Miller Range 03346, 090030, 090032, and 090136 715.2, 452.6, 532.5, 171 Grams Nakhlites

Miller Range 03346, 090030, 090032, and 090136 715.2, 452.6, 532.5, 171 grams Nakhlites

Figure 1: Four paired nakhlites from the Miller Range (MIL), Transantarctic Mountains; clockwise from upper left – MIL 03346, MIL 090030, MIL 090032, and MIL 090136

Introduction A large (~715 g) nakhlite – the first in the US Antarctic meteorite collection - was discovered Dec 15, 2003 in the Miller Range of the Transantarctic Mountains. About 60 % of the surface of MIL 03346 was covered with black, shiny wrinkled fusion crust (Figure 1). MIL 03346 is a nakhlite with abundant clinopyroxene and rare olivine set in a fine-grained mesostasis with some alteration (Righter and Satterwhite, 2004). Several years later, the 2009-2010 ANSMET team recovered three additional nakhlite samples that were quickly realized to be paired with MIL 03346 – MIL 090030, 090032, and 090136. These additional pairs are also sizable, and the combined mass of the pairing group is nearly 2 kg. These samples have provided new constraints on the source of the

1 nakhlites, the associated petrology of their setting on Mars, and many other aspects of the geologic, geochemical, and geophysical evolution of Mars.

Figure 2: Portion of the Miller Range where nakhlites were found.

Petrography MIL 03346 and pairs (pairing group abbreviated as MIL in the rest of this write-up) is a cumulate of abundant elongate clinopyroxene (0.2 to 2.5 mm) and minor olivine crystals (up to 1.7 mm) set in a dark-colored, fine-grained intercumulate mesostasis (Stopar et al. 2005; McKay and Schwandt 2005; Mikouchi et al. 2005; Rutherford et al. 2005; Day et al. 2006 and Imae and Ikeda 2007). Stopar et al. and Day et al. compared the grain size distribution of MIL with that of the other clinopyroxenites, finding that it had the largest average crystal size (0.43 x 0.26 mm).

Figure 3: Photomicrographs of MIL nakhlites

Early work on the modal mineralogy of MIL 03346 revealed its mesostasis-rich nature (20-35%; Figure 4; Stopar et al., 2005; Rutherford et al. (2005); McKay and Schwandt, 2005; Anand et al., 2005; Mikouchi et al. 2005; Day et al., 2006; Ikeda, 2007). Comparison of the textures and mineralogy of the paired masses have been carried out by Corrigan et al., (2015), Udry et al., (2012), and Hallis et al. (2013), and appear in Table 1. The higher fraction of mesostasis in MIL 03346 compared to Nakhla is evident in Figure 5.

Figure 4: X-ray chemical map of MIL 03346, illustrating the distribution of major and minor minerals and the relatively large fraction of mesostasis (from Stopar et al., 2008).

Figure 5: ternary plot of modal % olivine, pyroxene, and mesostasis in MIL nakhlites compared to Nakhla (from Corrigan et al., 2015).

From Udry et al. (2012)

The mesostasis (Figure 6) consists of a dendritic intergrowth of fayalite, ferro- hedenbergite, Ti-magnetite, cristobalite, apatite and feldspar glass (like that of NWA 817). No plagioclase has been found in MIL. Day et al. (2005, 2006) conclude that MIL is part of the same cumulate-rich lava flow as the other nakhlites, but that it experienced less equilibration and faster cooling than the other nakhlites.

Magmatic melt inclusions (Figure 7) are reported in the olivine (Rutherford et al. 2005) and in augite (Imae and Ikeda 2007; Ikeda, 2005). Various phases, including jarosite, saponite and Cl-rich amphibole, have been reported in these melt inclusions (McCubbin et al. 2008; Imae and Ikeda 2007; Sautter et al. 2006). Imae and Ikeda (2007) calculate the composition of the trapped (parental) magma from these melt inclusions.

Figure 6 (left): SEM image of mesostasis Figure 7 (right): magmatic melt inclusion in olivine

Olivine has “iddingsite-smectite” alteration in cracks, like that found in the other nakhlites (Arnand et al. 2005; Stopar et al. 2005). Mikouchi et al. (2005) note that the alteration in MIL 03346 (Antarctica) is like that in NWA 817 (Sahara Desert) and that this might indicate the alteration is pre-terrestrial. Stopar et al. (2005) report that “gypsum is found in cracks, voids and veins throughout the thin sections.” Sautter et al. (2005, 2007) report Cl-rich amphibole, chlorite, phosphate and a “mixed sulfate of Fe and S” which they interpret as derived from a soil component on Mars. Day et al. (2006) found that this alteration assemblage in MIL 03346 is probably a sub-micrometer mixture of smectite clay, iron oxy-hydroxides and salt minerals, with up to 14 wt. % H2O (as OH groups).

Mineral Chemistry Olivine: MIL has less olivine (3%) than the other nakhlites (Day et al. 2006). McKay and Schwandt (2005) found that large olivine grains (up to 1.7 mm) have uniform cores Fo44-43, but zone to Fo5 at their outer rims. Range of olivine reported from MIL pairs and other nakhlites is shown in Figure 8. Tiny skeletal fayalite is found in the mesostasis.

Pyroxenes: Cores of clinopyroxene cluster around Wo39En27. The rim zone increases in Fe and decreases in Ca to ~Wo34En14. Mikouchi et al. (2005), Anand et al. (2005) and McKay and Schwandt (2005) found that the outer rims, adjacent to the mesostasis, zone to ferro-hedenbergite (Figure 8). Imae and Ikeda found that the outer rims of pyroxene phenocrysts contain up to 10 wt.% Al2O3. Domeneghetti et al. (2006) found the iron in MIL was oxidized (Fe+3). The full range of reported clinopyroxene compositions is shown in Figure 8, along with comparisons to other nakhlites (Udry et al., 2012).

Ti-magnetite: Dendritic chains of Ti-magnetite are prevalent in the mesostasis (like NWA 817). Day et al. (2006) determined that magnetite was chemically zoned from pure magnetite towards ulvospinel (Figure 9). Both Dyar et al. (2006) and Morris et al. (2006) reported magnetite in their Mossbauer spectra. Righter et al. (2008, 2014) report trellis type exsolution lamellae in the titanomagnetite indicating oxy-exsolution.

Figure 8: Pyroxene and olivine chemistry in the MIL pairs, as well as some other nakhlites for comparison (from Udry et al., 2012).

Figure 9: Compositional variation in the magnetite-ulvospinel solid solution in MIL 03346 (from Day et al., 2006).

Glass: Feldspathic-glass compositions in the mesostasis are An29-38Or7-14 (Anand et al. 2005; Day et al. 2006).

Silica: Anand et al. (2005) and Mikouchi et al. (2005) report small (5 micron) blebs of silica in the mesostasis. Chennaoui Aoudjehane et al. (2006) used cathodoluminescence to study shock effects.

Amphibole: Sautter et al. (2006, 2007) reported the presence of Cl-rich amphibole (1.5 to 7% Cl) in melt inclusions in augite and in olivine.

Phosphates: Fries et al. (2006) studied phosphates in MIL 03346 by confocal Raman imaging techniques and found that they were “hydrated”.

Sulfides: Day et al. (2006) found that sulfide “blebs” are pyrrhotite – often altered.

Jarosite: The Martian sulfate mineral jarosite has been discovered in melt inclusions in augite (McCubbin et al. 2008) and in the interstices of MIL 03346 (Vicenzi et al. 2007).

Saponite: Imae and Ikeda (2007) reported an occurrence of a hydrated phase (saponite?), adjacent to fayalite, in a trapped melt inclusion – suggesting that the alteration occurred on Mars. Hicks et al. (2013) carried out a detailed study of the saponite.

Weathering (terrestrial and martian) Weathering on the surface of Mars has produced specific mineral assemblages, and terrestrial weathering has also affected the MIL nakhlites with a great diversity of phases documented and analyzed. Distinguishing between these two weathering environments is not easy, and has been the goal of many detailed studies. Kuebler (2013) reports laihunite that hosts stilpnomelane, as well as gypsum and bassanite, in MIL 03346 (Figure 10 middle), and argued that all phases originated on Mars. Ling and Wang (2015) made Raman spectroscopic and Raman imaging studies of MIL 03346, with an emphasis on the secondary mineral phases. Their study revealed three types of calcium sulfates (including basanite and γ-CaSO4), a solid solution of (K, Na)-jarosite, and two groups of hydrated species in the veins and/or mesostasis areas of the meteorite. They argue that bassanite may have formed by direct precipitation from a Ca-S-H2O brine, and that the close spatial relationship of (K, Na)-jarosite solid solutions with rasvumite (KFe2S3), magnetite, and alkali feldspar in the mesostasis suggests in situ formation of mesostasis jarosite from these Fe-K,Na-S-O-H2O species. Hicks et al. (2014) found amorphous olivine gel associated with martian weathering and with saponite in some other nakhlites. Hallis et al. (2014) found jarosite and gypsum, amorphous silicates, and Fe-oxides and hydroxides in studies of MIL 090032. Their smectite may be the same amorphous silicate found by Hicks et al. (2014). Cartwright et al. (2013) found noble gas and halogen evidence for brines playing a role in surface weathering processes on Mars. Stopar et al. (2013) found many secondary phases likely resulting from aqueous processes, including formation of poorly crystalline iddingsite-like veins in olivine, the precipitation of Ca-, Fe-, and K- sulfates from evaporating fluids, alteration of titanomagnetite to secondary Fe-oxides, and the dissolution of magmatic Ca-phosphates and residual glass in the mesostasis (Figure 10, left and right). Stopar et al. (2013) emphasized that although some of the secondary minerals may have originated on Mars, elevated S and REEs, Ce anomalies, and association of secondary minerals with post-impact cracks and voids indicate that terrestrial weathering has significantly affected MIL 03346. Distinguishing martian from terrestrial weathering can be difficult and is the topic of ongoing research.

Stopar et al. (2013) found evidence for etch-pits and olivine dissolution textures which were also documented by Velbel (2016) and ascribed to terrestrial weathering.

Whole-rock Composition The whole rock composition has been determined by Anand et al. (2005), Barret et al. (2006) and Day et al. (2006) (Table 2). Barrat et al. (2006) found that Co, Ni, Cu and Zn were like other nakhlites. The large ion lithophile elements are similar in relative abundances to other nakhlites, but elevated, compared with Nakhla and Lafayette (Figure 11). Note the lack of any Eu anomaly. Dreibus et al. (2006) reported 147 ppm F, 248 ppm Cl, 0.45 ppm Br, 610 ppm S and 315 ppm carbon. Shirai and Ebihara (2008) have also analyzed MIL 03346 (data reported in diagrams). Wang and Becker (2017) reported bulk Cu and Ag data.

Figure 10: Left – jarosite (magenta) within an alteration vein from Stopar et al. (2008); Middle –laihunite (blue) in the mesostasis of MIL 03346 from Kuebler et al., 2013); Right – Ca-sulfite along alteration veins and zones for MIL 03346 from Stopar et al. (2008).

Figure 11: REE diagram for MIL 03346 compared to several other nakhlites (from Day et al., 2006).

Table 2: Whole rock composition for MIL nakhlites

reference Anand2005 Barrat2006 Day2006 weight

SiO2 % 49.2 49.5 (b)

TiO2 0.07 0.69 ( a) 0.68 (b)

Al2O3 3.59 3.66 (a) 4.09 (b) FeO 19.23 19.12 (a) 19.1 (b) MnO 0.45 0.46 (a) 0.46 (b) MgO 9.33 9.99 (a) 9.26 (b) CaO 15 15.75 (a) 14.4 (b)

Na2O 1.01 1 (a) 0.96 (b)

K2O 0.29 0.27 (a) 0.2 (b)

P2O5 0.22 0.25 (a) 0.23 (b) S % 0.06 (b) sum

Sc ppm 46 54.5 (a) 52.9 (c ) V 184 208 (a) 210 (c ) Cr 1300 1192 (a) 1300 (c ) Co 25 35.7 (a) 38.7 (c ) Ni 60 49 (a) 58.1 (c ) Cu 13 8.2 (a) 13.3 (c ) Zn 65 61.3 (a) 61.5 (c ) Ga 6.51 (a) 6.77 (c ) Ge ppb As Se Rb 4.14 (a) 4.41 (c ) Sr 106 131.7 (a) 121.3 (c ) Y 7 8.44 (a) 8.5 (c ) Zr 23.29 (a) 21.2 (c ) Nb 3.98 (a) 3.65 (c ) Mo Ru Rh Pd ppb Ag ppb Cd ppb In ppb Sn ppb Sb ppb Te ppb Cs ppm 0.29 (a) 0.27 (c ) Ba 53 59.58 (a) 56.9 (c ) La 4.7 (a) 3.89 (c ) Ce 11.01 (a) 11.3 (c ) Pr 1.56 (a) 1.78 (c ) Nd 7.07 (a) 8.04 (c ) Sm 1.64 (a) 1.83 (c ) Eu 0.522 (a) 0.52 (c )

Gd 1.73 (a) 1.86 (c ) Tb 0.266 (a) 0.3 (c ) Dy 1.57 (a) 1.66 (c ) Ho 0.317 (a) 0.32 (c ) Er 0.851 (a) 0.84 (c ) Tm 0.13 (c ) Yb 0.766 (a) 0.8 (c ) Lu 0.114 (a) 0.13 (c ) Hf 0.69 (a) 0.66 (c ) Ta 0.23 (a) 0.21 (c ) W ppb 0.4 (a) Re ppb Os ppb Ir ppb Pt ppb Au ppb Th ppm 0.42 (a) 0.43 (c ) U ppm 0.09 (a) 0.11 (c ) technique: (a) ICP, (b) e.probe (c ) ICP-MS

Radiogenic Isotopes Murty et al. (2005) determined a U,Th-4He age of 1.02 ± 0.15 Ga and K-Ar age of 1.75 ± 0.26 Ga (based on U, Th, K contents of Nakhla). Bogard and Garrison (2006) determined an Ar plateau age of 1.44 ± 0.02 Ga. More extensive work on MIL 03346 and its pairs reveal Ar-Ar ages of 1.368 ± 0.083 Ga (mesostasis) and 1.334 ± 0.054 Ga (pyroxene) (Park et al., 2009; Figure 12), and 1.373 +/- 0.011 Ga (from Cassata et al., 2010; Figure 13). A comprehensive look at nakhlites by Cohen et al. (2017) shows an age of 1.392 +/- 0.010 Ga (Figure 14) as well as variation in ages within the nakhlites that range from 1.3 to 1.4 Ga (Figure 15), with MIL among the oldest. Shih et al. (2006) determined a Rb-Sr isochron of 1.29 ± 0.12 Ga and a Sm-Nd isochron of 1.36 ± 0.03 Ga (Figures 16 and 17).

Figure 12: Ar-Ar age data and K/Ca data for MIL 03346 from Park et al. (2009 for whole rock and pyroxene. Figure 13: Ar-Ar age data and Ca/K data for MIL 03346 from Cassata et al. (2010).

Figure 14: Ar-Ar age data for MIL 03346 from Cohen et al. (2017). Figure 15: Summary of Ar-Ar age dating by Cohen et al. (2017) for all nakhlites.

Figure 16: Rb-Sr isochron for MIL 03346 from Shih et al. (2006). Figure 17: Sm-Nd isochron for MIL 03346 from Shih et al. (2006).

Age data for MIL03346 Ar/Ar Rb/Sr Nd/Sm Bogard and Garrison 2006 1.44 ± 0.02 Park et al. (2009) 1.368 ± 0.083 1.334 ± 0.054 Cassata et al. (2010) 1.373 ± 0.011 Cohen et al. (2017) 1.392 ± 0.010 Shih et al. 2006 1.29 ± 0.12 1.36 ± 0.03

Stable Isotopes Many stable isotope studies are aimed at deciphering the building blocks of Mars, such as Ba, Li, Ca, Si, Mg, and Fe isotopes.

MIL samples were part of a study of Ba isotopes in the inner solar system (Bermingham et al., 2016). Ba isotope homogeneity in the early inner Solar System is evidenced by the Ba isotope compositions of H-chondrites, enstatite chondrites, eucrites, and Martian meteorites, which are all indistinguishable from terrestrial values.

MIL 03346 was used, along with a suite of martian meteorites, to estimate the Li isotopic composition of the martian mantle. This work by Magna estimated the 7Li for Mars to be 4.2 +/- 0.9, within error of the estimate for Earth’s mantle 3.5 +/- 1.0 (Magna et al., 2015a).

Magna et al. (2015b) measured Ca isotopes in a suite of martian meteorites, including MIL, and found that Mars has identical Ca isotopic composition to the Earth and Moon. They suggest the inner solar system is homogeneous with respect to Ca isotopic composition.

Zambardi et al. (2013) measured Si isotopes in a wide range of terrestrial and achondrite meteorites (including MIL) and found that Mars overlaps with HEDs and chondrites but are distinctly lighter than lunar and terrestrial samples. This difference could be explained by terrestrial core formation at high PT reduced conditions, and especially if Moon was derived from Earth’s mantle.

Magna et al. (2017) examined Mg isotopic composition of a suite of martian meteorites and made a similar finding to that for Li and Ca – that Mars silicate mantle has a 26Mg value that is identical to that for the rest of the inner solar system.

Paniello et al. (2012) measured 66Zn in lunar, martian, and terrestrial samples (including MIL) and found that martian shergottites and nakhlites essentially overlap terrestrial mantle samples. Lunar samples on the other hand, exhibit a wide range of Zn isotopic values suggesting potential for Zn fractionation in dry reduced magmatic environments as well as fire fountaining.

Finally, Sossi et al. (2016) and Wang et al. (2016) measured Fe isotopes in a suite of martian meteorites (including MIL) and found that when all are corrected for magmatic fractionation, the martian mantle has 57Fe slightly lighter than Earth, but identical to chondrites and HEDs. This finding is similar to that for Si isotopes.

Several studies of S, Cl, and Zn isotopes are primarily aimed at understanding magmatic processes – see section below.

Cosmogenic Isotopes Murty et al. (2005) determined an average exposure age of 9.5 ± 1.0 Ma for MIL 03346, which is the number one gets for all the nakhlites.

Petrology Mineralogic studies of the MIL augites have placed important constraints on the cooling rates, oxygen fugacity and volatile content of the MIL parent magma.

Cooling rates Hammer et al. (2009) examined textural features in MIL and deduced cooling rates of ~20 ˚C/hr., when compared to experimental constraints. Alvaro et al. (2015) show that the closure temperatures of MIL augite, based on Fe-Mg ordering, are ~600 ˚C, which correlates with a cooling rate near 6.8 ˚C/hr., slightly higher cooling rates than those proposed by Domeneghetti et al. (2006, 2013). Studies of Li zoning and diffusion in augite (Beck et al., 2006; Richter et al., 2014, 2016) show that MIL likely experienced slow cooling in a magma chamber followed by relatively rapid cooling during and after emplacement in a thin lava flow. Moreover, the cooling rates indicate that the lava flow drained shortly after emplacement.

Oxygen fugacity

MIL is thought to have a relatively high fO2 based on the presence of fayalite-rich olivine, titanomagnetite and silica (Righter et al., 2008) and the Ti/Al ratio in Ca-pyroxene phenocrysts is similar to experimental samples crystallized at fO2’s ranging between the QFM and NNO buffers (Hammer and Rutherford 2005). Righter et al. (2008) calculated 3+ Fe2O3 = 3.20-3.27 (XFe = 0.20) in augite, which is high for martian augites. McCanta et al. (2009) showed that Eu partitioning in augite also suggests IW+3.2 for MIL crystallization, close to FMQ buffer. Righter et al. (2014) summarize fO2 constraints on MIL formation and show that it may have initially crystallized near FMQ, increased slightly during crystallization in a magma chamber, followed by reduction during sulfur loss and degassing, and finally late oxidation due to Cl degassing and loss. This detailed history illustrates how a single rock can contain a record of the fO2.

Figure 18: exsolution in titanomagnetite (left) and fO2 history of MIL and other nakhlites based on summary in Righter et al. (2014).

Volatiles McCubbin et al. (2013) show that apatites record the presence of a Cl-rich magmatic fluid during the intermediate stages of magma emplacement. Cl-amphiboles in melt inclusions also record the history of a Cl-rich fluid. Later degassing of Cl affects the Cl content of the apatite, as well as the oxidation state of the magma (Righter et al., 2014). Filiberto et al. (2016) reviews the F, Cl, and water content of the martian mantle, concluding that martian magmas had similar water, Cl, and F contents to mid-ocean ridge basalt. Cl isotopes were measured in MIL by Williams et al. (2016), who found that martian meteorites in general range from 37Cl = -3.8 (mantle) to (+)ve values that are observed in the crust. MIL falls intermediate which suggests that the nakhlites were affected by fluid interaction or assimilation and/or fractional crystallization processes. Franz et al. (2014) and Dottin et al. (2018) measured S isotopic values for MIL and found that the 33S values coupled with the abundant titanomagnetite argue for assimilation of sulfate or sulfate-bearing brines by the nakhlite parent magma. They also suggest that MIL formed at the bottom of the nakhlite pile rather than near the top as usually argued. Such a position might be consistent with the bulk S contents of the mesostasis as well as other geochemical features and S degassing (Dottin et al., 2018).

Differentiation Wadhwa and Borg (2006) found that the 142Nd and 182W isotopic anomalies were like other nakhlites, concluding that nakhlites formed under relatively oxidizing conditions. Debaille et al. (2007, 2008) found evidence from the time integrated isotopic evolution of Sm-Nd and Lu-Hf system for early differentiation of the martian mantle, perhaps reflecting deep mantle phases and thus deep mantle fractionation in the early history of Mars. The 142Nd-143Nd record of the nakhlites is difficult to interpret because the nakhlites plot outside the two-stage evolutionary field in the 142Nd vs. 143Nd diagram defined by shergottites (Debaille et al., 2009). The 146Sm-142Nd systematics of the nakhlites are like those of the depleted shergottites, whereas the 147Sm-143Nd systematics reveal differences, which may indicate a disturbance of the Sm-Nd system after extinction of 146Sm. Although the 146,147Sm-142,143Nd systematics of the SNC meteorites exhibit evidence for differentiation of the Martian mantle 10-100 Ma after solar system formation, exact scenarios are model dependent and remain under investigation.

Figure 19: Nd-W isotopic diagram showing values for the nakhlites (open square) that is like depleted shergottites but lies at a higher W value (from Debaille et al., 2009).

Miscellaneous studies Blamey et al. (2015) measured methane and hydrogen released from MIL olivine and pyroxene, concluding that these gases were trapped in fluid inclusions or along fractures, and demonstrate that the martian subsurface is capable of hosting microbial life.

Murty et al. (2005) reported the isotopic ratios of rare gases extracted at different temperatures from MIL 03346.

Dyar et al. (2006) determined the Mossbauer, reflectance and thermal emission spectra of MIL 03346 (Figures 20, 21), arguing that this rock is highly oxidized with abundant Fe3+.

Kanner et al. (2007) studied spectroscopy of MIL 03346 and integrated the result into comprehensive examination of low and high Ca pyroxene modelling with OMEGA data.

Coulson et al. (2007) measured porosity (2.97 to 3.60 %) for MIL 03346.

Gattacecca et al. (2005) and Jambon et al. (2010) reported the magnetization of MIL 03346 and show that the intensity fabric is oblate, not unlike many terrestrial plutonic and volcanic rocks.

Figure 20: Mossbauer spectra of MIL 03345 whole rock and clinopyroxene separate (from Dyar et al., 2006). Figure 21: Reflectance spectra of MIL 03346 and Nakhla (from Dyar et al., 2006).

Summary MIL 03346 and its pairs have obviously contributed to our understanding of the geology of Mars - from the chemical building blocks of Mars to the timing and conditions of its early differentiation, to mantle melting, magma genesis and magmatism (volatiles and cooling history), to more recent weathering and surface processes. It has provided information about the magnetic field of Mars, organic geochemistry, and surface spectroscopy, and in general the redox evolution of Mars and its magmatic rocks. These samples will undoubtedly continue to provide important constraints on the geochemical and geophysical evolution of Mars.

Processing NASA-JSC received more than 50 requests for this sample for the Fall 2004 Meteorite Working Group meeting. As of 2014, it had been subdivided into >200 splits and distributed to ~70 scientists around the world for study. Righter and McBride (2011), Allen et al. (2011), and Righter et al. (2014) have presented information about the processing and allocation of MIL 03346. MIL 03346 was examined and split in dry-

18 nitrogen glove boxes at JSC which have been thoroughly cleaned and dried immediately before processing of this sample. The sample was only exposed to stainless steel, aluminum and Teflon, although the gloves, gaskets and band saw wheels are made of Neoprene and/or Viton. However, the sample itself was only handled with Teflon overgloves.

MIL 03346 was subdivided in three main stages: initial processing (13.15 g including 5 thin sections), slab allocations (46.46 g including 49 chips and 7 thin sections), and NE butt end allocations (32.05 g including 8 chips and 1 thin section butt). Small pieces were derived for the initial characterization of the sample, including a 2.1-g chip that was potted to make thin sections (Figure 22 and 23). Due to the large number of individual samples requested, bandsaw slabbing was considered the best way to preserve as much of the original mass as possible for future study while also documenting individual meteorite chips allocated (Figure 24-25). After the slab was totally subdivided and allocated (Figure 25), the NE butt end was subdivided (Figure 26). The total allocated mass of the main mass, the slab, and the NE butt end are summarized in Table 3.

After nearly 14 years of curation and study, much has been learned about Mars for the MIL pairing group, as summarized above. A 447-g piece of the main mass of MIL 03346 remains for future studies, as well as a total of ~600 g of material that has not been allocated. Clearly, many additional future studies are possible with this much mass available.

Table 3: Summary of major subdivisions of MIL 03346 (as of 2014)

Figure 22: Subdivision history of MIL 03346, circa 2005.

Figure 23: Summary of initial processing of MIL 03346.

Figure 24: Derivation of slab of MIL 03346 by bandsawing.

Figure 25: Subdivision of the MIL 03346 slab

Figure 26: Subdivision of the NE butt end (SW view).

References for MIL03346, 090030, 090032, 090136 (compiled by C. Meyer, Oct 2012; updated by K. Righter Oct. 2018)

Allen, C., Allton, J., Lofgren, G., Righter, K., Zolensky, M. E. (2011) Curating NASA's extraterrestrial samples-Past, present, and future, Chemie der Erde - Geochemistry 71, 1-20, http://dx.doi.org/10.1016/j.chemer.2010.12.003. Alvaro, M., Domeneghetti, M. C., Fioretti, A. M., Camara, F., Marinangeli, L. (2015) A new calibration to determine the closure temperatures of Fe-Mg ordering in augite from nakhlites, Meteoritics & Planetary Science 50, 499-507. Anand M., Williams C.T., Russell S.S., Jones G., James S., and Grady Monica M. (2005a) Petrology and geochemistry of Nakhlite MIL03346: A new martian meteorite from Antarctica (abs#1639). Lunar Planet. Sci. XXXVI Lunar Planetary Institute, Houston. Anand M., Burgess R., Fernandes Vera and Grady M.M. (2006b) Ar-Ar age and halogen characteristics of Nakhlite MIL03346: Records of crustal processes on Mars (abs#5257). Meteorit. & Planet. Sci. 41, A16. Barrat J-A., Benoit M. and Cotton J. (2006) Bulk chemistry of the Nakhlite Miller Range 03346 (MIL 03346) (abs#1569). Lunar Planet. Sci. Conf. XXXVII Lunar Planetary Institute, Houston. Beck P., Chaussidon M., Barrat J-A., Gillet Ph. and Bohn M. (2005d) An ion-microprobe study of lithium isotopes behavior in Nakhlites (abs#5044). Meteorit. & Planet. Soc. 40, A18. Beck, P., Chaussidon, M., Barrat, J. A., Gillet, P., Bohn, M. (2006) Diffusion induced Li isotopic fractionation during the cooling of magmatic rocks: The case of pyroxene phenocrysts from nakhlite meteorites, Geochimica et Cosmochimica Acta 70, 4813-4825, http://dx.doi.org/10.1016/j.gca.2006.07.025. Blamey, N. J., Parnell, J., Mcmahon, S., Mark, D. F., Tomkinson, T., Lee, M., Flemming, R. L. (2015) Evidence for methane in Martian meteorites. Nature communications 6.7399, http://dx.doi.org/10.1038/ncomms8399. Bogard, D. D. (2009) K-Ar dating of rocks on Mars: Requirements from Martian meteorite analyses and isochron modeling, Meteoritics & Planetary Science 44, 3-14, http://dx.doi.org/10.1111/j.1945-5100.2009.tb00713.x. Bogard Don D. and Garrison D.H. (2006) Ar-Ar dating of Martian Chassignites, NWA2737 and Chassigny, and Nakhlite MIL03346 (abs#1108). Lunar Planet. Sci. XXXVII, Lunar Planetary Institute, Houston. Bouvier, A., Blichert-Toft, J., Albarede, F. (2009) Martian meteorite chronology and the evolution of the interior of Mars. Earth and Planetary Science Letters 280, 285-295, http://dx.doi.org/10.1016/j.epsl.2009.01.042. Cartwright, J. A., Gilmour, J. D., Burgess, R. (2013) Martian fluid and Martian weathering signatures identified in Nakhla, NWA 998 and MIL 03346 by halogen and noble gas analysis. Geochimica et Cosmochimica Acta 105, 255-293, http://dx.doi.org/10.1016/j.gca.2012.11.046. Cassata, W. S., Shuster, D. L., Renne, P. R., Weiss, B. P. (2010) Evidence for shock heating and constraints on Martian surface temperatures revealed by 40Ar/39Ar thermochronometry of Martian meteorites, Geochimica et Cosmochimica Acta 74, 6900-6920, http://dx.doi.org/10.1016/j.gca.2010.08.027. Chennaoui Aoudjehane H., Jambon A. and Boudouma O. (2006a) Cristobalite and K-feldspar in the Nakhlite MIL03346: A cathodoluminescence study (abs#1037). Lunar Planet. Sci. XXXVII Lunar Planetary Institute, Houston.

Chennaoui Aoudjehane H. and Jambon A. (2006d) A cathodluminescence study of cristobalite and K-feldspar in the Nakhlite MIL03346 (abs#5220). Meteorit. & Planet. Sci. 41, A37. Chennaoui Aoudjehane H., Jambon A. and Boudouma O. (2010) A cathodluminescence study and K-feldspar in the Nakhlites MIL03346 and NWA5790 (abs#1934). Lunar Planet. Sci. LXI Lunar Planetary Institute, Houston. Corrigan, C. M., Velbel, M. A., Vicenzi, E. P. (2015) Modal abundances of pyroxene, olivine, and mesostasis in nakhlites: Heterogeneity, variation, and implications for nakhlite emplacement. Meteoritics & Planetary Science 50, 1497-1511, http://dx.doi.org/10.1111/maps.12492. Coulson, I. M., Beech, M., Nie, W. (2007) Physical properties of Martian meteorites: Porosity and density measurements. Meteoritics & Planetary Science 42, 2043-2054, http://dx.doi.org/10.1111/j.1945-5100.2007.tb01006.x. Day J.M.D., Taylor L.A., Floss C., McSween H.Y., Liu Y. and Hill E. (2005a) Petrogenesis of Martian Nakhlite MIL 03346 (abs#5288). Meteorit. & Planet. Sci. 40, A36. Day J.M.D., Taylor L.A., Valley J.W. and Spicuzza M.J. (2005b) Assimilation of high 18O/16O crust by Shergottite-Nakhlite-Chassigny (SNC) magmas on Mars (abs#P51-0902). AGU San Francisco Day J.M.D., Taylor L.A., Floss C. and McSween H.Y. (2006) Petrology and chemistry of MIL 03346 and its significance in understanding the petrogenesis of Nakhlites on Mars. Meteorit. & Planet. Sci. 40, 581-606. http://dx.doi.org/10.1111/j.1945-5100.2006.tb00484.x. Debaille V., Yin Q-Z., Brandon A.D., Jacobsen B. and Treiman A.H. (2007a) Lu-Hf and Sm-Nd isotopic studies of Shergottites and Nakhlites: Implications for Martian mantle sources (abs#1903). Lunar Planet. Sci. XXXVIII Lunar Planetary Institute, Houston. Debaille, V., Brandon, A. D., O'Neill, C., Yin, Q. Z., Jacobsen, B. (2009) Early martian mantle overturn inferred from isotopic composition of nakhlite meteorites . Nature Geoscience 2, 548-552, http://dx.doi.org/10.1038/ngeo579. Domeneghetti M.C., Fioretti A.M., Camara F., Molin G. and McCammon C. (2006b) Constraints on the thermal history and oxidation state of MIL03346 Martian meteorite: Single-crystal XRD, electron microprobe and Mossbauer analysis of clinopyroxene (abs#1238). Lunar Planet. Sci. XXXVII Lunar Planetary Institute, Houston. Domeneghetti, M. C., Fioretti, A. M., Camara, F., Mccammon, C., Alvaro, M. (2013) Thermal history of nakhlites: A comparison between MIL 03346 and its terrestrial analogue Theo's flow. Geochimica et Cosmochimica Acta 121, 571-581, http://dx.doi.org/10.1016/j.gca.2013.07.044. Dreibus G., Huisl W., Spettel B. and Haubold R. (2006a) Halogens in Nakhlites: Studies of pre- terrestrial and terrestrial weathering processes (abs#1180). Lunar Planet. Sci. Conf. XXXVII Lunar Planetary Institute, Houston. Dyar M.D., Pieters C.M., Hiroi T., Lane M.D. and Marchand G.J. (2005a) Integrated spectroscopic studies of MIL03346 (abs#1261). Lunar Planet. Sci. XXXVI Lunar Planetary Institute, Houston. Dyar M. Darby, Treiman A.H., Pieters C.M., Hiroi T., Lane M.D. and O’Connor V. (2005b) MIL03346, the most oxidized Martain meteorite: A first look at spectroscopy, petrography, and mineral chemistry. J. Geophys. Res. 110, E09005 doi: Filiberto, J., Gross, J., McCubbin, F. M. (2016) Constraints on the water, chlorine, and fluorine content of the Martian mantle. Meteorit Planet Sci 51, 2023-2035, doi:10.1111/maps.12624. Franz, H. B., Dottin Iii, J., Kim, S. T., Farquhar, J., Day, J. M. D., Economos, R. C., Mckeegan, K. D., Schmitt, A. K., Irving, A. J., Hoek, J. (2014) Isotopic links between atmospheric chemistry and the deep sulphur cycle on Mars. Nature 508, 364-368.

Fries M., Mysen B., Vicenzi E., Rost D. and Steele A. (2006) Hydrated phosphates in Nakhlite MIL03346 (abs#1180). Lunar Planet. Sci. Conf. XXXVII Lunar Planetary Institute, Houston. Giesting, P. A., Filiberto, J. (2016) The formation environment of potassic-chloro-hastingsite in the nakhlites MIL 03346 and pairs and NWA 5790: Insights from terrestrial chloro- amphibole. Meteorit Planet Sci 51, 2127-2153, doi:10.1111/maps.12675. Grady M.M., Anand M., Bridges J.C., Pearson V.K., Franchi I.A. and Wright I.P. (2005) Aqueous alteration of Nakhlites: Implications for water on Mars (abs#5119). Meteorit. & Planet. Sci.40, A59. Grady M.M., Anand M., Gilmour M.A., Watson J. and Wright I.P. (2007) Continuing investigation of the Nakhlite magma pile (abs#5171). Meteorit. & Planet. Sci. 42, A59. Hallis Lydia and Taylor G.J. (2011) Comparison of the four Miller Range Nakhlites, MIL03346, 090030, 090032 and 090136: Textural and compositional observations of primary and secondary mineral assemblages. Meteorit. & Planet. Sci. 46, 1787-1803. Hammer, J. E. (2009) Application of a textural geospeedometer to the late-stage magmatic history of MIL 03346. Meteoritics & Planetary Science 44, 141-154, http://dx.doi.org/10.1111/j.1945-5100.2009.tb00724.x. Hallis, L. J. (2013) Alteration assemblages in the Miller Range and Elephant Moraine regions of Antarctica: Comparisons between terrestrial igneous rocks and Martian meteorites. Meteoritics & Planetary Science 48, 165-179, http://dx.doi.org/10.1111/maps.12049. Hallis, L. J., Taylor, G. J., Nagashima, K., Huss, G. R., Needham, A. W., Grady, M. M., Franchi, I. A. (2012) Hydrogen isotope analyses of alteration phases in the nakhlite martian meteorites. Geochimica et Cosmochimica Acta 97, 105-119, http://dx.doi.org/10.1016/j.gca.2012.08.017. Hallis, L. J., Ishii, H. A., Bradley, J. P., Taylor, G. J. (2014) Transmission electron microscope analyses of alteration phases in martian meteorite MIL 090032 , Geochimica et Cosmochimica Acta 134, 275-288, http://dx.doi.org/10.1016/j.gca.2014.02.007. Hallis, L. J., Taylor, G. J. (2011) Comparisons of the four Miller Range nakhlites, MIL 03346, 090030, 090032 and 090136: Textural and compositional observations of primary and secondary mineral assemblages. Meteoritics & Planetary Science 46, 1787-1803, http://dx.doi.org/10.1111/j.1945-5100.2011.01293.x. Hammer J.E. and Rutherford M.J. (2005) Experimental crystallization of Fe-rich basalt: Application to cooling rate and oxygen fugacity of Nakhlite MIL03346 (abs#1999). Lunar Planet. Sci. XXXVI, Lunar Planetary Institute, Houston. Herd C.D.K. (2006a) Fractionation of K, U and Th during Martian alteration: Insights from MIL03346 (abs#2079). Lunar Planet. Sci. Conf. XXXVII Lunar Planetary Institute, Houston. Herd C.D.K. (2006c) An occurrence of Jarosite in MIL03346: Implications for conditions of Martian aqueous alteration (abs#5027). Meteorit. & Planet. Sci. 41, A74. Herd C.D.K. and Walton E.L. (2008) Cooling and crystalliation of the Miller Range 03346 Nakhlite: Insights from experimental petrology and mineral equilibria (abs#1496). Lunar Planet. Sci. XXXIX. Lunar Planetary Institute, Houston. Hicks, L. J., Bridges, J. C., Gurman, S. J. (2014) Ferric saponite and serpentine in the nakhlite martian meteorites, Geochimica et Cosmochimica Acta 136, 194-210, http://dx.doi.org/10.1016/j.gca.2014.04.010. Ikeda, Y. (2005) Magmatic inclusions in martian meteorites. Antarctic meteorite research 18, 170-187, http://ci.nii.ac.jp/naid/110001218496/en/. Imae N. and Ikeda Y. (2005) Comparative petrology of Yamato and MIL 03346 Nakhlites (abs#5058). Meteorit. & Planet. Sci. 40, A72.

Imae N. and Ikeda Y. (2007a) Petrology of the Miller Range 03346 Nakhlite in comparison with the Yamoto-000593 Nakhlite. Meteorit. & Planet. Sci. 42, 171-184. http://dx.doi.org/10.1111/j.1945-5100.2007.tb00225.x. Kim S-T. and Farquhar J. (2008) Multiple sulfur isotope compostions in Martian meteorite MIL03346 (abs#2151). Lunar Planet. Sci. XXXIX. Lunar Planetary Institute, Houston. Kinman W.S. and Neal C.R. (2005) Petrology of Nakhlite MIL03346 (abs#1660). Lunar Planet. Sci. XXXVI Lunar Planetary Institute, Houston. Kuebler, K. E. (2013) A combined electron microprobe (EMP) and Raman spectroscopic study of the alteration products in Martian meteorite MIL 03346. Journal of Geophysical Research: Planets 118, 347-368, http://dx.doi.org/10.1029/2012JE004244. Lentz R.C.F., McCoy T.J. and Taylor G.J. (2005a) Multiple Nakhlite lava flows? (abs#5298) Meteorit. & Planet. Sci. 40, A91. Ling, Z., and A. Wang (2015) patial distributions of secondary minerals in the Martian meteorite MIL 03346,168 determined by Raman spectroscopic imaging, J. Geophys. Res. Planets 120, 1141–1159, doi:10.1002/2015JE004805. Magna, T., Hu, Y., Teng, F. Z., & Mezger, K. (2017) Magnesium isotope systematics in Martian meteorites. Earth and Planetary Science Letters 474, 419-426, http://dx.doi.org/10.1016/j.epsl.2017.07.012. McBride K.M., Righter K., Satterwhite C.E., Schwarz C. and Robinson P. (2005) Curation and allocation of the new Antarctic Nakhlite MIL03346 (abs#1499). Lunar Planet. Sci. XXXVI Lunar Planetary Institute, Houston. McCanta M.C., Rutherford M.J. and Calvin C. (2005) Melt REE contents of Lherzolitic Shergottite ALH77005 and Nakhlite MIL03346: Application of the Eu-oxybarometer (abs#5249). Meteorit. & Planet. Sci. 40, A99. Mccanta, M. C., Elkins-Tanton, L., Rutherford, M. J. (2009) Expanding the application of the Eu-oxybarometer to the lherzolitic shergottites and nakhlites: Implications for the oxidation state heterogeneity of the Martian interior. , Meteoritics & Planetary Science 44, 725-745, http://dx.doi.org/10.1111/j.1945-5100.2009.tb00765.x. McCubbin F.M., Tosca N.J., Smirnov A., Nekvasil H., Fries M. and Steele A. (2008) Jarosite in a clinopyroxene-hosted melt inclusion from Martian meteorite MIL03346: Evidence for hydrothermal formation by sulfide oxidation (abs#1982). Lunar Planet. Sci. XXXIX Lunar Planetary Institute, Houston. McCubbin F.M., Tosca N.J., Smirnov A., Nekvasil H., Steele A., Fries M. and Lindsley D.H. (2009) Hydrothermal Jarosite and hematite in a pyroxene-hosted melt inclusion in Martian meteorite MIL03346: Implication for magmatic-hydrothermal fluids on Mars. Geochim. Cosmochim. Acta 73, 4907-4917. McCubbin, F. M., Tosca, N. J., Smirnov, A., Nekvasil, H., Steele, A., Fries, M., Lindsley, D. H. (2009) Hydrothermal jarosite and hematite in a pyroxene-hosted melt inclusion in martian meteorite Miller Range (MIL) 03346: Implications for magmatic-hydrothermal fluids on Mars, Geochimica et Cosmochimica Acta 73, 4907-4917, http://dx.doi.org/10.1016/j.gca.2009.05.031. McCubbin, F. M., Elardo, S. M., Shearer, C. K., Smirnov, A., Hauri, E. H., Draper, D. S. (2013) A petrogenetic model for the comagmatic origin of chassignites and nakhlites: Inferences from chlorine-rich minerals, petrology, and geochemistry. Meteoritics & Planetary Science 48, 819-853, http://dx.doi.org/10.1111/maps.12095. McKay G.A. and Schwandt C. (2005) Mineralogy and petrology of the new Antarctic Nakhlite MIL03346 (abs#2351). Lunar Planet. Sci. XXXVI Lunar Planetary Institute, Houston. McKay G.A. and Mikouchi T. (2005) Minor element zoning in Nakhlites: What’s going on? (abs#5335) Meteorit. & Planet. Sci. 40, A100.

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K. Righter, October 2018