 10010 38 6278 5361 640609 63 5032 410 318 6818 610 184 2838 708703 7.28 37.3 468 615 14555 269 203 4398 699909 7.56 55.1 117 211 1154 28 209 6381 716287 2.91 6.5 41 370 2509 133 4 11 708875 6.78 32.3 324 607 16015 8 226 4673 700901 17.0 85.6 250 409 15526 2696 382 4324 697265 11.1 90.6 211 261 1797 660 255 2642 715797 61.4 287.2 70 179 590 320 252 4366 714310 7.8 18.0 179 31 2578 493 443 4164 716564 27.0 142.5 43 38 1191 454 3912 715407 57.4 242.4 238 394 6080 77 3636 712442 12.2 50.0 464 229 30503 30 3195 645119 145.5 11.0 52 69 3133 721557 15.3 37 285 7763 35475 64502 1421 77906 336797 21.5 140 5157 1652 7023 37988 37 5396 634286 117.9 31 3282 613 7300 47461 100 5250 620426 113.1 11 1243 727 1170 39657 6 7442 642043 83.2 47 352 221 18309 457 87 14757 651822 19.0 15 3898 27420 140984 5521 87 2492 126468 34.8 133 3892 26583 121006 7407 63 2377 159124 43.2 178 3517 25784 133210 7319 28 3300 162544 49.7 99 2038 22566 304747 5688 19 2582 111080 39.3 25 1878 22661 316450 5765 29 2382 107793 36.5 27 1512 10441 146340 2888 47 1613 53625 21.1 39 2402 6474 33724 1781 102 5551 392982 10.4 138 1552 1220 21112 4442 109 515 534548 36.9 190 34 1716 9908 1673 56 621 601274 25.0 86 293 2275 20653 3303 64 342 605322 12.6 35.37 495 3123 24108 4468 470 291 593238 23.1 33.68 1005 9972 26224 829 40 16407 582408 13.4 33 1899 913 6588 2063 39 12966 598647 14.8 69 390 537 8430 740 223 863 587174 18.3 48.4 449 4759 30786 5005 140 267 543731 38.1 116 982 1350 12378 2729 1307 57 571591 41.7 72 161 2276 15958 5050 765 202 554415 31.3 37 593 2772 2901 2507 82 84 546719 194.3 52 453 7259 15157 3940 138 550 384635 39.1 67 919 25489 16249 7843 321 847 235061 36.7 138 8241 5146 32043 6249 394 6694 322928 102.5 425 3492 6217 36015 9701 243 7383 349500 170.1 842 8185 7479 35109 7580 260 6131 391681 80.7 363 1106 4159 32561 1312 94 112 395260 84.7 259 548 12044 93260 7045 11 550 250278 281.9 196 647 5724 42783 8606 8838 217 192194 64.9 149 Sr La U 5.066 0.331 11.700 0.461 0.055 18.076 0.489 0.076 13.969 0.596 0.002 20.091 0.536 0.022 13.172 0.306 42.101 0.407 12.414 0.191 24.518 0.397 27.48 0.371 0.016 11.67 0.303 15.89 0.571 0.033 22.51 0.664 0.003 6.04 0.386 19.19 0.848 0.027 10.23 0.270 0.054 0.31 0.008 9.95 0.404 110 16.520 0.310 2.296 0.182 0.022 3.114 0.008 103.30 0.24 0.81 57.099 0.339 0.293 6.909 0.326 0.062 1.322 0.026 0.007 11.184 2.001 0.115 4.070 0.122 0.001 13.463 0.188 0.048 8.264 0.588 0.104 1.017 0.026 0.006 5.303 0.090 0.015 1.077 0.024 0.062 2.389 20.973 0.418 0.101 1.913 0.024 0.002 50.9 4.54 3.14 30.0 13.233 0.135 27.4 3.847 0.091 25.8 2.734 0.119 117.4 5.735 0.696 1349 20.056 1.562 1377.9 19.994 1.373 1435.2 23.869 1.853 2128.1 19.699 1.389 2230.3 19.724 1.584 995.1 9.42 14.58 930.4 20.81 5.39 1172.3 25.67 3.42 859.9 11.160 1.180 508.3 34.976 4.304 651.2 19.294 2.820 119.1 5.890 0.998 132.8 15.998 2.147 3.730 0.214 0.109 447.1 66.3 5.114 2242.8 159.4 6.148 2021.6 81.2 7.685 128.6 76.4 2.595 243.2 31.45 2.98 307.7 107.25 8.69 1071.0 82.99 15.17 962.6 52.55 17.31 1517.1 51.86 10.30 577.9 120.34 2.54 1792.7 260.4 9.715 2892 71.97 11.7 Table S3. Elemental data (ppm) measured by ICP-MS for 12 BeLaU-type spherules and the CI normalizing values of Anders and Grevesse (1989). Type Sub-type Track Sample name Li Be Na Mg D-type BeLaU low Si 4 S10 IS4B SPH1 84.7 14.7 13864 2907 D-type BeLaU low Si 14 S21 IS14 SPH1 62.2 7.8 2618 2231 D-type BeLaU low Si 14 (6) IS14 SPH4 87.0 10.0 7902 4911 D-type BeLaU low Si 4 (19) IS4 SPH8 22.4 32.4 3977 2704 D-type BeLaU low Si 14 IS14 SPH3 37.7 11.4 9001 3336 D-type BeLaU low Si 17 17NMAG_35 162.7 34.6 13854 8615 D-type BeLaU low Si 17 17NMAG_33 108.9 17.6 4740 8348 D-type BeLaU low Si 17 17NMAG_2 170.0 15.0 11780 14941 D-type BeLaU low Si 19 19MAGx_4 216.0 13.5 6623 10360 D-type BeLaU low Si 17 17NMAG_29 102.2 13.4 13895 7152 D-type BeLaU high Si 13 (25) IS13 SPH5 120.4 114.7 13169 8884 D-type BeLaU high Si 17 17NMAG_5 154.4 19.1 17227 9240 CI(ppm) Anders and 1.5 0.025 5000 98990 Grevesse (1989) alizing values of Anders and Grevesse (1989). . Elemental data (ppm) measured by ICP-MS for 12 BeLaU-type spherules and the CI norm Al Si P K Ca Sc Ti V Cr 88610 449 4759 30786 36.3 5005 171 140 53878 982 1350 12378 20.9 2729 101 1307 90915 161 2276 15958 43.2 5050 220 765 115941 593 2772 2901 14.4 2507 57 82 49658 453 7259 15157 11.2 3940 98 138 137992 919 25489 16249 27.2 7843 202 321 136612 8241 5146 32043 34.0 6249 465 394 132262 3492 6217 36015 51.9 9701 277 243 126494 8185 7479 35109 31.9 7580 266 260 118488 1106 4159 32561 18.8 1312 36 94 236886 548 12044 93260 79.3 7045 323 11 148150 647 5724 42783 80.3 8606 372 8838 8680 106400 1220 558 9280 5.82 436 56.5 2660 Mn Fe Co Ni Cu Zn Ga Ge As 267 543731 38 116 117 44 42.3 8.44 2.06 57 571591 42 72 54 9 27.7 9.50 1.04 202 554415 31 37 47 20.2 9.21 1.41 84 546719 194 52 125 61.2 9.11 13.06 550 384635 39 67 1414 14.6 6.53 1.00 847 235061 37 138 478 28.8 3.91 2.96 6694 322928 103 425 24 542 51.6 5.57 2.59 7383 349500 170 842 1314 73.0 6.50 4.47 6131 391681 81 363 346 83 103.6 6.79 3.77 112 395260 85 259 1503 24.5 6.96 1.82 550 250278 282 196 108 68.8 4.90 4.24 217 192194 65 149 98 97 89.5 3.51 1.70 1990 190400 502 11000 126 312 10 32.7 1.86 Se Rb Sr Y Zr Nb Mo Ag Cd 0.25 17.6 447 135 465 38.2 4.9 0.24 0.09 0.25 4.5 2243 120 247 15.1 77.5 0.07 0.05 0.24 6.8 2022 133 626 34.5 19.8 0.21 0.06 0.24 13.9 129 188 199 7.1 22.7 0.11 0.13 40.9 243 44 131 12.8 6.7 0.05 0.29 0.28 173.9 308 86 441 29.2 10.3 0.03 0.11 27.8 1071 63 477 34.0 18.2 0.16 0.08 0.19 31.7 963 77 423 23.2 13.4 0.15 1.59 0.16 33.7 1517 61 420 21.0 14.2 0.08 0.12 0.37 11.6 578 255 153 4.3 27.4 0.03 0.02 0.71 46.7 1793 487 1008 84.8 179.2 0.23 0.24 0.44 22.6 2892 214 1117 71.2 5.4 0.304 0.132 18.6 2.3 7.8 1.56 3.94 0.246 0.928 0.199 0.686 Sb Cs Ba La Ce Pr Nd Sm Eu 1.28 1.09 914 66.3 128 14.5 58.2 12.4 2.68 0.05 0.18 759 159.4 267 25.6 89.4 16.0 2.96 0.55 0.37 1452 81.2 152 16.7 68.0 15.6 3.35 0.68 1.92 228 76.4 181 20.3 85.5 18.6 3.20 2.83 2.89 385 31.5 66 7.1 27.1 6.8 1.18 12.41 17.80 792 107.2 227 24.6 100.5 11.2 3.69 9.70 4.94 1404 83.0 214 25.7 99.4 14.0 2.57 11.61 4.62 1613 52.6 116 14.1 60.2 11.1 2.35 1.96 3.17 3052 51.9 110 12.4 50.3 11.3 2.57 10.35 2.27 740 120.3 170 20.5 88.7 22.8 4.83 2.35 5.67 2848 260.4 451 49.8 204.6 45.5 8.87 0.94 2.68 2573 72.0 159 19.2 82.5 21.2 4.90 0.142 0.187 2.34 0.235 0.603 0.089 0.452 0.147 0.056 Gd Tb Dy Ho Er Tm Yb Lu Hf 15.30 2.68 17.36 3.79 11.26 1.80 10.57 1.58 10.92 17.87 2.72 17.26 3.70 11.59 1.85 11.92 1.79 5.95 17.23 2.93 19.56 4.12 13.81 2.16 14.57 2.08 14.27 19.96 3.37 23.51 5.08 17.00 2.70 16.00 2.24 6.22 5.61 1.06 5.53 1.21 3.30 0.59 3.55 0.51 3.45 13.33 2.23 13.23 2.32 8.18 0.96 6.98 1.78 7.97 11.07 1.98 11.37 2.25 7.30 1.05 6.96 1.31 10.88 11.83 2.14 12.42 2.81 7.02 1.34 7.81 1.49 9.93 10.53 1.56 10.20 2.08 5.80 1.03 5.64 0.83 10.90 29.60 5.14 34.05 8.09 23.62 3.85 22.88 4.00 3.65 51.72 9.28 64.72 15.28 55.64 9.26 65.66 10.34 24.11 23.30 4.49 29.94 6.85 20.94 3.47 22.72 3.45 23.20 0.197 0.0363 0.243 0.0556 0.159 0.0242 0.163 0.0243 0.104 Ta W Re Tl Pb Bi Th U 1.45 17.96 0.001 0.322 3.76 0.032 14.70 5.11 0.63 7.53 0.002 0.34 0.002 8.41 6.15 1.34 4.39 0.002 0.001 1.01 15.32 7.68 0.60 8.62 0.002 1.55 8.26 2.60 0.76 7.12 0.131 0.338 2.20 0.461 9.90 2.98 1.50 12.64 0.015 1.221 4.35 0.999 38.73 8.69 1.23 20.12 0.022 0.611 17.85 0.119 19.80 15.17 1.40 9.28 0.010 0.153 10.05 0.656 56.05 17.31 1.57 12.13 0.002 0.010 2.46 0.079 23.33 10.30 0.08 669.18 0.015 0.210 3.90 0.557 4.13 2.54 2.64 63.34 0.008 0.044 10.49 0.021 18.76 9.72 2.03 6.71 0.005 0.053 7.78 0.040 24.28 11.69 0.014 0.093 0.0365 0.142 2.47 0.114 0.0294 0.0081