Sulfide ores are a major source of noble (Au, Ag, and Pt) and base (Cu, Pb, Zn, Sn, Co, Ni, etc.) metals and will, therefore, be vital for the self-sustainment of future Mars colonies. Martian meteorites are rich in sulfides, which is reflected in recent findings for surface Martian rocks analyzed by the Spirit and Curiosity rovers. However, the only high-resolution (18 m/pixel) infrared (IR) spectrometer orbiting Mars, the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), onboard the Mars Reconnaissance Orbiter (MRO), is not well-suited for detecting sulfides on the Martian surface. Spectral interference with silicates impedes sulfide detection in the 0.4–3.9 μm CRISM range. In contrast, at least three common hydrothermal sulfides on Earth and Mars (pyrite, chalcopyrite, marcasite) have prominent absorption peaks in a narrow far-IR (FIR) wavelength range of 23–28 μm. Identifying the global distribution and chemical composition of sulfide ore deposits would help in choosing useful targets for future Mars exploration missions. Therefore, we have designed a new instrument suitable for measuring sulfides in the FIR range called the Martian far-IR Ore Spectrometer (MIRORES). MIRORES will measure radiation in six narrow bands (~0.3 µm in width), including three bands centered on the sulfide absorption bands (23.2, 24.3 and 27.6 µm), two reference bands (21.5 and 26.1) and one band for clinopyroxene interference (29.0 µm). Focusing on sulfides only will make it possible to adapt the instrument size (32 × 32 × 42 cm) and mass (<10 kg) to common microsatellite requirements. The biggest challenges related to this design are: (1) the small field of view conditioned by the high resolution required for such a study (<20 m/pixel), which, in limited space, can only be achieved by the use of the Cassegrain optical system; and (2) a relatively stable measurement temperature to maintain radiometric accuracy and enable precise calibration.
We have developed a portable dual-wavelength laser fluorescence spectrometer as part of a multi-instrument optical probe to characterize mineral, organic, and microbial species in extreme environments. Operating at 405 and 532 nm, the instrument was originally designed for use by human explorers to produce a laser-induced fluorescence emission (L.I.F.E.) spectral database of the mineral and organic molecules found in the microbial communities of Earth's cryosphere. Recently, our team had the opportunity to explore the strengths and limitations of the instrument when it was deployed on a remote-controlled Mars analog rover. In February 2013, the instrument was deployed on board the Magma White rover platform during the MARS2013 Mars analog field mission in the Kess Kess formation near Erfoud, Morocco. During these tests, we followed tele-science work flows pertinent to Mars surface missions in a simulated spaceflight environment. We report on the L.I.F.E. instrument setup, data processing, and performance during field trials. A pilot postmission laboratory analysis determined that rock samples acquired during the field mission exhibited a fluorescence signal from the Sun-exposed side characteristic of chlorophyll a following excitation at 405 nm. A weak fluorescence response to excitation at 532 nm may have originated from another microbial photosynthetic pigment, phycoerythrin, but final assignment awaits development of a comprehensive database of mineral and organic fluorescence spectra. No chlorophyll fluorescence signal was detected from the shaded underside of the samples.
Magma White is an analog Mars rover platform created by ABM SE and offered to the developers of scientific equipment built for space exploration missions, who want to test their devices at low-and mid-Technology Readiness Levels in demanding conditions of desert, Alpine and polar regions or artificial environments. The rover offers a remote access to the payload through the Magma White mission control system. The paper summarizes the background of the analog solution. It covers universal interfacing setup and issues related to the team and technological partners, who supply elements of the payloads. Two analog missions provide a case study: Dachstein 2012, when "WISDOM" ground penetrating radar for Exomars was tested onboard Magma White, and Morocco 2013, with "L.I.F.E." payload and complete remote access from Europe.
Lunar sulfides and oxides are a significant source of noble and base metals and will be vital for future human colonies’ self-sustainability. Sulfide detection (pyrite and troilite) applies to many technological fields and use cases, for example, as a raw material source (available in situ on the Lunar surface) for new solar panel production methods. Ilmenite is the primary iron and titanium ore on the Moon and can provide helium-3 for nuclear fusion and oxygen for rocket fuel. The most important ore minerals have prominent absorption peaks in a narrow far-infrared (FIR) wavelength range of 20–40 μm, much stronger than the spectral features of other common minerals, including significant silicates, sulfates, and carbonates. Our simulations based on the linear mixing of pyrite with the silicates mentioned above indicated that areas containing at least 10%–20% pyrite could be detected from the orbit in the FIR range. MIRORES, Multiplanetary far-IR ORE Spectrometer, proposed here, would operate with a resolution down to <5 m, enabling the detection of areas covered by 2–3 m2 of pyrite (or ilmenite) on a surface of ∼17 m2 from an altitude of 50 km, creating possibilities for detecting large and local smaller orebodies along with their stockworks. The use of the Cassegrain optical system achieves this capability. MIRORES will measure radiation in eight narrow bands (0.3 µm in width) that can include up to five bands centered on the ore mineral absorption bands, for example, 24.3, 24.9, 27.6, 34.2, and 38.8 µm for pyrite, marcasite, chalcopyrite, ilmenite, and troilite, respectively. The instrument size is 32 x 32 x 42 cm, and the mass is <10 kg, which fits the standard microsatellite requirements.
Sulfides and oxides are major sources of noble and base metals and will, therefore, be vital for the self-sustainment of future martian or lunar colonies. Martian and lunar meteorites are rich in sulfides (Fitt et al., this session), and this is also reflected in analyzes of surface martian rocks by the Spirit and Curiosity rovers. However, on Mars, the only high-resolution (18 m/pixel) infrared (IR) spectrometer, the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), onboard the MRO (Zalewska et al., this session), is not suited for detecting ore minerals. Spectral interferences with the most common martian silicates impede ore mineral detection in the 0.4-3.9 μm CRISM range. The most important ore minerals on have prominent absorption peaks in a narrow far-IR (FIR) wavelength range of 22-28 μm. Our simulations based on linear mixing of pyrite with the aforementioned silicates indicated that fields containing 10-20% pyrite could be detected from the orbit in the far-IR range. However, ore deposits including massive pyrite on Earth are maximally hundreds of meters by hundreds of meters large (Ciazela M. et al., this session). Therefore, active space FIR spectrometers with spatial resolutions down to ~3 km are not sufficient for searching ore mineralization. Thus, we have designed a new instrument suitable for sulfide identification in the FIR range called MIRORES. The field view of 16.5 x 19.9 m enables detection of areas covered by 33-66 m 2 of pyrite on a surface of ~330 m 2 creating possibilities for detecting large and moderate-size orebodies and probably also their stockworks. MIRORES will measure radiation in six 0.3-0.4-μm-wide bands including those centered at 23.2 μm for marcasite, 24.3 μm for pyrite, 27.6 μm for chalcopyrite, and three reference bands (21.5, 26.0, and 29.0 μm). Troilite (23.8 μm) or ilmenite (22.7 μm) abundant on the Moon can also be measured instead of other minerals. The most advanced, martian version of the instrument should be integrated into a satellite planned to be launched to Mars in 2028. Creation and testing of the MIRORES prototype are scheduled for 2022-2023 within an ESA project no. AO/1-10824/21/NL/RA, supported by an NCN project no.
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