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Spectral and Geochemical Characteristics of Lake Superior Type Banded Iron Formation: Analog to the Martian Hematite Outcrops

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Spectral and Geochemical Characteristics of Lake Superior Type Banded Iron Formation: Analog to the Martian Hematite Outcrops Lunar and Planetary Science XXXV (2004) 1176.pdf SPECTRAL AND GEOCHEMICAL CHARACTERISTICS OF LAKE SUPERIOR TYPE BANDED IRON FORMATION: ANALOG TO THE MARTIAN HEMATITE OUTCROPS. Alicia Fallacaro1 and Wendy M. Calvin1, 1University of Nevada, Reno. Introduction: The Thermal Emission Spectrome- tance in the TIR (5 to 50 mm). Geochemical analyses ter (TES) onboard Mars Global Surveyor discovered including thin section analysis, X-ray diffraction grey, crystalline hematite based on its fundamental (XRD), and scanning electron microscopy (SEM) were oxide vibrational features at 300, 450, and 525cm-1 at also performed on the samples to attain more detailed Sinus Meridiani (SM), Aram Chaos (AC), and various compositional information and to corroborate mineral- small outcrops within the Valles Marineris (VM) [1]. ogy identified with spectroscopy. The minerals com- One of the proposed formation mechanisms for the posing the separate BIF facies are possible auxiliary grey, crystalline hematite is through precipitation of minerals to the hematite deposits on Mars. Data col- ferric oxides in iron rich waters as in terrestrial banded lected in this study can be directly compared to data iron formation (BIF) [1]. Subsequent burial metamor- gathered by the Mars Exploration Rover Opportunity phism would crystallize the deposit. (MER-B) at the Meridiani Planum landing site to de- Archean earth banded iron formation was first termine whether or not a banded iron formation like suggested as a possible terrestrial analog for early process has occurred. This is significant because it Mars based on the hypothesis that dark regions on requires the stability of a large body of water for an Mars could be chemically altered, containing ferrous extended period of time at some point in Mars’ history. clay alteration minerals similar to those in BIF [2]. A Oxide facies. The oxide samples occur in two dis- recent study of the Mariner 6 and 7 spectra shows in- tinct forms of grey, crystalline hematite along with creased hydration signatures in the SM and AC hema- chert and minor magnetite. The hematite exists as dis- tite regions further supporting an aqueous formation tinct, thin bands alternating with chert bands in typical mechanism [3]. Due to the lack of a volcanic source BIF structure (figure 1), and in a more metamorphosed and subsequent volcanic features surrounding the state as bulk, crystalline hematite with a schistose tex- Martian hematite regions, and the increased hydration ture. The schistose samples are also associated with signatures, a sedimentary, aqueous depositional envi- accessory metamorphic minerals. ronment is the preferred interpretation for this re- search, and thus terrestrial BIF is chosen as an appro- priate analog. Terrestrial BIF: James (1954) [4] has defined iron formation as being a chemical sedimentary rock, typi- cally thin banded and/or finely laminated, containing at least 15% iron of sedimentary origin and commonly but not necessarily containing layers of chert. Iron formation consists of four facies: sulfide, carbonate, silicate, and oxide. Their occurrence is controlled by the Eh/pH levels within the depositional environment. A reducing environment precipitates iron sulfide (py- Figure 1. Photographs of banded oxide sample at rite), intermediate conditions precipitate iron carbonate the two orientations measured for emission spectra. (siderite) and iron silicates such as chamosite and stilpnomelane, and an oxidizing environment precipi- The banded oxide samples are dominated by tates iron oxide (hematite). In the Lake Superior BIF, hematite features in the VNIR/SWIR. The emission the iron oxide magnetite accompanies the carbonate, spectra vary with a hematite versus a banded (cross silicate, and oxide facies as it is a combination of fer- sectional) face. The banded faces are dominated by rous (Fe2+) and ferric (Fe3+) iron and precipitates in quartz features, and the hematite face is dominated by intermediate to oxidizing conditions. Lake Superior oxide features with weak to non-existent quartz fea- Type BIF differs from other types of BIF due to its tures (figure 2). The schistose samples have much sedimentary (rather than volcanic) origin [5]. weaker hematite features in the VNIR/SWIR consis- Samples from the oxide, carbonate, and silicate fa- tent with coarser grained hematite. However, the ox- cies have been collected from Lake Superior Type BIF ide emission features in the schistose samples are two in northern Michigan from the Marquette and Gogebic to three times stronger than in the banded samples. iron districts. They have been measured for reflec- tance in the VNIR/SWIR (0.4 to 2.5 mm) and emit- Lunar and Planetary Science XXXV (2004) 1176.pdf Figure 2. Banded oxide emission spectra measured at two orientations. The red arrows denote hematite features and the green arrows denote quartz features. Carbonate facies. The carbonate samples generally consist of banded quartz and siderite with minor amounts of magnetite and chlorite. Carbonate sample spectra vary with weathered versus fresh surfaces in Figure 3. Emission spectra of weathered and fresh surfaces of reflectance and emittance. In reflectance, the weath- carbonate facies BIF. Green arrows are denoting quartz fea- ered surfaces show evidence of ferric iron, while the tures and blue arrows call out carbonate features. fresh surfaces show only ferrous iron associated with the mineral siderite. However, neither the fresh nor Detecting BIF on Mars: Current and future mis- weathered surfaces exhibit carbonate features around sions to Mars will be further investigating the surface 2.35 mm. This could be due to the very fine grain size, composition of Mars, with special interest in the or the presence of opaques scattered throughout the hematite regions. MER-B “Opportunity”, lands at Me- sample. ridiani Planum on 1/24/04 to analyze the hematite de- In emittance, the weathered surfaces show weak to posit. CRISM (Compact Reconnaissance Imaging non-existent carbonate features, and quartz features. Spectrometer for Mars) is a hyperspectral instrument The fresh surfaces show much stronger carbonate scheduled for launch in 2005 on the Mars Reconnais- bands in addition to the quartz bands (figure 3). sance Orbiter (MRO). Silicate facies. There are two silicate samples; one MER B is equipped with six instruments capable of is silicate iron formation and the other is a Precambrian imaging, and assessing geochemistry on the surface of greenstone from the underlying basement rock. In Mars at a spatial resolution comparable to holding a reflectance the weathered greenstone and the silicate hand sample. Several compositional and textural diag- iron formation show ferric iron features consistent with nostic characteristics of BIF should be identifiable with chlorite. The greenstone also has features around 2.3 this payload. mm that are consistent with chlorite. The hyperspectral nature of the CRISM instr ument In emittance, the silicate BIF has a feature at 1060 should easily detect spectral differences in iron miner- cm-1 that closely resembles amesite, a Mg endmember alogy associated with BIF in the VNIR/SWIR region serpentine, as well as quartz features at the longer from 0.4 to 4.0mm. wavelengths. The greenstone is a weathered basalt and References: [1] Christensen, P.R. et al. (2001) can be modeled with plagioclase, chlorite, and some JGR, 106, 23,873-23,885. [2] Calvin, W.M. (1998) quartz. GRL, 25, 1597-1600. [3] Calvin, W.M. et al. (2003) 6th Mars, Abstract #3075. [4] James, H.L. (1954) Eco- nomic Geology, 49, 235-291. [5] Gross, G.A. (1983) Precambrian Research, 20, 171-187..
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