Hamed Pourkhorsandi
email: hamed.pourkhorsandi@ulb.ac.be

Jérôme Gattacceca

Pierre Rochette

Thomas Smith

Lydie Bonal

Massimo D'orazio

Bertrand Devouard

Sonzogni

Vinciane Debaille

The Famenin fall and other ordinary chondrites intermediate 2 between H and L groups

Keywords: Fall, Intermediate chondrite, HL, ordinary chondrites, classification 51 52 53

The Famenin meteorite fell around 08:30 am local time (GMT+4.5) on 27 June 2015 27 on the roof of a house in Famenin town, NW Iran. A single 640 grams stone was 28 recovered, shattered into several pieces upon impact. The shape of the impact hole and 29 the relative position of the recovered meteorites indicate a N-NW fall direction. Famenin 30 is an ordinary chondrite with well preserved chondrules of various types, (Fe,Ni) metal, 31 troilite, phosphate, and chromite. The organic matter systematics and the olivine and 32 low-Ca compositional distributions (percent mean deviations 18% and 31%, 33 respectively) indicate it is a type 3.4/3.8 chondrite. Considering the average chemical 34 compositions of olivine (Fa 17.5±4.7 ) and low-Ca pyroxene (Fs 16.8±7.5 ), average Co content 35 of the kamacite (5.6 mgg -1 ), and Cu/Ni and Ga/Ni ratios, Famenin should be classified 36 as an H chondrite. However, saturation magnetization is 26.0 Am 2 /kg, indicating a bulk 37 metal content similar to L chondrites. Similarly, the whole rock Ni and Co contents 38 (13073 and 540 µgg -1 , respectively), and average chondrule diameter (550 µm) are 39 closer to typical values for L chondrites than H chondrites. The (Fe,Ni) metal modal 40 abundance (5 vol%), magnetic susceptibility, and possibly whole rock oxygen isotopic 41 composition indicate intermediate properties between H and L chondrites. Noble gas 42 composition and cosmic ray exposure (CRE) ages of Famenin and El Médano 195 43 (another intermediate ordinary chondrite) shows their gas-rich character and an older 44 ejection age from their parent body than those for the majority of H and L chondrites. 45 Famenin, together with similar intermediate ordinary chondrites, increases the diversity 46 of this meteorite clan and suggests the existence of a separate ordinary chondrite group 47 with a composition broadly intermediate between H and L groups for which a different 48 designation (HL) is proposed. Ordinary chondrites likely originate from more than three 49 parent bodies (H, L, and LL) as traditionally proposed.

166

The Raman spectroscopy was performed at Laboratoire de Géologie de Lyon Terre, 167

Planètes, Environnement (ENS Lyon) with a Labram spectrometer (Horiba-Jobin-Yvon)

168 equipped with a Spectra Physics Argon ion laser and using 514.5 nm excitation.

169 Carbonaceous matter is sensitive to laser-induced heating and can be locally altered.

170

Moreover, the Raman bands of the polyaromatic carbonaceous matter are dispersive.

171 Thus, to avoid any laser alteration of the carbonaceous matter and to have a meaningful 30 matrix fragments (typical apparent diameter around 30 µm) were then manually 177 selected according to their color and texture under a binocular microscope. The selected 178 matrix fragments were pressed between two glass slides that were also used as substrate

179
for the Raman analysis. This procedure allows working on ''fresh" samples and helps 180 enhance heat dissipation, thereby minimizing thermal damage. Measurements made 181 over two different sessions on two aliquots provided similar results.

182

Gamma spectroscopy and intensity measurements of 7 Be, 54 Mn, 22 Na, and 26 Al of the 183 two larger fragments (total ~23 g) were carried out from 16 to 24 July 2015 (683500 184 seconds) in LSCE (Gif-sur-Yvette, France).

185

The noble gas concentrations and isotopic ratios ( 3,4 He, 20,21,22 Ne, and 36,38,40 Ar) of and purification line. The He standard is the "He Standard of Japan" ("HESJ"), with a 193 calibrated 3 He/ 4 He ratio of 20.6±0.1 Ra (Matsuda et al. 2002), where Ra stands for the 194 3 He/ 4 He ratio of air (i.e. 1.4×10 -6 ). The average sensitivities for 4 He, 22 Ne, and 36 Ar are, 195 in units of cm 3 STP/counts, 3.67×10 -15 , 3.17×10 -15 , and 4.26×10 -16 , respectively. Blanks 196 were frequently measured using the exact same procedure as for the samples (see 197 details below). They contribute for less than 1% for He, less than 2% for Ne, and less Subsequently, the Ne is separated from the remaining He by using a cryogenic cold trap 205 at 35K for 10 minutes. A fraction of the He gas is then inlet into the mass spectrometer.

206

The Ne fraction is released at 80K for 30 minutes and the total gas fraction is inlet into composition range than the olivine (Fs0.7-36.6 vs. Fa5.9-30.9) (Fig. 5). The percent Table 3).

286

In accordance with the equilibrated texture, the mineral composition of olivine and 287 low-Ca pyroxene of SJ 041 shows a narrow distribution ( chondrite is 3.42 ± 1.1 mg/g (n = 24, Table 3).

295

Magnetic properties

296

The average magnetic susceptibility of Famenin measured on four pieces with 297 masses in the range 5 -11 grams is logχ = 5.07 ± 0.05 (1σ) with χ in 10 -9 m 3 kg -1 .

298

Saturation magnetization measured on a 80 mg fragment is M S = 24.9 Am 2 kg -1 .

299

Hysteresis parameter ratios are M RS /M S = 1.02x10 (Fig. 6S) and as well as W which is closer to mean L chondrites (Fig. 6) However, when The observed Raman spectral parameters scatter reflects variable thermal 418 metamorphism experienced by Famenin: type "A" spectra reflect thermal metamorphism 419 comparable to that experienced by type 3.4 chondrites, while type "B" spectra reflect a 420 higher thermal metamorphism (>3.7) (Fig. 12). It has to be noted that the type "A" spectra et al. 1980; 1982).

429

Based on the olivine optical microscopy, and using the classification of Stöffler et al. as well characterized by 4 He≥10 -4 cm 3 STP/g (Megrue and Steinbrunn 1971). This is the 474 case for Famenin, with 4 He concentration of 3.0×10 -4 cm 3 STP/g (see Table 5). The 475 isotopic 4 He/ 3 He ratios for EM 195 and Famenin are 1503 and 3061, respectively. For 476 comparison, the ( 4 He/ 3 He) SW is 2155 [START_REF] Heber | 744 Noble gas composition of the solar wind as collected by the Genesis mission[END_REF]). However, the Solar Flare (SF)

477

He obtained by Rao et al. (1991) is close to ( 4 He/ 3 He) SF = 3800±200. We assume here 478 that 3 He is entirely cosmogenic.

479

In Fig. 1b, one can observe the presence of mm to cm clasts, indicating that EM 195 480 (Fig. S2) and Famenin are breccias. In addition, as mentioned above and as shown in 481 Mountain 90174 [START_REF] Leya | Cosmogenic nuclides in 758 the solar gas-rich H3-6 chondrite breccia Frontier Mountain 90174[END_REF]. This clearly indicates that EM 195 and Famenin

486

were exposed as a regolith before their compaction and are regolith breccias.

487

Based on the quality assignments in [START_REF] Graf | Collisional history of H chondrites[END_REF] associated with a continuous supply of meteoroids [START_REF] Graf | Collisional history of H chondrites[END_REF]. magnetization (M S = 28.9 Am 2 kg -1 ) [START_REF] Gattacceca | Metal phases in ordinary chondrites: Magnetic hysteresis 725 properties and implications for thermal history[END_REF]. Although based on 582 mineral chemistry (Table 2), it is an H chondrite (close to the lower range), our oxygen 583 isotope data put it away from the H chondrite field and within the L chondrite field (Fig. ). However, it does not plot in the vicinity of H/L field but shows a similar Δ 17 O.

585

Following these and the fact that Gursum is an equilibrated chondrite whose departing 586 oxygen isotope composition cannot be related to heterogeneities found in unequilibrated 587 chondrites, we suggest its classification to be updated to an H5-anomalous chondrite. and that would deserve a specific classification nomenclature (Table 8). We propose to 616 call these latter HL chondrites.

617

Olivine and low-Ca pyroxene data of HL chondrites show that except when they are 618 unequilibrated chondrites (such as Famenin and EM 195), their olivine and low-Ca 619 pyroxene composition is between H and L chondrite ranges (Fig. 9). This phenomenon is 620 more evident in olivine Fa content (Fig. 13) as it equilibrates faster than low-Ca pyroxene 621 during parent body thermal metamorphism [START_REF] Dodd | A survey of the unequilibrated ordinary 714 chondrites[END_REF]. However, it 622 becomes complicated in the case of some HL chondrites such as NWA series 4152-4156

908

Bulk rock data are from Wasson and Kallemeyn (1988) and [START_REF] Kallemeyn | Ordinary chondrites: 752 Bulk compositions, classification, lithophile-element fractionations and composition-753 petrographic type relationships[END_REF].

909

Fayalite data are from Rubin (1990).

933

Bulk rock data are from Wasson and Kallemeyn (1988) and [START_REF] Kallemeyn | Ordinary chondrites: 752 Bulk compositions, classification, lithophile-element fractionations and composition-753 petrographic type relationships[END_REF].

934

Fayalite data are from Rubin (1990).

977

The given uncertainties (1σ) include the uncertainties for the ion current measurements and uncertainties caused by the corrections for interfering isotopes and 978 corrections for instrumental mass fractionation. Systematic uncertainties in the calibration standard are included; they amount to about 4% for concentrations and

979

1% for isotope ratios.

980

*Assuming 3 He to be entirely cosmogenic.

981 982

  of CEREGE. Laser fluorination coupled with isotope ratio 143 mass spectrometry (IRMS)(Alexandre et al., 2006;[START_REF] Crespin | IR 702 Laser Extraction Technique Applied to Oxygen Isotope Analysis of Small Biogenic 703 Silica Samples[END_REF] adapted for 144 measurement of extraterrestrial materials (Suavet et al. 2010) was used for this 145 purpose. The three oxygen isotopic compositions were measured with a dual-inlet mass 146 spectrometer Thermo-Finnigan Delta Plus. In addition to Famenin, we analyzed 1.5 mg 147 samples of Bremervӧrde (H/L3), EM 195 (H/L3), Gursum (H5), Pavel (H3-anomalous), 148 SJ 041 (H/L6) as well as Ochansk (H4), Paranaiba (L6), and Homestead (L5), as 149 example of regular ordinary chondrites. The initial bulk sample was powdered, sieved 150 between 100 and 400 µm, cleaned with 1M HCl at 50°C for several hours to remove 151 metal and sulfides, and rinsed with ethanol. Additional leaching with mono-152 ethanolamine-thioglycolate (EATG) was performed for weathered finds, to remove 153 oxyhydroxides formed during weathering on Earth (see Greenwood et al. 2017 for the 154 use of EATG in this context). The average mass of the initial bulk samples was 73 mg, 155 ensuring that the 1.5 mg aliquot is representative of the bulk oxygen isotopic 156 composition. The oxygen isotope results are expressed in ‰ versus the international 157 reference standard V-SMOW: δ 18 O = [( 18 O/ 16 O) sample /( 18 O/ 16 O) V-SMOW -1]×1000 and δ 17 O 158 = [( 17 O/ 16 O) sample /( 17 O/ 16 O) V-SMOW -1]×1000. The δ 18 O and δ 17 O values of the reference 159 gas were calibrated with measurements of NBS28 standard (δ 18 O=9.60‰, Gröning, 160 2004). ∆ 17 O is computed as ∆ 17 O= δ 17 O-0.52 x δ 18 O. The δ 17 O value of the NBS28 161 standard (δ 17 O = 4.992‰) was computed so as to give ∆ 17 O=0‰. The measurements 162 were corrected on a daily basis using 1.5 mg quartz internal laboratory standard 163 "Boulangé" (Alexandre et al. 2006; Suavet et al. 2010). During the analyzing period, the 164 analytical uncertainties (1σ) derived from repeated measurement (n= 7) of this internal 165 laboratory standard are 0.10‰, 0.16‰, 0.02‰ for δ 17 O, δ 18 O and ∆ 17 O, respectively.

186EM 195 ,

 195 SJ 041, and Famenin were measured using a Noblesse (Nu) multi-collector 187 noble gas mass spectrometer in the noble gas laboratory at the Institute of Geology and 188 Geophysics, Chinese Academy of Sciences, Beijing, China. The analytical approach 189 follows the same procedures as described in Ranjith et al. (2017). Briefly, samples with 190 masses ranging from ~3 to ~5 mg were first washed with ethanol in an ultrasonic bath, 191 weighed, and then loaded into the laser sample chamber of the noble gas extraction 192

  Ar isotopes. Noble gases have been extracted by heating the samples in a 199 single extraction step, using a CO 2 laser (1.064 μm wavelength, 3 mm diameter) for ~30 200 minutes. The released gases were cleaned from all reactive gases such as 201 hydrocarbons, etc. using a series of getters, operating at room temperature and 200°C 202 (Ranjith et al. 2017). The He-Ne fraction is separated from the Ar fraction using an 203 activated charcoal held at the temperature of liquid nitrogen (LN 2 ) for 20 minutes.

207

  the mass spectrometer; remaining background gases, such as hydrocarbons and Ar, 208 which would compromise the Ne measurements, are further reduced using a charcoal 209 held at LN 2 temperature during the Ne measurements. Finally, Ar is released at ~150°C 210 for 20 minutes, and a known fraction of the gas is measured. on the ground, the Famenin meteorite fragmented into two large 215 and eight small pieces. The total recovered mass is 630 g. The two larger pieces total 216 565 g while the smaller fragments have masses between 5 and 25 g (Fig.1). Famenin 217 has weakly developed regmaglypts and the fusion crust has a black to dark-brown color 218 with shiny patches of glassy material covering the fusion crust as an additional layer.219The remnants of roofing asphalt material can be seen as black patches with sizes up to 220 5 cm. 221 The meteorite broken surface reveals a light grey interior. Distinct chondrules, (Fe,Ni) 222 metal and troilite are easily discernible with the naked eye. (Fe,Ni) metal grains show no 223 sign of weathering. A few fine-grained mm to cm-sized clasts with light lithology are also 224 visible (Fig. 1b), although they were not present in the studied type specimen. shows a vesicular texture with magnetite grains in the outermost 228 layer and thin troilite veinlets formed by melting and recrystallization of the primary 229 troilite during atmospheric passage of the meteoroid (Fig. 2, 3a). Point counting of a ~ 230 10 cm 2 surface under reflected light optical microscopy, with a step-size of 50 μm, yields 231 the following proportions: 90.0 vol% silicates, 5.0 vol% (Fe,Ni) metal, and 5.0 vol%

413

  we consider the Cu/Ni and Ga/Ni ratios (Fig.11c,d), which are known to increase from H 414 to LL chondrites (Wasson and Kallemeyn 1988), Famenin falls in the range of H 415 chondrites. Considering these evidences, we classify Famenin as a meteorite 416 intermediate between H and L chondrites.

  417

  421are internally quite variable as well, with spectral parameters of individual spectrum 422 distributed over the metamorphic range observed in Bishunpur (3.1) toTieschitz (3.6).423This can be related to the structural grade of the polyaromatic carbonaceous matter which 424 reveals variable degrees of thermal metamorphism in different parts of the meteorite. The 425 PMD of olivine Fa content is 18%, indicating a petrologic type 3.8 (Sears et al. 1980),in 426 broad agreement with data obtained by Raman spectroscopy (type "B" spectra). Based 427 on these observations, we classify Famenin as a petrologic type 3 chondrite in the 3.4 to 428 3.8 range (Sears

  584

  7

Fig. 1 :Fig. 2 :Fig. 3 :Fig. 4 :Fig. 5 :Fig. 6 :Fig. 7 :Fig. 8 :Fig. 9 :

 123456789 Figure captions:

Fig. 11 :

 11 Fig. 11: Chemical composition of Famenin in comparison with ordinary chondrites.

910Fig. 12 :Fig. 13 :

 1213 Fig. 12: Spectral parameters of Raman bands of carbonaceous materials in Famenin and

Fig. S3 :Fig. S4 :Fig. S5 :Fig. S6 :

 S3S4S5S6 Fig. S1: Famenin fall location.

990

  et al. (2003), and Gattacceca et al. (2014), respectively. Same data for Cali and Pavel are from Trigo-Rodríguez et al. (2009) and Dekov et al. (2017), 991 respectively. Magnetic susceptibility and saturation magnetization data of Tieschitz and Gursum from Rochette et al. (2003) and Gattacceca et al. (2014),

FFig. 12 :

 12 Fig. 12: Spectral parameters of Raman bands of carbonaceous materials in Famenin and in reference chondrites: FWHMD vs. ID/IG. Averages (points) and standard deviations (bars) are plotted for reference samples (black symbols) and for Famenin (open symbols). Spectral parameters of individual spectrum are plotted for Famenin (small grey diamonds). Reference chondrites data from Bonal et al. (2016). 160x144mm (220 x 220 DPI)

  Bonal et al. (2016) were used. Raman spectra of the 174 carbonaceous matter in Famenin were obtained both on isolated matrix grains and in-situ 175 in a polished section. A raw piece of approximately 200 mg was gently crushed. Around

	173 analytical conditions as in 176
	F o r
	P e
	e r
	R e
	v
	i e
	w
	O
		n l
		y
	7	Famenin-Pourkhorsandi et al

172

comparison with reference meteorites from the literature, the same experimental and

Table 2

 2 Fs 14.2±0.2 Wo 1.3±0.1 (n = 6), respectively (Table2). Cobalt concentration of kamacite in this

	F o r
	P e
	e r
	R e
	v
	i e
	w
	O
	n l
	y

). PMD for olivine and 288 low-Ca pyroxene is 0.8% and 3.5%, respectively. Average olivine and low-Ca pyroxene 289 compositions are Fa 22.5±0.2 (n =4) and Fs 18.3±0.8 Wo 1.1±0.9 (n = 5), respectively. The 290 average Co content of kamacite is 5.9 ± 0.9 mg/g (n = 24).

However, Cs content in 309 Famenin is closer to mean LL values than H and L chondrites. Lower concentrations of 310 Ba and Be and higher Sr and Nb in Famenin compared to the OCs are other noticeable

  -2 and B CR /B C = 26.5.

	349	Noble gas concentrations and isotopic ratios
	350	The measured isotopic noble gas concentrations of the three chondrites corrected
	351	from interferences from H2O + , 40 Ar ++ , and CO 2 ++ (on Ne isotopes) and for instrumental
	352	mass discrimination are presented in Table 5.
	353	The cosmogenic Ne concentrations and isotopic ratios (index "cos") have been
	354	calculated and are reported in Table 6; To calculate the cosmogenic Ne concentrations
	355	and isotopic ratios in Famenin, we estimate Ne is a mixture between cosmogenic and
	356 357 358	F o r SW endmembers ("SW" index). We assume ( 20 Ne/ 22 Ne) SW =13.78±0.03 and F ( 21 Ne/ 22 Ne) SW =0.0329±0.0001 (Heber et al. 2009) as the SW endmember. To calculate o r the cosmogenic Ne concentrations and isotopic ratios in EM 195, we estimate a mixture
	359 360	P e between three endmembers: cosmogenic, SW, and air, the latter being characterized by P e ( 20 Ne/ 22 Ne) air =9.80 and ( 21 Ne/ 22 Ne) air =0.029. And ( 20 Ne/ 22 Ne) cos =0.82 and
	361 362	e r ( 21 Ne/ 22 Ne) cos =0.89 corresponding to the measured concentrations in SJ 041 (Fig. 8). e r The determined cosmogenic ratios ( 22 Ne/ 21 Ne) cos vary between 1.12 for SJ 041, and
	363 364	R e 1.95-2.52 for EM 195 and Famenin. R e The measured 36 Ar/ 38 Ar and 40 Ar/ 36 Ar range from 3.96-5.04 and 90-535, respectively.
	365 366	v i e v In order to calculate the amount of cosmogenic 36 Ar cos and 38 Ar cos , we used a three-i e component deconvolution assuming that the isotopic compositions are a mixture
	367 368	w between cosmogenic, air, and SW endmembers. We used the following w ( 36 Ar/ 38 Ar) cos =0.63, ( 36 Ar/ 38 Ar) air =5.32, and ( 36 Ar/ 38 Ar) SW =5.47.
			O O
	311	differences between them. Besides differences in absolute concentrations, deviations n l n l
	312	also exist in elemental ratios such as Sr/Ba which is 4.4, higher than the mean value for y y
	313	H (2.4), L (3.0), and LL (2.3) chondrites.
	314	Oxygen isotopic composition
	315	The whole rock oxygen isotopic composition analysis results for two aliquots of
	316	Famenin along with the data for other H, L, and intermediate ordinary chondrites that we
	317	analyzed are reported in the Table 4. Fig. 7 depicts the Δ 17 O versus δ 18 O values of
	318	Famenin along with the data for H, L, LL, and H/L chondrites. Literature data for
		13	Famenin-Pourkhorsandi et al

300

The magnetic susceptibilities of EM 195 (W1) and SJ 041 (W2) are logχ = 4.99 and 301 logχ = 4.59, respectively.

302

Trace element bulk chemistry 303

The whole rock trace element composition of Famenin is reported in Table

1

. CI-304 normalized spider diagrams of Famenin along with the mean values reported for H, L, 305 and LL OCs (Wasson and Kallemeyn 1988) are shown in Fig. 6. Trace element content 306 of Famenin is chondritic and it follows the general trend of OCs. Some highly volatile 307 elements such as Rb, Li, Pb, and Ga in Famenin and OCs follow a similar enrichment 308 and depletion patterns in relation to mean CI chondrites.

The cosmogenic 36 Ar cos 369 and 38 Ar cos concentrations are reported in Table 6.

	380 410	L and LL chondrites (Wasson and Kallemeyn 1988) (Fig. 11b). Same applies for the Ga
	381 411	DISCUSSION content (4.9 µg/g), in relation to mean H (6 µg/g), L (5.7 µg/g) and L (5 µg/g) chondrites
	382 412	Classification of Famenin
	383	Considering its mineralogy, bulk rock chemical composition, low abundance of matrix,
	384	and oxygen isotopic composition, Famenin is undoubtedly an ordinary chondrite, but it
	385	shares properties with both H and L chondrites, making its classification problematic. Its
	386	average chondrule size is closer to the value for L chondrites than for H chondrites
	387 388 389	F o r (Metzler et al. 2018). On the other hand, average olivine and low-Ca pyroxene compositions are Fa 17.5±4.7 (n = 71) and Fs 16.8±7.5 Wo 4.3±5.9 (n = 35), respectively, in the range of H chondrites values (Fig. 9) (Bearley and Jones, 1998). Oxygen isotopic bulk F o r
	390 391 392 393 394 395 396 397 398	P e e r R e v i e w composition of Famenin is different from values measured in H chondrites (Fig. 7). Its P e Δ 17 O is in the low range for L chondrites; however, δ 18 O is higher in Famenin and is closer to the field of Tieschitz and Bremervӧrde H/L chondrites. The mean Co content in e r kamacite (4.7 mg/mg) is in the range of values reported for H chondrites (4.4-5.1 mg/g) (Fig. 10) (Afiattalab and Wasson 1980; Rubin 1990). The modal (Fe,Ni) metal abundance R e in Famenin is lower than the average H chondrite values (5 vol% versus 8 vol%) v (Weisberg et al. 2006). Magnetic susceptibility χ and saturation magnetization (M S ) are i e other proxies to the bulk metal content, and can be used for the classification of meteorites (Rochette et al. 2003; Gattacceca et al. 2014). Magnetic susceptibility of Famenin (logχ w
	370 371 399 400 401 372 403 402	Cosmic-ray exposure ages = 5.07) is intermediate between H (5.32 ± 0.10, n = 145 falls) and L chondrites (4.87 ± O n l O 0.10, n = 144 falls) , and similar to the magnetic susceptibility of Tieschitz (4.97) and Bremervӧrde (4.98) H/L chondrites (Rochette et al. 2003). Saturation magnetization of n l The CRE ages (Table 7) have been calculated using the concentrations in for L3 and L4 chondrites falls (22.1±5.1 Am 2 kg -1 , N = 7) and much lower than the values cosmogenic 3 He cos , 21 Ne cos , and 38 Ar cos , later labelled T 3 , T 21 , and T 38 , as described in y Famenin (M S = 24.9 Am 2 kg -1 ) is in the range of values reported in Gattacceca et al. (2014) y
	373 404	e.g. Li et al. (2017) and using correlations given by (Eugster 1988). Based on these for H3 and H4 falls (44.8±4.5 Am 2 kg -1 , N = 8). Hysteresis parameter ratios are similar to
	374 405	assumptions, CRE ages range from 4.99-8.71 Ma for SJ 041, with the common trend the values observed in L and H chondrites, reflecting a combination of kamacite and
	375 406	T 3 <T 21 <T 38 , from 17.7-59.2 Ma for EM 195, and finally from 47.4-66.4 Ma for Famenin. taenite (Fig. S5). With a Ni content of 13.1 mg/g compared to the average values of H
	376 407	Note that due to large discrepancies (most likely due to production rate calculation (16.0 mg/g), L (12.0 mg/g), and LL (10.2 mg/g) chondrites, Famenin is closer to the L
	377 408	issues and/or He diffusive losses), we did not report the 3 He CRE ages T 3 for EM 195 chondrite range (Fig. 11a,b). Its bulk Co content is 540 µg/g, which compared to the
	378 409	and Famenin. In addition, for these two chondrites, we observe that the calculated T 38 average values of H (810 µg/g), L (590 µg/g) and LL (490 µg/g) chondrites, lies in between
	379	ages are systematically lower than T 21 .
		14 15	Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al

  With a 20 Ne/22 Ne ratio of 0.82, we assume that Ne in SJ 041 is almost entirely 443 cosmogenic (with ( 20 Ne/ 22 Ne) cos ~0.80, e.g.,Leya et al., 2013). However, the measured 444 20 Ne/ 22 Ne ratios of 9.27 and 12.45 for EM 95 and Famenin, respectively, indicate that, in distinct from the pure SW signature with 20 Ne/ 22 Ne = 13.7 due to 448 fractionation processes. The measured 21 Ne/ 22 Ne ratios vary between 0.097 -0.19 for

	441	Gas compositions
	442
		F o r F o r
		P e P e
		e r e r
		R e R e
		v v
		i e i e
		w w
		O O
			n l n l
			y y
	440	chondrite.
		16	Famenin-Pourkhorsandi et al

430

(2018), Famenin is very weakly shocked (S2 shock stage). However, random troilite 431 polycrystalline texture in some parts (Fig.

3h

) might suggest a higher shock degree 432

(Ruzicka and Hugo 2018)

. Even though we did not study the two clasts visible in Fig.

1b

433 in detail, but the macroscopic studies by us and (McCausland et al., 2016), 434 heterogeneity observed in Raman spectroscopy data, and the noble gas compositions 435 of Famenin favors its classification as a breccia. It should be mentioned that as the 436 mentioned clasts are small relative to the bulk meteorite, in agreement with McCausland 437 et al. (2016), we believe that they would not affect our main conclusions regarding 438 Famenin's intermediate properties. 439 Putting all these data together, we classify Famenin as an H/L3 (S2) brecciated 445 addition to cosmogenic noble gases, there is as well a contribution from a trapped 446 component, here likely a solar wind (SW) contribution. The solar Ne isotopic ratios in 447 meteorites are always 449 Famenin and EM 195, respectively. These data are in relatively good agreement with 450 previous observations for other gas-rich meteorites, and consistent with a SW influence 451 (Talahito and Keisuke 2006; Leya et al. 2009). The Ne three-isotope plot (Fig. 8) shows 452 the Ne isotopic data (blank-and fractionation-corrected) for EM 195 and Famenin. The 453 Ne isotopic ratios from SW, from solar cosmic-ray production (SCR-Ne), from galactic 454 cosmic-ray production (GCR-Ne) and from air are also shown. From this plot, two 455 important observations can be made. First, one can notice that the Ne isotopic 456 composition of Famenin is a clear mixture between a cosmogenic component (here 457 GCR-Ne) and SW; second, it appears the isotopic composition of EM 195 is a mixture 458 between three components: cosmogenic, SW, and air. This is not surprising as EM 195 459 is a find which has been subjected to hot desert weathering and influenced by 460 atmospheric contamination. 461 The range of 36 Ar/ 38 Ar ratios clearly indicate the presence of a trapped component, 462 most likely atmospheric (SJ 041) and/or SW (presumably for EM 195 and Famenin).

463

The composition of the bulk SW, measured by Genesis is ( 36 Ar/ 38 Ar) SW = 5.47±0.01 464

[START_REF] Heber | 744 Noble gas composition of the solar wind as collected by the Genesis mission[END_REF]

; given the fact that only two Ar isotopes can be dominated by solar 465 signature (i.e.

36,38

Ar,

40

Ar is mainly radiogenic and dominated by decay of 40 K), an Ar 466 three-isotope plot would not, unlike Ne, help to decipher the Ar endmember 467 contributions (e.g.

Rao et al. 1991

). 468 Our gas data suggests that EM 195 and Famenin belong to a group of meteorites 469 called "gas-rich" meteorites, i.e., meteorites that contain large amounts of primordial 470 noble gases. Noble gas isotope records in gas-rich meteorites are explained by an 17 Famenin-Pourkhorsandi et al 471 incorporation of gases produced by solar wind (SW) radiations (Suess et al. 1964), for a 472 short period over few million years (Osawa and Nagao 2006). Gas-rich meteorites are 473

Table 5 ,

 5 EM 195 and Famenin contain solar-wind implanted noble gases, with e.g., 482 20 Ne/ 22 Ne ratios of 9.27 and 12.45, respectively. Note that the solar 20 Ne/ 22 Ne

483 endmember of 12.45 measured for Famenin is in really good agreement with the range 484 of values of e.g.

, 11.6 -11.9 in Fayetteville (Wieler at al., 1989)

or 12.4 in Frontier 485

  , both meteorites have 488 20 Ne/22 Ne ratios which exceed the required conditions (i.e.,20 Ne/ 22 Ne >2; 36 Ar/ 38 Ar and Famenin, with 20 Ne/ 22 Ne ratios of 9.27 and 12.45, respectively, and 493 36 Ar/ 38 Ar of 4.74 and 5.04, respectively (see Table5). Consequently, the CRE ages for -capture produced 36 Cl, the amount of calculated trapped Ar can be 502 overestimated therefore leading to wrong T 38 ages. Given that the amount of neutron-

	Page 31 of 78		Running Head
	501 decay of neutron503 capture nuclides increase with both size and shielding depth, calculation of CRE ages
	504	can be disturbed in the cases of large objects. Finally, one also has to bear in mind that
	505	the calculation of CRE ages for solar gas-rich meteorites is likely to be affected by
	506	erroneous shielding corrections. However, calculated T 38 age seems quite consistent in
	507	the case of SJ 041. Additionally, one can invoke heterogeneities in the chemical
	508 509 510	composition within the samples, and in particular in the target elements for the F production of 38 Ar (e.g., Ca), which could lead to some discrepancies. Note that we only o r measure samples between ~ 3 -5 mg, which might introduce a bias considering the
			P e
			e r
			R e
			v
			i e
			w
			O
				n l
				y
	525	of the trapped component. A small cluster at ~ 60 Ma is observed (only 7 H chondrite
	496 526	ages when evoking the CRE ages of EM 195 and Famenin. members), except for H3 ordinary chondrites where such a peak is absent (Graf and
	497 527	Regarding lower T 38 than T 21 for EM 195 and Famenin, this trend has been already Marti, 1995). Such old CRE ages would therefore suggests that EM 195 and Famenin
	498 528	reported by Osawa and Nagao (2006). Several reasons can be invoked to explain this may originate from a different parent body, or that both of the meteorites result in a
		18	Meteoritics & Planetary Science	Famenin-Pourkhorsandi et al

489

>4.39) defined by the authors. Based on their work, only meaningful cosmogenic 490 concentrations and hence CRE ages can be calculated if the uncertainties due to the 491 corrections of the trapped component are moderate. This is obviously not the case for 492 both EM 195 494 EM 195 and Famenin suffer from high uncertainties and should be considered with 495 extreme caution. We will therefore refer in the following discussion as "nominal" CRE 499 trend: first, by underestimating the 38 Ar production rates. As explained in Graf and Marti 500 (1995), for shielding conditions where e.g., contributions of 36 Ar are due to radioactive 511 bulk composition of the meteorite, whereas the equations used for the production rates 512 are for bulk compositions (e.g. Di Gregorio et al. 2019). 513 The nominal CRE ages for Famenin and EM 195 are generally older than the 514 average values reported for H or L chondrites (Graf and Marti 1995; Marti and Graf 515 1992). The CRE age histogram for H chondrites in characterized by major peak 516 centered around 6 -10 Ma and another cluster identified around 33 Ma (Graf and Marti, 517 1995; Herzog and Caffee, 2014). Older CRE ages (i.e., T>40Ma) are observed to a 518 lesser extent. Interestingly, the petrologic type H3 (to which Famenin belongs) has CRE 519 age spanning from 5 -40 Ma, without showing any cluster for CRE ages greater than 40 520 Ma (Herzog and Caffee, 2014). Our nominal CRE age data suggest that both Famenin 521 and EM 195 were ejected at ~ 60 Ma, during an impact event different from those 522 responsible for the ejection of the majority of H and L chondrites (Graf and Marti, 1995; 523 Herzog and Caffee, 2014). However, as mentioned earlier in the discussion, these CRE 524 ages are just nominal, and might suffer from high uncertainties due to huge corrections 529 slight deviation from the expected exponential distribution of ordinary chondrites 530

  [START_REF] Grossman | White paper report for the Nomenclature Committee 739 on the composition of olivine and pyroxene in equilibrated ordinary chondrites[END_REF]. More importantly, its oxygen isotopic composition, especially Δ 17 O is 563 close to the field of Tieschitz, Bremervӧrde, and Famenin. For weathered meteorites,

	Page 33 of 78		Running Head Running Head	Page 32 of 78
	531 561	Chondrites intermediate between H and L groups the Meteoritical Bulletin Nomenclature Committee for L chondrites (Grossman and
	532 562		Mineralogical and oxygen isotope evidence indicate that ordinary chondrites
	533	originated from multiple parent bodies (Greenwood et al. 2020). In addition to the
	534 564	traditional H-L-LL sequence, accretion of ordinary chondrite parent bodies in conditions heavier composition (higher δ 18 O) can be explained by their high weathering degree
	535 565	more reduced than for H chondrites, and intermediate between the three main groups which is shown to alter oxygen isotopic composition in this manner (Clayton and
	536 566	(H/L and L/LL) have been described (Kallemeyn et al. 1989; Trigo-Rodríguez et al. Mayeda 1991) or differences in the metamorphic history or conditions, or even pre-
	537 567	2009; Wittmann et al. 2011; Pourkhorsandi et al. 2017; Pratesi et al. 2019; Greenwood metamorphic alteration history (Reimold et al., 2004). As for SJ 041, the weathering
	538 539 568 569 570	F o r et al. 2020). This is in agreement with models indicating that the three main OC groups are portions of an incompletely sampled fractionation sequence (e.g., Müller et al., products (oxides/oxyhydroxides) were removed before the isotopic analysis, the first F scenario is less likely to be responsible for its relatively heavier composition. Such o r classification complications also is the case for EM 195 which with an intermediate log χ
			P e P e
			e r e r
			R e R e
			v v
			i e i e
			w w
			O O
				n l n l
				y y
	556	(Gattacceca et al., 2014; Dekov et al., 2017). However, for SJ 041 because of its
	557	significant terrestrial weathering (W2 grade) this value cannot be interpreted as robustly
	558	in terms of original metal content, but it is more in agreement with L chondrite values
		19 20	Meteoritics & Planetary Science Meteoritics & Planetary Science	Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al

540

1971). Based on this evidence,

[START_REF] Greenwood | Linking asteroids and 736 meteorites to the primordial planetesimal population[END_REF]

suggest between 3 to 6 parent 541 bodies as the source of ordinary chondrites. Considering the gradual oxygen fugacity 542 changes between different regions in the Solar nebula (e.g., Rubin 1990), the 543 occurrence of meteorites originating from parent bodies with intermediate compositions 544 between H and L chondrites is reasonable

[START_REF] Kallemeyn | Ordinary chondrites: 752 Bulk compositions, classification, lithophile-element fractionations and composition-753 petrographic type relationships[END_REF] Trigo-Rodríguez et 545 al. 2009; Wittmann et al. 2011;[START_REF] Greenwood | Linking asteroids and 736 meteorites to the primordial planetesimal population[END_REF]

). Based on their fall date 546 (between May and July), Trigo-Rodríguez et al. (2016) went further and suggested that 547 Bremervörde, Tieschitz, Cali, and Famenin originated from a high-inclination stream of 548 meteoroids formed as a result of disruption of comet C/1919 Q2 Metcalf. However, 549 these meteorites do not have the expected properties of cometary materials (Campins 550 and Swindle 1998; Greenwood et al. 2020). 551 In addition to Famenin, our work on Bremervӧrde, EM 195, and SJ 041 shows that 552 these meteorites too have intermediate characteristics. One piece of evidence is the 553 magnetic susceptibility values of Tieschitz, Bremervӧrde, Famenin, EM 195, and SJ 041 554 which are intermediate between mean H and L chondrite values (Rochette et al., 2001). 555 It is also the case for some the samples with available saturation magnetization data 559 (Rochette et al. 2012). SJ 041's Fa and Fs values are near the lower limits of L 560 chondrites (Brearley and Jones 1998), but still are outside the limits recommended by 571 has average olivine and low-Ca pyroxene compositions of Fa 16.9±6.0 (n = 13) and 572 Fs 17.2±5.6 Wo 17.2±5.9 (n = 10), respectively that are in the range of H chondrites values 573 (Brearley and Jones 1998). Meanwhile, similar to Famenin its average chondrule size is 574 higher than in H chondrites. Oxygen isotopic composition of EM 195 is outside the 575 range of equilibrated H and L chondrites. It should be noted that since the Bremervӧrde 576 (H/L3.9), Tieschitz (H/L3.6), EM 195 (H/L3) and Famenin (H/L3.5/3.7) chondrites are 577 unequilibrated their oxygen isotope composition is expected to show a larger scatter 578 than for equilibrated ordinary chondrites, which prevents robust conclusions to be drawn 579 from this dataset. The other interesting case is Gursum that caught our attention 580 because of its intermediate log χ (5.09) (Rochette et al. 2003) and saturation 581

  Table 8 lists 66 meteorites classified as intermediate chondrites in the Meteoritical 593 Bulletin Database Database as of October 2021. The commonly used H/L designation is 594 ambiguous. As described by[START_REF] Kallemeyn | Ordinary chondrites: 752 Bulk compositions, classification, lithophile-element fractionations and composition-753 petrographic type relationships[END_REF], H/L refers to the chondrites with

	592
	595	bulk chemical properties intermediate between H and L chondrites. However, H/L is
	596	also often used by classifiers to describe meteorites whose assignation to H or L group
	597	is unclear, with a meaning close to the H(L) or L(H) classification. While some well-
	598	described meteorites such as Bremervörde, Cali, LaPaz Icefield (LAP) 031047 and
	599 600 601	Tieschitz are classified as H/L chondrites based on their truly intermediate F characteristics (Kallemeyn et al. 1989; Trigo-Rodríguez et al. 2009; Wittmann et al. o r 2011), the majority of meteorites classified as H/L are simply H or L chondrites that
		P e
		e r
		R e
		v
		i e
		w
		O
			n l
	615		y
	588	Pavel is an anomalous H3 chondrite that has an intermediate log χ (5.11) and saturation
	589	magnetization (M S = 26 Am 2 kg -1 ) in the range of L3 and L4 chondrites falls (Gattcceca
		21	Famenin-Pourkhorsandi et al

590 et al., 2014), but its δ 18 O is higher than H chondrites without a similarity to the 591 intermediate chondrites studied here. 602 have actually not been classified thoroughly for one or several reasons: unequilibrated 603 mineral composition and low number of analyzed minerals, no estimate of chondrule 604 size, lack of mineral chemistry data, and high weathering grade which decreases the 605 efficiency of magnetic classification. Based on the characteristics of truly intermediate 606 H/L chondrites (Bremervörde, Cali, EM 195, Famenin, LaPaz Icefield (LAP) 031047, SJ 607 041, and Tieschitz), we define ranges for their different characteristics as an attempt to 608 identify the "real" intermediate H/L chondrites in the meteorite collection. We define the 609 following criteria (Table 9): magnetic susceptibility (logχ) in the 4.95 -5.20 range, for 610 equilibrated ones (type 4 or higher) an average Fa content in the 20 -24 mol% range, 611 average apparent chondrule size in the L chondrites range (~ 500 µm), and Δ 17 O 612 between 0.8 and 1.2 ‰. After filtering out the poorly classified meteorites, we are left 613 with a population of 36 H/L chondrites possibly truly distinct from H and L chondrites 614 corresponding to 0.0006% of the total number of classified ordinary chondrites (56417),

  that have average Fa values of ~ 20, consistent with H chondrites, while average 624 Fs value of ~ 20.4 and out of the range of H chondrites. Other characteristics for HL

	Page 35 of 78		Running Head
	623 653 654 681 682 818 846 847 (HL6) 625 sampled. We propose to use a new designation (HL) for these meteorites rather than the ambiguous H/L designation that is also and mostly used for rather poorly and Colin F. 2006. Oxygen isotope analyses of fine silica grains using laser-extraction technique: Comparison with oxygen isotope data obtained from ion Sears D. W., Grossman J. N., and Melcher C. L. 1982. Chemical and physical studies of Weisberg M. K., Ebel D. S., Nakashima D., Kita N. T., and Humayun M. 2015. Petrology and geochemistry of chondrules and metal in NWA 5492 and GRO 95551: A new chondrites, such as oxygen isotopic composition, siderophile content, and metal 655 characterized meteorites that could be either H or L chondrite. Following previous works 683 microprobe analyses and application to quartzite and silcrete cement investigation. 848 type of metal-rich chondrite. Geochimica et Cosmochimica Acta 167:269-285.
	626 656 684 849	abundance, suggest that they are indeed distinct chondrites. Considering the fact that on the diversity of ordinary chondrites, this work emphasizes again the existence of Geochimica et Cosmochimica Acta 70:2827-2835. Wieler R., Baur H., Pedroni A., Signer P., and Pellas P. 1989. Exposure history of the
	627 657 685 850	meteorites are being classified mostly based on their olivine and low-Ca compositions, it more than the three ordinary chondrite groups H, L, and LL, with possibly more than Bonal L., Quirico E., Flandinet L., and Montagnac G. 2016. Thermal history of type 3 regolithic chondrite Fayetteville: I. Solar-gas-rich matrix. Geochimica et
	628 658 686 851	is possible that some unequilibrated HL chondrites have been overlooked and classified three associated parent bodies. Measuring oxygen isotopic composition of equilibrated chondrites from the antarctic meteorite collection determined by Raman Cosmochimica Acta 53:1441-1448.
	629 630 631 632 659 687 852 660 661 662 853	F o r either as H3 or L3 chondrites. The existence of ordinary chondrites with properties outside of the usual ranges, such as the HL chondrites, can be accounted for by the existence of more than three parent bodies or by compositional heterogeneity of the three main parent bodies. This F o r HL chondrites, and CRE ages of a larger population of HL chondrites may help to test this hypothesis. spectroscopy of their polyaromatic carbonaceous matter. Geochimica et Wittmann A. et al. 2011. H/L chondrite LaPaz Icefield 031047 -A feather of Icarus? F o r F o r F o r F o r F o r F o r r o F Geochimica et Cosmochimica Acta 75:6140-6159.
			P e P e P e P e P e P e P e P e P e
			e r e r e r e r e r e r e r e r e r
			R e R e R e R e R e R e R e R e R e
			v v v v v v v v v
			i e i e i e i e i e i e i e i e i e
			w w w w w w w w w
			O O O O O O O O O
	644			n l n l n l n l n l n l n l n l n l
	645	CONCLUSIONS		y y y y y y y y y
	646	Famenin meteorite is a type 3.4/3.8 OC with characteristic distinct from the H and L
	647	chondrites. In addition to its primary characteristics (metal content, chondrule size, bulk
	648	composition, oxygen isotope composition, olivine and low-Ca pyroxene compositions
	649	etc.), Famenin's noble gas composition and CRE age distinguish it from the majority of
		22 23 24 28 29 30	Meteoritics & Planetary Science	Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al

633

latter hypothesis would require extending the accepted ranges for the three main 634 groups. Discriminating between the two hypotheses require a more detailed 635 investigation using a larger and a multi-proxy database.

636

Hints for the existence of an HL chondrite cluster in the oxygen isotope dataset (Fig. 637

7) suggest that analyses of more equilibrated HL chondrites should be undertaken to 638 validate the difference in oxygen isotopic composition between these chondrite and H-L-639 LL sequence. This also applies for noble gas composition measurements and CRE age 640 distribution and comparison with those of the main ordinary chondrite groups. In 641 addition, measurements of bulk rock and (Fe,Ni) metal compositions of the anomalous 642 and intermediate ordinary chondrites would be helpful to unravel their relationship with 643 the three main groups. 650 H and L chondrites. Famenin along with 36 similar OCs might be member of another 651 ordinary chondrite group originating from a different parent body than H, L, and LL 652 chondrites, or originating from regions of these parent bodies that have rarely been 854 Wlotzka F. 1993. A weathering scale for the ordinary chondrites. Meteoritics 28:460.

Table 8

 8

) chondrites. Ordinary chondrites with compositions intermediate between H 917 and L are shown as HL (more details in text). Only ordinary chondrites with petrologic 918 types ≥4 are included. Data source: (https://www.lpi.usra.edu/meteor/).

Table 1 (

 1 Pourkhorsandi et al.): Trace element (µg/g) determined by ICP-MS for 957 Famenin and Allende as reference sample. Allende composition is reported from theThe unit is µg/g. aJarosewich et al. 1987. b Friedrich et al. 2003. c Dauphas and Pourmand 2015.

	Page 47 of 78

Table 2 (

 2 Pourkhorsandi et al.):Representative olivine and low-Ca compositions (in wt%) fromFamenin, EM 195, and SJ

							Running Head					Page 50 of 78
	962	041.
			SiO 2	Al 2 O 3	TiO 2	FeO	Cr 2 O 3	MnO	MgO	CaO	Total	Fa (mol%)	Fs (mol%)
		Famenin	41.90	0.04	0.03	6.11	0.65	0.43	49.99	0.09	99.25	6.39	-
			41.59	1.55	0.01	12.27	0.11	0.28	44.84	0.13	100.78	13.26	-
			40.79	0.03	0.00	14.40	0.14	0.27	45.45	0.10	101.18	15.05	-
			40.04	b.d.l.	b.d.l.	15.45	0.33	0.31	43.35	0.11	99.53	16.60	-
			39.81	0.03	0.03	15.63	0.17	0.30	43.70	0.13	99.79	16.65	-
			39.31	0.03	b.d.l.	16.69	0.06	0.28	42.91	0.07	99.35	17.85	-
			39.43	0.04	0.01	16.90	0.02	0.59	42.59	0.02	99.60	18.09	-
			39.86	b.d.l.	0.11	17.04	0.03	0.46	42.89	0.03	100.39	18.13	-
			39.95	0.01	0.02	17.06	0.00	0.38	42.78	0.02	100.22	18.20	-
			39.75	b.d.l.	0.01	17.09	0.02	0.45	42.36	0.03	99.71	18.37	-
			39.39	0.00	0.03	17.04	b.d.l.	0.50	42.16	0.01	99.12	18.38	-
			39.75	0.01	0.02	17.21	0.03	0.48	42.54	b.d.l.	100.03	18.40	-
			39.43	0.01	0.03	17.25	0.01	0.51	41.98	0.01	99.23	18.63	-
			39.52	0.02	0.02	17.37	0.00	0.43	42.28	0.04	99.68	18.64	-
			39.18	0.05	0.07	17.28	0.07	0.48	41.86	0.05	99.04	18.70	-
			40.13	0.05	0.02	17.20	0.37	0.42	41.55	0.05	99.79	18.75	-
			39.05	0.04	0.06	17.34	0.24	0.48	41.67	0.01	98.90	18.82	-
			39.36	b.d.l.	0.04	17.62	0.03	0.49	42.13	0.00	99.64	18.90	-
			40.17	0.25	0.04	17.38	0.15	0.47	41.20	0.08	99.74	19.03	-
			39.06	0.00	b.d.l.	18.11	0.00	0.45	41.76	0.01	99.37	19.47	-
			38.16	0.10	0.00	22.53	0.22	0.30	38.17	0.07	99.54	24.79	-
			58.67	0.36	0.07	3.63	1.11	0.58	34.16	1.97	100.56	-	6.27
			58.80	0.11	0.03	4.17	0.31	0.29	36.36	0.26	100.33	-	6.41
			56.77	0.14	0.13	10.88	0.12	0.52	30.99	0.68	100.21	-	16.90
			56.61	0.82	0.11	11.31	0.98	0.29	29.69	0.97	100.77	-	17.71
			55.11	0.05	0.01	17.62	0.59	0.66	25.44	0.29	99.78	-	28.67
							Meteoritics & Planetary Science

Table 3 (

 3 Pourkhorsandi et al.): (Fe,Ni) metal compositions (in wt%) in Famenin, EM 195, Gursum, and SJ 041.

						Running Head			Page 52 of 78
	Meteorite	Fe	Co	Ni	Total	Meteorite	Fe	Co	Ni	Total
	Famenin	96.79	0.58	3.22	100.58	EM 195	93.71	0.30	6.65	100.66
		95.52	0.70	4.64	100.87		93.37	0.36	6.69	100.43
		94.99	0.75	5.21	100.95		93.32	0.20	6.67	100.48
		94.88	0.34	5.42	100.65		93.30	0.29	7.11	100.70
		94.48	0.34	6.64	101.4		92.65	0.28	6.72	99.65
		94.36	0.49	6.07	100.92		92.57	0.32	7.18	100.07
		93.86	0.56	6.70	101.11		92.36	0.34	7.09	99.78
		93.36	0.30	6.65	100.31		91.55	0.28	6.85	98.68
		93.16	0.48	6.40	100.04	Gursum	93.97	0.30	6.50	100.76
		93.16	0.25	6.89	100.29		93.24	0.15	6.41	99.80
		92.81	0.34	6.74	99.89		93.23	0.29	6.28	99.80
		92.63	0.30	6.85	99.78		93.00	0.23	6.31	99.53
		92.19	0.29	6.72	99.21		92.23	0.29	6.24	98.76
		91.90	0.59	6.11	98.60		91.84	0.41	6.73	98.98
		75.40	0.19	25.27	100.86		91.71	0.17	6.42	98.30
		72.80	0.22	27.81	100.82		91.68	0.21	6.26	98.15
						Meteoritics & Planetary Science

Table 4 (Pourkhorsandi et al.):

 4 Results of the whole rock oxygen isotopes analyses.

	Page 53 of 78					Running Head
		Group				Bulk
			δ 18 O	δ 17 O	Δ 17 O	sample mass
	Meteorite		(‰)	(‰)	(‰)	(mg)
	Bremervörde	H/L3	5.53	3.84	0.96	27
	El Médano 195	H/L3	5.01	3.41	0.81
	Famenin	H/L3	5.73	3.98	1.00	51
		H/L3	5.17	3.65	0.97	51
	Gursum	H5-an	4.28	3.35	1.12
	Pavel	H3-an	5.05	3.26	0.63	27
	Ochansk	H4	4.33	2.97	0.72	59
	Homestead	L5	5.41	3.87	1.06	119
	Paranaiba	L6	4.99	3.71	1.11	80
	San Juan 041	H/L6	5.99	4.14	1.02
	970
					Meteoritics & Planetary Science

Table 5 (

 5 Pourkhorsandi et al.):Measured He, Ne, and Ar concentrations and isotopic ratios in the studied meteorites.The given uncertainties (1σ) include the uncertainties for the ion current measurements and uncertainties caused by the corrections for interfering isotopes and 973 corrections for instrumental mass fractionation. Systematic uncertainties in the calibration standard are included; they amount to about 4% for concentrations and

		Meteorite	Mass (mg)	3 He (10 -8 cm 3 STP/g)	3 He/ 4 He (×10 -4 )	20 Ne (10 -8 cm 3 STP/g)	20 Ne/ 22 Ne	21 Ne/ 22 Ne	38 Ar (10 -8 cm 3 STP/g)	36 Ar/ 38 Ar	40 Ar/ 36 Ar
		SJ 041	5.43	8.02±0.30	0.095±0.004	1.16±0.13	0.82±0.02	0.89±0.02	0.63±0.06	3.96±0.57	250±36
		EM 195	3.06	0.28±0.03	6.65±0.13	60.2±6.9	9.27±0.02	0.19±0.01	2.62±0.27	4.74±0.69	535±78
		Famenin	3.60	0.98±0.08	3.27±0.04	80.1±9.1	12.45±0.02	0.097±0.005	2.46 ±0.25	5.04±0.73	90±13
	972
	974	1% for isotope ratios.
	975
	976

Table 6 (

 6 Pourkhorsandi et al.): Cosmogenic He, Ne, and Ar concentrations and isotopic ratios in the studied meteorites.

	Meteorite	Mass (mg)

3 He

cos * (10 - 8 cm 3 STP/g) 3 He/ 4 He (×10 -4 ) 21 Ne cos (10 - 8 cm 3 STP/g) ( 22 Ne/ 21 Ne) cos 36 Ar cos (10 - 8 cm 3 STP/g) 38 Ar cos

	San Juan 041	5.43	8.02±0.30	0.095±0.004	1.76±0.20	1.12±0.06	0.232±0.026	0.368±0.042
	El Médano195	3.06	0.28±0.03	6.65±0.13	1.13±0.13	1.95±0.10	0.116±0.013	0.184±0.021
	Famenin	3.60	0.98±0.08	3.27±0.04	0.52±0.06	2.52±0.13	0.205±0.023	0.325±0.037

Table 7 (

 7 Pourkhorsandi et al.): Production rates P 3 , P 21 , and P 38 (10 -8 cm 3 STP/g/Ma) and cosmic-ray exposure ages T 3 , Dar al Gani, b El Médano, c Jiddat al Harasis, d LaPaz Icefield, e Northwest Africa, f San Juan, g Sayh al Uhaymir, h Yamato.989Data source: Meteoritical Bulletin. Mineral chemistry, magnetic susceptibility, and saturation magnetization data for Bremervörde are fromRubin (1990), Rochette

	983	T 21 , and T 38 (Ma).
		Meteorite	Mass (mg)	P 3	T 3	P 21	T 21	P 38	T 38
		SJ 041	5.43	1.61±0.06	4.99±0.60	0.332±0.004	5.30±0.6	0.042±0.005	8.71±0.99

Table 9 (Pourkhorsandi et al.):

 9 Suggested criteria for classifying HL chondrites.

		Running Head	Page 58 of 78
	Criteria	Suggested values
	Magnetic susceptibility (log χ)	4.95-5.20
	Average chondrule size (µm)	~ 500
	Fa content (mol%)	20-24
	Δ 17 O (‰)	0.8-1.2
	995
	996
	997
		Meteoritics & Planetary Science

Table 1S (

 1S Pourkhorsandi et al.): (Fe,Ni) metal compositions (in wt%) of Catalina 396, Taqtaq-e Rasoul, Agen, Andila, 999 Djadjarm, Ausson, and Bensour.

	Page 59 of 78					Running Head Running Head	Page 60 of 78
	1002	Andila (L6)	92.99	6.17	0.73	99.86
		Andila (L6)	93.60	5.98	0.77	100.40
		Andila (L6)	Fe 93.93	4.82	0.96	99.79
		Meteorite Andila (L6)	(wt%) 93.95	Ni (wt%) 6.47	Co (wt%) 0.80	Total 101.25
		Catalina 396 (H6) Catalina 396 (H6) Taqtaq-e Rasoul (H5) Taqtaq-e Rasoul (H5) Taqtaq-e Rasoul (H5) Taqtaq-e Rasoul (H5) Taqtaq-e Rasoul (H5) Taqtaq-e Rasoul (H5) Taqtaq-e Rasoul (H5) Taqtaq-e Rasoul (H5) Taqtaq-e Rasoul (H5) Agen (H5) Agen (H5) Agen (H5) Agen (H5) Agen (H5) Agen (H5) Bensour (LL6) Andila (L6) Djadjarm (L6) Djadjarm (L6) Djadjarm (L6) Djadjarm (L6) Djadjarm (L6) Djadjarm (L6) Ausson (L5) Ausson (L5) Ausson (L5) Ausson (L5) Ausson (L5) Ausson (L5) Bensour (LL6) Bensour (LL6)	94.44 95.16 66.65 67.68 68.03 93.85 93.92 94.09 94.34 94.75 94.79 50.11 92.01 93.28 93.35 93.50 93.58 62.86 F o r P e e r R e v i e w 6.86 0.43 101.73 7.09 0.52 102.76 34.97 b.d.l. 101.52 32.84 0.15 100.67 32.30 0.14 100.55 6.46 0.35 100.76 6.68 0.42 100.99 6.42 0.35 100.85 6.48 0.31 101.16 6.38 0.59 101.71 5.76 0.16 100.73 48.43 b.d.l. 98.53 5.97 0.38 98.83 6.29 0.40 100.01 6.09 0.27 99.79 6.19 0.37 100.01 5.71 0.51 0.03 b.d.l. 97.83 99.82 94.04 6.61 0.45 101.07 46.13 51.74 0.03 97.91 58.03 32.06 0.03 90.17 61.28 37.08 0.03 98.47 94.39 6.72 0.96 102.19 94.49 6.32 0.70 101.55 95.18 6.10 0.86 102.10 58.92 37.54 0.04 96.54 59.63 38.35 b.d.l. 97.93 65.85 32.33 0.03 98.29 66.47 31.32 0.08 97.89 77.99 18.59 0.73 97.42 78.67 18.55 0.56 97.81 51.09 45.94 1.74 98.85 51.59 45.98 1.81 99.29 F o r P e e r R e v i e w	O n l y O n l y
		Agen (H5) Bensour (LL6)	93.92 63.05	5.71 b.d.l.	0.47 b.d.l.	100.09 98.18
		Bensour (LL6)	63.38	0.00	0.06	98.57
		Andila (L6) Bensour (LL6)	44.56 63.55	54.19 b.d.l.	0.19 b.d.l.	98.97 98.70
	1000	Andila (L6) b.d.l. = below detection limit. Detection limits (wt%) = Fe (0.21), Co (0.18), Ni (0.18). 60.32 38.40 0.12 98.93
		Andila (L6)	72.70	26.61	0.23	99.49
	1001	Andila (L6)	74.54	25.58	0.49	100.65
		46 47			Meteoritics & Planetary Science Meteoritics & Planetary Science	Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al

Table 2S (

 2S Pourkhorsandi et al.): Whole-rock oxygen isotopes composition of ordinary chondrites. Data source: Clayton & Mayeda (1991) and Meteoritical Bulletin Database (https://www.lpi.usra.edu/meteor/).

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		Križevci Bjurböle Nan Yang Po Hamlet	H6 L4 L6 LL4	3.99 4.90 4.40 5.31	2.76 3.55 3.26 4.12	0.68 1.00 0.97 1.36
		Towada Clarendon (c) NWA 8684 Savtschenskoje	H6 L4 L6 LL4	4.04 4.88 5.15 5.10	2.79 3.66 3.88 3.94	0.69 1.13 1.20 1.28
	1003	Meteorite Dhajala Sharps Queen's Mercy Xingyang Cynthiana NWA 13194 Soko Banja NWA 13195 Witsand Farm NWA 2898 Kendleton NWA 13196 Guidder RaSa 430 JaH 567 NWA 1709 NWA 3358 NWA 8061 Bath Beaver Creek Kesen Ochansk Tysnes Island Weston Thuathe Carancas Allegan Ambapur Nagla Beardsley Forest Vale Glenrothes Leighton Mason Gully Pantar Richardton Tamdakht Cape Girardeau Charsonville Dhofar 1559 Guareña Kernouve Mount Browne NWA 4226 NWA 4229 NWA 7024 NWA 8400 NWA 12236 Bremervörde Tieschitz Aba Panu Catalina 001 Dhofar 2056 Hallingeberg Khohar Mezö-Madaras NWA 6744 NWA 6745 NWA 6864 NWA 6925 NWA 8257 NWA 8258 NWA 8276 NWA 10774 RdDL 067 SaU 564 Hedjaz Atarra Saratov Tennassilm NWA 10954 NWA 7556 Ausson Barwell Borkut Chervettaz Elenovka Ergheo Farmington Homestead Knyahinya Mifflin NWA 11744 NWA 11745 NWA 12386 NWA 13192 NWA 13193 Park Forest Qidong Mocs Tathlith Tillaberi Viñales Xiujimgin Dhofar 008 PAT 91501 Bishunpur Chainpur Krymka Manych Ngawi NWA 2748 NWA 3260 NWA 4522 NWA 6082 NWA 6742 NWA 6867 NWA 8059 NWA 8124 NWA 8649 NWA 10786 NWA 8691 Khanpur Olivenza Paragould Siena Appley Bridge Bensour Dhurmsala Dongtai Ensisheim Jelica Mangwendi NWA 6503 NWA 7988 NWA 12575 St. Mesmin Saint-Séverin Vavilovka NWA 969 JaH 513 NWA 6426 Renchen Parnallee NWA 7030 Bachmut SaU 565 NWA 10103 Bori Semarkona NWA 12534 Cabezo de Mayo St. Mary's County NWA 12921 Katol Leighlinbridge Modoc (1905) Bo Xian Albareto Vicência	Class H3 H3 H6 H6 L4 L6 LL4 L6 LL4 H7 L4 L6 LL4-6 H3 H3 H3 H3 H3 H4 H4 H4 H4 H4 H4 H4/5 H4/5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H5 H6 H6 H6 H6 H6 H6 F o r P e e r R e v i e w  18 O  17 O  17 O 4.12 2.84 0.70 3.95 2.70 4.08 2.84 0.72 3.89 2.83 5.44 3.91 4.98 3.67 1.08 4.85 3.85 1.33 1.08 4.85 3.61 1.09 5.32 4.12 1.35 0.81 4.4 2.90 0.62 4.61 3.43 1.03 5.20 3.83 1.12 4.77 3.67 1.19 0.65 5.12 3.17 0.51 5.55 3.63 0.74 4.45 2.84 0.53 4.67 2.91 0.48 5.78 3.32 0.32 4.19 2.89 0.71 4.27 2.98 0.76 4.51 2.98 0.63 3.85 2.82 0.82 4.19 2.88 0.70 4.08 3.00 0.88 4.55 3.12 0.75 4.43 2.98 0.68 3.97 2.68 0.61 3.94 2.80 0.75 4.20 2.93 0.75 3.82 2.64 0.65 4.21 2.69 0.50 3.87 2.88 0.87 4.42 3.04 0.74 4.09 2.69 0.56 4.08 2.74 0.61 5.01 3.26 0.65 3.79 2.69 0.72 3.83 2.64 0.65 4.62 3.00 0.59 4.10 2.89 0.76 4.15 2.94 0.78 3.88 2.71 0.69 H7 4.64 3.18 0.77 H7 4.40 3.03 0.74 H7 4.24 2.83 0.63 H7 4.64 2.93 0.52 H7 4.50 2.94 0.60 H/L3 4.57 3.35 0.97 H/L3 5.55 3.83 0.94 L3 5.08 3.68 1.04 L3 5.15 3.66 0.98 L3 4.74 4.03 1.57 L3 4.79 3.33 0.84 L3 4.52 3.48 1.13 L3 4.81 3.45 0.95 L3 5.05 3.43 0.80 L3 5.26 3.54 0.80 L3 5.87 3.84 0.79 L3 5.57 4.04 1.14 L3 4.64 3.27 0.86 L3 5.38 3.66 0.86 L3 4.79 3.05 0.57 L3 5.39 3.84 1.04 L3 5.48 3.77 0.92 L3 4.83 3.63 1.12 L3-6 4.57 3.51 1.13 L4 4.88 3.68 1.14 F o r P e e r R e v i e w L4 4.74 3.48 1.02 L4 4.56 3.52 1.15 L4 4.05 3.11 1.01 L4-6 5.36 3.87 1.08 L5 4.60 3.53 1.14 L5 4.63 3.57 1.17 L5 4.61 3.46 1.06 L5 4.64 3.66 1.25 L5 4.56 3.44 1.07 L5 5.00 3.58 0.98 L5 4.80 3.63 1.13 L5 4.62 3.52 1.12 L5 4.99 3.64 1.05 L5 4.84 3.65 1.13 L5 5.14 3.78 1.11 L5 4.93 3.69 1.13 L5 4.81 3.55 1.05 L5 5.23 3.88 1.16 L5 4.78 3.64 1.16 L5 4.69 3.44 1.00 L5 4.95 3.66 1.09 L5-6 4.55 3.50 F o r P e e r R e v i e w L6 4.33 3.40 1.15 L6 4.54 3.33 0.97 L6 4.54 3.48 1.12 L6 4.51 3.41 1.06 L7 5.67 3.81 0.86 L7 4.7 3.7 1.26 LL3 6.00 4.11 0.99 LL3 5.72 4.01 1.04 LL3 5.60 4.09 1.18 LL3 5.37 3.75 0.96 LL3 5.40 3.98 1.17 LL3 7.21 4.89 1.14 LL3 5.65 3.57 0.63 LL3 5.55 3.84 0.95 LL3 5.95 3.83 0.74 LL3 6.36 4.24 0.93 LL3 5.66 3.54 0.60 LL3 4.40 2.55 0.26 LL3 5.16 3.00 0.32 LL3 5.01 3.25 0.65 LL3 5.28 3.66 0.91 LL4-6 5.67 3.98 1.03 LL5 5.03 4.03 1.41 LL5 4.88 3.66 1.13 LL5 5.11 4.05 1.39 LL5 5.32 4.09 1.32 LL6 5.07 3.93 1.29 LL6 5.30 4.00 1.24 LL6 5.09 3.80 1.15 LL6 5.08 3.66 1.02 LL6 4.80 3.90 1.40 LL6 4.76 3.75 1.27 LL6 4.75 3.91 1.44 LL6 5.30 3.98 1.23 LL6 5.03 3.82 1.20 LL6 5.48 4.03 1.18 F o r P e e r R e v i e w LL6 5.13 3.80 1.13 LL6 4.76 3.63 1.15 LL6 4.83 3.72 1.21 LL6/7 5.30 4.00 1.24 LL7 5.73 4.07 1.09 LL7 4.75 3.71 1.24 1.13 L5-6 4.74 3.63 LL3 5.15 3.82 1.14 LL7 6.15 4.36 1.16 1.17 L6 4.40 3.45 LL3 4.95 3.72 1.15 LL7 5.19 3.93 1.24 1.16 L6 4.62 3.46 LL3 6.09 4.24 1.07 LL7 5.36 4.02 1.23 1.06 L6 5.02 3.65 LL3 5.66 4.18 1.24 LL7 5.59 4.26 1.35 1.04 L6 4.91 3.57 L6 4.44 3.46 L6 4.65 3.50 1.08 LL4 5.58 4.06 1.16 1.15 LL4 5.31 3.96 1.20 1.02 LL3 5.36 3.77 0.98	O n l y O n l y O n l y O n l y
	48 49 50 51				Meteoritics & Planetary Science Meteoritics & Planetary Science Meteoritics & Planetary Science Meteoritics & Planetary Science Meteoritics & Planetary Science	Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al Famenin-Pourkhorsandi et al

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Acknowledgments