Knut Metzler
email: knut.metzler@uni-muenster.de

Dominik C Hezel

Jens Barosch

Elias Wölfer

Jonas Schneider

Jasper Berndt

Andreas Stracke

Jérôme Gattacceca

Richard C Greenwood

Ian A Franchi

Christoph Burkhardt

Thorsten Kleine

The Loongana (CL) group of carbonaceous chondrites

A coordinated study of the petrology, mineral chemistry, and bulk chemical and isotopic composition of the five ungrouped carbonaceous chondrites Coolidge, Loongana 001, Los Vientos (LoV) 051, Northwest Africa (NWA) 033, and NWA 13400 reveals that these meteorites have a similar set of properties that distinguishes them from the other carbonaceous chondrite groups and allows definition of the new Loongana (CL) group of carbonaceous chondrites. The characteristics of the investigated samples include: (1) Fe-Ni metal abundances considerably higher than for CV chondrites, but similar to CR chondrites; (2) Chondrule size-frequency distributions similar to CV chondrites, but dissimilar to CR chondrites; (3) Mean CAI abundances of ~1.4 vol%, i.e., lower than in CV but much higher than in CR chondrites; (4) Very low amounts of inter-chondrule matrix (17-21 vol%), the lowest among the main carbonaceous chondrite groups (CI, CY, CM, CO, CV, CR, CK); (5) Nearly equilibrated olivine with mean fayalite (Fa) values of olivine between 12.5 mol% (Loongana 001) and 14.7 mol% (NWA 13400) as a metamorphic effect; (6) Lower Al 2 O 3 and higher MgO and Cr 2 O 3 concentrations in inter-chondrule matrix compared to matrix in CV, CK, and CR chondrites; (7) Considerable bulk depletion of volatile lithophile elements (Mn, Na, K, Rb, Cs) and chalkophile elements (Zn, Se, Te, Pb, Tl) compared to all other main carbonaceous chondrite groups; (8) Bulk O isotope compositions plotting along the CCAM line (∆ 17 O -3.96 to -5.47‰), partly overlapping with the CV and CK chondrite field but including samples that are more 16 O-rich; (9) Unique positions in the є 54 Cr-є 50 Ti isotope plot, with є 54 Cr values similar to CV and є 50 Ti values similar to CR chondrites.

Taking all observations together, it can be concluded that CL chondrites are unrelated to CR chondrites but may be genetically related to CV and CK chondrites. All CL chondrites studied here are of petrologic type 3.9 to 4, indicating that they have been thermally overprinted on the parent body.

The diagnostic features of CL chondrites detailed here should provide a basis for identifying CL members of lower petrologic types. Such samples would be important in determining the pristine state of these meteorites and their components.

INTRODUCTION

Chondrites are cosmic sediments, which consist of up to 92% chondrules (e.g. [START_REF] Weisberg | Systematics and evaluation of meteorite classification[END_REF][START_REF] Metzler | Ultrarapid chondrite formation by hot chondrule accretion? Evidence from unequilibrated ordinary chondrites[END_REF], i.e., once molten silicate spherules with sizes mostly between 0.1 and 1 millimeter. Further components are metal and sulfide grains, refractory objects like Ca-Al-rich inclusions and amoeboid olivine aggregates (CAIs, AOAs; e.g. [START_REF] Krot | Refractory inclusions in carbonaceous chondrites: Records of early solar system processes[END_REF] and fine-grained interchondrule matrix. These components occur in variable and often characteristic amounts in the distinct chondrite groups (e.g. [START_REF] Weisberg | Systematics and evaluation of meteorite classification[END_REF]. Beside the Rumuruti (R) and Kakangari (K) groups, chondrites are subdivided into three classes, namely the ordinary, enstatite, and carbonaceous chondrites. The latter class consists of nine groups, namely the CI, CY [START_REF] King | The Yamato-type (CY) carbonaceous chondrite group: Analogues for the surface of asteroid Ryugu[END_REF], CM, CO, CV, CK, CR, CH, and CB chondrites. Of these, the CI group is particularly distinctive, as these meteorites do not contain any recognizable chondrules and because their bulk chemistry agrees closely with that of the solar photosphere (e.g. [START_REF] Lodders | Solar system abundances and condensation temperatures of the elements[END_REF][START_REF] Lodders | Abundances of the elements in the solar system[END_REF]. Each chondrite group is thought to represent a single parent body (or several related parent bodies; e.g., [START_REF] Gattacceca | CV chondrites: more than one parent body[END_REF], and so the presence of different groups allows investigating the accretion and early evolution of several distinct primitive planetesimals. As such, identification of a new chondrite group is important for understanding the diversity of planetesimals formed in the early solar system, and the processes that led to this diversity.

In addition to the established carbonaceous chondrite groups there are also ungrouped carbonaceous chondrites, which cannot be assigned to one of these groups. Based on similar properties some ungrouped chondrites can be combined into grouplets (consisting of less than 5 individual members), as in the case of Coolidge and Loongana 001 [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF].

Coolidge is a well-studied meteorite which was originally classified as a CV4 chondrite [START_REF] Van Schmus | Mineralogy, petrology and classification of types 3 and 4 carbonaceous chondrites[END_REF]. However, McSween (1977a) concludes that it cannot simply be a metamorphosed sample of a reduced CV chondrite. By contrast, [START_REF] Kallemeyn | The compositional classification of chondrites: III. Ungrouped carbonaceous chondrites[END_REF] concludes that Coolidge represents a CV chondrite, which "was probably subjected to open-system metamorphic reheating", a conclusion also reached by [START_REF] Scott | Petrology of types 4-6 carbonaceous chondrites[END_REF]. However, [START_REF] Kallemeyn | Compositional comparisons of metamorphosed carbonaceous chondrites[END_REF] subsequently argued that the strong depletion of volatile elements more likely reflects nebular processes and that this meteorite, therefore, may not be a CV chondrite. Further, [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] found that, compared to the reduced CV chondrite Efremovka, chondrules and matrix in Coolidge are systematically depleted in Na, which also points to a nebular rather than a metamorphic process. Finally, based on petrographic observations and characteristic differences in the inventories of volatile elements, [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] demonstrated that Coolidge clearly does not belong to the CV group, but together with the newly discovered meteorite Loongana 001, defines a new carbonaceous chondrite grouplet. This study will show that the three ungrouped carbonaceous chondrites Los Vientos (LoV) 051, Northwest Africa (NWA) 033 and NWA 13400 have similar properties as the Coolidge-Loongana 001 grouplet. This makes it possible to combine these five samples into a new carbonaceous chondrite group, which we term the Loongana (CL) group and we define the basic criteria for identifying further members of this group. Since the investigated chondrites have some similarities to CV red chondrites (e.g., McSween 1977a;[START_REF] Gattacceca | CV chondrites: more than one parent body[END_REF] and CR chondrites (e.g., [START_REF] Kallemeyn | The compositional classification of chondrites: VI. The CR carbonaceous chondrite group[END_REF], our discussion concentrates on these groups when comparing petrographic, chemical and isotopic data of CL chondrites.

SAMPLES

Five ungrouped carbonaceous chondrite finds, namely Coolidge (USA, found 1937), Loongana 001 (Australia, found 1990), LoV 051 (Chile, found 2010), NWA 033 (Northwest Africa, found 1999), and NWA 13400 (Northwest Africa, found 2016) are investigated in this study. Polished thin sections (PTS), polished epoxy mounts and polished massive samples (slices) of these chondrites were used for petrographic and microchemical characterization. Subsample designations and masses of analyzed material are given in Table 1. To assess data quality and accuracy, representative bulk powder samples of the Allende CV3 chondrite were analyzed together with those of the above specimens. For comparison, we also determined the matrix fraction of Allende (CV3 oxA ), Vigarano (CV3 red ), and NWA 7020 (CR2) as well as the chondrule size-frequency distributions in Allende and NWA 7020.

In the following, the meteorite Loongana 001 is termed Loongana for short and we collectively refer to the five investigated meteorites as "CL chondrites" and "CL samples". The reasoning for naming the proposed new group "CL" is given in section 5.3.1.

METHODS

All subsamples, including those that were subsequently powdered, were investigated and documented by optical and scanning electron microscopy. Samples of each meteorite were powdered in an agate mortar for obtaining the bulk chemical and isotopic compositions by various techniques.

Aliquots for all laboratories, with the exception of LA-ICP-MS (Sc, Se, Te), were taken from the same sample powder (Table 1). All chemical data are given in wt.% or ppm (µg/g), respectively.

Polarizing microscopy

Polished thin sections (PTS) of all samples were used to determine shock stages and weathering grades by polarizing microscopy. Shock stages were determined according to the instructions given in [START_REF] Stöffler | Shock metamorphism of planetary silicate rocks and sediments: Proposal for an updated classification system[END_REF]; weathering grades have been determined according to [START_REF] Wlotzka | A weathering scale for the ordinary chondrites (abstract)[END_REF]. The latter method was initially developed to characterize ordinary chondrites, but we adopt it here for the use in cases of metal-rich carbonaceous chondrites.

Scanning electron microscopy (SEM)

The scanning electron microscope (SEM; Jeol JSM-6610LV) of the Interdisciplinary Centre for Electron Microscopy and Microanalysis (ICEM; University of Münster) was used to characterize the sample textures and to identify mineral phases. All subsamples, including slices for subsequent destructive chemical analysis, were documented by preparing photomosaics (backscatter electron images; BSE) of their polished surfaces. BSE images were also used to identify the various meteorite components (chondrules, CAIs, amoeboid olivine aggregates (AOAs), inter-chondrule matrix) and to determine modal abundances and apparent chondrule sizes. For element mapping we used the SEM (Zeiss Sigma 300 VP) at the Institut für Geologie und Mineralogie, University of Cologne.

Energy-dispersive X-ray (EDX) analysis

Mineral analyses were obtained using an energy-dispersive X-ray (EDX) analyzing system (INCA, Oxford Instruments); all data were automatically normalized to 100 wt.%. Samples and appropriate mineral standards were measured at a working distance of 10 mm and an acceleration voltage of 20 KV. The beam current constancy was controlled by a Faraday cup. The standard ZAF correction procedures were applied [START_REF] Bence | Empirical correction factors for the electron micro-analysis of silicates and oxides[END_REF]. Minerals of known composition (olivine, low-Ca pyroxene and plagioclase from the L6 chondrite Leedey; [START_REF] Feldstein | Disequilibrium partial melting experiments on the Leedey L6 chondrite: Textural controls on melting processes[END_REF] were measured repeatedly as reference materials to ensure the reproducibility of the EDX system. All mineral analyses were checked for stoichiometry. Since none of the chosen analysis methods in this study was able to measure the bulk chondrite S content of the samples, the following procedure was used to obtain a rough estimate of bulk S concentrations. By using the lowest possible magnification (30x) and a duration of 40 seconds each, EDX analyses of 2-3 different PTS regions of each CL sample and Allende were recorded and averaged. The mean S concentration for Allende, obtained by this method, is 1.67 wt.%, compared to the literature value of 2.10 wt.% [START_REF] Jarosewich | The Allende meteorite reference sample[END_REF]. The obtained values for S concentrations in the other samples were multiplied by the resulting correction factor of 1.26.

Element mapping (phase maps)

We performed element mapping in order to produce phase maps of entire chondrite sections. For this application, the electron beam scanned the stationary sample surface over small areas (~500x400 μm, pixel size ~4 μm) with a dwell time of 10 ms per pixel. The accelerating voltage was set to 20 kV and the aperture diameter to 60 μm. The sample was then moved to a new center and the next map was rastered. The phase maps were then produced with the PHAPS application (e.g., Fig. 1; [START_REF] Hezel | A mathematica code to produce phase maps from two element maps[END_REF]. These display every mineral phase in false color and allow their visual identification. We further used the phase maps and the software "Measure" (Datinf GmbH, Tübingen, Germany) to determine the modal abundances of CAIs.

Determination of apparent (2D) chondrule sizes

The first author of this publication determined the distributions of apparent (2D) chondrule sizes in the five CL chondrites plus those in Allende (CV3 oxA ) and NWA 7020 (CR2) for comparison. For this purpose the software "Measure" (Datinf GmbH, Tübingen, Germany) was used, stringently following a raster on the BSE photomosaics to not overlook any chondrule cut face. Apparent chondrule sizes were obtained by measuring the diameters of chondrule cut faces at an angle of 45° from the line of the maximum apparent diameter, and thereby a reasonable average between minimum and maximum. It was calculated by [START_REF] Eisenhour | Determining chondrule size distributions from thin-section measurements[END_REF] that this method provides a good approximation (within 2%) of the diameter of a circle equal in area to that of the measured ellipse. Except for metal grains, sulfide grains, and CAIs, every subrounded, more or less isometric (aspect ratio <~2) object was considered as a chondrule. Chondrules consisting of welded smaller chondrules were measured as one single chondrule. The same holds for chondrules with adhering layers of smaller chondrules and for the rare chondrules with igneous rims. Chondrule fragments with angular fracture surfaces were only included when their original outline could be unequivocally reconstructed (~half chondrules).

Other chondrule fragments and angular monomineralic grains were omitted. It cannot be ruled out that the data sets contain small fractions of unrecognized roundish chondrule fragments, especially in the smallest size bins (<300 µm).

Electron microprobe (EMPA)

The electron microprobe (JEOL 8900RL) at the Institut für Geologie und Mineralogie (University of Cologne) was used for chemical analysis. Mineral compositions (olivine, low-Ca pyroxene, Ca-rich pyroxene) were determined by spot analyses using a focused, stationary beam of 1 μm, an accelerating voltage of 20 kV, and a beam current of 20 nA. For the analyses of inter-chondrule matrix, the beam was defocused to 30 μm and the accelerating voltage was set to 15 kV. The ZAF-algorithm was used for correction [START_REF] Bence | Empirical correction factors for the electron micro-analysis of silicates and oxides[END_REF]). Mineral analyses with totals between 98.5 and 101.5 wt.% were accepted.

X-ray fluorescence (XRF)

The sample preparation method initially developed by [START_REF] Wolf | The solar system abundances of phosphorus and titanium and the nebular volatility of phosphorus[END_REF] and later modified as described in [START_REF] Stracke | Refractory element fractionation in the Allende meteorite: Implications for solar nebula condensation and the chondritic composition of planetary bodies[END_REF] has been used, with a few additional, minor modifications. A sample to standard ratio of 1:30 was used, with typically 120 mg sample material mixed with 3.6 g lithium tetraborate (Li 2 B 4 O 7 ) flux agent. Before mixing, the sample was pre-treated with aqua regia for a few hours at 120 °C to oxidize the metals. A Claisse LeNeo fluxer was used to automatically produce 27 mm diameter glass disks. The Panalytical Zetium sequential wavelength dispersive X-ray spectrometer at the University of Cologne was used for sample measurements. Standard calibration lines were calculated from 7 identically prepared standard rock samples. The precision for all elements analyzed is below 1% [START_REF] Wolf | The solar system abundances of phosphorus and titanium and the nebular volatility of phosphorus[END_REF]). An Allende glass disk was produced and measured in the same way as the samples. The obtained data for Allende are in excellent agreement with literature data. Some CL samples showed low totals which most likely resulted from loss of sample material (~2 mg, estimated) during sample preparation as well as loss of material during sample fluxing. The latter was possibly caused by the decomposition of weathering products (hydroxides, calcite) and loss of volatile components (H 2 O, CO 2 ). There was only enough powder to determine the loss on ignition (LOI) of NWA 13400 (2.76%, when 120 mg are heated at 1000°C for 2h). This LOI equals ~3 mg loss of sample material. We recalculated samples with low totals considering an estimated total loss of material of 5 mg. However, some totals are still low, possibly indicating an underestimation of material loss.

Trace element compositions

Trace element concentrations were analyzed on aliquots of the investigated meteorites and an Allende Standard powder (Allende MS-A) for Li, V, Co, Rb, Sr, Y, Zr, Nb, Mo, Cs, Ba, the REE, Hf, Ta, Tl, Pb,Th, and U by isotope dilution sector field inductively coupled plasma mass spectrometry (ID-SF-ICP-MS), as desribed in detail in [START_REF] Stracke | Refractory element fractionation in the Allende meteorite: Implications for solar nebula condensation and the chondritic composition of planetary bodies[END_REF].

Concentrations of Sc, Se, and Te in the samples and Allende as a reference material were analysed by LA-ICP-MS at the University of Münster (Institut für Mineralogie). Sample ablation along linear tracks (50 mm each) across the polished sample surfaces (thin and thick sections) was done using 193 nm ArF excimer laser (Analyte G2, Photon Machines). A repetition rate of 10 Hz and an energy of ∼ 3-4 J/cm2 were used throughout the entire session. The beam spot diameter varied between 80 and 100 µm. Elemental analysis has been carried out with an Element 2 mass spectrometer (ThermoFisher). Forward power was 1300 W and reflected power < 2 W, gas flow rates were 1.2 l/m for He (carrier gas of ablated material), 0.8 l/m and 1.1 l/m for the Ar-auxiliary and sample gas, respectively. Cooling gas flow rate was set to 16 l/min. Before starting analysis, the system has been tuned (torch position, lenses, gas flows) on a NIST 612 glass measuring 139 during ablation. The above elements were quantitatively analysed using the NIST 612 glass as an external standard and 43 Ca as internal standard; Ca concentrations had been previously determined by XRF. Concentrations of measured elements were calculated using the Glitter software [START_REF] Griffin | Laser Ablation ICP-MS in the Earth Sciences: Current Practices and Outstanding Issues[END_REF]. Standard reference glasses GSD1-G and GSE1-G were analysed as monitor for precision and accuracy. Obtained results match the published range of concentrations given in the GeoReM database (version 24;[START_REF] Jochum | GeoReM: A New Geochemical Database for Reference Materials and Isotopic Standards[END_REF].

Titanium and chromium isotopes

Aliquots of ~35 mg sample powder (equivalent to ~20-30 µg Ti) were digested in HF-HNO 3 -HClO 4

(2:1:0.05) on a hotplate at 180-200 °C for five days and in aqua regia (HCl-HNO 3 ) at 130-150 °C for another two days. Thereafter, the samples were dissolved in 12 M HNO 3 , and ~65 mg H 3 BO 3 was added. Ti was separated from the sample matrix via a two-stage anion exchange chromatography adapted from the previously established procedure from [START_REF] Zhang | A new method for MC-ICP-MS measurement of titanium isotopic composition: Identification of correlated isotope anomalies in meteorites[END_REF]. In a first step, the sample solutions were loaded onto columns prepacked with 2 ml TOGDA® anion exchange resin, where Ti was eluted in 20 ml 12 M HNO 3 -1 wt.% H 2 O 2 . Afterwards, the Ti cuts were dissolved in 2.5 ml 4 M HF and loaded onto clean-up columns filled with 0.8 ml Bio-Rad® AG1-X8 anion exchange resin, where Ti was eluted in 6 ml 9 M HCl-0.01 M HF.

Titanium isotope measurements were performed in two lines using a ThermoScientific Neptune Plus MC-ICP-MS (Institut für Planetologie, University of Münster) in medium resolving power mode [START_REF] Zhang | A new method for MC-ICP-MS measurement of titanium isotopic composition: Identification of correlated isotope anomalies in meteorites[END_REF]. Solutions containing about 200 ppb Ti in 0.3 M HNO 3 -0.0014 M HF were introduced through a Cetac Aridus II desolvating system, resulting in a ~3.5×10-10 A ion beam on 48 Ti.

Measurements consisted of a 30 s baseline measurement (deflected beam) followed by 40 isotope ratio measurements of 4.2 s each. Mass bias was corrected using the exponential law and 49 Ti/ 0.749766. The Ti isotope anomalies are reported as parts per ten thousand deviation (ε-notation) from the terrestrial OL-Ti [START_REF] Millet | Ultra-precice titanium stable isotope measurements by doublespike high resolution MC-ICP-MS[END_REF] bracketing standard. The sample uncertainty is reported as the Student-t 95% confidence interval based on repeated analyzes (N=12) of the sample solution.

Chromium was collected during the first step of the two-stage anion exchange chromatography used for the separation of Ti, where Cr is eluted in 25 ml 12 M HNO 3 (+ trace H 3 BO 3 ) together with most other matrix elements. Aliquots (equivalent to ~30 µg Cr) were taken from this solution, dried down, and redissolved in 1 ml 6 M HCl. Afterwards, Cr was separated from the sample matrix using a single-stage anion exchange chemistry for the removal of Fe (Bio-Rad® AG1-X8 anion exchange resin), followed by a two-stage cation exchange chromatography (Bio-Rad® AG50W-X8 cation exchange resin) as described by [START_REF] Yamakawa | Chemical separation and mass spectrometry of Cr, Fe, Ni, Zn, and Cu in terrestrial and extraterrestrial material using thermal ionization mass spectrometry[END_REF] Cr values as the parts per ten thousand deviation from the terrestrial NIST SRM3112a Cr standard. The sample uncertainty is reported as the Student-t 95% confidence interval based on repeated analyses (N=8-12).

Oxygen isotopes

Oxygen isotope analyses were obtained at the Open University using an infrared laser-assisted fluorination system [START_REF] Miller | High precision Δ 17 O isotope measurements of oxygen from silicates and other oxides: Methods and applications[END_REF][START_REF] Greenwood | Melting and differentiation of early-formed asteroids: The perspective from high precision oxygen isotope studies[END_REF]. Samples and standards were weighed out into a Ni sample block with each aliquot having a mass of approximately 2 mg. The block was loaded into a vacuum-tight chamber and heated to 70°C under vacuum overnight to remove surfacebound moisture. The system was then flushed with BrF 5 to reduce the final blank level to <60 nmoles O 2 . Oxygen was released from the samples by heating in the presence of BrF 5 using a 50 W infrared CO 2 laser. After fluorination, the released oxygen gas was purified by passing it through two cryogenic nitrogen traps and over a bed of heated KBr to remove any excess fluorine. Oxygen gas was analyzed using a MAT 253 dual inlet mass spectrometer.

Magnetic measurements

All magnetic measurements were performed at CEREGE (Aix-en-Provence, France). Hysteresis measurements were performed with a Princeton Micromag Vibrating Sample Magnetometer (VSM) with a maximum applied field of 1 T and a sensitivity of ~5x10 -9 Am 2 . The analysis of hysteresis loops provided the ratio of saturation remanent magnetization (M RS ) to saturation magnetization (M S ) and the coercive force (B C ). High field susceptibility (χHF) was determined by a linear fit for applied fields > 0.9

T of the hysteresis loops. Remanent coercive force (B CR ) was determined by back field experiments performed with the VSM. The low field specific susceptibility (χ in m3/kg) was measured using Agico MFK1 apparatus with sensitivity of 5x10 -13 m3, operating at 200 A/m and a frequency of 976 Hz. We determined the S-300 ratio, defined as the isothermal remanent magnetization (IRM) obtained after applying a 3 T field and then a back field of 0.3 T normalized to the IRM acquired in 3 T. For this experiment, IRM were imparted using a pulse magnetizer from Magnetic Measurement.

RESULTS

Meteorite textures

The investigated samples are mainly composed of the typical carbonaceous chondrite components, namely type I chondrules, refractory inclusions (CAIs, AOAs), some inter-chondrule sulfide and metal grains and a fine-grained inter-chondrule matrix. Cut faces of the least weathered sample (LoV 051) show well-preserved tiny metal beads within and at the periphery of chondrules.

Occasionally, large fragments of chondrules and refractory inclusions occur, but all samples are macroscopically unbrecciated. Their overall textures show some resemblance to the reduced CV chondrites (CV red ) and CR chondrites, but differ in having a very low amount of inter-chondrule matrix (see section 4.7.3) and consequently a relatively high chondrule content. The compositions and textures of Coolidge and Loongana have been described by [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] and [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF]. The overall texture of Loongana is shown in Fig. 1 both as a photomosaic of SEM-BSE images (a) and a phase map (b). The following components can be distinguished in Fig. 1: abundant porphyritic (1,6) and rare non-porphyritic chondrules (2), rare Al-rich chondrules (3), chondrule fragments (4), adhering chondrules (5), olivine chondrules (6) with thick pyroxene rims (7), and CAIs (8). These components are described in detail below (section 4.7).

Petrologic types

Coolidge and Loongana are listed as being C4-ungrouped in the Meteoritical Bulletin Database (MBDB). However, they have also been classified as type 3.8 to 4 and type 3.8 by [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] and [START_REF] Guimon | Chemical and physical studies of type 3 chondrites XII: The metamorphic history of CV chondrites and their components[END_REF]. The samples NWA 033 and LoV 051 are listed as C3ungrouped in the MBDB, without allocation to a certain petrologic subtype. NWA 13400 is listed as C3ungrouped, with a proposed petrologic subtype of 3.9. One of the standard methods to identify a chondrite´s subtype is determining the frequency distribution of fayalite (Fa) values of randomly chosen olivine grains. The percentage mean deviation (PMD) of these values is used as a measure for the equilibration state of a given meteorite (e.g. [START_REF] Hutchison | Meteorites -A petrologic, chemical and isotopic synthesis[END_REF]his Table 2.6). We determined these distributions in all samples, together with the frequency distributions of ferrosilite (Fs) values of their low-Ca pyroxene grains; the results are shown in Fig. 2. Occasionally, chondrules and chondrule fragments with relict Mg-rich core compositions of olivine can be found in all samples. The PMD values for Coolidge, Loongana, and NWA 033 are below 5% (Table 2), indicating that these samples belong to petrologic type 4, whereas those of LoV 051 and NWA 13400 are between 5% and 10%, indicating a 3.9 subtype.

Shock stages

All olivine grains in the investigated CL chondrites show undulatory extinction, but grains with planar fractures are rare or absent. Thus, all these samples are weakly shocked (Table 2) and belong to shock stage C-S2 [START_REF] Stöffler | Shock metamorphism of planetary silicate rocks and sediments: Proposal for an updated classification system[END_REF], corresponding to the previously defined shock stage S2 [START_REF] Stöffler | Shock metamorphism of ordinary chondrites[END_REF].

Weathering grades

Most samples are moderately to heavily weathered (W2-W3/4) and crosscut by veins composed of the secondary alteration products of metals and sulfides. Nevertheless, variable amounts of Fe-Ni metal are still visible on cut faces of all samples. The estimated degrees of weathering for the CL samples, which were determined using the scheme of [START_REF] Wlotzka | A weathering scale for the ordinary chondrites (abstract)[END_REF], are given in Table 2. The least weathered CL chondrite of this study is LoV 051 (W1/2), which still contains considerable amounts of pristine metal.

Magnetic properties

The magnetic properties of four CL chondrites from this study are given in Table 3, together with data for the various CV subgroups (CV red , CV oxA , CV oxB ) and CR chondrites for comparison. The magnetic properties of all samples, with the notable exception of LoV 051, have been considerably modified by terrestrial weathering. Thus, the data for LoV 051 are the most relevant for defining the primary characteristics of the proposed CL group. Its magnetic susceptibility (Table 3) is log = 5.24

(where  is in 10 -9 m 3 kg -1

), higher than the corresponding values for Coolidge, Loongana, and NWA 033. This difference can be accounted for by terrestrial weathering, which lowers the susceptibility of metal-bearing meteorites [START_REF] Gattacceca | Magnetic Classification of Stony Meteorites: 2. Non-Ordinary Chondrites[END_REF]. The susceptibility of LoV 051 (log = 5.24) is slightly higher compared to CR chondrites, which have an average log = 5.04±0.12 as measured on 14 CR meteorites [START_REF] Gattacceca | Magnetic Classification of Stony Meteorites: 2. Non-Ordinary Chondrites[END_REF], and almost identical to the value for the only CR chondrite fall Renazzo (log = 5.17). The observed hysteresis loop for LoV 051 is typical of kamacite-bearing rocks [START_REF] Gattacceca | Metal phases in ordinary chondrites: magnetic hysteresis properties and implications for thermal history[END_REF], including a curvature up to above 700 mT, very low coercivity (B C =3.08 mT), very low M RS /M S ratio (0.0155), and high B CR /B C ratio (6.10). Together with the S -300 value of 1.00, there is strong evidence that the magnetic mineralogy is dominated by kamacite.

Modal compositions

The modal compositions of all samples, as well as Allende (CV3 oxA ) and Vigarao (CV red ) for comparison, were obtained by point counting on SEM-BSE images. The results for the CL chondrites are summarized in Table . 2. The modal abundances (area% = vol%) of chondrules and chondrule fragments in our samples vary between 67 vol% (Loongana) and 79 vol% (Coolidge). The interchondrule metal and sulfide concentration, modified by terrestrial weathering, varies between 3 vol% (Coolidge) and 6 vol% (NWA 033, NWA 13400; Table 2). The concentration of CAIs, measured on phase maps (e.g., Fig. 1), appears highly variable (from 0.1 vol% for Coolidge to 8 vol% for Loongana). For the modal abundance of inter-chondrule matrix we obtained values between 17 vol% (LoV 051, NWA 13400) and 21 vol% (NWA 033; Table 2).

To verify our method, we also determined the abundances of matrix in Allende (CV oxA ) and Vigarano (CV red ) and found values of 46 vol% and 35 vol%, respectively. The value for Allende is in the range of values obtained by McSween (1977a;38.4 vol%) and [START_REF] Gattacceca | CV chondrites: more than one parent body[END_REF]50 vol%).

Our Vigarano value is nearly identical to that of McSween (1977a;34.5 vol%) and identical to that given in [START_REF] Gattacceca | CV chondrites: more than one parent body[END_REF]. Thus, our method reproduces literature values well, demonstrating that CL chondrites contain significantly less matrix than CV chondrites and most other carbonaceous chondrites.

Lithologic components

Chondrules

The investigated CL chondrites consist mainly of chondrules (67-79 vol%; Table 2), including minor amounts of chondrule fragments. In the following the term "chondrules" also includes chondrule fragments, if not stated otherwise.

Chondrule textures, types, and mineralogical compositions

Chondrules in the investigated meteorites are mostly porphyritic olivine (PO) and porphyritic olivine-pyroxene (POP) chondrules of chemical type I. A high percentage of these show pyroxene rims (see section 4.7.1.3). Many of these have non-circular, irregular boundaries, which has already been described for Coolidge and Loongana by [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF]. Many chondrules in our samples, especially the smaller ones, give the impression of rapidly crystallized droplets from fragmented or shredded melts, which partly accumulated in a viscous state. They show remarkably irregular shapes with lobate outlines and protuberances (Fig. 3a) and sometimes display an amoeboidal shape (Fig. 3b). In some cases it is difficult to define the outlines and boundaries between adjacent objects (Fig. 3c). Many chondrules are the result of adhesive growth from smaller chondrules, i.e. they are part of welded chondrule agglomerates or adhere to the surface of larger chondrules.

They form irregular layers of smaller roundish chondrules stacked on top of each other. A striking example is shown in Fig. 3d (white outline), which appears to be an agglomeration of small chondrules and lobate melt droplets around a central chondrule, separated by an Fe-Ni layer (white).

Chondrule olivine is nearly equilibrated in most samples (Table 4; Fig. 2a). The lowest Fa values for olivine grains found in this study (beside the rare relict Mg-rich olivine cores) are around 10 mol%.

This value is also the arbitrarily defined boundary between the chemical chondrule types I (<10 mol% Fa) and II (McSween, 1977b;[START_REF] Jones | Chemical, mineralogical and isotopic properties of chondrules: Clues to their origin[END_REF][START_REF] Lauretta | Petrology and origin of ferromagnesian silicate chondrules[END_REF]. However, the presence of Fe-Ni metal in most chondrules in our samples (Figs. 3a-f) relates them to type I. In case of larger chondrules there is a tendency that metal occurs as outer shells (e.g., Fig. 3g). In several cases, metal forms one or two concentric layers within the chondrules (Figs. 3e-f), which may indicate that these structures formed by agglomeratic growth. The largest Fe-Ni metal grains in chondrules were found in

LoV 051 (1.1 mm) and Coolidge (1.6 mm). The metal mainly consists of polycrystalline kamacite with small amounts of taenite exsolutions (Fig. 4a). The Ni concentration in kamacite is fairly constant in all samples, with mean concentrations ranging between 7.1 wt.% (NWA 13400) and 8.0 wt.% (NWA 033).

Measured Ni concentrations in taenite are variable, with values between 13.5 wt.% and 41.0 wt.%. This is consistent with the results of [START_REF] Scott | Petrology of types 4-6 carbonaceous chondrites[END_REF] and [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] who found mean Ni concentrations of 6.4-7.1 wt.% and 19.2-20.9 wt.% for kamacite and taenite, respectively, in Coolidge.

In many kamacite grains, tiny subrounded grains of chromite, merrilite, and SiO 2 occur as exsolutions along internal metal grain boundaries (Fig. 4a). A side-by side occurrence of isolated kamacite and taenite grains in chondrules was only rarely observed (Fig. 4b). Polycrystalline, primary sulfide grains (troilite, FeS) up to 500 µm large and frequently intergrown with kamacite, can also be found in these chondrules (Fig. 4c-d). In some chondrule cut faces the sulfide + metal portion exceeds 50 area%.

Some metal grains up to 1 mm in size occur outside of chondrules. Chondrule plagioclase compositions are variable (An 72 -An 99 ) with negligible K concentrations. [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] found values of An 27 -An 95 in Coolidge. Plagioclase is concentrated in chondrule mesostases, frequently in the shape of lath-like intergrowths with Ca-rich pyroxene.

Some Al-rich chondrules have been observed in Loongana (Fig. 3g) and LoV 051, and nonporphyritic chondrules (barred olivine; BO) were found in Coolidge and NWA 13400 (Fig. 3h).

In all samples Mg-rich relict olivine cores are found, attesting that type I chondrules were present prior to thermal metamorphism. Occasionally, chondrules of chemical type II can be observed in the samples (e.g. BO chondrule in Fig. 3h) which can be identified by their metal-free composition.

Chemistry of main minerals

The chemical compositions of the main mineral phases found in chondrules (olivine, low-Ca pyroxene, and Ca-rich pyroxene) were measured by EMPA. Relict Mg-rich olivine cores are occasionally found in all samples, but were not measured during the random analyses. A number of 30 to 49 olivine grains were measured in each sample and the variation of Fa values is shown in Fig. 2a.

The mean Fa values (mol%; Table 4) vary between 12.5 (Loongana) and 14.7 (NWA 13400). The Fa values for Coolidge and Loongana (14.5 and 12.5) are similar to those presented in earlier studies. [START_REF] Scott | Petrology of types 4-6 carbonaceous chondrites[END_REF] and [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] found Fa values of 14 in Coolidge; [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] give a value of 13.6. The mean Fa value for Loongana found by the latter is 11.8. The mean FeO/MnO ratios (wt.%/wt.%) in olivine of our samples vary between 52 (Loongana) and 61 (NWA 13400). [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] found a mean value of 64 in Coolidge, compared to our value of 60.

Between 20 and 49 low-Ca pyroxene grains were measured in each sample and the Fs variation is presented in Fig. 2b. The mean Fs values (mol%; Table 5) vary between 6.6 (NWA 13400) and 10.4

(Loongana). [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] and [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] found mean Fs values of 10.1 and 9.3, respectively, in Coolidge, compared to our value of 9.4. The mean Fs value of 6.9 for Loongana given in [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] is somewhat lower than our value (10.4), possibly indicating sample inhomogeneity. The mean wollastonite (Wo) values in all samples vary between 0.9 and 1.1 mol% (Table 5). The mean FeO/MnO ratios (wt.%/wt.%) in low-Ca pyroxene are similar and vary between 38 (NWA 13400) and 46 (Coolidge). Low-Ca pyroxene phenocrysts with extremely high Al 2 O 3 contents (9-13 wt.%) have been found in a quenched Al-rich chondrule in Loongana (Fig. 3g; dark gray crystals). Similar pyroxene compositions have been found by [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] in a BO chondrule from Coolidge.

Ca-rich pyroxene is another major mineral phase in chondrules. Between 8 and 38 grains were measured in each sample and the mean Fs and Wo variations (mol%) are presented in Table 6. The mean Fs values vary between 4.2 (NWA 13400) and 6.6 (Coolidge) and the mean FeO/MnO ratios (wt.%/wt.%) vary between 13 and 20. The mean Wo values vary between 30.9 (Loongana, NWA 13400) and 38.6 (NWA 033; Table 6).

Fractions of chondrules with pyroxene rims

Many of the type I PO and POP chondrules, especially the larger ones, are mantled by low-Ca pyroxene layers (Figs. 1, 3e), a typical feature in carbonaceous (and other) chondrites (e.g. [START_REF] Friend | The conditions of chondrule formation, Part II: Open system[END_REF][START_REF] Barosch | Mineralogically zoned chondrules in ordinary chondrites as evidence for chondrule open system behavior[END_REF]. We systematically quantified the 2-dimensional fractions of mineralogically zoned chondrules using the produced phase maps. Fractions are lowest in Coolidge (57%), intermediate in LoV 051 (58%), Loongana (59%) and NWA 033 (60%), and highest in NWA 13500 (62%). [START_REF] Barosch | Sectioning effects of porphyritic chondrules: implications for the PP/POP/PO classification and correcting modal abundances of mineralogically zoned chondrules[END_REF] demonstrated that 2D studies underestimate the true (3D) zoned chondrule fractions and proposed a 2D-3D correction factor of 1.24 for carbonaceous chondrites. The so calculated average 3D zoned chondrule fraction in the investigated samples is ~73%, a value typical for carbonaceous chondrites [START_REF] Friend | The conditions of chondrule formation, Part II: Open system[END_REF][START_REF] Barosch | Sectioning effects of porphyritic chondrules: implications for the PP/POP/PO classification and correcting modal abundances of mineralogically zoned chondrules[END_REF].

Apparent chondrule sizes

We measured the apparent (2D) chondrule sizes in the five CL chondrites as well as in Allende and the CR2 chondrite NWA 7020 for comparison. Obvious chondrule fragments and angular monomineralic grains were excluded from these measurements (see section 3.2.3). The identification of chondrule outlines were sometimes obfuscated by the complex chondrule textures described in section 4.7.1.1). Our chondrule sizes (diameters) include the irregular layers of adhering smaller chondrules and (rarely observed) igneous rims. The statistics for the size-frequency distributions are

given in Table 7. The original size data can be found in the Electronic Annex of this publication. We measured between 145 and 512 chondrules per sample and found a fairly restricted range of mean apparent (2D) chondrule sizes, which are between 404 µm (Coolidge) and 477 µm (NWA 13400).

These are similar to that of the CV ox chondrite Allende (470 µm), but considerably smaller than that of the CR chondrite (mean 633 µm; Table 7). The same holds for the values of the median sizes and standard deviations. The measured size-frequency distributions of the investigated CL chondrites are shown in Fig. 5a. In Fig. 5b their mean size distribution is compared to the distributions found in the present study for the CV chondrite Allende and the CR chondrite NWA 7020. The mean CL distribution is similar to that of Allende, but the CR distribution differs in having much larger fractions of large (> 600 µm) chondrules and correspondingly lower fractions of smaller chondrules.

Refractory inclusions (CAIs and AOAs)

The largest CAIs found in our study are from NWA 13400 and Loongana, with maximum apparent sizes of 3.8 and 2.8 mm, respectively. The occurrence of CAIs in Loongana and Coolidge has been described by [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] and [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] with maximum sizes of 500 µm in Coolidge. All CAIs in our samples are fine-grained and consist mainly of an intergrowth of spinel, plagioclase, and Ca-rich pyroxene. Similar CAI textures were also described by [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] for the

Coolidge meteorite. A complex CAI in Loongana is shown in Fig. 6a, which consists of fine-grained subunits (anorthite, spinel), rimmed by Ca-rich pyroxene. Some FeS is also present in this CAI.

Several other CAIs are rich in FeS, probably a result of secondary alteration on the parent asteroid. An example is shown in Fig. 6b from NWA 13400, which consists of anhedral to euhedral spinel grains, embedded in a fine-grained groundmass of spinel, FeS, and plagioclase. This inclusion is partially rimmed by Ca-rich pyroxene. Spinel grains in all CAIs are zoned, with decreasing Mg-and Al-contents and increasing Cr-and Fe-contents from core to rim. This confirms observations by [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] for

Coolidge. In a CAI from this meteorite we found an assemblage of spinel + FeS + TiO 2 (probably rutile; Fig. 6c). This CAI is rimmed by an outer layer of diopside and an inner layer of spinel, possibly remnants of a former Wark-Lovering rim. CAIs in the investigated meteorites are frequently accompanied by large grains of Cl-apatite, either on their edges (up to 500 µm) or in their interiors (up to 100 µm; Fig. 6d). These phosphates possibly formed by the release of large amounts of Ca during alteration of CAIs. This relation was also observed in Coolidge by [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF]. Moreover, we found a small (7 µm) refractory metal nugget with high concentrations of Os, Ir, Pt, and Ru in a CAI in Loongana, placed within a region of altered Fe-Ni metal (Fig. 6e).

Small (< a few hundred µm) amoeboid olivine aggregates (AOAs) were found in Coolidge by [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF]. We found a large AOA with an apparent maximum size of 900 µm in LoV 051 (Fig. 6f), which consists of a porous part rich in olivine and a more compact part that contains small CAI-like units. These units mainly consist of Ca-rich plagioclase (An 70 ) and chromian spinel.

Inter-chondrule matrix

The modal amount of inter-chondrule matrix (termed "matrix" in this section) is low in the investigated samples (17-21 vol%; Table 2). The matrix mainly consists of an assortment of olivine grains with smaller amounts of low-Ca pyroxene and some plagioclase. Similar observations were described by [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] for the Coolidge meteorite. Fe-rich materials fills the pore spaces and probably represent oxidation products of metals and sulfides (Fig. 7a), a conclusion also given in McSween (1977a). The grain size distribution of matrix components is bimodal, where larger grains (~5-30 µm) are embedded in a groundmass of smaller grains with sizes mostly between ~0.2 and ~1 µm (Fig. 7b-f). ). These results are also included in Table 9.

Compared to Allende, the CL chondrites are slightly depleted in Al and K and strongly depleted in Mn and Na. Hence, they are chemically well discriminated from the other groups of carbonaceous chondrites on, e.g., an Al 2 O-MnO plot (Fig. 8a).

Trace elements

The measured bulk concentrations of trace elements in the samples and in the Allende reference sample are listed in 10). As noted above, severe weathering effects were detected for Loongana and NWA 033. For example, in these meteorites the light rare earth elements (REEs) were enriched during terrestrial weathering, a process described by, e.g., Pourkhorsandi et al. (2017a). These data and some for the other samples are shown in italics in Table 10 and are neither included in the figures nor will they be included in the discussion.

Only few literature data exist on the chemical composition of Coolidge [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF][START_REF] Weckwerth | Instrumental neutron activation analyses of the most Earth-like meteorites[END_REF]; Table 10). Compared to these, our values for Sc and Se are higher and those for V and Hf are somewhat lower (Table 10). Compared to literature data [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF], our Loongana value for Se is somewhat higher and those for V and Zn are somewhat lower.

Again, since our values for the respective elements in the Allende reference sample are in the range of literature data, there is no systematic analytical bias. The investigated CL chondrites are chemically well discernable from the other carbonaceous chondrite groups on Al 2 O 3 vs. Zn (Fig. 8b) and Zr vs. Rb (Fig. 8c) plots, which reveal the typical depletion of volatile elements such as Rb and Zn.

Bulk meteorite isotope compositions

Oxygen isotopes

The measured values for δ

Titanium and chromium isotopes

The Ti and Cr isotopic data are provided in Table 12 and visualized in Fig. 12. In Fig. 12a and so the mean Ti and Cr isotope composition of the CL group can be precisely defined from these data. This in turn makes it possible to use these data for evaluating the genetic relationship of CL chondrites relative to other carbonaceous chondrite groups.

DISCUSSION

Characteristics of CL chondrites and differences to other chondrite groups

The investigated samples share many textural, chemical, and isotopic properties. Macroscopically they remotely resemble CV red and CR chondrites, but there are many differences to these and other carbonaceous chondrite groups, as discussed in the following.

Chondrules

Most chondrules are PO and POP varieties of petrologic type I, rich in Fe-Ni metal. Many small chondrules show a remarkably irregular outer shape with lobate outlines and protuberances (Fig. 3a)

or even have an amoeboidal shape (Figs. 3b,c). Many of the small chondrules are concentrated in layers around larger chondrules (Fig. 3d). However, such textures are not unique to these samples, but were occasionally observed by us in the CV red chondrite Vigarano and the CR chondrite NWA 7020, as well. A distinctive feature of the CL samples is their high chondrule abundance (67 to 79 vol%; Table 2). [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] [START_REF] Krot | Classification of meteorites and their genetic relationships[END_REF], i.e. considerably lower than in CL chondrites.

Apparent chondrule sizes

The observed range of mean apparent chondrule sizes in the CL samples is restricted to values between 404 and 477 µm (Table 7). To verify our method, we also measured the apparent (2D) chondrule sizes in the CR2 chondrite NWA 7020 and the CV chondrite Allende ( 1995) are larger than those found by us (404 µm and 414 µm). The likely explanation is that we measured a large number of chondrules (145 and 235; Table 7) on BSE photomosaics, whereas the literature values were obtained from only 23-52 chondrules (Kallemeyn and Rubin 1995) using optical microscopy. This could have led to an overrepresentation of large chondrules in their statistics.

Our mean value for the CR2 chondrite (633 µm) is in the range of published values for five other CR chondrites (490-770 µm) and close to the corresponding average value (658 µm; [START_REF] Kallemeyn | The compositional classification of chondrites: VI. The CR carbonaceous chondrite group[END_REF]. In case of Allende a verification of our mean value (470 µm) is more complicated since literature data vary considerably, with mean values of 915 µm [START_REF] Teitler | Statistical tests of chondrule sorting[END_REF], 765 µm [START_REF] Gattacceca | CV chondrites: more than one parent body[END_REF], and 310 µm [START_REF] Simon | Particle size distributions in chondritic meteorites: Evidence for pre-planetesimal histories[END_REF]. Sample inhomogeneity may be partly responsible for these variations. Furthermore, the different methods of investigation certainly contribute to these differences, i.e., chondrule separation (true chondrule sizes; [START_REF] Teitler | Statistical tests of chondrule sorting[END_REF], optical microscopy (apparent chondrule sizes; [START_REF] Gattacceca | CV chondrites: more than one parent body[END_REF], and scanning electron microscopy (apparent chondrule sizes; x-ray compositional images, [START_REF] Simon | Particle size distributions in chondritic meteorites: Evidence for pre-planetesimal histories[END_REF]BSE images, this work). Furthermore, the classification of small subrounded particle cut faces as chondrules or fragments is a source of subjective bias.

From the presented results it can be concluded that the chondrule-size-frequency distributions and mean chondrule sizes in CL chondrites are similar to each other and to those in CV chondrites, but dissimilar to those in CR chondrites (Fig. 5; Table 7).

Mean olivine compositions

Similar mean compositions of olivine (Fa 12.5-14.7 mol%; Table 4) are a further distinctive feature of CL chondrites. However, this property is of secondary origin, established by thermal metamorphism on the parent body. This cannot not be a criterion for recognizing unequilibrated CL samples that may be identified in the future (see section 5.3.3). On the other hand, this restricted range of Fa values characterizes the redox conditions at which metamorphism occurred. These conditions were more reducing than those for the CV and CR meteorites, since mean Fa values of olivine in metamorphosed samples from these groups are much higher. For example, olivine in the CV4 chondrite NWA 8418 [START_REF] Mallozzi | Northwest Africa 8418: A CV4 chondrite, with new insight into secondary processes on the CV parent body[END_REF], originally classified as C3 (MBDB), shows a mean Fa value of~40 mol%, with a pronounced peak at ~38 mol%, far away from the Fa values in CL samples. The CR6 chondrites NWA 6921, NWA 7317, and NWA 11561 show mean Fa values between 29 and 38 mol% (MBDB), which is also much higher than in CL chondrites. Due to these differences it is obvious that CL chondrites do not represent thermally altered CV and CR chondrites.

Fe-Ni metal abundance

Another distinctive feature of CL compared to CV chondrites is the high amount of Fe-Ni metal, which influences their magnetic properties. The magnetic susceptibility of LoV 051, the least weathered sample, is log = 5.24 (where  is in 10

-9 m 3 .kg -1
), which is similar to the mean value for CR chondrites of log = 5.04±0.12 ( [START_REF] Bonal | Water and heat: new constraints on the evolution of the CV chondrite parent body[END_REF], translating into 6.8±2.8 wt.%.

CAI abundances

The CAI abundances appear to be another characteristic property of the CL chondrites, although our data base is limited. The modal abundance of CAIs is highly variable (from 0.1 vol% for Coolidge to 8 vol% for Loongana; Table 2), probably due to the small section sizes (52 -361 mm 2 ; ), the average CAI abundance is 1.4 vol%. Hence, our best guess for the CAI concentration in these samples is ~1.4 vol%, which is much higher than in CR chondrites (0.12 vol%) and distinctly lower than in CV chondrites (~3 vol% or ~4 vol%; Hezel et al., 2008;[START_REF] Ebel | Abundance, major element composition and size of components and matrix in CV, CO and Acfer 094 chondrites[END_REF]. Our estimate is comparable to that given in [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] for Coolidge and Loongana (1-2 vol%).

Inter-chondrule matrix

Complementary to the high chondrule concentration, the low amount of inter-chondrule matrix (17-21%; Table 2) is another important distinctive feature of CL chondrites. The mean modal abundances of matrix in CV and CR chondrites are much higher, i.e., 52 vol% and 40 vol% in CV ox and CV red , respectively, [START_REF] Gattacceca | CV chondrites: more than one parent body[END_REF] and 35 vol% in CR chondrites [START_REF] Schrader | The formation and alteration of the Renazzo-like carbonaceous chondrites I: Implications of bulk-oxygen isotopic composition[END_REF]. Our value of 18% for Coolidge is nearly identical to the value (17.6%) given by McSween (1977a). The value for matrix in Coolidge as obtained by [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] is higher (~30%), but may reflect sample inhomogeneity. Their value for matrix abundance in Loongana is ~20%, identical to the value found in the present study (Table 2).

It was found by [START_REF] Noguchi | Petrology and mineralogy of the Coolidge meteorite (CV4)[END_REF] 8). This characteristic was already described by [START_REF] Mcsween | The composition of carbonaceous chondrite matrix[END_REF] for the Coolidge chondrite. The clearest difference to matrix compositions of CR, CK, and the different CV chondrite subgroups are the extraordinarily high MgO concentrations in the matrices of the investigated CL samples (mean 28.3 wt.%), compared to mean values of 18.2-21.7 wt.% in the other groups (Table 8). Furthermore, S is considerably depleted in the CL matrix (mean value 0.14 wt.%), compared to CR chondrites and the CV red and CV oxA groups. Only CK chondrites show a lower mean concentration (0.09 wt.%). However, CL3.9/CL4 and CK4 chondrites were affected by thermal metamorphism on their parent asteroids, by which the fine-grained matrix may have undergone considerable chemical modifications.

Bulk chemical compositions

The most characteristic chemical difference between CL chondrites and all other carbonaceous chondrite groups (besides CB and CH) is their strong depletion of volatile lithophile and chalkophile elements. The differences to the CV chondrite Allende can be seen in Tables 9-10 and Figs. 9-10.

This distinctive feature was previously noticed for Coolidge and Loongana (e.g. [START_REF] Kallemeyn | The compositional classification of chondrites: III. Ungrouped carbonaceous chondrites[END_REF][START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF][START_REF] Weckwerth | Instrumental neutron activation analyses of the most Earth-like meteorites[END_REF]. The CL chondrites are well resolved from other carbonaceous chondrite groups on, for example Al 2 O 3 vs. MnO (Fig. 8a), Al2O3 vs. Zn (Fig. 8b), and Zr vs. Rb (Fig. 8c) plots, since volatile elements like Mn, Zn, and Rb are moderately to strongly depleted.

In Fig. 9a the CI-normalized concentrations [START_REF] Lodders | Abundances of the elements in the solar system[END_REF]) of all measured lithophile elements in the CL samples and the Allende reference sample are shown (see Table 10), together with Allende literature data (dotted line). Elements in Figs. 9 and 10 are arranged in the order of increasing volatility [START_REF] Wood | The condensation temperatures of the elements: A reappraisal[END_REF]. While elements from Zr (most refractory) to ~Eu in the CL chondrites and Allende exhibit similar CI-normalized abundances, elements from V to Cs are increasingly depleted. This trend steepens for elements more volatile than Cr (Mn, Na, K, Rb, and Cs), with much stronger depletions in the CLs compared to Allende. This can also be seen in the mean CL values in Fig. 9b, when compared to mean values for the other carbonaceous chondrite groups (CM, CO, CV, CR, CK4). The CL chondrites are characterized by strong enrichments of refractory and the strongest depletions for volatile elements among all carbonaceous chondrite groups.

Figure 10 shows the CI-normalized concentrations of siderophile and chalkophile elements in CL chondrites. In Fig. 10a the values for individual CL chondrites are given, again in comparison to Allende values (measurements and literature data). In Fig. 10b the mean CL values are given, compared to the mean values of the other main carbonaceous chondrite groups. For the siderophile elements Mo, Ni, Co, Fe, and P all samples show a similar pattern, which is also similar to that of the Allende chondrite (Fig. 10a). The mean CL values (Fig. 10b) are in the range of those in the other groups, with the highest concentration of Mo, the most refractory element in this plot. The chalcophile element concentrations in the CL chondrites show some scatter, but are consistently lower than in Allende (Fig. 10a). The mean CL values for chalcophile elements are plotted in Fig. 10b, compared to mean values for the other carbonaceous chondrite groups. The CL mean values indicate the strongest depletions of these elements compared to all other groups, which is in line with the strong depletions of volatile lithophile elements (Fig. 9). Recently, [START_REF] Braukmüller | The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration[END_REF] have shown that the major groups of carbonaceous chondrites show about the same depletions for the most volatile elements.

Specifically, these authors observed that volatile elements with 50% condensation temperatures below 800 K (from Zn to Tl in Fig. 10) are depleted to about the same extent and they, therefore, termed them "plateau volatile elements". The CL chondrites investigated in this study seem to deviate from a plateau-like pattern, since the Zn, Pb, and Tl concentrations appear low compared to the Se and Te concentrations (Fig. 10b). However, Braukmüller et al. ( 2018) also showed that in the ungrouped carbonaceous chondrite EET 96026 the relative concentrations of the plateau volatile elements were strongly modified during thermal metamorphism. As such, the deviations for the CL chondrites observed in this study most likely also reflect element fractionations during thermal metamorphism. This issue will be further discussed below (section 5.2).

Bulk isotopic compositions

Figure 11 shows that the O isotopic compositions of CL chondrites (Table 11) do not define a tight cluster, but exhibit a range of isotopic compositions along the CCAM line (∆ 17 O -3.96 to -5.47‰). This is also typical of the CV and CK groups and may be indicative of some form of genetic relationship between these groups. (Hezel et al., 2008). Contrary to Ti, CAIs are strongly depleted in Cr relative to the major components of chondrites (e.g., chondrules and matrix), and so varying CAI abundances have a negligible effect on the Cr isotopic composition of bulk chondrites. Consistent with this, the ε 54 Cr values of CL chondrites are comparable to those of the CAI-rich CV, CO, and CK chondrites (Fig. 12). Of note, given the large amount of sample material provided for analysis, it is likely that the less-pronounced ε 50 Ti excesses of the CL chondrite samples relative to CV, CO, and CK chondrites are genuine features, and are not related to sampling bias (e.g., lower CAI abundances in the selected sample aliquot).

Volatile depletions: nebular fractionation or thermal metamorphism on the parent body?

The low concentrations of volatile elements in Coolidge, Loongana and the three other CL samples is probably a reflection, to some extent, of their relatively low modal abundance of inter-chondrule matrix (17-21%; Table 2). This component is usually the carrier of volatile elements and its abundance in CL chondrites is only about half as high as in the CV and CR chondrites (40% and 30-50%; [START_REF] Krot | Classification of meteorites and their genetic relationships[END_REF]. On the other hand, the samples were heated on their parent asteroid, which might have caused volatile loss. This effect was investigated for Allende (CV oxA ; [START_REF] Wulf | Fractionation of volatile elements in the early solar system: evidence from heating experiments on primitive meteorites[END_REF] and for Murchison (CM2; [START_REF] Braukmüller | The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration[END_REF] with heating experiments under oxidizing and reducing conditions. Since the five CL meteorites are characterized by high original amounts of Fe-Ni metal, the thermal metamorphism most likely occurred under reducing conditions. The depletions of the volatile lithophile elements Mn, Na, K, Rb, and Cs is one of the most distinctive features of CL chondrites (Figs. 8a,9). However, [START_REF] Braukmüller | The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration[END_REF] did not observe considerable depletions of these elements during their heating experiments (Mn was not considered). The behavior of Mn was investigated by [START_REF] Wulf | Fractionation of volatile elements in the early solar system: evidence from heating experiments on primitive meteorites[END_REF] who found that Mn does not show any depletions, even not in the experiments performed at 1300°C, neither under oxidizing nor reducing conditions. Considerable depletions of chalcophile elements like Zn, Te, Pb, and Tl were found by [START_REF] Wulf | Fractionation of volatile elements in the early solar system: evidence from heating experiments on primitive meteorites[END_REF] and [START_REF] Braukmüller | The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration[END_REF] under reducing conditions. However, the experimentally produced depletion of Pb is higher than for Zn [START_REF] Braukmüller | The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration[END_REF], whereas these two elements are depleted in CL chondrites to about the same extent (Fig. 10b). From these observations we conclude that the consistently low bulk concentrations of the volatile lithophile elements (Mn, Na, K, Rb, and Cs) and the chalkophile elements (Zn, Se, Te, Pb and Tl) in CL chondrites are a primary feature and do not result from thermal metamorphism on the parent body. However, it is possible that the latter process affected the chalcophile element concentrations in the CL samples to some extent. In particular, the relative abundances of the plateau volatile elements appear to have been modified by this process, because the ratios of these elements vary considerably among individual CL samples (Fig. 10a), possibly indicating local redistribution on the parent body.

Proposal for the new Loongana (CL) group of carbonaceous chondrites

Based on their common characteristics we conclude that the five investigated meteorites can be combined together to form a new group of carbonaceous chondrites. The foundation for this was given by [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF], who defined the Coolidge-Loongana grouplet.

Proposed naming as the CL group of carbonaceous chondrites

Among the investigated samples only Coolidge was given an individual meteorite name; the others are named by serial numbers (Table 1). Hence, the first alphabetic character of Coolidge would be the best candidate to name this group, leading to the CC group of carbonaceous chondrites, which is precluded by the already existing CC meteorite class (CC for carbonaceous chondrites). Since

Loongana 001 was the first meteorite for which a close relation to Coolidge was described [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF], we propose to use its first alphabetic character for naming this new group as the CL group.

Other meteorites proposed to belong to the Coolidge-Loongana grouplet

There are some other ungrouped carbonaceous chondrites, which may belong to the Coolidge-Loongana grouplet. However, as will be argued below, none of these samples share the characteristic properties of the five CL chondrites of this study. Nevertheless, future determination of Ti and Cr isotopic compositions of these meteorites will probably help to clarify their relationship to the CL chondrites and other groups of carbonaceous chondrites.

NWA 779

Weckwerth et al. (2001) proposed that NWA 779 belongs to the Coolidge-Loongana grouplet.

However, the determined mean Fa concentration in olivine is 21 mol%, largely different from the Fa values of Loongana (12.5 mol%), Coolidge (14.5 mol%) and the other samples described by us (12.8-14.7 mol%; Table 4). Several volatile element concentrations are considerably higher in NWA 779. These are, for example K 2 O (0.08 wt.% in NWA 779 compared to 0.01-0.02 wt.% in the CLs; Table 9), MnO (0.20 wt.% compared to 0.14-0.16 wt.%; Table 9), and Zn (110 ppm compared to 33-57 ppm;

Table 10). A further obvious difference is the low concentration of Ni and Co in NWA 779 (6000 and 300 ppm, respectively), compared to 12800-13900 ppm and 560-600 ppm, respectively, in the five investigated CL meteorites (Table 9). This is difficult to explain by terrestrial weathering, since most of the CL samples are also strongly weathered. Obviously, NWA 779 contains (as a primary feature) much lower amounts of Fe-Ni metal than the CL meteorites. For these reasons, NWA 779 does not belong to the proposed CL group, but appears to be correctly classified as CV3 (of high petrologic type) in the MBDB.

Hammada al Hamra (HaH) 073

Weckwerth and Weber (1998) and [START_REF] Weckwerth | Instrumental neutron activation analyses of the most Earth-like meteorites[END_REF] space (MBDB). Its mean Fa content in olivine is 17.9 mol%, i.e. outside the range of the five investigated CL samples (12.5-14.7 mol%) and it contains considerably more (~33 vol%) fine-grained matrix [START_REF] Weckwerth | The 3rd member of the Coolidge type grouplet: implications for element fractionations trends in carbonaceous chondrites[END_REF] than the here studies samples (17-21 vol%; Table 2). The mean apparent chondrule size of HaH 073 is 580 µm [START_REF] Weckwerth | The 3rd member of the Coolidge type grouplet: implications for element fractionations trends in carbonaceous chondrites[END_REF], also outside the range of the measured CL values (404-477 µm; Table 7). The concentrations of Ni and Co in HaH 073

(12600 and 575 ppm, respectively; [START_REF] Choe | Compositions and taxonomy of 15 unusual carbonaceous chondrites[END_REF] are slightly lower than those in the CL samples (12800-13900 ppm and 560-600 ppm, respectively; Table 9), indicating a slightly lower abundance of Fe-Ni metal. The concentrations of many volatile elements in HaH 073 are considerably higher than in CL chondrites. The Na 2 O concentrations in the latter are 0.18-0.32 wt.% (Table 9), compared to 0.51 [START_REF] Weckwerth | The 3rd member of the Coolidge type grouplet: implications for element fractionations trends in carbonaceous chondrites[END_REF] and 0.50 [START_REF] Choe | Compositions and taxonomy of 15 unusual carbonaceous chondrites[END_REF], respectively, in HaH 073. The same is true for K, which shows low concentrations of 0.01-0.02 wt.% in CL chondrites (Table 9) and high concentrations between 0.034 [START_REF] Choe | Compositions and taxonomy of 15 unusual carbonaceous chondrites[END_REF] and 0.040 wt.% [START_REF] Weckwerth | The 3rd member of the Coolidge type grouplet: implications for element fractionations trends in carbonaceous chondrites[END_REF] in

HaH 073. The MnO concentration in HaH 073 (0.17 wt.%; [START_REF] Weckwerth | The 3rd member of the Coolidge type grouplet: implications for element fractionations trends in carbonaceous chondrites[END_REF][START_REF] Choe | Compositions and taxonomy of 15 unusual carbonaceous chondrites[END_REF] is somewhat higher than in the CL samples (0.14-0.16 wt.%), and the Zn concentration is distinctly higher, namely 63-66 ppm [START_REF] Weckwerth | The 3rd member of the Coolidge type grouplet: implications for element fractionations trends in carbonaceous chondrites[END_REF][START_REF] Choe | Compositions and taxonomy of 15 unusual carbonaceous chondrites[END_REF], compared to 33-57 ppm in our samples. However, [START_REF] Weckwerth | Instrumental neutron activation analyses of the most Earth-like meteorites[END_REF] revised several HaH 073 values from an earlier publication [START_REF] Weckwerth | The 3rd member of the Coolidge type grouplet: implications for element fractionations trends in carbonaceous chondrites[END_REF] and some of the new results are closer to the range of CL values, e.g., MnO (0.13 wt.%) and Zn (20 ppm). However, the new data for Na 2 O (0.43 wt.%) and K 2 O (0.037 wt.%) are still much higher than those in the CL chondrites. Taking the above differences together, it appears that HaH 073 may be related to, but is not a full member of the CL chondrite group.

Sahara 00182

Weckwerth (2014) argued that Sahara 00182 (C3-ung; MBDB) belongs to the Coolidge-Loongana grouplet. This meteorite with a mean Fa value of 7.8 mol% [START_REF] Smith | NWA 1152 and Sahara 00182: New primitive carbonaceous chondrites with affinities to the CR and CV groups[END_REF]) is probably paired with Sahara 00177 (C3/4-ung; MBDB), which shows a mean Fa value of 7.6 mol%. These Fa values are far outside the range for CL chondrites (12.5-14.7 mol%). Due to the absence of phyllosilicates, [START_REF] Weisberg | Sahara 00182, the first CR3 chondrite and formation of multi-layered chondrules[END_REF] classified Sahara 00182 as the first CR3 chondrite. However, its oxygen isotopic composition plots on the CCAM line in δ 18 O-δ 17 O space (MBDB), which excludes a relationship to CR chondrites. A mean apparent chondrule size of 1010 µm was determined by [START_REF] Smith | NWA 1152 and Sahara 00182: New primitive carbonaceous chondrites with affinities to the CR and CV groups[END_REF], a much higher value compared to the CL samples (404-474 µm; Table 7). The modal abundance of inter-chondrule matrix is ~28 vol% [START_REF] Smith | NWA 1152 and Sahara 00182: New primitive carbonaceous chondrites with affinities to the CR and CV groups[END_REF], a value which is outside the observed range in CL chondrites (17-21 vol%; Table 2). The concentration of Ni and Co in Sahara 00182 (14900 and 691 ppm, respectively; [START_REF] Choe | Compositions and taxonomy of 15 unusual carbonaceous chondrites[END_REF] are higher than CL values (12800-13900 ppm and 560-600 ppm, respectively; Table 9), indicating a higher abundance of Fe-Ni metal. Furthermore, Na 2 O and K 2 O concentrations in Sahara 00182 are higher than in the CL chondrites, namely 0.29-0.36 and 0.03 wt.%, respectively [START_REF] Choe | Compositions and taxonomy of 15 unusual carbonaceous chondrites[END_REF][START_REF] Weckwerth | Instrumental neutron activation analyses of the most Earth-like meteorites[END_REF], compared to 0.18-0.27 wt.% and 0.01-0.02 wt.% (Table 9). Due to these differences it is improbable that Sahara 00182 is closely related to the CL chondrites. The strongest argument against such a relationship is provided by the distinctly different chemical composition of inter-chondrule matrix. The SiO 2 and MgO concentrations in the matrix of Sahara 00182 are 24.2 and 21.7 wt.%, respectively, compared to 30.3 and 28.3 wt.% in the CL chondrites (Table 8). These values from [START_REF] Smith | NWA 1152 and Sahara 00182: New primitive carbonaceous chondrites with affinities to the CR and CV groups[END_REF] have been recalculated to totals of 95 wt.% for comparison. There are even more extreme differences in the matrix concentrations of CaO and S. While the matrix in CL chondrites is characterized by very low concentrations of CaO and S (0.97-1.61 wt.% and 0.04-0.35 wt.%, respectively; Table 8), matrix in Sahara 00182 contains 5.75 wt.% CaO and 2.50 wt.% S [START_REF] Smith | NWA 1152 and Sahara 00182: New primitive carbonaceous chondrites with affinities to the CR and CV groups[END_REF].

Anticipated characteristics of unmetamorphosed, yet to be detected samples

Since all investigated CL meteorites are affected by thermal metamorphism (petrologic types 3.9 to 4; Table 2) the question remains how unmetamorphosed samples might look like. It cannot be ruled out that such samples are hidden among the tangled mass of CV red and CR chondrites from Northwest Africa (NWA) and other dense collection areas. On a first glance, those samples would appear unusual due to their very high chondrule abundances and the correspondingly low amounts of finegrained inter-chondrule matrix (Table 2). Depending on the weathering grade, they would more or less stand out against CV red chondrites by their high metal content and high magnetic susceptibility (Table 3). The O isotopic compositions would plot on the CCAM line, within the range of CV-CK chondrites or to the direction of lighter isotopes (Fig. 12). In the end, unmetamorphosed CL chondrites would be definitely uncovered by their characteristic depletions of volatile lithophile and chalkophile elements (Figs. 9, 10), and their Ti and Cr isotopic compositions (Fig. 12b).

Possible genetic relationships between CL chondrites and CV and CK chondrites

The recognition of a further distinct carbonaceous chondrite group raises questions about how the characteristics of each of these groups was initially established. Oxygen and Cr isotopic data as well as chondrule size-frequency distributions suggest a relationship between the CL chondrites and CV and CK chondrites. Perhaps their parent bodies formed in a similar nebular region (heliocentric distance) distinct from those of the other carbonaceous chondrite groups. Compared to CV and CK asteroids, the CL asteroid(s) obviously formed from a distinct mix of components, with higher amounts of chondrules and lower amounts of CAIs and matrix. The low matrix content may indicate a correspondingly low amount of co-accreted water ice which led to more reducing conditions during thermal metamorphism.

However, most CV chondrites are of low petrologic type (3.1-3.6; e.g. [START_REF] Bonal | Determination of the petrologic type of CV3 chondrites by Raman spectroscopy of included organic matter[END_REF], which is in strong contrast to CK and CL chondrites. Most CK chondrites are of petrologic type 4 to 6 and all yet identified members of the CL group are of petrologic types 3.9 to 4 (Table 2). One explanation for these differences is a possible bias of material delivery to Earth by secondary parent bodies, which are in a suitable resonance position just by chance. [START_REF] Greenwood | Linking asteroids and meteorites to the primordial planetesimal population Geochim[END_REF] discuss the relationship between primary and secondary parent bodies, where the latter derived from the former through impact break-up. By this process, secondary bodies form, which do not fully represent the material of the primary body. Even if all primary bodies would have had a similar, for example, onion shell structure of petrologic types (type 6 in the interior, types 5-3 in the outer layers), secondary fragments would mostly consist of material with a restricted range of petrologic types. These types would be overrepresented in our collections, if such secondary parent bodies are the main source of a given meteorite group (e.g., CL chondrites) due to their favorite resonance position.

SUMMARY AND CONCLUSIONS

The five ungrouped carbonaceous chondrites Coolidge, Loongana 001, LoV 051, NWA 033, and NWA 13400 can be grouped together to establish the Loongana (CL) group of carbonaceous chondrites. Based on the presented data we conclude that CL chondrites are characterized by:

1. Fe-Ni metal abundances considerably higher than for CV chondrites, but similar to CR chondrites 2. Chondrule size-frequency distributions similar to CV chondrites, but dissimilar to CR chondrites 3. Mean CAI abundances of ~1.4 vol%, i.e. lower than in CV, but much higher than in CR Loongana-type (CL) chondrites show many similarities to CV and CK chondrites and may have accreted from the same nebular reservoir. Although the average magnetic susceptibility of CL chondrites is similar to CR chondrites, these groups are not related. This is mainly indicated by their different isotopic compositions of O (Figs. 12, 13a) and Ti (Fig. 13b), but also by their different sizefrequency distributions of apparent chondrule sizes (Table 7, Fig. 5).

The interesting question remains, if unidentified or misidentified CL members of lower petrologic types are hidden in our collections, possibly among the large number of CV red and CR chondrites from hot and cold deserts. Such samples would be important to investigate the pristine state of these meteorites and their components. [START_REF] Wlotzka | A weathering scale for the ordinary chondrites (abstract)[END_REF]; 5 partly/largely replaced by oxidation products;

TABLES

6 Highly variable due to small thin section sizes (see Hezel et al., 2008). 6±3.2 (1.4-10.8) 5.4±3.1 (1.6-9.8) 5.5±2.9 (1.4-12.0) 4.8±2.2 (0.7-8.6) 4.2±2.9 (0.8-10.2) Wo 33. 5±8.8 (18.4-43.6) 30.9±13.5 (12.3-43.7) 35.5±7.6 (16.3-45.6) 38.6±5.4 (27.1-49.3) 30.9±9.4 (10.7.1-4.6 1 defocused beam (30 µm)

2 CV subgroups: CVred = reduced; CVoxA = oxidized Allende-type; CVoxB = oxidized Bali-type [START_REF] Weisberg | CV3 chondrites: three subgroups, not two[END_REF] * [START_REF] Mcsween | The composition of carbonaceous chondrite matrix[END_REF]; recalculated to 95.00 wt.% for comparison **Unpublished data (Friend, pers. communication) nd: not determined n: number of analyzed areas [START_REF] Wolf | The solar system abundances of phosphorus and titanium and the nebular volatility of phosphorus[END_REF][START_REF] Weckwerth | Instrumental neutron activation analyses of the most Earth-like meteorites[END_REF][START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] in parenthesis. nd: not determined 4 Literature data [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] in parenthesis 5 Literature data [START_REF] Jarosewich | The Allende meteorite reference sample[END_REF]Stracke et al., 2012, average of 39 samples;[START_REF] Braukmüller | The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration[END_REF] 3 Literature data [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF][START_REF] Weckwerth | Instrumental neutron activation analyses of the most Earth-like meteorites[END_REF] in parenthesis; nd: not determined 4 Literature data [START_REF] Kallemeyn | Coolidge and Loongana 001: A new carbonaceous chondrite grouplet[END_REF] [START_REF] Lodders | Abundances of the elements in the solar system[END_REF]; Others (mean values, where possible): [START_REF] Kallemeyn | Compositional comparisons of metamorphosed carbonaceous chondrites[END_REF]Wasson (1981, 1982); [START_REF] Jarosewich | The Allende meteorite reference sample[END_REF]; [START_REF] Kallemeyn | The compositional classification of chondrites: V. The Karoonda (CK) group of carbonaceous chondrites[END_REF][START_REF] Kallemeyn | The compositional classification of chondrites: VI. The CR carbonaceous chondrite group[END_REF]; [START_REF] Wolf | The solar system abundances of phosphorus and titanium and the nebular volatility of phosphorus[END_REF]; [START_REF] Jarosewich | Chemical analysis of meteorites at the Smithsonian Institution: An update[END_REF]; [START_REF] Greenwood | The relationship between CK and CV chondrites[END_REF]; [START_REF] Braukmüller | The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration[END_REF]. [START_REF] Knab | The distributions of trace elements in carbonaceous chondrites[END_REF]; [START_REF] Kallemeyn | The compositional classification of chondrites: I. The carbonaceous chondrite groups[END_REF]; [START_REF] Jarosewich | The Allende meteorite reference sample[END_REF]; [START_REF] Kallemeyn | The compositional classification of chondrites: V. The Karoonda (CK) group of carbonaceous chondrites[END_REF][START_REF] Kallemeyn | The compositional classification of chondrites: VI. The CR carbonaceous chondrite group[END_REF]; [START_REF] Alexander | A multi-technique search for the most primitive CO chondrites[END_REF], CV3 and CK [START_REF] Greenwood | The relationship between CK and CV chondrites[END_REF], and CR chondrites [START_REF] Schrader | The formation and alteration of the Renazzo-like carbonaceous chondrites I: Implications of bulk-oxygen isotopic composition[END_REF][START_REF] Schrader | A water-ice rich minor body from the early Solar System: The CR chondrite parent asteroid[END_REF] are shown for comparison. All samples plot on or slightly to the side of the Carbonaceous Chondrite Anhydrous Mineral (CCAM) line [START_REF] Clayton | Oxygen isotope studies of carbonaceous chondrites[END_REF]. Other reference lines:

Primitive Chondrule Minerals line (PCM) [START_REF] Ushikubo | Primordial oxygen isotope reservoirs of the solar nebula recorded in chondrules in Acfer 094 carbonaceous chondrite[END_REF]; Young and Russell line (Y&R) [START_REF] Young | Oxygen reservoirs in the early solar nebula inferred from an Allende CAI[END_REF]

  investigated CL chondrites and Allende are listed in Table 11 and plotted in Fig. 11. The compositional fields for CR, CV3, CK, and CO3 chondrites are shown for comparison. All CL samples plot along the Carbonaceous Chondrite Anhydrous Mineral (CCAM) line (Clayton and Mayeda, 1999) with ∆ 17 O values between -3.96 and -5.47‰. The CL data plot either directly on this line (NWA 033, NWA 13400) or slightly off it and in the direction of the Primitive Chondrule Minerals (PCM) line[START_REF] Ushikubo | Primordial oxygen isotope reservoirs of the solar nebula recorded in chondrules in Acfer 094 carbonaceous chondrite[END_REF]. Three of the CL samples (Loongana, NWA 033, NWA 13400) plot within the range of CV3 and CK chondrites,

  the є 54 Cr data are plotted vs. the corresponding ∆ 17 O values and in Fig. 12b the є 54 Cr values are plotted vs. the є 50 Ti data. In such diagrams the dichotomy between non-carbonaceous and carbonaceous chondrites is strikingly evident (Warren, 2011; Kleine et al., 2020). Although the є 54 Cr values of the five CL chondrites are similar to the mean compositions of CO and CV chondrites (Fig. 12a), the CL chondrites plot in a distinctly different region of the є 54 Cr-є 50 Ti diagram, where they do not overlap with the compositions of CO and CV chondrites (Fig. 12b). Instead, in terms of є 50 Ti the CL chondrites are more similar to CM and CR chondrites. All CL chondrites have indistinguishable

  conclude that Hammada al Hamra (HaH) 073, currently classified as C4 (MBDB), belongs to the Coolidge-Loongana grouplet. The O isotopic composition of this sample plots within the range of CV-CK chondrites on the CCAM line in

chondrites 4 .

 4 Very low amounts of inter-chondrule matrix (17-21 vol%), the lowest among the main carbonaceous chondrite groups (CI, CY, CM, CO, CV, CR, CK) 5. Nearly equilibrated olivine with mean fayalite (Fa) values between 12.5 mol% (Loongana) and 14.7 mol% (NWA 13400) as a metamorphic effect 6. Lower Al 2 O 3 and higher MgO and Cr 2 O 3 concentrations in inter-chondrule matrix compared to matrix in CV, CK, and CR chondrites, as a possible metamorphic effect 7. Considerable bulk depletion of the volatile lithophile elements Mn, Na, K, Rb, and Cs, and the chalcophile elements Zn, Se, Te, Pb, and Tl, compared to all other main carbonaceous chondrite groups 8. Bulk O isotope compositions plotting along the CCAM line (∆ 17 O -3.96 to -5.47‰), partly overlapping with the CV and CK chondrite field but including samples that

  of Cologne, Inst. f. Geologie und Mineralogie, Germany; 2: Senckenberg Forschungsinstitut und Naturmuseum, Frankfurt, Germany; 3: CEREGE (CNRS/University Aix-Marsaille), France; 4: University of Münster, Inst. f. Planetologie, Germany; 5: Mirko Graul, Bernau, Germany.

in parenthesis 5

 5 Literature data for Allende. Averaged values are shown in Figs. 9-10. Stra: Stracke et al. (2012; average of 39 subsamples; * XRF/ICP-MS average). Brauk: Braukmüller et al. (2018; Smithsonian standard). Others: a Barrat et al. (2012); b Pourkhorsandi et al. (2017b); c Greenwood et al. (2010); d Hezel and Palme (2008); e Wang et al. (2014); f Burkhardt et al. (2014).

Fig. 1 .

 1 Fig. 1. Overall texture and lithologic components of the Loongana 001 meteorite as an example for the proposed CL group of carbonaceous chondrites (a: back-scatter electron image; b: phase map including color coding). Beside the omnipresent metal-rich porphyritic type-I chondrules (PO, POP)with irregular shapes (1), the following components are visible: 2) Barred olivine (BO) chondrule; 3) Alrich chondrule; 4) Chondrule fragment; 5) Irregularly shaped chondrule adhering to a larger one; 6) Chondrule with thick pyroxene rim (7) and olivine-rich core; 8) Ca-Al-rich inclusion (CAI).

Fig. 2 .

 2 Fig. 2. Frequency distributions of fayalite (Fa) values (a) and ferrosilite (Fs) values (b) in olivine and low-Ca pyroxene, respectively, in CL chondrites. Coolidge, Loongana, and NWA 033 show narrow Fa distributions. The samples LoV 051 and NWA 13400 show broader distributions, indicating a less intensive metamorphic overprint.

Fig. 3 .

 3 Fig. 3. Chondrule textures in CL chondrites. a) Typical porphyritic olivine-pyroxene (POP) chondrule with irregular and lobate outline (Coolidge). b) Chondrule with several protuberances in NWA 13400. c) Assortment of differently sized and irregularly shaped chondrules or melt shreds (NWA 13400). d) Extreme complex chondrule (white outline), consisting of a porphyritic olivine (PO) chondrule core with irregular layers of adhering smaller chondrules or melt shreds, stacked on top of each other. The central chondrule is separated from these layers by an Fe-Ni layer (white). e) Layered olivine chondrule with concentric inner Fe-Ni layer and thin pyroxene rim (LoV 051). f) Multi-layered olivine chondrule with two cocentric inner Fe-Ni layers and an outer Fe-Ni layer (NWA 13400). g) Al-rich chondrule with fine-grained quench texture and large Al-rich enstatite crystals (dark gray; Loongana). h) Barred olivine (BO) chondrule of chemical type II with igneous rim in NWA 13400. SEM-BSE images; dark gray: low-Ca pyroxene; medium gray: olivine; white to light gray: Fe-Ni metal, sulfides; white to light gray linear features are terrestrial oxidation products along cracks (SEM-BSE images).

Fig. 4 .

 4 Fig. 4. Opaque phases in CL chondrites. a) Polycrystalline kamacite grain in a Coolidge chondrule, showing taenite exsolutions (light gray) and exsolutions of chromite and merrilite (black dots) along kamacite grain boundaries; b) Rare side-by-side occurrence of isolated kamacite (right center) and taenite grains (left center) in a chondrule in NWA 033. Other grains are FeS; c) Intergrowth texture of sulfide (FeS; gray) and kamacite (white) in a LoV chondrule; d) Very large polycrystalline FeS grain in a Coolidge chondrule; white: kamacite. (SEM-BSE images).

Fig. 5 .

 5 Fig. 5. Frequency distributions of apparent chondrule sizes (100 µm binning), measured on BSE photomosaics. a) Frequency distributions in the investigated CL chondrites; b) Average distribution in CL chondrites (blue solid line, calculated from data in a). Frequency distributions for the CV chondrites Allende (CV oxA , red dashed line) and the CR chondrite NWA 7020 (black dotted line), obtained in this study, are shown for comparison. Please note the different scaling of the size axes in a) and b). n: number of measured chondrules.

Fig. 6 .

 6 Fig. 6. Textures and components of refractory inclusions in CL chondrites. a) Complex CAI in Loongana, consisting of fine-grained subunits (anorthite, spinel) which are rimmed by Ca-rich pyroxene (medium gray), and some FeS (white); b) CAI in NWA 13400, mainly consisting of subhedral-euhedral spinel (medium-dark gray), FeS (white), partly surrounded by a spinel rim; c) CAI in Coolidge, rimmed by a spinel and diopside layer, probably a former Wark-Lovering rim. This inclusion contains a mineral assemblage consisting of FeS, TiO 2 , and spinel, embedded in extremely fine-grained groundmass; d) Cl-apatite in a CAI in NWA 13400 (left center, light gray); e) Refractory metal nugget (light gray to white; rich in Os, Ir, Pt, Ru) in a CAI in Loongana; f) Amoeboid olivine aggregate (AOA) in LoV, intermingled with CAI material (right part of the inclusion). White to light-gray linear features in the images are terrestrial oxidation products along cracks (SEM-BSE images).

Fig. 7 .

 7 Fig. 7. Inter-chondrule matrix in CL chondrites. a) Overview of Loongana matrix, showing chondrule and mineral fragments (mostly olivine and low-Ca pyroxene), embedded in a fine-grained groundmass of very small grains of olivine and low-Ca pyroxene, with interstitial oxidation products of metals and sulfides. Microtextures of inter-chondrule matrix are shown for the CL chondrites Loongana (b), Coolidge (c), LoV 051 (d), NWA 033 (e), and NWA 13400 (f). The size distributions are bimodal with a coarser-grained fragment population, cemented by a finer-grained groundmass. The latter possibly crystallized during thermal metamorphism. Black to medium gray: silicates (olivine and pyroxene); light gray to white: oxidation products of metals and sulfides (SEM-BSE images).

Fig. 8 .

 8 Fig. 8. Bulk chemical compositions of CL chondrites (encircled red filled circles) and other groups of carbonaceous chondrites (CI, CM, CO, CV, CR, CK4; literature data). a) Al 2 O 3 vs. MnO concentrations; the volatile lithophile element Mn is considerably depleted in CL chondrites compared to the other groups; the Al 2 O 3 concentrations are in the range of CV and CK chondrites. b) Al 2 O 3 vs. Zn concentrations; the CL chondrites show, on average, the lowest Zn concentrations among all major carbonaceous chondrite groups. c) Zr vs. Rb concentrations; CL chondrites show a characteristic combination of low Rb and high Zr concentrations. Literature data: CI (Lodders et al., 2009); Others

Fig. 9 .

 9 Fig.9. CI-normalized[START_REF] Lodders | Abundances of the elements in the solar system[END_REF] lithophile element concentrations in CL chondrites and other carbonaceous chondrite groups. Elements are arranged in the order of increasing volatility[START_REF] Wood | The condensation temperatures of the elements: A reappraisal[END_REF]). a) Data for CL chondrites (colored curves, circles) and Allende (black curve, squares), together with Allende literature data (dashed curve; see Tables9-10). The volatile lithophile elements Mn, Na, K, Rb, and Cs are moderately to strongly depleted compared to Allende. b) Mean concentrations in the CL chondrites (red solid curve, filled circles) and other carbonaceous chondrite groups (CM, CO, CV, CR, CK4; literature values; black curves). The CL-trend of volatile element depletion and enrichment of other elements is evident. Literature data (mean values, where possible):

  [START_REF] Wolf | The solar system abundances of phosphorus and titanium and the nebular volatility of phosphorus[END_REF];[START_REF] Jarosewich | Chemical analysis of meteorites at the Smithsonian Institution: An update[END_REF];[START_REF] Greenwood | The relationship between CK and CV chondrites[END_REF];[START_REF] Mccoy-West | The neodymium stable isotope composition of the silicate Earth and chondrites[END_REF];[START_REF] Braukmüller | The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration[END_REF].

Fig. 10 .

 10 Fig.10. CI-normalized[START_REF] Lodders | Abundances of the elements in the solar system[END_REF] concentrations of siderophile and chalkophile elements in CL chondrites and other carbonaceous chondrite groups. Elements are arranged in the order of increasing volatility[START_REF] Wood | The condensation temperatures of the elements: A reappraisal[END_REF]). a) Data for CL chondrites (colored curves, circles) and Allende (black curve, squares), together with Allende literature data (dashed curve; see Tables9-10). b) Mean concentrations in the CL chondrites (red curve, filled circles) and other carbonaceous chondrite groups (CM, CO, CV, CR, CK4; literature values; black curves). The concentrations of siderophile elements in CL chondrites are in the range of those in the other groups, with the highest value for the most refractory element (Mo). The concentrations of chalcophile elements in CL chondrites are the lowest of all other groups. Literature data (mean values, where possible):[START_REF] Matza | Volatile/mobile trace elements in Karoonda (C4) chondrite[END_REF] Tl in the Karoonda CK chondrite);[START_REF] Kallemeyn | The compositional classification of chondrites: I. The carbonaceous chondrite groups[END_REF];[START_REF] Palme | The cosmic abundance of molybdenum[END_REF][START_REF] Jarosewich | The Allende meteorite reference sample[END_REF];[START_REF] Bischoff | Paired Reanazzotype (CR) carbonaceous chondrites from the Sahara[END_REF] Mo in the Acfer 059/El Djouf 001 CR chondrite);[START_REF] Kallemeyn | The compositional classification of chondrites: V. The Karoonda (CK) group of carbonaceous chondrites[END_REF][START_REF] Kallemeyn | The compositional classification of chondrites: VI. The CR carbonaceous chondrite group[END_REF];[START_REF] Wolf | The solar system abundances of phosphorus and titanium and the nebular volatility of phosphorus[END_REF];[START_REF] Jarosewich | Chemical analysis of meteorites at the Smithsonian Institution: An update[END_REF];[START_REF] Greenwood | The relationship between CK and CV chondrites[END_REF];[START_REF] Burkhardt | Evidence for Mo isotope fractionation in the solar nebula and during planetary differentiation[END_REF] Mo in the Karoonda CK chondrite);[START_REF] Braukmüller | The chemical composition of carbonaceous chondrites: Implications for volatile element depletion, complementarity and alteration[END_REF].

Fig. 11 .

 11 Fig. 11. Bulk oxygen isotopic compositions of CL chondrites (red squares). Data fields for CO3

  , Terrestrial Fractionation Line (TFL) are shown for comparison. Three of the samples plot within the fields of CV3 and CK chondrites, together with Allende (this study). The meteorites Coolidge and LoV 051 plot outside these fields and are characterized by a

Fig. 12 .

 12 Fig. 12. Bulk isotopic compositions of CL chondrites (filled circles; red). a) є 54 Cr vs. ∆ 17 O; b) є 54 Cr vs.

FIGURES

  FIGURES

  Fig. 5

  Fig. 8

Fig. 11

 11 Fig. 11

  mixture of isometric to slightly elongated grains, which may have crystallized during thermal metamorphism. The mean chemical compositions of matrix in the investigated samples, obtained by EMPA, are listed in Table8, together with literature data for other carbonaceous chondrite groups. To provide a better comparison with our values, the literature data of[START_REF] Mcsween | The composition of carbonaceous chondrite matrix[END_REF] in this table have been recalculated to totals of 95%. The measured bulk concentrations of major and minor elements in the CL chondrites and the Allende reference sample are listed in Table 9, together with literature data for Coolidge, Loongana, and Allende. The measured values for Allende are well within or close to the range of literature values. Our FeO (30.99 wt.%) and Na 2 O (0.32 wt.%) value for Coolidge appears high compared to literature values (24.83-27.04 and 0.24-0.26 wt.%, respectively). However, our values for FeO and Na 2 O of the Allende reference sample are in the range of literature values, thus showing no systematic analytical

	4.8 Bulk meteorite elemental compositions
	4.8.1 Major and minor elements

The majority of larger grains represent fragments of larger objects, probably chondrules, with fracture surfaces and irregular outlines. Beside some angular fragments, the smaller grains are a bias. None of the chosen analysis methods of this study was able to measure the bulk S content of the samples and we used SEM-EDX data to obtain a rough estimate of the S concentrations (see section 3.2.1

Table 10

 10

, together with literature data for Coolidge, Loongana, and Allende. Our measurements are plotted in Figs. 8b-c and Figs. 9-10, together with data for major and minor elements. The measured values for Allende are well within or close to the range of literature values (Table

  found nearly the same chondrule abundance in Loongana (~70% vs. 67% in this study), but a lower abundance in Coolidge (60-65% vs. 79% in this study), possibly reflecting sample heterogeneity. McSween et al. (1977a) found 67 vol% chondrules in Coolidge. For comparison, chondrule concentrations in CV and CR chondrites are 45% and 50-60%, respectively

Table 7 ;

 7 Fig.5b). It is found that the CL values of mean chondrule sizes overlap with those in the CV chondrite Allende (CV oxA ; 470 µm; Table7). Other statistical parameters of the CL chondrites size-frequency distributions (median size, standard deviation, and skewness) are also similar to those displayed by Allende (Table7), hinting at a possible relationship to CV chondrites. The mean sizes are distinctly smaller than the 633 µm found in the CR chondrite NWA 7020 (Tab. 7). Literature values of mean apparent chondrule sizes for Coolidge and Loongana (610 µm and 700 µm;Kallemeyn and Rubin,

Table 3 ;

 3 [START_REF] Gattacceca | Magnetic Classification of Stony Meteorites: 2. Non-Ordinary Chondrites[END_REF]. The value for the saturation magnetization M S (32.3 Am

2

/kg) translates into a kamacite content of 14.4 wt.% for LoV 051. The hysteresis properties of the investigated samples are similar to those of Renazzo CR chondrite. They are markedly different from those of CV chondrites

[START_REF] Weisberg | CV3 chondrites: three subgroups, not two[END_REF]

, including CV red that show the highest Fe-Ni metal abundances. Indeed, CV red meteorites contain much less metal than LoV 051, i.e. 2.73±1.12 vol% (average ± s.d., n=9;

Table 1

 1

	). It

  Na 2 O concentration of 0.25 wt.% in Coolidge matrix, which is only half the concentration found in Vigarano Matrix (0.54 wt.%;[START_REF] Mcsween | The composition of carbonaceous chondrite matrix[END_REF]; Table8). However, the Na 2 O concentration in CL matrix varies considerably between 0.09 wt.% (NWA 13400) and 0.53 wt.% (NWA 033), with a mean value of 0.30 wt.% (Table8). The mean concentration of Al 2 O 3 in CL chondrite matrix (1.84 wt.%) is

	considerably lower than in the matrices of the various CV chondrite subgroups, as well as in CR and
	CK chondrites (2.04-7.63 wt.%; Table 8). Another striking difference is the enrichment of Cr 2 O 3 (mean
	value 0.71 wt.%) in the CL chondrite matrix, compared to 0.35-0.44 wt.% in CV, CK, and CR
	chondrites (Table

that Coolidge matrix is depleted in Na, compared to the reduced CV chondrite Efremovka. This can be confirmed by our measurements, since we found a

Table 1 :

 1 Sample allocation, weight, and designation of the investigated (sub)samples of CL chondrites.

		Coolidge	Loongana 001	LoV 051	NWA 033	NWA 13400
	Powder sample, total (mg)	559	565	513	598	610
	ICP-MS
	University of Münster, Inst. f. Planetologie
	Sample powder (mg)	128	137	81	163	178
	ICP-MS
	University of Münster, Inst. f. Mineralogie
	Sample powder (mg)	86	86	87	84	86
	Laser fluorination
	Open University, Milton Keynes
	Sample powder (mg)	10	10	15	10	10
	XRF
	University of Cologne
	Sample powder (mg)	131	130	130	134	135
	SEM-EDX, Polarizing microscopy
	University of Münster, Inst. f. Planetologie Polished thin section numbers (size; mm 2 )
	LA-ICP-MS
	University of Münster, Inst. f. Mineralogie
	Thick section numbers (size; mm

Table 2 :

 2 Classification details for the investigated CL chondrites and modal abundances of their lithologic components.

		Coolidge	Loongana 001	LoV 051	NWA 033	NWA 13400
	Proposed petrologic type 1 PMD Fa 2 Shock stage 3 Weathering grade 4	4 2.5 C-S2 W2	4 3.1 C-S2 W3	3.9 9.2 C-S2 W1/2	4 4.4 C-S2 W3/4	3.9 8.9 C-S2 W2/3
	Modal abundances (vol%)
	Chondrules + fragments	79	67	78	72	76
	Inter-chondrule matrix Inter-chondrule metal/sulfides 5 CAIs 6	18 3 0.1	20 5 8.0	17 5 0.4	21 6 0.9	17 6 1.0
	1 According to Hutchison (2004); 2 PMD Fa: Percentage mean deviation (mol%) of fayalite values in olivine grains (see also
	Table 4); 3 according to Stöffler et al. (2018); 4 according to

Table 3 .

 3 Magnetic properties of the investigated CL chondrites, compared to literature data for other[START_REF] Gattacceca | Magnetic Classification of Stony Meteorites: 2. Non-Ordinary Chondrites[END_REF] and[START_REF] Bonal | Water and heat: new constraints on the evolution of the CV chondrite parent body[END_REF] with the addition of Catalina 300 (CVOxB) from[START_REF] Gattacceca | CV chondrites: more than one parent body[END_REF]. Susceptibility data for CR chondrites, Loongana, and Coolidge:[START_REF] Gattacceca | Magnetic Classification of Stony Meteorites: 2. Non-Ordinary Chondrites[END_REF]. MS and MRS data for CV chondrites:[START_REF] Bonal | Water and heat: new constraints on the evolution of the CV chondrite parent body[END_REF].

	groups of carbonaceous chondrites (CVred, CVoxA, CVoxB, CR). magnetic susceptibility; sd: standard
	deviation; M S : saturation magnetization; M RS : saturation remanent magnetization; B C : coercive force;
	B CR : remanent coercive force.
	Meteorite	log	sd	n or studied mass (g)	MS (Am 2 /kg)	MRS (Am 2 /kg)	BC (mT)	BCR (mT) MRS/MS	BCR/BC	n or studied mass (mg)
	Coolidge	4.94		23.4 g
	Loongana 001 LoV 051	4.97 5.24		4.3 g 15.0 g	32.3	0.50	3.08	18.8	1.55x10 -2 6.10	205 mg
	NWA 033 CVred CVoxA CVoxB CR	4.69 4.43 3.62 4.39 5.04	0.22 0.27 0.27 0.12	22.7 g 10 11 10 14	8.03±4.40 0.58±0.26 0.69±0.37 0.053±0.018 5.52±2.78 1.19±0.49 47.3 0.43	16.9±7.0 66.1±37.2 7.22x10 -2 3.91 15.4±0.6 64.6±12.1 7.68x10 -2 4.19 23.9±5.5 44.8±7.0 2.16x10 -1 1.87 1.33 16.1 9.09x10 -3 12.11	10 11 10 259 mg
	Susceptibility data for CV chondrites:

Table 4 .

 4 Mean chemical composition of olivine in the investigated CL chondrites (EMPA; wt.%).

		Coolidge	Loongana 001	LoV 051	NWA 033	NWA 13400
	SiO2	40.9±0.2	41.1±0.3	40.5±0.3	40.7±0.2	40.2±0.4
	TiO2	0.07±0.05	0.06±0.04	0.04±0.04	0.05±0.03	0.03±0.03
	Al2O3	0.05±0.08	0.02±0.04	0.02±0.02	0.03±0.04	0.03±0.05
	Cr2O3	0.09±0.18	0.04±0.03	0.05±0.04	0.04±0.03	0.05±0.05
	FeO	13.8±0.4	11.9±0.4	12.5±1.1	12.8±0.6	14.1±1.2
	MnO	0.23±0.03	0.23±0.03	0.24±0.03	0.24±0.04	0.23±0.05
	MgO	45.8±0.3	47.0±0.4	47.5±0.8	46.2±0.5	45.8±1.1
	CaO	0.03±0.04	0.02±0.02	0.01±0.01	0.02±0.02	0.04±0.04
	Na2O	0.01±0.01	0.01±0.02	0.01±0.02	0.01±0.02	0.01±0.02
	NiO	0.02±0.02	0.02±0.02	0.02±0.02	0.02±0.02	0.03±0.03
	Total	101.00	100.40	100.89	100.11	100.52
	Fa	14.5±0.4 (12.8-15.1)	12.5±0.4 (11.0-13.2)	12.8±1.2 (10.5-15.0)	13.5±0.6 (10.1-14.5)	14.7±1.3 (10.2-16.0)
	FeO/MnO	60	52	52	53	61
	n	44	49	47	46	30
	Fa: Fayalite content in olivine (mol%); ±: 1 standard deviation; Numbers in parenthesis: range of measured values.

Table 5 .

 5 Mean chemical composition of low-Ca pyroxene in the investigated CL chondrites (EMPA; wt.%).

		Coolidge	Loongana 001	LoV 051	NWA 033	NWA 13400
	SiO2	58.5±0.7	58.2±0.8	57.6±0.7	58.4±0.9	58.0±1.0
	TiO2	0.12±0.06	0.10±0.05	0.13±0.06	0.10±0.06	0.10±0.06
	Al2O3	0.81±0.25	0.59±0.23	0.67±0.24	0.73±0.30	0.71±0.16
	Cr2O3	0.37±0.11	0.33±0.07	0.32±0.07	0.39±0.09	0.40±0.07
	FeO	6.37±2.59	6.99±1.40	6.99±2.26	5.32±2.04	4.51±2.55
	MnO	0.14±0.08	0.16±0.05	0.16±0.08	0.13±0.06	0.12±0.05
	MgO	34.2±1.8	33.5±0.9	34.2±1.6	34.6±1.4	35.7±1.5
	CaO	0.48±0.07	0.44±0.15	0.57±0.16	0.45±0.12	0.55±0.05
	Na2O	0.01±0.01	0.01±0.01	0.01±0.02	0.02±0.02	0.02±0.02
	NiO	0.02±0.04	0.05±0.05	0.03±0.02	0.04±0.03	0.09±0.08
	Total	101.02	100.37	100.68	100.18	100.20
	Fs	9.4±3.9 (1.3-14.1)	10.4±2.1 (6.9-14.0)	10.2±3.3 (2.7-14.6)	7.9±3.1 (3.1-15.2)	6.6±3.7 (1.2-15.9)
	Wo	0.9±0.1(0.7-1.2)	0.9±0.3 (0.5-1.5)	1.1±0.3 (0.7-1.9)	0.9±0.2 (0.4-1.3)	1.0±0.1 (0.8-1.2)
	FeO/MnO	46	44	44	41	38
	n	27	24	45	49	20
	Fs, Wo: Ferrosilite, wollastonite content in low-Ca pyroxene (mol%); ±: 1 standard deviation; Numbers in parenthesis: range of
	measured values.

Table 6 .

 6 Mean chemical composition of Ca-rich pyroxene in the investigated CL chondrites (EMPA; wt.%).

		Coolidge	Loongana 001	LoV 051	NWA 033	NWA 13400
	SiO2	54.6±1.1	54.2±2.1	53.7±1.2	53.9±0.7	54.3±0.9
	TiO2	1.09±0.33	0.93±0.48	0.96±0.31	1.07±0.29	1.06±0.38
	Al2O3	2.75±1.15	3.91±2.40	3.38±1.40	3.33±1.32	2.91±0.89
	Cr2O3	0.69±0.16	0.84±0.46	0.69±0.22	0.98±0.31	0.59±0.14
	FeO	4.12±1.97	3.40±2.03	3.42±1.80	2.95±1.36	2.64±1.85
	MnO	0.21±0.05	0.22±0.10	0.17±0.04	0.23±0.08	0.16±0.05
	MgO	21.0±2.5	22.2±4.5	20.6±2.2	19.4±1.6	23.1±3.4
	CaO	16.3±4.2	14.7±6.1	17.3±3.6	18.4±2.6	15.2±4.4
	Na2O	0.30±0.14	0.19±0.14	0.29±0.18	0.33±0.23	0.09±0.12
	NiO	0.03±0.04	0.04±0.07	0.03±0.04	0.04±0.04	0.07±0.05
	Total	101.09	100.63	100.54	100.63	100.12
	Fs	6.

Table 7 .

 7 Statistics (µm) for the distributions of apparent chondrule sizes in the investigated CL chondrites, Allende (CV), and NWA 7020 (CR).

		Coolidge	Loongana 001	LoV 051	NWA 033	NWA 13400	Allende	NWA 7020
	Mean	404 (610) 1	414 (700) 1	476	455	477	470	633
	Median StDev 2	270 405	288 347	403 327	332 349	342 421	357 366	506 468
	Skewness 2.60 Min 3 55 Max 4 2790 n 5 145	2.13 75 2295 235	2.07 75 2490 397	1.69 65 2070 274	2.02 50 2930 512	2.10 70 2670 421	1.20 65 2540 148
	1 Literature data (Kallemeyn and Rubin, 1995); 2 Standard deviation; 3 Size of the smallest chondrule; 4 Size of the largest
	chondrule; 5 Number of analyzed chondrules.

Table 8 .

 8 Bulk composition of inter-chondrule matrix in the investigated CL chondrites (EMPA

	1 ; wt.%).

Table 9 .

 9 Bulk chemical composition (major and minor elements; wt.%) of the investigated CL chondrites and Allende. Literature data for Allende are given for comparison.

			Lab 1	RSD (%) 2	Coolidge	3	Loongana 001 4	LoV 051	NWA 033	13400 NWA	Allende 5
	SiO2	A	< 1	33.05		34.64	33.94	34.36	34.26	34.05
					(33.59; 33.52; nd)					(34.3, 34.15; nd)
	TiO2	A	< 1	0.14		0.15	0.15	0.15	0.15	0.15
					(0.14; 0.14; nd)					(0.15; 0.15, 0.13)
	Al2O3	A	< 1	3.15		2.91	3.20	3.07	3.11	3.20
	Cr2O3	A	< 1	(2.83; 2.83; 3.74) 0.51 6	(3.36) 0.49	0.51	0.52	0.52	(3.28; 3.23, 3.15) 0.50
					(0.46; 0.43; 0.64)	(0.53)				(0.53; 0.53; 0.53)
	FeO	A	< 1	30.99		29.83	30.46	29.02	30.07	29.82
					(27.02; 27.04; 24.83)	(29.46)				(30.3; 30.31; 30.60)
	MnO	A; B	< 1; 1.3	0.15; 0.15	0.16; 0.16	0.14; 0.15	0.16; 0.15	0.15; 0.15	0.19; 0.19
					(0.14; 0.14; 0.15)	(0.14)				(0.19; 0.19; 0.19)
	MgO	A	< 1	24.52		25.32	25.30	25.39	24.47	24.83
					(24.58; 24.57; 24.87)	(24.04)				(24.6; 24.56; 24.79)
	CaO	A	< 1	2.13		2.09	2.84	2.47	2.17	2.48
					(2.06; 2.06; 2.74)	(2.46)				(2.58; 2.61; 2.49)
	Na2O	A	< 1	0.32		0.20	0.27	0.27	0.18	0.49
					(nd; 0.24; 0.26)	(0.22)				(0.46; nd; 0.43)
	K2O	A	< 1	0.02		0.02	0.01	0.02	0.01	0.03
					(nd; 0.04; 0.02)	(0.02)				(0.04; nd; 0.03)
	P2O5	A	< 1	0.24		0.23	0.22	0.25	0.25	0.25
					(0.18; nd; nd)					(0.24; 0.24; 0.24)
	Co	B	4.2	0.060		0.057	0.058	0.056	0.061	0.061
					(0.08; 0.06; 0.06)	(0.06)				(0.06; 0.068; 0.066)
	Ni	A	< 1	1.39		1.30	1.31	1.28	1.28	1.33
	S	7	C	-	(1.13; 1.20; nd) 2.1	0.7	0.5	0.5	0.9	(1.42; 1.39*; 1.42) 2.1
					(nd; nd; nd)					(2.10; nd; 2.08)
	Total			98.98		98.10	98.91	97.52	97.58	99.49

1 Analytical method, laboratory: A: XRF, Institut für Geologie und Mineralogie, University of Cologne; B: ICP-MS, Institut für Mineralogie, University of Münster; C: SEM-EDX, Institut für Planetologie, University of Münster 2 Relative standard deviation of measured values in % 3 Literature data

Table 10 .

 10 Bulk chemical composition of the investigated samples (trace elements; ppm). Numbers in italics indicate values that show evidence for modification by terrestrial weathering.

		Lab 1	RSD (%)	2	Coolidge	3	Loongana 001 4	051 LoV	033 NWA	13400 NWA	Allende			Allende (Literature) 5
												Stra	Brauk	Others
	Li	B	1.7		2.10		2.13	2.07	2.10	1.97	1.69				1.81	a ; 1.64	b
	Sc	D	4.9		15.5		10.5	15.3	10.6	11.5	11.8				11.3	a ; 10.8	b ; 10.7	c
	V	B	2.2		(12.0; 9.4) 85.6		(11.2) 73.3	85.5	81.4	81.6	95.9	90.2	*	92.6	95.2	a; 91	b; 91	c
	Zn	A	< 1		(106; 91) 56.7		(102) 33.7	32.5	43.5	51.6	102	106		123	119	a ;118	d
	Se	D	32		(60; 33) 5.05		(50) 5.78	2.62	5.18	3.04	9.57				9.21	d ; 8.25	e
	Rb Sr Y Zr Nb Mo Te Cs Ba La	B B B B B B D B B B	2.3 0.6 1.2 0.7 2.4 0.2 8.6 2.8 0.3 0.2		(3.2; 3.2) 0.29 14.8 2.66 6.82 0.519 1.52 0.781 0.024 33.9 0.642		(3.3) 0.92 15.3 3.75 8.89 0.620 1.50 0.575 0.060 15.2 1.482	0.42 18.8 2.81 7.40 0.662 1.64 0.528 0.042 13.0 0.527	0.50 24.2 3.77 9.15 0.574 1.40 0.588 0.044 61.6 0.959	0.18 15.5 2.48 6.20 0.535 1.57 0.611 0.011 73.3 0.461	1.21 14.6 2.60 6.60 0.531 1.51 1.21 0.088 4.49 0.487	1.32 15.7 2.63 6.77 0.569 1.45 0.098 4.74 0.490	1.15 6.45 0.503 1.04 0.080 4.21 0.471	1.18 15.6 2.88 6.61 0.573 a ; 1.17 b c b ;15.6 a b ; 2.77 a b ; 7.1 a ; 0.58 1.64 e f ; 1.44 e 0.94 b 0.086 4.53 a ; 4.6 b ; 4.7 b 0.516 a ; 0.498 b	e
	Ce Pr Nd Sm	B B B B	0.1 0.6 0.4 0.2		(0.505; 0.89) 1.400 0.228 1.116 0.335	3.114 0.459 2.006 0.506	1.318 0.201 1.006 0.324	2.148 0.316 1.515 0.427	1.152 0.179 0.891 0.283	1.24 0.193 0.975 0.316	1.24 0.192 0.967 0.313	1.21 0.191 0.998 0.328	1.29 0.201 a ; 1.29 a ; 0.195 b 1.02 a b ; 0.989 0.329 a ; 0.310	b b ; 0.331	e
	Eu	B	0.4		(0.311; 0.34) 0.115	0.153	0.117	0.139	0.109	0.111	0.115	0.110	0.114	a ; 0.108	b
	Gd Tb Dy Ho Er Tm Yb	B B B B B B B	0.1 0.2 0.4 0.1 0.4 0.8 0.1		(0.118; 0.12) 0.404 0.074 0.482 0.107 0.309 0.054 0.317	0.596 0.102 0.661 0.150 0.432 0.057 0.360	0.407 0.074 0.496 0.110 0.318 0.053 0.343	0.530 0.091 0.582 0.133 0.403 0.057 0.345	0.364 0.067 0.441 0.098 0.287 0.048 0.305	0.397 0.073 0.479 0.104 0.300 0.054 0.326	0.401 0.072 0.479 0.100 0.299 0.053 0.319	0.439 0.074 0.499 0.304 0.053 0.327	0.417 0.076 0.508 0.107 0.310 0.056 0.325	a ; 0.409 a ; 0.073 a ; 0.483 a ; 0.103 a ; 0.305 a ; 0.050 a ; 0.302	b b b b b b b
	Lu	B	1.8		(0.329; 0.3) 0.046	(0.338) 0.062	0.048	0.061	0.043	0.044	0.046	0.047	0.046	a ; 0.046	b
	Hf	B	2.6		(0.052; 0.04) 0.203	0.264	0.206	0.262	0.178	0.192	0.188	0.191	0.202	a ; 0.199	b
	Ta Tl Pb Th U	B B B B B	0.1 10 0.6 3.9 4.1		(nd; 0.25) 0.030 0.004 0.325 0.080 0.037		0.037 0.022 0.635 0.315 0.041	0.032 0.006 0.196 0.076 0.028	0.032 0.064 0.508 0.106 0.100	0.028 0.007 0.183 0.072 0.031	0.033 0.071 1.29 0.084 0.015	0.033 1.52 0.078 0.017	0.062 1.08 0.056 0.013	0.034 0.059 1.27 a ; 1.25 a ; 0.041 e b 0.059 a ; 0.082 0.015 a ; 0.018	b b

b 1 Analytical method and laboratory: A: XRF, Institut für Geologie und Mineralogie, University of Cologne; B: ICP-MS, Institut für Mineralogie, University of Münster, Germany; D: LA-ICP-MS, Institut für Mineralogie, University of Münster.

Table 11 .

 11 Bulk O isotopic composition of the investigated CL chondrites.

			Coolidge	Loongana 001 LoV 051	NWA 033	NWA 13400
	 17 O ±  (‰)*	-6.835 ± 0.216 -4.781 ± 0.170 -7.626 ± 0.486	-3.911 ± 0.164 -4.017 ± 0.023
	 18 O ±  (‰)*	-3.336 ± 0.169 -1.035 ± 0.136 -4.151 ± 0.518	0.102 ± 0.228	-0.021 ± 0.007
		17 O ±  (‰)* -5.101 ± 0.128 -4.243 ±0.099	-5.467 ± 0.216	-3.964 ± 0.046 -4.006 ± 0.026
	Mean of 2 measurements, each. ±: 1 standard deviation

Table 12 .

 12 Bulk Ti and Cr isotopic composition of the investigated CL chondrites and Allende.

		N [Ti]	ε 46 Ti ± 2σ	ε 48 Ti ± 2σ	ε 50 Ti ± 2σ	N [Cr]	ε 53 Cr ± 2σ	ε 54 Cr ± 2σ
	Coolidge	10	0.50 ± 0.09	0.07 ± 0.10	2.63 ± 0.10	8	0.07 ± 0.08	0.81 ± 0.10
	Loongana 001	10	0.43 ± 0.13	-0.07 ± 0.07	2.57 ± 0.09	11	0.06 ± 0.08	0.68 ± 0.18
	LoV 051	10	0.52 ± 0.06	-0.05 ± 0.04	2.85 ± 0.08	8	0.05 ± 0.07	0.76 ± 0.12
	NWA 033	10	0.44 ± 0.10	-0.08 ± 0.09	2.35 ± 0.05	12	0.05 ± 0.11	0.64 ± 0.12
	NWA 13400	10	0.53 ± 0.06	-0.05 ± 0.03	2.60 ± 0.07	9	0.14 ± 0.13	0.70 ± 0.13
	Average CL		0.48 ± 0.04	-0.03 ± 0.03	2.60 ± 0.05			0.07 ± 0.04	0.71 ± 0.06
	Allende	12	0.70 ± 0.06	-0.06 ± 0.04	3.21 ± 0.11	6	*	0.12 ± 0.12*	0.96 ± 0.22*
						4*	0.11 ± 0.10*	1.06 ± 0.30*
	All reported uncertainties are Student-t 95% confidence intervals (95% CI). N: Number of analyses of the same solution.

[START_REF] Schneider | Early evolution of the solar accretion disk inferred from Cr-Ti-O isotopes in individual chondrules[END_REF]

Ti =

ACKNOWLEDGEMENTS

We thank Dr. Jutta Zipfel (Senckenberg Forschungsinstitut und Naturmuseum, Frankfurt, Germany) and Mirko Graul (Bernau, Germany) for providing samples of Loongana 001 and NWA 13400, respectively. This work was supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation), grant number ME 1115/10-1 and Project-ID 263649064 -TRR 170. This is TRR 170 pub. no. XX.

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