# A new tektite strewn field in Australia ejected from a volcanic arc impact crater 11 Myr ago

Anna Musolino, Pierre Rochette, Jean-Alix Barrat, Fred Jourdan, Bruno Reynard, Bertrand Devouard, Valerie Andrieu, Jérôme Gattacceca, Vladimir Vidal

► To cite this version:

Anna Musolino, Pierre Rochette, Jean-Alix Barrat, Fred Jourdan, Bruno Reynard, et al.. A new tektite strewn field in Australia ejected from a volcanic arc impact crater 11 Myr ago. Earth and Planetary Science Letters, 2025, 670, pp.119600. 10.1016/j.epsl.2025.119600. hal-05256344

HAL Id: hal-05256344

https://hal.science/hal-05256344v1

Submitted on 17 Sep 2025

HAL is a multi-disciplinary open access
archive for the deposit and dissemination of sci-
entific research documents, whether they are pub-
lished or not. The documents may come from
teaching and research institutions in France or
abroad, or from public or private research centers.

L'archive ouverte pluridisciplinaire HAL, est
destinée au dépôt et à la diffusion de documents
scientifiques de niveau recherche, publiés ou non,
émanant des établissements d'enseignement et de
recherche français ou étrangers, des laboratoires
publics ou privés.

<figure><img src="image_1.png" /></figure>

Distributed under a Creative Commons Attribution 4.0 International License
<figure><img src="image_2.png" /></figure>

<figure><img src="image_3.png" /></figure>

# A new tektite strewn field in Australia ejected from a volcanic arc impact crater 11 Myr ago

Anna Musolino<sup>a,∗</sup> <sup>ID</sup>, Pierre Rochette<sup>a</sup> <sup>ID</sup>, Jean-Alix Barrat<sup>b,c</sup> <sup>ID</sup>, Fred Jourdan<sup>d</sup>, Bruno Reynard<sup>e</sup>, Bertrand Devouard<sup>a</sup> <sup>ID</sup>, Valerie Andrieu<sup>a</sup>, Jérôme Gattacceca<sup>a</sup> <sup>ID</sup>, Vladimir Vidal<sup>a</sup>

## ARTICLE INFO

Editor: Dr C. M. Petrone

Keywords:

HNa/K-australites
Tektites
Strewn-field
Impact
Glass
Crater

## ABSTRACT

This study re-evaluates the anomalous subgroup of australites known as high Na/K (HNa/K) tektites (Chapman and Scheiber, 1969). Although previous compositional and isotopic analyses suggested a distinct origin, the group has never been formally recognized as a separate tektite strewn field. We present new data from six HNa/K tektites, complementing the eight specimens already described. We conducted a comprehensive investigation, including petrographic (optical and electron microscopy, and micro-X-ray tomography), geochemical (major and trace element compositions, Sr-Nd isotopic composition, ⁴⁰Ar/³⁹Ar dating), and spectroscopic (for the identification of inclusions) analyses. We concluded that the HNa/K tektites originated from a separate impact event compared to Australasian tektites; they have an andesitic to dacitic composition and arc-related trace element signatures. Lechatelierite (and phosphate) inclusions as well as high levels of chondritic contamination support an impact origin, for which we provide a more precise ⁴⁰Ar/³⁹Ar age: 10.76 ± 0.05 Ma. For now, Sr-Nd isotopic data and trace elements composition point to three possible sources associated with active volcanic arcs: Luzon (Philippines), Sulawesi (Indonesia), and the Bismarck region (Papua New Guinea). Systematic petrographic and geochemical differences observed between tektites from the western and eastern parts of the ~900-km-wide hypothesized strewn field (located in Southern Australia) may help to constrain the location of the source crater, but they need to be confirmed by the study of more specimens. We propose the name "Ananguite" for this new group of tektites.

## 1. Introduction

Tektites are a specific type of impact-produced glass, defined in particular by their occurrence within large strewn fields lying at long distances from their source crater. Only five different strewn fields are known: the four “classic” ones known for nearly a century, from Central Europe (~14 Ma), North America (~35 Ma), Ivory Coast (~1 Ma), and a large area spread from China to Australia (~0.78 Ma) (Glass, 1990; Koeberl, 1994; Glass and Simonson, 2013) and a more recently discovered strewn field in Central America (~0.8 Ma) (Rochette et al., 2021). The corresponding tektites are called moldavites, bediasites-georgiaites,

ivorites, australasites, and belizites, respectively.

Tektites are nearly pure glasses (practically no crystalline inclusions), showing low vesicularity and chemical homogeneity at the specimen scale. However, at the strewn field scale, chemical variability may be significant, particularly in the case of australasites, although the vast majority of specimens display only a narrow range of composition. The most comprehensive survey of this chemical variability has been put forward by Chapman and Scheiber (1969). To identify rare cases of outlying compositions, Chapman and Scheiber conducted a survey of 47, 000 specimens in various collections around the world. Based on specific gravity measurements, they sorted out 530 samples for major elements

<footnote><sup>a</sup> Aix Marseille Univ, CNRS, IRD, INRAE, CEREGE, Aix-en-Provence, France</footnote>

<footnote><sup>b</sup> Univ Brest, CNRS, Ifremer, IRD, LEMAR, Institut Universitaire Européen de la Mer (IUEM), rue Dumont d'Urville, 29280 Plouzané, France</footnote>

<footnote><sup>c</sup> Institut Universitaire de France, Paris, France</footnote>

<footnote><sup>d</sup> Western Australian Argon Isotope Facility, School of Earth and Planetary Sciences, John de Laeter Centre for Isotope Research and C-FIGS, Curtin University, GPO Box U1987, Perth WA6845, Australia</footnote>

<footnote><sup>e</sup> Laboratoire de Geologie de Lyon, CNRS UMR 5276, Ecole Normale Superieure de Lyon, 46, Allee d'Italie, 69364 Lyon Cedex 7, France</footnote>

<footnote>* Corresponding author.</footnote>

<footnote>E-mail addresses: musolino@cerege.fr, anna_musolino@yahoo.it (A. Musolino), rochette@cerege.fr (P. Rochette), barrat@univ-brest.fr (J.-A. Barrat), F.Jourdan@exchange.curtin.edu.au (F. Jourdan), bruno.reynard@ens-lyon.fr (B. Reynard), devouard@cerege.fr (B. Devouard), andrieu@cerege.fr (V. Andrieu), gattacceca@cerege.fr (J. Gattacceca), vvidal@cerege.fr (V. Vidal).</footnote>
analysis, and out of them, 380 were analyzed for trace elements. Thanks to this survey, they defined different chemical groups describing the chemical variability of australasites. Among these groups, one was outlying by the fact that it showed a completely different composition, while for the others, the limits between groups were more arbitrary. The most outlying geochemical feature of this former group was a very high Na₂O/K₂O ratio, in the 2.7-3.6 range, while all other australasites have Na₂O<K₂O. Therefore, this group was called "High Na/K australites" (hereafter referred to as HNa/K). The term "australites" refers to Australasian tektites from Australia. The chemical composition of HNa/K australites is andesitic (conversely, other Australasian tektites are dacitic to rhyolitic, with overall lower alkali contents), with an anomalously high amount of Ni and Cr (up to 875 and 385 ppm, respectively). Its ⁸⁷Sr/⁸⁶Sr isotopic ratio is near 0.704 when other australites range from 0.7135-0.7180 (Compston & Chapman, 1969). The group counted eight specimens, all found in Southern Australia. Specimen aspect, shape, and microscopic features were described to be similar to other tektites found in the same area: a homogeneous glass with low vesicularity and a lack of crystalline inclusions. The very low water content measured by Beran and Koeberl (1997) (between 40-80 ppm on four samples) rules out a volcanic origin and, instead, is typical for a tektite. Their water content falls in the lower range when compared to Australasian tektites (Beran and Koeberl, 1997; Watt et al., 2011). Finally, fission track analysis (Fleischer et al., 1969; Storzer, 1985), K/Ar dating (Storzer and Müller-Sohnius, 1986), and a preliminary attempt at ⁴⁰Ar/³⁹Ar dating (Bottomley and Koeberl, 1999) suggest that the impact age occurred between ca. 11 and 2.5 Ma, significantly older than the australasite event at 0.78 Ma (Jourdan et al., 2019). If the age range was correct, it would suggest that these objects belong to a distinct type of tektite-like impact glass, unrelated to the australasite event. However, the impact age was still largely uncertain, and this material had not been studied in enough detail to unambiguously establish it as a new tektite strewn field. The purpose of the present contribution is to revisit the HNa/K australites, with more accurate ⁴⁰Ar/³⁹Ar dating and a more detailed characterization of 6 newly identified samples. Demonstrating the existence of a new tektite strewn field helps increase our knowledge of the frequency of extreme impacts on Earth, and distinguishes independent events from the larger Australasian impact, whose origin and source crater remain subject to debate. For consistency throughout the paper, we use the term "ananguites" for this glass strewn field; a detailed explanation for this name is provided in Section 4.

## 2. Samples and methods

**Selection of the samples** – The eight samples identified by Chapman and Scheiber (1969) in the South Australian Museum (SAM) collection, Adelaide, were not available for our study. Therefore, we conducted a comprehensive survey of the SAM collection using physical property measurements. The first screening was conducted by systematic determination of specific gravity (SG) and/or magnetic susceptibility (χ). Some samples were measured using both techniques or only one, depending on sample mass. Previous specific gravity surveys indicated that most australasites have SG ≤ 2.45, while ananguites have SG ≥ 2.53 (Chapman and Scheiber, 1969). Therefore, we prepared a water and lithium heteropolytungstate (LST) heavy liquid mixture set at 2.45 SG. Pools of specimens from the same reference were immersed in the liquid. Specimens found floating or suspended in the liquid were rejected, while specimens sinking to the bottom were selected. The SG value of the flotation liquid was frequently controlled using a specific gravity hydrometer with a resolution of 0.001, and adjusted to 2.45 if needed. This technique is efficient for any sample mass, but not practical for samples above 10 g.

We also used specific magnetic susceptibility measurements that were previously shown to be an efficient way to find outliers in tektite collections based on the very narrow χ range shown by a given tektite strewn field (Rochette et al., 2015, 2019, 2021; Soro et al., 2023). This is

because tektites are mostly paramagnetic (with Fe in the 2+ state), thus making χ a good proxy for the total Fe amount in tektite. Based on Chapman and Scheiber (1969), FeO content in ananguites is 5.9 ± 0.4 wt%, while it is on average 4.9 wt% for australasites (Koeberl, 1990). The corresponding average χ reported by Rochette et al. (2019) for australites is 86 ± 8 × 10⁻⁹ m³/kg. Therefore, a threshold at 95 × 10⁻⁹ m³/kg was chosen to set apart samples with anomalously high susceptibility. To rapidly measure a large collection, we used a portable SM150 instrument that has the advantage of measuring simultaneously magnetic susceptibility and sample mass, which is necessary to compute mass-normalized χ. The reproducibility of the measurement is approximately 10⁻⁹ m³/kg when the mass exceeds 10 g. Small specimens were pooled (up to a total mass of ~40 g), and in case of high susceptibility, the pool was progressively split until the magnetic outlier was identified. As the precision on magnetic susceptibility decreases with mass, samples below 2 g were not measured systematically.

Samples set apart at the SAM museum were brought to the Centre de Recherche et d'Enseignement des Géosciences de l'Environnement (CEREGE), Aix-en-Provence, France, for further characterization. First, samples were cleaned in alcohol and ultrasonic baths to get rid of dust that could influence their physical properties. Visible soil incrustations were removed with a stainless-steel needle. Mass was measured with a precision balance and χ determined with a higher sensitivity and reproducibility instrument MFK1 Kappabridge.

The chemical composition was measured on the full specimen using a portable XRF Bruker Tracer 4 instrument, using a high-energy mode (50 kV) adapted for relatively heavy elements. Based on the instrumental reported uncertainties, we collected reliable data for the following elements: K, Ca, Fe, Ti, Cr, Mn, Ni, Rb, Sr, Zr, and Th. We do not discuss data calibration as we will only use relative variations.

**Petrography** – A slice of ~1 mm-thick sample was embedded in epoxy to prepare a polished section for observations under the optical microscope using a Keyence VHX-7000N digital microscope and under the Hitachi S-3000N Scanning Electron Microscope (SEM) with a Bruker Energy Dispersive X-ray Spectrometer (EDS) at CEREGE. Sample, bubbles, inclusion sizes, and porosity were calculated using the digital microscope from a polished sample for each ananguite.

Raman spectra were collected with a Horiba LabRam HR800 Soleil spectrometer using a 532.3 nm excitation from DPSS laser, x100 objective (volume excitation of a few microns), and 1800 gr/mm gratings at the Laboratory of Geology from Lyon (LGL) in ENS, Lyon. Typical recording times are 30 s repeated ten times for an output power of 11 mW.

**Major elements composition** – For each sample, quantitative elemental analyses were conducted on polished sections using electron microprobe analyses (EPMA) Cameca SX100 at the Université Pierre et Marie Curie (UPMC) CAMPARIS facility. Two to four points were analyzed for each sample. The operating conditions were 15 kV accelerating voltage with a current of 10 nA and a counting time of 30 s, with a defocused beam (nominal diameter of 10 µm). Both natural and synthetic standards were used for calibration: albite for Na; anorthite for Al; chromite for Cr; apatite for P; garnet for Ca; orthoclase for K; MnTiO₃ for Mn and Ti; olivine for Fe, Si, Mg; and NiO for Ni. Typical detection limits are (in ppm): 454 for Na, 484 for Al, 290 for Mg, 593 for Si, 317 for Ca, 293 for K, 703 for Mn, 1458 for Ti, 806 for Fe, 999 for Ni, 1211 for Cr, and 278 for P. Unless otherwise stated, all uncertainties are reported as ±1σ.

A subset of samples was then cut using a wire saw to perform destructive analyses. An end-cut was used to prepare fragments or powders for chemical analyses.

**Trace elements composition** – Whole-rock major and trace elements were determined at the Pôle Spectrométrie Océan, Institut Universitaire Européen de la Mer (PSO/IUEM) in Brest, France. Major and trace elements were measured with a Thermo® Element XR HR-ICP-MS. A total of 100-150 mg of glass was digested on a hotplate heated to 120°C using sequential mixtures of HF/HNO₃, HNO₃, and HCl. Concentrations were
determined following the procedure described by Barrat et al. (2012, 2016). The reproducibility is always much better than 5%.

**Sr and Nd isotope composition** – Isotopic compositions were determined at the PSO/IUEM. Strontium and Nd fractions were prepared using the same sample solutions following conventional ion exchange techniques. They were analyzed using a Thermo® Triton TIMS spectrometer. Isotopic ratios were normalized against $^{86}$Sr/$^{88}$Sr = 0.1194 and $^{146}$Nd/$^{144}$Nd = 0.7219. The values obtained for NBS 987 and La Jolla standards during the study are respectively $^{87}$Sr/$^{86}$Sr = 0.710254 ± 0.000003 (2σ, n=8) and $^{143}$Nd/$^{144}$Nd = 0.511844 ± 0.000003 (2σ, n=6).

**3D characterization** – X-ray micro-computed tomography (μ-XCT) of samples T1196a and T1281, weighing 4.4 and 4.1 g, respectively, was performed using the microXCT-400 X-ray microscope (Zeiss) of the MATRIX platform at CEREGE. Data were acquired with a tungsten X-ray source at an accelerating voltage of 80 kV and a power of 10 W (125 μA). Each scan consisted of 1201 projections, with an exposure time of 4 seconds per projection, collected over a 360° rotation of the sample. Samples were placed in a polypropylene sample holder and blocked with a polystyrene spacer. 3D volume reconstruction was carried out using back-projection filtering (by XMRReconstructor: Xradia software), achieving an isotropic voxel size of 18.21 µm for T1196a and 20.27 µm for T1281, with corresponding field-of-view of 18.21×18.21×18.21 and 20.27×20.27×20.27 mm, respectively. The different voxel sizes of the samples are due to varying sample-to-detector distances: 150 mm for T1196a and 129.1 mm for T1281. The sample-to-source distance is the same for both samples, i.e., 55 mm. Visualization, processing, and analysis were conducted using Avizo 2020 software (Thermo Scientific, Hillsboro, OR, USA).

**$^{40}$Ar/$^{39}$Ar dating** – Each of the two tektites analyzed (T1196a and T1202a) has been crushed into several large pieces prior to sample preparation. For each tektite, we selected one large piece for further crushing. Glass fragments were hand-picked from either the 800-500 µm or the 500-212 µm fractions, grain-by-grain under the binocular stereomicroscope for each tektite, and were selected to avoid any bubbles or inclusions. Sub-samples weighing between 118 mg to 18 mg were sent for irradiation. The disc containing the samples was irradiated for 3 hours alongside FCs standards (Jourdan and Renne, 2007), for which an age of 28.294 Ma (± 0.13%) was used (Renne et al., 2011). The discs were Cd-shielded (to minimize undesirable nuclear interference reactions) and irradiated in the Oregon State University nuclear reactor (USA) in the central position. The mean J-values computed from standard grains within the small pits yielded a value of 0.0008222 (± 0.15%). Mass discrimination was monitored regularly through the analysis using an automated air pipette and provided mean values of 0.991077 (±0.07%) and 0.993045 (±0.05%) per dalton (atomic mass unit) relative to an air ratio of 298.56 ± 0.31 (Lee et al., 2006). The correction factors for interfering isotopes were ($^{39}$Ar/$^{37}$Ar) Ca = 6.95 × 10⁻⁴ (± 1.3 %), ($^{36}$Ar/$^{37}$Ar) Ca = 2.65 × 10⁻⁴ (± 0.84 %) and ($^{40}$Ar/$^{39}$Ar) K = 7.30 × 10⁻⁴ (± 12.4 %; Renne et al., 2013). The $^{40}$Ar/$^{39}$Ar analyses were performed at the Western Australian Argon Isotope Facility at Curtin University. Glass fragment populations were step-heated using a continuous 100 W PhotonMachine© CO2 (IR, 10.6 µm) laser fired on the crystals during 60 seconds. Each of the standard crystals was fused in a single step.

The gas was purified in an extra low-volume stainless steel extraction line of 240cc and using one SAES AP10 and one GP50 getter. Ar isotopes were measured in static mode using a low volume (600 cc) ARGUS VI mass spectrometer from Thermofisher© set with a permanent resolution of ~200. Measurements were carried out in multi-collection mode using four faradays to measure mass 40 to 37 and a low-background compact discrete dynode ion counter to measure mass 36. We measured the relative abundance of each mass simultaneously using 10 cycles of peak-hopping and 16 seconds of integration time for each mass. Detectors were calibrated to each other electronically and using Air shot beam signals. The raw data were processed using the ArArCALC software

(Koppers, 2002), and the ages were calculated using the decay constants recommended by Renne et al. (2011). Blanks were monitored every 3 to 4 steps. All parameters and relative abundance values are provided in Appendices B to E and have been corrected for blank, mass discrimination, and radioactive decay. Individual errors in Appendices B-E are given at the 1σ level.

Our criteria for the determination of plateaus are as follows: plateaus must include at least 70% of $^{39}$Ar. The plateau should be distributed over a minimum of 3 consecutive steps, agreeing at a 95% confidence level and satisfying a probability of fit (P) of at least 0.05. Plateau ages are given at the 2σ level and are calculated using the mean of all the plateau steps, each weighted by the inverse variance of their individual analytical error. Uncertainties include analytical and J-value errors. Errors with all sources of uncertainties provided for the weighted mean age preferred for the age of the tektite are indicated by a square bracket (e.g., ± [0.05] Ma).

## 3. Results

### 3.1. Preliminary screening and characterization

In four full days of magnetic susceptibility and SG screening of the SAM collection, we were able to survey several thousand specimens thanks to the pooling technique. A total of 417 specimens from 75 museum entries were selected as outliers based on anomalous SG and/or susceptibility. Once these specimens were brought to CEREGE, observation under a stereomicroscope after cleaning allowed us to identify some non-tektite material (rocks, asphalt, and a plaster cast). There, we measured mass and χ with more precision and confirmed the anomalously magnetic samples. Portable XRF measurement of all samples allowed to set apart a group of 6 specimens characterized simultaneously by low K (0.8 wt% versus 2 wt% on average for the other samples), high Ca/K (> 5 versus < 3), high Ni (> 300 ppm), high Sr/Rb (> 15 versus < 4), and low Th (< 15 ppm versus > 40 ppm) contents. All these features are typical of ananguites, as confirmed in the next sections. The magnetic susceptibility of the 6 samples ranges from 97 to 132 × 10⁻⁹ m³/kg (Table 1). The immersion of these samples in a heavy liquid mixture with SG = 2.5 confirmed that they all have SG > 2.5 (i.e., they sank to the bottom) like no other australite apart from the high Na/K type (Chapman and Scheiber, 1969). A similar survey was performed in two large tektite collections from Perth (i.e., mostly found in Western Australia), and no such samples were identified.

Fig. 1 depicts the six ananguite samples that come from four localities within northern South Australia. One sample from Williams Creek (T1196b) is a flake likely resulting from arrowhead preparation. The sample from Mount Davies (T1281) has a contorted shape never observed in other australites. The sample from Finniss Spring (T566) has a splash-form morphology. T566 and the other three samples have elliptical shapes quite typical for australites, as described by Chapman and Scheiber (1969), with significant abrasion. The 8 samples from Chapman and Scheiber (1969) come from two localities also represented in the present selection – Wilson Lake, the most productive, and Williams Creek (Table 1) – but also another locality: Raspberry Creek. In total, the 14 known ananguites come from 5 localities, with individual masses from 0.9 to 19 g and a cumulative mass of 53 g. In Fig. 2, the map depicts a strewn field that can be fit in an ellipse with a ~900 km long axis oriented N110. We note that high-mass samples and those with high susceptibility tend to be concentrated in the East, while the largest number of specimens is found in the West (Wilson Lake). This may be an artifact of the exceptionally productive Wilson Lake site, where thousands of small-sized tektites were recovered.

### 3.2. Petrography

Based on their petrographic analysis (porosity, presence of inclusions, and compositional heterogeneities, namely schlieren), samples
<caption>**Table 1**</caption>

List of the six ananguites characterized in this work, with their find location, geographical position within the strewn field (west/east), mass, magnetic susceptibility, and petrographic data on porosity and inclusions in all sections. For T1196a and T1281, more detailed results obtained through µ-XCT analysis are available in Table A1.

<table><thead><tr><th>Sample</th><th>T1202a</th><th>T1202b</th><th>T1281</th><th>T1196a</th><th>T1196b</th><th>T566</th></tr></thead><tbody><tr><td>Locality</td><td>Wilson Lake</td><td>Wilson Lake</td><td>Mount Davies</td><td>Williams Creek</td><td>Williams Creek</td><td>Finniss Spring</td></tr><tr><td>W/E</td><td>W</td><td>W</td><td>W</td><td>E</td><td>E</td><td>E</td></tr><tr><td>Mass (g)</td><td>1.9</td><td>1.4</td><td>4.1</td><td>4.4</td><td>1.4</td><td>19</td></tr><tr><td>χ (E-09 m³/kg)</td><td>105</td><td>110.7</td><td>115.1</td><td>114.9</td><td>131.9</td><td>132</td></tr><tr><td>Porosity (%)</td><td>0.9</td><td>0.1</td><td>0.7</td><td>0.2</td><td>0</td><td>0</td></tr><tr><td>Size range (µm)</td><td>4.9-377.4</td><td>4.9-75.2</td><td>100-400</td><td>7.4-195.8</td><td>nd</td><td>nd</td></tr><tr><td>Average (µm)</td><td>56.5±69</td><td>35.4±23</td><td>170.0±100</td><td>72.8±48</td><td>nd</td><td>nd</td></tr><tr><td>Porosity (mm²)</td><td>0.31</td><td>0.01</td><td>0.3</td><td>0.22</td><td>nd</td><td>nd</td></tr><tr><td>Inclusions (%)</td><td>0.02</td><td>nd</td><td>0.01</td><td>nd</td><td>nd</td><td>nd</td></tr><tr><td>Inclusion size (µm)</td><td>~100 µm (n=2)</td><td>nd</td><td>~100 µm (n=2)</td><td>nd</td><td>nd</td><td>nd</td></tr><tr><td>V<sub>tot</sub> (mm³)</td><td>3.05</td><td>2.96</td><td>7.3</td><td>18.69</td><td>1.37</td><td>3.24</td></tr></tbody></table>

<figure><img src="image_4.png" /><figcaption>**Fig. 1.** (a) Picture of the six high Na/K australites studied. The find location of each tektite is indicated at the top of each column, and the mass is reported for each specimen. (b) Polished sections of the same samples under the optical microscope. For samples from the same location, the specimen with higher mass is labelled ‘a’ and the other ‘b’. All scale bars correspond to 2 mm.</figcaption></figure>

can be subdivided into three groups: (i) 0 % porosity, no inclusions, no schlieren (T1196b, T566; from Williams Creek and Finniss Spring), (ii) low porosity (0.1-0.2 %), no inclusions, no schlieren (T1202b, T1196a; from Wilson Lake and Williams Creek), (iii) porosity 0.7-0.9 %, 100-µm-sized inclusions (< 0.02 area%), schlieren textures (< 6 area%) (T1202a and T1281; from Wilson Lake and Mount Davies) (Table 1). When present, the inclusions have been identified as lechatelierite using Raman spectroscopy (see below).

To further investigate the porosity and presence of inclusions in the tektites, we used µ-XCT characterization on two samples representative of the types of samples: T1196a (homogeneous) and T1281 (non-homogeneous) (Fig. 3). The absence of both vesicles and lechatelierite inclusions in the polished samples of T1196b and T566 led us to favor the other samples for 3D investigation. The results are summarized in Table A1.

T1196a has a porosity of 2.2 vol.%. Bubbles are isolated and have a highly heterogeneous distribution. They are spherical and have a right-skewed size distribution, with 98 % of the bubbles having a size range of 23-847 µm, and a median diameter of 104.3 µm. There are a few large

bubbles, with a maximum diameter of 3300 µm. Though on average sphericity is high (ψ = 0.9), some bubbles show preferential orientation (ψ = 0.7-0.8), especially the ones surrounding the biggest bubble at the center of the sample (Fig. 3a,c,d). As for the petrographic analysis, no inclusions are found in T1196a using µ-XCT. One schlieren texture is observed.

T1281 has a porosity of 0.8 vol.%. Bubbles are isolated, with a heterogeneous and right-skewed size distribution and a median diameter of 107 µm. The biggest one has an equivalent diameter of 1187 µm. Bubbles are not oriented, being practically perfect spheres (ψ = 1.0) (Fig. 3b-d). T1281 counts 31 similar inclusions from the µ-XCT analysis (two inclusions of lechatelierite were observed in the polished sample). The inclusions are identified for their darker color compared to the surrounding glass (Fig. A1) and have been manually selected from the volume of the tektite. The inclusions have an equivalent diameter of 183 ± 62 µm and occupy 0.01 vol.%. Schlieren textures are frequently observed in the volume of T1281.
<figure><img src="image_5.png" /><figcaption>**Fig. 2.** Simplified map of the ananguites strewn field, based on the tektite locations reported by Chapman and Scheiber (1969) and this study.</figcaption></figure>

### 3.3. Geochemistry

Major and trace element compositions are presented in Tables 2 and 3, respectively. Overall, ananguites have andesitic to dacitic composition, on average (in wt%): SiO₂ 63.2 ± 0.8, Al₂O₃ 16.9 ± 0.5, FeO 5.8 ± 0.7, CaO 5.0 ± 0.7, MgO 3.9 ± 0.4, Na₂O 3.3 ± 0.5, K₂O 1.0 ± 0.1 (± 1σ) (Fig. A2). Geochemical differences are observed when comparing ananguites from the western and the eastern regions of the strewn field (hereafter W- and E-ananguites), including the samples in Chapman and Scheiber (1969). W-ananguites are richer in alkali (specifically Na₂O) compared to the E-counterpart (3.71 ± 0.16 vs. 2.92 ± 0.4 wt%). Other systematic variations in the composition are observed for CaO (4.42 ± 0.03 vs. 5.78 ± 0.11 wt%), MgO (3.61 ± 0.24 vs. 4.13 ± 0.49 wt%), and Al₂O₃ (17.26 ± 0.08 vs. 16.50 ± 0.18 wt%) (Fig. A3).

In terms of trace elements composition, ananguites display negative anomalies in Nb, Ta, and Ti, and a positive anomaly in Sr, and no Eu anomaly. Their distribution patterns are shown in Fig. 4, alongside those of Australasian tektites for comparison. The rare earth element (REE) pattern is characterized by enrichment in light REEs (LREE) relative to heavy REEs (HREE), with $\Sigma_{LREE}/\Sigma_{HREE}$ ratios ranging from 2.7 to 2.9 (in contrast, Australasian tektites typically display ratios close to 10; Koeberl, 1990). The average La/Sc and Th/Sc ratios are 1.31 ± 0.07 and 0.34 ± 0.01 ppm, respectively. W-ananguites, compared to E-ananguites, show lower concentrations of Cr (194 ± 36 vs. 319 ± 41 ppm), Co (43 ± 8 vs. 65 ± 8 ppm), and Ni (589 ± 144 vs. 819 ± 78 ppm), and higher concentrations in Zn (13 ± 2 vs. 3 ± 3 ppm), Cu (11 ± 1 vs. 7 ± 5 ppm), and Pb (1.5 ± 0.1 vs. 0.6 ± 0.5 ppm). In addition, W-ananguites are slightly richer in REE than E-ananguites, although both groups display the same overall REE distribution pattern (Fig. A4).

The correlation between FeO content and magnetic susceptibility, corrected for the minor contribution of Mn, Cr, and Ni, indicates that iron is mainly in the Fe²⁺ state (Fig. A5, after Rochette et al., 2015; 2019).

The isotopic composition of Nd and Sr is reported in Table 3. The value of ¹⁴³Nd/¹⁴⁴Nd ranges from 0.512870–0.512917, and ⁸⁷Sr/⁸⁶Sr from 0.703576–0.703813. $\varepsilon_{Nd}$ is the measured deviation of the ¹⁴³Nd/¹⁴⁴Nd from the present-day chondritic uniform reservoir (CHUR) 0.512630 (Bouvier et al., 2008), in parts per 10⁴, and ranges from 4.7 to 5.6. The isotopic composition of ananguites, in terms of ⁸⁷Sr/⁸⁶Sr and $\varepsilon_{Nd}$, is shown in Fig. 5, alongside convergent arc andesites within 5000

km around Australia and another Australian hypothesized source rock (New England batholith, Australia), addressed in the Discussion section.

### 3.4. Raman spectroscopy

Inclusions of lechatelierite have been identified using SEM-EDS and Raman spectroscopy in T1202 and T1281 (Fig. A6). In T1281, tiny spherical inclusions in silica display a glass-like to crystalline phosphate signature, along with silica-rich glass features similar to unmixed domains observed in phosphate-bearing synthetic glasses (Toplis and Reynard, 2000) and tektites (Zanetta et al., 2024). Spectra collected in the OH stretching region display no measurable OH or water (Di Muro et al., 2006).

### 3.5. ⁴⁰Ar/³⁹Ar dating

Each of the four analyzed aliquots from two tektite specimens yielded a well-defined plateau age with concordant ages ranging from 10.74 ± 0.11 Ma to 10.81 ± 0.09 Ma and with P-values > 0.10 (Fig. 6). The two samples analyzed come from the western (1202a) and eastern (T1196a) parts of the strewn field. Plateaus include between 92 and 100 % of the total ³⁹Ar released. Inverse isochrons show indistinguishable ages ranging from 10.59 ± 0.15 to 10.74 ± 0.40 Ma along with ⁴⁰Ar/³⁶Ar intercept ratios ranging from 334 ± 28 to 305 ± 41. Three of the intercept values are well within the composition of the atmosphere of ~ 299 (Lee et al., 2006). A global inverse isochron including all samples yields an age of 10.67 ± 0.09 Ma (P = 0.69), whereas a weighted mean age of the four inverse isochrons yields an age of 10.66 ± 0.10 Ma (P = 0.69).

We calculated a combined age of 10.76 ± [0.05] Ma (MSWD = 0.97; P = 0.54) including all sources of uncertainties, using the four plateau ages, and interpreted it as representing the best estimate of the age of the impact which produced the ananguites.

## 4. Discussion

**Geochemistry** – Ananguites have SiO₂ contents lower than the average of other tektites, except for belizites (also andesitic composition but richer in alkalis, Koeberl et al. [2022]; Fig. A2). Overall, the samples analyzed show no difference compared to the samples analyzed in Chapman and Scheiber (1969). Compared to Australasian tektites, ananguites show different trace element patterns and higher total REE content, with no Eu anomaly. The number of samples considered is too small to confidently state the existence of a significant difference between western and eastern samples. However, differences in major oxides, trace elements, Sm and Nd, as well as ⁸⁷Sr/⁸⁶Sr and ¹⁴³Nd/¹⁴⁴Nd ratios, suggest a slight compositional variation between the two locations, based on samples from this and previous studies.

The Ni, Co, and Cr contents in tektites, in particular Co/Ni and Cr/Ni ratios, can be used to identify terrestrial and extraterrestrial reservoirs (Glass et al., 2004; Goderis et al., 2017; Folco et al., 2018). Ananguites are enriched in Ni, Co, and Cr compared to upper continental crust (UCC), with Ni reaching 704 ppm – 15 times higher than UCC levels – while Co and Cr are 54 and 257 ppm, respectively, about three times the UCC values (Rudnick and Gao, 2004; Taylor and McLennan, 1995). Ni is also enriched relative to Australasian tektites, which typically contain < 430 ppm, with a median value of 35 ppm (Folco et al., 2023). This distinction from the Australasian tektites was previously noted in studies on the target rock of the Australasian strewn field (Goderis et al., 2017). Goderis et al. (2017) also documented that the Cr vs. Ni contents of ananguites are consistent with a chondritic impactor (see their Fig. 2a). The Co/Ni (0.05-0.09) and Cr/Ni (0.29-0.44) values are close to chondritic compositions (Folco et al., 2018). The chondritic Ni enrichment is also evident in Fig. A7, where the Mg and Ni compositions of ananguites are plotted alongside those of andesites from the surrounding volcanic arcs (discussed in the next paragraphs) and a chondritic (CI)
<figure><img src="image_6.png" /><figcaption>**Fig. 3.** µ-XCT images of (a) T1196a and (b) T1281. (c) Bubble size distribution vs. sphericity in T1196 and T1281. (d) Bubble size distribution curves of T1196 (blue) and T1281 (green), showing frequency as a function of equivalent sphere diameter (µm). T1281 is dominated by smaller bubbles of smaller compared to T1196. The bubble frequency in T1281 decreases sharply after the peak, while T1196 has a slower decrease, indicating a broader size distribution. The more gradual decline of T1196 indicates that it contains more numerous bigger particles.</figcaption></figure>

composition. The correlations between Co and Ni, as well as Cr and Ni, using both Chapman's and our data, are shown in Fig. A3e,f.

The trace element spidergram is consistent with a typical subduction-related signature. The ε$_{Nd}$ values of ananguites range from 4.7 to 5.6. These values overlap those of oceanic island arcs and are distinct from other tektites, which, except for belizites, have ε$_{Nd}$ < 0 (Fig. 5). In particular, they are significantly different from Australasian tektites (Muong Nong and splash-form), which exhibit higher $^{87}$Sr/$^{86}$Sr ratios (0.716361-0.720206) and strongly negative ε$_{Nd}$ values (~ -11; e.g., Fig. 2 in Shaw and Wasserburg, 1982; Ackermann et al., 2020; Blum et al., 1992) more akin to continental crust.

**Do ananguites deserve to be ranked among the tektite strewn fields?** – Ananguites occur as splash forms and show a narrow range of chemical and isotopic compositions. Iron is present primarily as Fe$^{2+}$, and the water content is < 80 ppm (Beran and Koeberl, 1997). They have low vesicularity, with lechatelierite as the only inclusion observed, apart from a few micron-sized phosphate droplets, which are also found in other tektites (Zanetta et al., 2024). These characteristics, along with distinct extraterrestrial contamination, clearly indicate they are impact

glasses. Combined with a strewn field extension of ~ 900 km (Fig. 2), these characteristics also point toward tektites. Their andesitic composition is not standard for tektites, but the same is true for belizites, and it is likely to be because andesite is not an abundant type of crustal rock overall. They stand out due to their significant extraterrestrial contamination compared to other tektite fields. Based on these combined features, we propose that they deserve to be ranked among bona fide tektites, making them the sixth tektite strewn field confirmed in a peer-reviewed publication. This recent increase from 4 to possibly 8 strewn fields, including the two only proposed in abstracts (Ferrière et al., 2017; Crósta et al., 2024), might suggest that tektite-producing impacts are less rare occurrences in the impact record than previously thought.

We propose the name “ananguites” for this new tektite strewn field. It is the only one found exclusively in Australia, but the name “australite” is already in use. The area lacks a specific geographic name; however, it is the territory of one particular Aboriginal group that belongs to the “Central Occidental Desert” cultural group. In particular, the Pitjantjatjara (whose territory includes the famous Uluru Mountain) and
<caption>**Table 2**</caption>

Microprobe and HR-ICP-MS results for major element composition of ananguites from this study and Chapman & Scheiber (1969). All values have been normalized to 100.

<table><thead><tr><th></th><th>Sample</th><th>Location</th><th>W/ E</th><th>SiO<sub>2</sub></th><th>TiO<sub>2</sub></th><th>Al<sub>2</sub>O<sub>3</sub></th><th>FeO</th><th>MnO</th><th>MgO</th><th>CaO</th><th>Na<sub>2</sub>O</th><th>K<sub>2</sub>O</th><th>NiO</th><th>P<sub>2</sub>O<sub>5</sub></th><th>Na/ K</th></tr></thead><tbody><tr><td rowspan="7">Microprobe</td><td>T1202a</td><td>Wilson Lake</td><td>W</td><td>63.40</td><td>0.68</td><td>17.33</td><td>5.50</td><td>0.09</td><td>3.72</td><td>4.45</td><td>3.59</td><td>1.03</td><td>0.09</td><td>0.12</td><td>3.12</td></tr><tr><td>T1202b</td><td>Wilson Lake</td><td>W</td><td>64.68</td><td>0.59</td><td>17.18</td><td>4.60</td><td>0.08</td><td>3.34</td><td>4.39</td><td>3.90</td><td>1.06</td><td>0.06</td><td>0.12</td><td>3.29</td></tr><tr><td>T1281</td><td>Mount Davies</td><td>W</td><td>63.27</td><td>0.61</td><td>17.29</td><td>5.58</td><td>0.10</td><td>3.78</td><td>4.43</td><td>3.65</td><td>1.07</td><td>0.08</td><td>0.14</td><td>3.05</td></tr><tr><td>T1196a</td><td>Williams Creek</td><td>E</td><td>62.99</td><td>0.66</td><td>16.47</td><td>5.63</td><td>0.06</td><td>3.57</td><td>5.91</td><td>3.32</td><td>1.14</td><td>0.10</td><td>0.15</td><td>2.60</td></tr><tr><td>T1196b</td><td>Williams Creek</td><td>E</td><td>62.11</td><td>0.63</td><td>16.33</td><td>6.66</td><td>0.08</td><td>4.43</td><td>5.72</td><td>2.9</td><td>0.98</td><td>0.09</td><td>0.05</td><td>2.64</td></tr><tr><td>T566</td><td>Finniss Spring</td><td>E</td><td>62.02</td><td>0.53</td><td>16.76</td><td>6.49</td><td>0.13</td><td>4.49</td><td>5.81</td><td>2.65</td><td>0.95</td><td>0.12</td><td>0.06</td><td>2.49</td></tr><tr><td>T1202a</td><td>Wilson Lake</td><td>W</td><td>64.0</td><td>0.60</td><td>16.52</td><td>5.71</td><td>0.10</td><td>3.84</td><td>4.43</td><td>3.64</td><td>1.07</td><td>nd</td><td>0.10</td><td>3.03</td></tr><tr><td rowspan="7">HR-ICP-MS</td><td>T1202b</td><td>Wilson Lake</td><td>W</td><td>65.0</td><td>0.57</td><td>16.57</td><td>4.76</td><td>0.09</td><td>3.39</td><td>4.44</td><td>4.03</td><td>1.02</td><td>nd</td><td>0.09</td><td>3.54</td></tr><tr><td>T1281</td><td>Mount Davies</td><td>W</td><td>62.1</td><td>0.64</td><td>17.50</td><td>6.09</td><td>0.10</td><td>3.85</td><td>4.58</td><td>3.94</td><td>1.10</td><td>nd</td><td>0.10</td><td>3.20</td></tr><tr><td>T1196a</td><td>Williams Creek</td><td>E</td><td>62.7</td><td>0.56</td><td>16.30</td><td>5.76</td><td>0.10</td><td>3.83</td><td>6.21</td><td>3.34</td><td>1.12</td><td>nd</td><td>0.08</td><td>2.65</td></tr><tr><td>T1196b</td><td>Williams Creek</td><td>E</td><td>62.6</td><td>0.57</td><td>16.17</td><td>6.62</td><td>0.11</td><td>4.48</td><td>5.83</td><td>2.69</td><td>0.89</td><td>nd</td><td>0.02</td><td>2.72</td></tr><tr><td>T566</td><td>Finniss Spring</td><td>E</td><td>62.4</td><td>0.56</td><td>16.20</td><td>6.97</td><td>0.11</td><td>4.45</td><td>5.79</td><td>2.56</td><td>1.01</td><td>nd</td><td>0.01</td><td>2.28</td></tr><tr><td rowspan="7">Chapman & Scheiber (1969)</td><td>23</td><td>South of Lake Wilson</td><td>W</td><td>63.6</td><td>0.6</td><td>16.9</td><td>5.7</td><td>nd</td><td>3.8</td><td>4.5</td><td>3.7</td><td>1.1</td><td>0.10</td><td>nd</td><td>3.3</td></tr><tr><td>24</td><td>South of Lake Wilson</td><td>W</td><td>63.6</td><td>0.6</td><td>16.9</td><td>5.7</td><td>nd</td><td>3.7</td><td>4.5</td><td>3.9</td><td>1.1</td><td>0.10</td><td>nd</td><td>3.6</td></tr><tr><td>25</td><td>South of Lake Wilson</td><td>W</td><td>62.3</td><td>0.6</td><td>18.1</td><td>5.8</td><td>nd</td><td>3.8</td><td>4.4</td><td>3.8</td><td>1.1</td><td>0.10</td><td>nd</td><td>3.5</td></tr><tr><td>26</td><td>South of Lake Wilson</td><td>W</td><td>64.1</td><td>0.7</td><td>16.5</td><td>5.6</td><td>nd</td><td>3.6</td><td>4.5</td><td>3.8</td><td>1.1</td><td>0.10</td><td>nd</td><td>3.6</td></tr><tr><td>27</td><td>South of Lake Wilson</td><td>W</td><td>63.6</td><td>0.5</td><td>17</td><td>5.9</td><td>nd</td><td>3.8</td><td>4.5</td><td>3.5</td><td>1</td><td>0.10</td><td>nd</td><td>3.5</td></tr><tr><td>28</td><td>South of Lake Wilson</td><td>W</td><td>63.4</td><td>0.6</td><td>17.2</td><td>5.6</td><td>nd</td><td>3.6</td><td>4.6</td><td>3.8</td><td>1.1</td><td>0.10</td><td>nd</td><td>3.5</td></tr><tr><td>21</td><td>Williams Creek</td><td>E</td><td>62.4</td><td>0.6</td><td>15.8</td><td>6.9</td><td>nd</td><td>4.7</td><td>5.8</td><td>2.8</td><td>0.9</td><td>0.10</td><td>nd</td><td>3.1</td></tr><tr><td>22</td><td>Raspberry bore</td><td>E</td><td>64.1</td><td>0.5</td><td>15.8</td><td>6</td><td>nd</td><td>3.7</td><td>6</td><td>2.8</td><td>1</td><td>0.10</td><td>nd</td><td>2.7</td></tr></tbody></table>

Yankunytjatjara people (in the western part of the strewn field) refer to themselves as *Anangu* (“human being”). Alternatively, “uluruite” would follow the geographic naming tradition used for other strewn fields, but Uluru is a specific location in the Northern Territory, whereas all these tektites were found in Southern Australia.

The low number of known ananguites (14 specimens) is somewhat unusual compared to other strewn fields: from more than 600,000 australasite specimens (McCall, 2001) to less than a thousand ivorite specimens (Soro et al., 2023). Their occurrence and similarity with the larger australasite strewn field may explain why so few have been discovered so far. We suspect that more specimens remain to be identified among australite collections. As for the case of Lake Wilson, it is possible that, at least in some areas, the ratio of ananguites over australites could be on the order of 1 %. We also note that the 900 km extent of the ananguite distribution exceeds that of belizites (~ 60 km; Rochette et al., 2021), ivorites (~ 105 km; Soro et al., 2023), and moldavites (~ 300 km; Stöffler et al., 2002), while it is smaller than that of bediasites-georgiaites and australasites (> 5000 km in size; Glass and Simonson, 2013; Folco et al., 2016). As a first approximation, increasing sizes of strewn fields (belizites, ivorites < moldavites < bediasites-georgiaites) may be associated with progressively larger craters. This might suggest that the source crater could be significantly larger than the ones of the former mentioned strewn fields (Pantasma = 14 km, Bosumtwi = 10.5 km, and Ries = 26 km), i.e. > 26 km in diameter.

**Age and source crater** – The impact age is 10.76 ± 0.05 Ma, confirming no relationship with known tektite strewn fields. The younger and different ages obtained by previous fission tracks (Fleischer et al., 1969; Storzer, 1985) have already been dismissed by the more recent K/Ar and $^{40}$Ar/$^{39}$Ar dating on the same samples (Storzer and Müller-Sohnius, 1986; Bottomley and Koeberl, 1999). These latest measurements on ananguite specimens classified by Chapman and Scheiber (1969) are in agreement with the more accurate age obtained in this work on newly identified samples. No well-dated crater of compatible age is currently known. If we consider a strewn field-to-crater distance similar to that of belizites, ivorites, or moldavites (< 2000 km), the source crater should be located within Australia. Based on age alone, only Piccaninny (< 383 Ma, 7 km), Toondina (< 125 Ma, 4 km), and Connolly (23-70 Ma, 9 km) are vaguely compatible, although the real age of these impact structures is more than uncertain (Quintero et al., 2021). Toondina is the closest candidate, as it lies within the strewn field area (Fig. 7). All these structures are poorly studied (and not even

confirmed using present-day criteria), but they can be readily excluded based on their geochemical mismatch with ananguites. For example, Connolly and Toondina formed in Mesozoic intracratonic detrital sediments, while the Lake Reaside target consists of granitic rocks, both inconsistent with the subduction-related geochemical signature observed in the tektites. Overall, only the New England Orogen (Eastern Australia), of Permo-Triassic age, may provide such a signature in Australia (Phillips et al., 2011). A single, unconfirmed structure approximately 20 km in diameter has been proposed within this orogen: Tingha (Quintero et al., 2021). However, the geological context suggests a magmatic intrusion of adamellite composition (Glikson, 2018). Therefore, it is much more likely that the source crater should be sought in the subduction-related island arcs surrounding Australia. Within a 3500 km radius of Lake Wilson, potential areas include subduction zones extending from Java to New Zealand. This distance is consistent with the known relationships between strewn fields and their source craters, as observed in both the North American and Australasian tektite strewn fields. A large, 11 Ma-old crater could easily have been overlooked in regions like Papua New Guinea, where circular structures are commonly attributed to volcanic processes. We also refrain from using the elongation of the strewn field or the size distribution of the tektites to suggest a preferred azimuth for the impact zone, given the currently limited number of observations.

To determine the source of the ananguites, we considered rocks with similar major element compositions within a 5000 km radius of the strewn field center (arbitrary size threshold to ensure that no potential source candidates were excluded), using the GEOROC Compilation database (https://doi.org/10.25625/PVFZCE) (Fig. 7). The convergent arcs considered include Sunda, Banda, Sulawesi, Luzon, Halmahera, Bismarck/New England, Solomon, New Hebrides/Vanuatu, Tonga, Kermadec, and New Zealand. The $^{87}$Sr/$^{86}$Sr and eNd values of ananguites fall within the range observed in andesites from convergent volcanic arcs in the Philippines (Luzon Arc, Maquiling; Defant et al., 1991; Knittel et al., 1997; Vogel et al., 2006), Indonesia (Sulawesi Arc; Leterrier et al., 1990; Priadi et al., 1994; Polvé et al., 1997; Elburg and Foden, 1998; Elburg and Foden, 1999; Polvé et al., 2001; Elburg et al., 2003; Zhang et al., 2022), New Guinea and Lamington Mountain (Bismarck Arc; Hickey and Frey, 1982; Arculus et al., 1983; Hegner and Smith, 1992; Cunningham et al., 2009; König et al., 2010; Zhang et al., 2015; Patia et al., 2017; Hohl et al., 2022). Comparing trace element compositions of the selected areas, the ananguite patterns are similar to those of the Luzon Arc (Maquiling), Sulawesi Arc (Sulawesi), and Bismarck Arc
<table><caption>**Table 3**
Trace elements abundances and Sr and Nd isotopic compositions of ananguites.</caption><thead><tr><th></th><th></th><th>T1202a<br>Wilson Lake<br>W</th><th>T1202b<br>Wilson Lake<br>W</th><th>T1281<br>Mount Davies<br>W</th><th>T1196a<br>Williams Creek<br>E</th><th>T1196b<br>Williams Creek<br>E</th><th>T566<br>Finniss Spring<br>E</th><th>Average</th><th>S.D.</th></tr></thead><tbody><tr><td>Li</td><td>ppm</td><td>24.29</td><td>25.42</td><td>25.34</td><td>32.22</td><td>34.54</td><td>32.03</td><td>28.97</td><td>4.44</td></tr><tr><td>Be</td><td>ppm</td><td>1.33</td><td>1.28</td><td>1.30</td><td>1.22</td><td>1.26</td><td>1.22</td><td>1.27</td><td>0.04</td></tr><tr><td>P</td><td>ppm</td><td>411</td><td>388</td><td>479</td><td>329</td><td>92.1</td><td>52</td><td>292</td><td>177</td></tr><tr><td>K</td><td>ppm</td><td>8799</td><td>8927</td><td>9973</td><td>10218</td><td>8251</td><td>8191</td><td>9060</td><td>857</td></tr><tr><td>Sc</td><td>ppm</td><td>13.16</td><td>11.69</td><td>13.35</td><td>11.74</td><td>13.51</td><td>13.25</td><td>12.78</td><td>0.84</td></tr><tr><td>Ti</td><td>ppm</td><td>3537</td><td>3451</td><td>3845</td><td>3194</td><td>3371</td><td>3388</td><td>3464</td><td>218</td></tr><tr><td>V</td><td>ppm</td><td>90.53</td><td>78.52</td><td>99.10</td><td>87.35</td><td>87.80</td><td>90.40</td><td>88.95</td><td>6.64</td></tr><tr><td>Cr</td><td>ppm</td><td>204</td><td>155</td><td>224</td><td>274</td><td>328</td><td>356</td><td>257</td><td>77</td></tr><tr><td>Mn</td><td>ppm</td><td>745</td><td>678</td><td>800</td><td>761</td><td>836</td><td>849</td><td>778</td><td>64</td></tr><tr><td>Co</td><td>ppm</td><td>44.68</td><td>33.74</td><td>49.31</td><td>55.13</td><td>67.27</td><td>71.18</td><td>53.55</td><td>14.08</td></tr><tr><td>Ni</td><td>ppm</td><td>632</td><td>428</td><td>706</td><td>818</td><td>741</td><td>897</td><td>704</td><td>163</td></tr><tr><td>Cu</td><td>ppm</td><td>11.51</td><td>10.18</td><td>12.64</td><td>12.43</td><td>3.76</td><td>5.74</td><td>9.38</td><td>3.74</td></tr><tr><td>Zn</td><td>ppm</td><td>14.04</td><td>11.53</td><td>14.71</td><td>6.16</td><td>1.59</td><td>1.39</td><td>8.24</td><td>6.03</td></tr><tr><td>Ga</td><td>ppm</td><td>26.97</td><td>28.22</td><td>30.08</td><td>25.91</td><td>21.64</td><td>22.41</td><td>25.87</td><td>3.30</td></tr><tr><td>Rb</td><td>ppm</td><td>24.84</td><td>24.62</td><td>26.13</td><td>26.36</td><td>20.19</td><td>21.36</td><td>23.92</td><td>2.56</td></tr><tr><td>Sr</td><td>ppm</td><td>421</td><td>462</td><td>449</td><td>388</td><td>406</td><td>401</td><td>421</td><td>29</td></tr><tr><td>Y</td><td>ppm</td><td>15.06</td><td>13.90</td><td>15.81</td><td>13.08</td><td>13.86</td><td>13.76</td><td>14.25</td><td>1.00</td></tr><tr><td>Zr</td><td>ppm</td><td>135</td><td>139</td><td>141</td><td>127</td><td>130</td><td>129</td><td>134</td><td>6</td></tr><tr><td>Nb</td><td>ppm</td><td>4.03</td><td>4.03</td><td>4.21</td><td>3.62</td><td>3.84</td><td>3.77</td><td>3.92</td><td>0.21</td></tr><tr><td>Cs</td><td>ppm</td><td>1.87</td><td>1.32</td><td>1.34</td><td>1.45</td><td>0.80</td><td>1.06</td><td>1.31</td><td>0.36</td></tr><tr><td>Ba</td><td>ppm</td><td>360</td><td>354</td><td>362</td><td>334</td><td>346</td><td>342</td><td>349</td><td>11</td></tr><tr><td>La</td><td>ppm</td><td>16.53</td><td>16.50</td><td>17.98</td><td>15.53</td><td>16.48</td><td>17.48</td><td>16.75</td><td>0.86</td></tr><tr><td>Ce</td><td>ppm</td><td>35.30</td><td>34.53</td><td>36.59</td><td>31.37</td><td>33.56</td><td>33.21</td><td>34.09</td><td>1.81</td></tr><tr><td>Pr</td><td>ppm</td><td>4.25</td><td>4.11</td><td>4.39</td><td>3.77</td><td>3.99</td><td>3.97</td><td>4.08</td><td>0.22</td></tr><tr><td>Nd</td><td>ppm</td><td>16.96</td><td>16.31</td><td>17.54</td><td>14.94</td><td>15.89</td><td>15.63</td><td>16.21</td><td>0.94</td></tr><tr><td>Sm</td><td>ppm</td><td>3.41</td><td>3.22</td><td>3.56</td><td>2.99</td><td>3.17</td><td>3.14</td><td>3.25</td><td>0.20</td></tr><tr><td>Eu</td><td>ppm</td><td>1.02</td><td>0.989</td><td>1.07</td><td>0.904</td><td>0.952</td><td>0.941</td><td>0.979</td><td>0.059</td></tr><tr><td>Gd</td><td>ppm</td><td>2.94</td><td>2.80</td><td>2.98</td><td>2.53</td><td>2.71</td><td>2.66</td><td>2.77</td><td>0.17</td></tr><tr><td>Tb</td><td>ppm</td><td>0.448</td><td>0.413</td><td>0.462</td><td>0.380</td><td>0.406</td><td>0.404</td><td>0.419</td><td>0.031</td></tr><tr><td>Dy</td><td>ppm</td><td>2.57</td><td>2.38</td><td>2.64</td><td>2.23</td><td>2.37</td><td>2.33</td><td>2.42</td><td>0.15</td></tr><tr><td>Ho</td><td>ppm</td><td>0.511</td><td>0.475</td><td>0.528</td><td>0.444</td><td>0.474</td><td>0.468</td><td>0.483</td><td>0.031</td></tr><tr><td>Er</td><td>ppm</td><td>1.43</td><td>1.32</td><td>1.51</td><td>1.25</td><td>1.33</td><td>1.32</td><td>1.36</td><td>0.10</td></tr><tr><td>Yb</td><td>ppm</td><td>1.36</td><td>1.26</td><td>1.42</td><td>1.20</td><td>1.28</td><td>1.28</td><td>1.30</td><td>0.08</td></tr><tr><td>Lu</td><td>ppm</td><td>0.199</td><td>0.185</td><td>0.209</td><td>0.177</td><td>0.186</td><td>0.186</td><td>0.190</td><td>0.011</td></tr><tr><td>Hf</td><td>ppm</td><td>3.44</td><td>3.56</td><td>3.60</td><td>3.28</td><td>3.39</td><td>3.34</td><td>3.43</td><td>0.13</td></tr><tr><td>Ta</td><td>ppm</td><td>0.253</td><td>0.261</td><td>0.254</td><td>0.203</td><td>0.238</td><td>0.214</td><td>0.237</td><td>0.024</td></tr><tr><td>Pb</td><td>ppm</td><td>1.56</td><td>1.36</td><td>1.50</td><td>1.15</td><td>0.39</td><td>0.36</td><td>1.05</td><td>0.55</td></tr><tr><td>Th</td><td>ppm</td><td>4.24</td><td>4.19</td><td>4.34</td><td>4.12</td><td>4.54</td><td>4.44</td><td>4.31</td><td>0.16</td></tr><tr><td>U</td><td>ppm</td><td>0.863</td><td>0.857</td><td>0.864</td><td>0.924</td><td>0.815</td><td>0.847</td><td>0.862</td><td>0.035</td></tr><tr><td><sup>87</sup>Sr/<sup>86</sup>Sr</td><td></td><td>0.703612</td><td>0.703576</td><td>0.703618</td><td>0.703795</td><td>0.703806</td><td>0.703813</td><td></td><td></td></tr><tr><td>2SE</td><td></td><td>0.000006</td><td>0.000006</td><td>0.000006</td><td>0.000006</td><td>0.000006</td><td>0.000006</td><td></td><td></td></tr><tr><td><sup>143</sup>Nd/<sup>144</sup>Nd</td><td></td><td>0.512902</td><td>0.512917</td><td>0.512898</td><td>0.512889</td><td>0.512870</td><td>0.512873</td><td></td><td></td></tr><tr><td>2SE</td><td></td><td>0.000008</td><td>0.000011</td><td>0.000005</td><td>0.000005</td><td>0.000007</td><td>0.000007</td><td></td><td></td></tr><tr><td>ε<sub>Nd</sub></td><td></td><td>5.3</td><td>5.6</td><td>5.2</td><td>5.0</td><td>4.7</td><td>4.7</td><td></td><td></td></tr></tbody></table>

(Lamington Mountain) (Fig. A8a-f). New Guinea in the Bismarck Arc, with possibly matching Sr-Nd isotopic compositions, displays distinct trace element features (Fig. A8g-h) and is therefore excluded as a possible source. A useful tool to identify the most likely source among the ones identified can be the differences between western and eastern tektites, as discussed in the next paragraph.

**Western vs. eastern ananguites** – Geochemical analyses reveal slight but systematic variations between the western and eastern samples. Petrographic observations (vesiculation, bubble size distributions, number of inclusions) also highlight differences between the two locations.

Relying solely on the find location of tektites could lead to erroneous conclusions, as these glasses could have been transported over time by humans, for the fabrication of tools (e.g., arrowheads), and by animals, such as emus in Australia, which use them as gastroliths (rocks swallowed to aid digestion). However, the presence of geochemical differences among geographically separated tektites of the same strewn field suggests that tektites have been collected rather close to the areas where they originally fell.

Considering all samples, and in agreement with 3D results, two-dimensional analysis of inclusions and porosity reveals that those with the highest vesiculation and inclusions are found in the western part of

the strewn field (Mount Davies and Wilson Lake), while those with no inclusions and no vesiculation are found in the east (Williams Creek and Finniss Spring) (Tables 1 and A1). Samples with intermediate characteristics, based on the petrographic analysis, include one from the west (T1202b, Wilson Lake) and one from the east (T1196a, Williams Creek). However, for example, for T1202b, only a very thin polished section was analyzed, which may introduce bias in the porosity and inclusion count.

Worth mentioning, highly volatile metals such as Cu, Zn, and Pb are lower in E-ananguites (except for T1196a, which shows similar values to W-ananguites), and Ni, Cr, and Co are more enriched in E-ananguites. This may suggest that E-ananguites experienced higher temperatures and that the impactor signature is more pronounced in E-ananguites than W-ananguites. Another compositional difference observed is the variation in total REE content in W- and E-ananguites. The difference could result from variations in the extent of partial melting, with the higher REE content in W-ananguites likely due to less extensive partial melting (and so lower temperatures, allowing more REEs, being incompatible elements, to enter the melt). On the contrary, a lower total REE content of E-ananguites could be attributed to a more extensive partial melting (higher temperatures), leading to dilution of their concentration. Geochemical variation with distance has also been observed in Australasian tektites (Chapman, 1971; Blum et al., 1992), as seen in
<figure><img src="image_7.png" /><figcaption>**Fig. 4.** (a) Trace element and (b) REE patterns for ananguites, normalized to the primitive mantle and CI chondrite, respectively, are compared to those of Australasian tektites (in red; Ackermann et al., 2020).</figcaption></figure>

different degrees of melting between indochinites and australites, for example.

Based on these observations, E-ananguites seem to have experienced higher temperatures compared to their western counterparts. This would explain a different vesiculation distribution, as higher-temperature silicate melts facilitate gas diffusion and the formation of larger bubbles (Lesher and Spera, 2015), such as in T1196a. When volatiles are completely lost, the samples formed have no vesiculation, as seen for some E-ananguites. This loss in volatiles is also observed in microtektites and explained with the “bubble-stripping” mechanism proposed by Folco et al. (2010a): the decrease in pressure during their ballistic flight in the atmosphere causes the progressive exsolution of volatiles in tektites, and the growth and migration of bubbles toward their external surface.

Similar geochemical and inclusion variations with distance from the putative crater region have been observed in the Australasian strewn field (Folco et al., 2010b). Following the same logic, our results suggest that western samples are closer to the source crater, as they contain more volatiles, exhibit higher vesiculation, have more inclusions, and

therefore, they were subjected to lower temperatures. This suggests that Sulawesi and Maquiling could be more likely sources than Lamington (Fig. 7). However, compared to Australasian tektites, the scale of these variations is different: in Australasian tektites and microtektites, they occur over thousands of kilometers, whereas in ananguites, over <900 km. These interpretations are based on a limited number of samples, and to further clarify the diversity between W- and E-ananguites, additional analyses and more samples are needed.

**5. Conclusions**

Based on their morphology, chemical homogeneity, low water content, presence of lechatelierite, extraterrestrial contamination (Ni, Co, Cr), geochemical and isotopic composition, and distinct age from Australasian tektites, HNa/K tektites can be defined as a new tektite group, which we propose to name ananguites. The impact crater remains unidentified but resulted from the collision between a chondritic impactor and an andesitic target at 10.76 ± 0.05 Ma. The active arcs surrounding Australia are the most likely sources, with best-matching isotopic and
<figure><img src="image_8.png" /><figcaption>**Fig. 5.** $^{87}$Sr/$^{86}$Sr versus εNd composition of ananguites, compared to convergent arcs and andesites from Barrington Tops (New England Batholith; Landenberger et al., 2000). The εNd values for Barrington Tops have been recalculated based on the CHUR value (0.51263) used for the other data points. Sulawesi, Luzon, and Bismarck arcs are the only ones showing compositions similar to those of ananguites.</figcaption></figure>

<figure><img src="image_9.png" /><figcaption>**Fig. 6.** $^{40}$Ar/$^{39}$Ar age spectra obtained on two specimens (two aliquots each): (a,b) T1196a and (c,d) T1202.</figcaption></figure>

trace element signatures from the Philippines (Luzon), Indonesia (Sulawesi), and Papua New Guinea (Bismarck), although a source within the New England paleo-subduction arc cannot be totally ruled out. Although the limited number of ananguites recovered – combining our study and that of Chapman – warrants some caution, the samples have highly homogeneous average elemental and isotopic compositions, except for siderophile elements (Ni, Co, Cr) and volatile metals (Cu, Zn). Geochemical and petrographic systematic differences between western and eastern ananguites, which still need to be confirmed with additional samples, may help constrain the location of the impact. However, it is

also possible that the crater has been buried during the past 11 million years.

### CRediT authorship contribution statement

**Anna Musolino:** Writing – review & editing, Writing – original draft, Validation, Project administration, Investigation, Formal analysis, Data curation, Conceptualization.
**Pierre Rochette:** Writing – review & editing, Writing – original draft, Validation, Supervision, Resources, Investigation, Funding acquisition, Data curation, Conceptualization.
<figure><img src="image_10.png" /><figcaption>**Fig. 7.** Map of the ananguite strewn field and of the volcanic arcs considered as potential impact sources (from the GEOROC Compilation database), within a 5000 km radius from the center of the strewn field. Yellow stars indicate the locations in the Sulawesi, Luzon, and Bismarck arcs where major and trace element composition, and Sr-Nd isotopic composition, show the best match with ananguites. The differently colored points represent the full compositional dataset used to identify the source crater within the various volcanic arcs. The closest craters, Connolly and Toondina, as well as the Tingha structure (New England Batholith; Glikson, 2018), are marked with red stars.</figcaption></figure>

**Jean-Alix Barrat:** Writing – review & editing, Validation, Methodology, Investigation, Data curation. **Fred Jourdan:** Writing – review & editing, Methodology, Investigation, Data curation. **Bruno Reynard:** Writing – review & editing, Methodology, Investigation, Data curation. **Bertrand Devouard:** Supervision, Investigation. **Valerie Andrieu:** Investigation. **Jérôme Gattacceca:** Writing – review & editing, Methodology, Investigation. **Vladimir Vidal:** Methodology, Investigation.

Declaration of competing interest

The authors have no competing interests to declare.

Acknowledgments

This research was funded by ANR ET-Megafire project (ANR-21-CE49-0014-03). We acknowledge A. Cavosie (Curtin University) and P. Downes (Western Australia Museum) for their help in measuring tektite collections in Perth. The continuing support of the South Australian Museum curator, Ben McHenry, was essential for the success of our survey in Adelaide; he is warmly acknowledged. We thank L. Folco, the anonymous reviewer, and the associate editor C. M. Petrone for their constructive comments and suggestions, which helped improve the manuscript.

Supplementary materials

Supplementary material associated with this article can be found, in the online version, at doi:10.1016/j.epsl.2025.119600.

Data availability

All data supporting the findings of this study are included in the

article and its supplementary materials.

References

Ackerman, L., Žák, K., Skála, R., Rejšek, J., Krížová, Š., Wimpenny, J., Magna, T., 2020. Sr-Nd-Pb isotope systematics of Australasian tektites: implications for the nature and composition of target materials and possible volatile loss of Pb. Geochim. Cosmochim. Acta 276, 135–150. https://doi.org/10.1016/j.gca.2020.02.025.

Arculus, R.J., Johnson, R.W., Chappell, B.W., McKee, C.O., Sakai, H., 1983. Ophiolite-contaminated andesites, trachybasalts, and cognate inclusions of Mount Lamington, Papua New Guinea: anhydrite-amphibole-bearing lavas and the 1951 cumulodome. J. Volcanol. Geothermal Res. 18 (1-4), 215–247. https://doi.org/10.1016/0377-0273(83)90010-0.

Barrat, J.A., Jambon, A., Yamaguchi, A., Bischoff, A., Rouget, M.L., Liorzou, C., 2016. Partial melting of a C-rich asteroid: lithophile trace elements in ureilites. Geochim. Cosmochim. Acta 194, 163–178. https://doi.org/10.1016/j.gca.2016.08.042.

Barrat, J.A., Zanda, B., Moynier, F., Bollinger, C., Liorzou, C., Bayon, G., 2012. Geochemistry of CI chondrites: major and trace elements, and Cu and Zn isotopes. Geochimica et Cosmochimica Acta, 83, 79–92. https://doi.org/10.1016/j.gca.2011.12.011.

Beran, A., Koeberl, C., 1997. Water in tektites and impact glasses by fourier-transformed infrared spectrometry. Meteorit. Planet. Sci. 32 (2), 211–216. https://doi.org/10.1111/j.1945-5100.1997.tb01260.x.

Blum, J.D., Papanastassiou, D.A., Koeberl, C., Wasserburg, G.J., 1992. Neodymium and strontium isotopic study of Australasian tektites: new constraints on the provenance and age of target materials. Geochim. Cosmochim. Acta 56 (1), 483–492. https://doi.org/10.1016/0016-7037(92)90146-A.

Bottomley, R.J., Koeberl, C., 1999. The age of a separate Australian tektite event. Meteorit. Planet. Sci. 34 (Supplement) p. A15, 34, A15. https://articles.adsabs.harva rd.edu/full/seri/M+PSA/0034/0000015.000.html.

Bouvier, A., Vervoort, J.D., Patchett, P.J., 2008. The Lu-Hf and Sm-Nd isotopic composition of CHUR: constraints from unequilibrated chondrites and implications for the bulk composition of terrestrial planets. Earth. Planet. Sci. Lett. 273 (1-2), 48–57. https://doi.org/10.1016/j.epsl.2008.06.010.

Chapman, D.R., 1971. Australasian tektite geographic pattern, crater and ray of origin, and theory of tektite events. J. Geophys. Res. 76 (26), 6309–6338. https://doi.org/10.1029/JB076i026p06309.

Chapman, D.R., Scheiber, L.C., 1969. Chemical investigation of Australasian tektites. J. Geophys. Res. 74 (27), 6737–6776. https://doi.org/10.1029/JB074i027p06737.
Compston, W., Chapman, D.R., 1969. Sr isotope patterns within the Southeast Australasian strewn-field. Geochim. Cosmochim. Acta 33 (9), 1023-1036. https://doi.org/10.1016/0016-7037(69)90058-1.

Crósta, A.P., Silva, G.G., Ferrière, L., Barrat, J.A., Libowitzky, E., 2004. A new tektite strewn field discovered in Brazil: Geraisites. LPI Contributions 303, 6019. https://ui.adsabs.harvard.edu/abs/2024LPICo3036.6019C/abstract.

Cunningham, H.S., Turner, S.P., Dosseto, A., Patia, H., Eggins, S.M., Arculus, R.J., 2009. Temporal variations in U-series disequilibria in an active caldera, Rabaul, Papua New Guinea. J. Petrol. 50 (3), 507-529. https://doi.org/10.1093/petrology/egp009.

Defant, M.J., Maury, R.C., Ripley, E.M., Feigenson, M.D., Jacques, D., 1991. An example of island-arc petrogenesis: geochemistry and petrology of the southern Luzon arc, Philippines. J. Petrol. 32 (3), 455-500. https://doi.org/10.1093/petrology/32.3.455.

Di Muro, A., Villemant, B., Montagnac, G., Scaillet, B., Reynard, B., 2006. Quantification of water content and speciation in natural silicic glasses (phonolite, dacite, rhyolite) by confocal microRaman spectrometry. Geochim. Cosmochim. Acta 70 (11), 2868-2884. https://doi.org/10.1016/j.gca.2006.02.016.

Elburg, M., Foden, J., 1998. Temporal changes in arc magma geochemistry, northern Sulawesi, Indonesia. Earth. Planet. Sci. Lett. 163 (1-4), 381-398. https://doi.org/10.1016/S0012-821X(98)00143-5.

Elburg, M.A., Foden, J., 1999. Geochemical response to varying tectonic settings: an example from southern Sulawesi (Indonesia). Geochim. Cosmochim. Acta 63 (7-8), 1155-1172. https://doi.org/10.1016/S0016-7037(98)00298-1.

Elburg, M., van Leeuwen, T., Foden, J., 2003. Spatial and temporal isotopic domains of contrasting igneous suites in Western and Northern Sulawesi, Indonesia. Chemical Geology 199 (3-4), 243-276. https://doi.org/10.1016/S0009-2541(03)00084-6.

Ferrière, L., Barrat, J.A., Giuli, G., Koeberl, C., Schulz, T., Topa, D., Wegner, W., 2017. A new tektite strewn field discovered in Uruguay. In: 80th Annual Meeting of the Meteorological Society, 80, p. 6195. https://ui.adsabs.harvard.edu/abs/2017LPICo1987.6195F/abstract.

Fleischer, R.L., Price, P.B., Woods, R.T., 1969. A second tektite fall in Australia. Earth. Planet. Sci. Lett. 7 (1), 51-52. https://doi.org/10.1016/0012-821X(69)90011-9.

Folco, L., Glass, B.P., D'Orazio, M., Rochette, P., 2010a. A common volatilization trend in Transantarctic Mountain and Australasian microtektites: implications for their formation model and parent crater location. Earth. Planet. Sci. Lett. 293 (1-2), 135-139. https://doi.org/10.1016/j.epsl.2010.02.037.

Folco, L., Perchiazzi, N., D'Orazio, M., Frezzotti, M.L., Glass, B.P., Rochette, P., 2010b. Shocked quartz and other mineral inclusions in australasian microtektites. Geology, 38 (3), 211-214. https://doi.org/10.1130/G30512.1.

Folco, L., D'Orazio, M., Gemelli, M., Rochette, P., 2016. Stretching out the Australasian microtektite strewn field in Victoria Land Transantarctic Mountains. Polar Science 10 (2), 147-159. https://doi.org/10.1016/j.polar.2016.02.024.

Folco, L., Glass, B.P., D'Orazio, M., Rochette, P., 2018. Australasian microtektites: impactor identification using Cr, Co and Ni ratios. Geochim. Cosmochim. Acta 222, 550-568. https://doi.org/10.1016/j.gca.2017.11.017.

Folco, L., Rochette, P., D'Orazio, M., Masotta, M., 2023. The chondritic impactor origin of the Ni-rich component in Australasian microtektites and microtektites. Geochim. Cosmochim. Acta 360, 231-240. https://doi.org/10.1016/j.gca.2023.09.90112-L.

Glass, B.P., 1990. Tektites and microtektites: key facts and inferences. Tectonophysics. 171 (1-4), 393-404. https://doi.org/10.1016/0040-1951(90)90112-L.

Glass, B.P., Huber, H., Koeberl, C., 2004. Geochemistry of cenozoic microtektites and clinopyroxene-bearing spherules. Geochim. Cosmochim. Acta 68 (19), 3971-4006.

Glass, B.P., Simonson, B.M., 2013. Distal Impact Ejecta Layers: A Record of Large Impacts in Sedimentary Deposits, 716. Springer, Heidelberg.

Glikson, A., 2018. Structure and origin of Australian ring and dome features with reference to the search for asteroid impact events. Tectonophysics. 722, 175-196. https://doi.org/10.1016/j.tecto.2017.11.003.

Goderis, S., Tagle, R., Fritz, J., Bartoschewitz, R., Artemieva, N., 2017. On the nature of the Ni-rich component in splash-form Australasian microtektites. Geochim. Cosmochim. Acta 217, 28-50. https://doi.org/10.1016/j.gca.2017.08.013.

Hegner, E., Smith, I.E., 1992. Isotopic compositions of late cenozoic volcanics from southeast Papua New Guinea: evidence for multi-component sources in arc and fault environments. Chemical geology 97 (3-4), 233-249. https://doi.org/10.1016/0009-2541(92)90078-7.

Hickey, R.L., Frey, F.A., 1982. Geochemical characteristics of boninite series volcanics: implications for their source. Geochim. Cosmochim. Acta 46 (11), 2099-2115. https://doi.org/10.1016/0016-7037(82)90188-0.

Hohl, S.V., Schuth, S., Münker, C., König, S., Garbe-Schönberg, D., Kuduon, J., 2022. Geochemical evolution of the Rabaul volcanic complex, Papua New Guinea-insights from HFSE, Sr-Nd-Hf, and Fe isotopes. Lithos. 408, 106560. https://doi.org/10.1016/j.lithos.2021.106560.

Jourdan, F., Nomade, S., Wingate, M.T., Eroglu, E., Deino, A., 2019. Ultraprecise age and formation temperature of the Australasian tektites constrained by 40Ar/39Ar analyses. Meteorit. Planet. Sci. 54 (10), 2573-2591. https://doi.org/10.1111/maps.13305.

Jourdan, F., Renne, P.R., 2007. Age calibration of the Fish Canyon sanidine 40Ar/39Ar dating standard using primary K-Ar standards. Geochim. Cosmochim. Acta 71 (2), 387-402. https://doi.org/10.1016/j.gca.2006.09.002.

Knittel, U., Hegner, E., Bau, M., Satir, M., 1997. Enrichment processes in the sub-arc mantle; a Sr Nd Pb isotopic and REE study of primitive arc basalts from the Philippines. The Canadian Mineralogist 35 (2), 327-346. In: pubs.geosciencworld.org/mac/canmin/article-abstract/35/2/327/12851/Enrichment-processes-in-the-sub-arc-mantle-a-Sr-Nd.

Koeberl, C., 1990. The geochemistry of tektites: an overview. Tectonophysics. 171 (1-4), 405-422. https://doi.org/10.1016/0040-1951(90)90113-M.

Koeberl, C., 1994. Tektite origin by hypervelocity asteroidal or cometary impact. Target rocks, source materials, and mechanisms. In: Dressler, B.O., Grieve, R.A.F., Shartpon, V.L. (Eds.), Large Meteorite Impacts and Planetary Evolution. Geological Society of America, pp. 133-152. Special Paper 293.

Koeberl, C., Glass, B.P., Schulz, T., Wegner, W., Giuli, G., Cicconi, M.R., Trapananti, A., Stabile, P., Cestelli-Guidi, M., Park, J., Herzog, G.F., Caffee, M.W., 2022. Tektite glasses from Belize, Central America: petrography, geochemistry, and search for a possible meteoritic component. Geochim. Cosmochim. Acta 325, 232-257. https://doi.org/10.1016/j.gca.2022.02.021.

König, S., Münker, C., Schuth, S., Luguet, A., Hoffmann, J.E., Kuduon, J., 2010. Boninites as windows into trace element mobility in subduction zones. Geochim. Cosmochim. Acta 74 (2), 684-704. https://doi.org/10.1016/j.gca.2009.10.011.

Koppers, A.A., 2002. ArArCALC—Software for 40Ar/39Ar age calculations. Comput. Geosci. 28 (5), 605-619. https://doi.org/10.1016/S0098-3004(01)00095-4.

Landenberger, B., Collins, W. J., Nakajima, T., & Whitford, D. J. (2000). Mantle influence on the character of I-type granitoids of the New England batholith: evidence from Sr and Nd isotopes. Centre of Isotope Studies, CSIRO, North Ryde, NSW, Research Report 1995-2000, 15-20. https://inis.iea.org/records/errz-q6gk50.

Lee, J.Y., Marti, K., Severinghaus, J.P., Kawamura, K., Yoo, H.S., Lee, J.B., Kim, J.S., 2006. A redetermination of the isotopic abundances of atmospheric Ar. Geochim. Cosmochim. Acta 70 (17), 4507-4512. https://doi.org/10.1016/j.gca.2006.06.1563.

Lesher, C.E., Spera, F.J., 2015. Thermodynamic and transport properties of silicate melts and magma. The encyclopedia of volcanoes. Academic Press, pp. 113-141. https://doi.org/10.1016/B978-0-12-385938-9.00005-5.

Leterrier, J., Yuwono, Y.S., Soeria-Atmadja, R., Maury, R.C., 1990. Potassic volcanism in central Java and south Sulawesi, Indonesia. J. Southeast. Asian Earth. Sci. 4 (3), 171-187. https://doi.org/10.1016/S0743-9547(05)80011-X.

McCall, G.J.H., 2001. Tektites in the geological record: showers of glass from the sky. Geological Society, London.

Patia, H., Eggins, S.M., Arculus, R.J., McKee, C.O., Johnson, R.W., Bradney, A., 2017. The 1994-2001 eruptive period at Rabaul, Papua New Guinea: petrological and geochemical evidence for basalt injections into a shallow dacite magma reservoir, and significant SO2 flux. Journal of Volcanology and Geothermal Research 345, 200-217. https://doi.org/10.1016/j.jvolgeores.2017.08.011.

Phillips, G., Landenberger, B., Belousova, E.A., 2011. Building the New England Batholith, eastern Australia—Linking granite petrogenesis with geodynamic setting using Hf isotopes in zircon. Lithos. 122 (1-2), 1-12. https://doi.org/10.1016/j.lithos.2011.11.005.

Polvé, M., Maury, R.C., Bellon, H., Rangin, C., Priadi, B., Yuwono, S., Joron, J.L., Atmadja, R.S., 1997. Magmatic evolution of Sulawesi (Indonesia): constraints on the cenozoic geodynamic history of the Sundaland active margin. Tectonophysics. 272 (1), 69-92. https://doi.org/10.1016/S0040-1951(96)00276-4.

Polvé, M., Maury, R.C., Vidal, P., Priadi, B., Bellon, H., Soeria-Atmadja, R., Joron, J.L., Cotten, J., 2001. Melting of lower continental crust in a young post-collision setting: a geochemical study of plio-quaternary acidic magmatism from central Sulawesi (Indonesia). Bulletin de la Société géologique de France 172 (3), 333-342. https://doi.org/10.2113/172.3.333.

Priadi, B., Polve, M., Maury, R.C., Bellon, H., Soeria-Atmadja, R., Joron, J.L., Cotten, J., 1994. Tertiary and quaternary magmatism in Central Sulawesi: chronological and petrological constraints. J. Southeast. Asian Earth. Sci. 9 (1-2), 81-93. https://doi.org/10.1016/j.s0743-9547(94)90067-1.

Quintero, R.R., Cavosie, A.J., Cox, M.A., Miljković, K., Dugdale, A., 2021. Australian impact cratering record: updates and recent discoveries. In: Reimold, W.U., Koeberl, C. (Eds.), Large Meteorite Impacts and Planetary Evolution VI. GSA. https://doi.org/10.1130/2021.2550(02). Special Vol. 550, Ch. 2.

Renne, P.R., Balco, G., Ludwig, K.R., Mundil, R., Min, K., 2011. Response to the comment by WH Schwarz et al. on "joint determination of 40K decay constants and 40Ar*/40K for the Fish Canyon sanidine standard, and improved accuracy for 40Ar/39Ar geochronology", by PR Renne et al. (2010). Geochim. Cosmochim. Acta 75 (17), 5097-5100. https://doi.org/10.1016/j.gca.2011.06.021.

Renne, P.R., Deino, A.L., Hilgen, F.J., Kuiper, K.F., Mark, D.F., Mitchell III, W.S., Morgan, L.E., Mundil, R., Smit, J., 2013. Time scales of critical events around the cretaceous-paleogene boundary. Science (1979) 339 (6120), 684-687. https://doi.org/10.1126/science.1230492.

Rochette, P., Beck, P., Bizzarro, M., Braucher, R., Corjec, N., Debaille, V., Devouard, B., Gattacceca, J., Jourdan, F., Moustard, F., Moynier, F., Nomade, S., Reynard, B., 2021. Impact glasses from Belize represent tektites from the pleistocene Pantasma impact crater in Nicaragua. Commun. Earth. Environ. 2 (1), 94. https://doi.org/10.1038/s43247-021-00155-1.

Rochette, P., Bezaeva, N.S., Kosterov, A., Gattacceca, J., Masaitis, V.L., Badyukov, D.D., Giuli, G., Lepore, G.O., Beck, P., 2019. Magnetic properties and redox state of impact glasses: A review and new case studies from Siberia. Geosciences. (Basel) 9 (5), 225. https://doi.org/10.3390/geosciences9050225.

Rochette, P., Gattacceca, J., Devouard, B., Moustard, F., Bezaeva, N.S., Cournède, C., Scaillet, B., 2015. Magnetic properties of tektites and other related impact glasses. Earth. Planet. Sci. Lett. 432, 381-390. https://doi.org/10.1016/j.epsl.2015.10.030.

Rudnick, R.L., Gao, S., 2004. The composition of the continental crust. In: Rudnick, R.L., Holland, H.D., Turekian, K.K. (Eds.), The Crust. Treatise on Geochemistry. The Crust. Treatise on Geochemistry, 3. Elsevier-Pergamon, Oxford, pp. 1-64.

Shaw, H.F., Wasserburg, G.J., 1982. Age and provenance of the target materials for tektites and possible impactites as inferred from Sm-Nd and Rb-Sr systematics. Earth. Planet. Sci. Lett. 60 (2), 155-177. https://doi.org/10.1016/0012-821X(82)90001-2.

Soro, P., Rochette, P., Baratoux, D., Kouamelan, A.N., Andrieu, V., Monda, O., 2023. Revisiting the Côte d'Ivoire tektite strewn field. J. African Earth Sci. 205, 104990. https://doi.org/10.1016/j.jafrearsci.2023.104990.
Stöffler, D., Artemieva, N.A., Pierazzo, E., 2002. Modeling the Ries-Steinheim impact event and the formation of the moldavite strewn field. Meteorit. Planet. Sci. 37 (12), 1893–1907. https://doi.org/10.1111/j.1945-5100.2002.tb01171.x.

Storzer, D., 1985. The fission track age of high sodium/potassium australites revisited. Meteoritics. 20, 765, 20, 765. https://adsabs.harvard.edu/full/1985Metic..20..765S.

Storzer, D., Müller-Sohnius, D., 1986. The K/Ar age of high sodium/potassium australites. Meteoritics. 21, 518. Vol. 21, p. 518. https://adsabs.harvard.edu/full/1986Metic..21..518S.

Taylor, S.R., McLennan, S.M., 1995. The geochemical evolution of the continental crust. Reviews of geophysics 33 (2), 241–265. https://doi.org/10.1029/95RG00262.

Toplis, M.J., Reynard, B., 2000. Temperature and time-dependent changes of structure in phosphorus containing aluminosilicate liquids and glasses: in situ Raman spectroscopy at high temperature. J. Non. Cryst. Solids. 263, 123–131. https://doi.org/10.1016/S0022-3093(99)00628-6.

Vogel, T.A., Flood, T.P., Patino, L.C., Wilmot, M.S., Maximo, R.P.R., Arpa, C.B., Arcilla, C.A., Stimac, J.A., 2006. Geochemistry of silicic magmas in the Macolod Corridor, SW Luzon, Philippines: evidence of distinct, mantle-derived, crustal

sources for silicic magmas. Contributions to Mineralogy and Petrology 151, 267–281. https://doi.org/10.1007/s00410-005-0050-7.

Watt, N., Bouchet, R.A., Lee, C.T.A., 2011. Exploration of tektite formation processes through water and metal content measurements. Meteorit. Planet. Sci. 46 (7), 1025–1032. https://doi.org/10.1111/j.1945-5100.2011.01207.x.

Zanetta, P.M., Seydoux-Guillaume, A.M., Rochette, P., Reynard, B., Tricaud, V., Toro, P., Singsoupho, S., Kouamelan, A.N., Monda, O., Baratoux, D., 2024. Origin of the Ca-phosphate inclusions in Ivory Coast and australasian Muong-Nong-type tektites. Geochim. Cosmochim. Acta 387, 63–82. https://doi.org/10.1016/j.gca.2024.09.021.

Zhang, J., Davidson, J.P., Humphreys, M.C.S., Macpherson, C.G., Neill, I., 2015. Magmatic enclaves and andesitic lavas from Mt. Lamington, Papua New Guinea: implications for recycling of earlier-fractionated minerals through magma recharge. J. Petrol. 56 (11), 2223–2256. https://doi.org/10.1093/petrology/egv071.

Zhang, X., Huang, T.N., Chung, S.L., Maulana, A., Mawaleda, M., Tien, C.Y., Lee, H.Y., Liu, P.P., 2022. Late Eocene subduction initiation of the Indian Ocean in the North Sulawesi Arc, Indonesia, induced by abrupt Australian plate acceleration. Lithos. 422, 106742. https://doi.org/10.1016/j.lithos.2022.106742.