Compact Reconnaissance Imaging Spectrometer for Mars

A NASA engineer and the CRISM instrument.

The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) is a visible-infrared spectrometer aboard the Mars Reconnaissance Orbiter searching for mineralogic indications of past and present water on Mars. The CRISM instrument team comprises scientists from over ten universities and led by principal investigator Scott Murchie. CRISM was designed, built, and tested by the Johns Hopkins University Applied Physics Laboratory.

Objectives

CRISM is being used to identify locations on Mars that may have hosted water,[1] a chemical considered important in the search for past or present extraterrestrial life. In order to do this, CRISM is mapping the presence of minerals and chemicals that may indicate past interaction with water - low-temperature or hydrothermal.[2] These materials include iron and oxides, which can be chemically altered by water, and phyllosilicates and carbonates, which form in the presence of water. All of these materials have characteristic patterns in their visible-infrared energy and are readily seen by CRISM. In addition, CRISM is monitoring ice and dust particulates in the Martian atmosphere to learn more about its climate and seasons.

Investigation description

CRISM measures visible and infrared electromagnetic radiation from 370 to 3920 nanometers in 6.55 nanometer increments. The instrument has two modes, a multispectral untargeted mode and a hyperspectral targeted mode. In the untargeted mode, CRISM reconnoiters Mars, recording approximately 50 of its 544 measurable wavelengths at a resolution of 100 to 200 meters per pixel. In this mode CRISM will map half of Mars within a few months after aerobraking and most of the planet after one year.[3] The objective of this mode is to identify new scientifically interesting locations that could be further investigated.[3] In targeted mode, the spectrometer measures energy in all 544 wavelengths. When the MRO spacecraft is at an altitude of 300 km, CRISM detects a narrow but long strip on the Martian surface about 18 kilometers across and 10,800 kilometers long. The instrument sweeps this strip across the surface as MRO orbits Mars to image the surface.[4]

Instrument design

A diagram of the CRISM instrument.

The data collecting part of CRISM is called the Optical Sensor Unit (OSU) and consists of two spectrographs, one that detects visible light from 400 to 830 nm and one that detects infrared light from 830 to 4050 nm. The infrared detector is cooled to –173° Celsius (–280° Fahrenheit) by a radiator plate and three cryogenic coolers.[5] While in targeted mode, the instrument gimbals in order to continue pointing at one area even though the MRO spacecraft is moving. The extra time collecting data over a targeted area increases the signal to noise ratio as well as the spatial and spectral resolution of the image. This scanning ability also allows the instrument to perform emission phase functions, viewing the same surface through variable amounts of atmosphere, which can be used to determine atmospheric properties. The Data Processing Unit (DPU) of CRISM performs in-flight data processing including compressing the data before transmission.

CRISM's Investigations and New Discoveries (2006-present)

CRISM began its exploration of Mars in late 2006. Results from the OMEGA visible/near-infrared spectrometer on Mars Express (2003–present), the Mars Exploration Rovers (MER; 2003–present), the TES thermal emission spectrometer on Mars Global Surveyor (MGS; 1997-2006), and the THEMIS thermal imaging system on Mars Odyssey (2004–present) helped to frame the themes for CRISM's exploration:

Persistently Wet Environments

Aqueous minerals are minerals that form in water, either by chemical alteration of pre-existing rock or by precipitation out of solution. The minerals indicate where liquid water existed long enough to react chemically with rock. Which minerals form depends on temperature, salinity, pH, and composition of the parent rock. Which aqueous minerals are present on Mars therefore provides important clues to understanding past environments. The OMEGA spectrometer and the MER rovers both uncovered evidence for aqueous minerals. OMEGA revealed two distinct kinds of aqueous deposits.[6] The first, containing sulfates such as gypsum and kieserite, is found in layered deposits of Hesperian age (Martian middle age, roughly from 3.7 to 3 billion years ago). The second, rich in several different kinds of phyllosilicates, instead occurs rocks of Noachian age (older than about 3.7 billion years). The different ages and mineral chemistries suggest an early water-rich environment in which phyllosilicates formed, followed by a dryer, more saline and acidic environment in which sulfates formed. The MER Opportunity rover spent years exploring sedimentary rocks formed in the latter environment, full of sulfates, salts, and oxidized iron minerals.

Soil forms from parent rocks through physical disintegration of rocks and by chemical alteration of the rock fragments. The types of soil minerals can tell us if the environment was cool or warm, wet or dry, or whether the water was fresh or salty. Because CRISM is able to detect many minerals that form in soil, a goal was to use the instrument to help decipher ancient Martian environments. CRISM has found a characteristic layering pattern of aluminum-rich clays overlying iron- and magnesium-rich clays in many areas scattered through Mars' highlands.[7] Surrounding Mawrth Vallis, these "layered clays" cover hundreds of thousands of square kilometers.[8][9][10][11][12][13][14][15][16][17][18] Similar layering occurs near the Isidis basin, in the Noachian plains surrounding Valles Marineris,[19] and in Noachian plains surrounding the Tharsis plateau. The global distribution of layered clays suggests a global process. Layered clays are late Noachian in age, dating from the same time as water-carved valley networks. The layered clay composition is similar to what is expected for soil formation on Earth - a weathered upper layer leached of soluble iron and magnesium, leaving an insoluble aluminum-rich residue, with a lower layer that still retains its iron and magnesium. Some researchers have suggested that the Martian clay "layer cake" was created by soil-forming processes, including rainfall, at the time that valley networks formed.[20]

The delta in Eberswalde crater, as imaged by MOC

Lake and marine environments on Earth are favorable for fossil preservation, especially where the sediments they left behind are rich in carbonates or clays. Hundreds of highland craters on Mars have horizontally layered, sedimentary rocks that may have formed in lakes. CRISM has taken many targeted observations of these rocks to measure their mineralogy and how the minerals vary between layers. Variation between layers helps us to understand the sequence of events that formed the sedimentary rocks. The Mars Orbiter Camera found that where valley networks empty into craters, commonly the craters contain fan-shaped deposits. However it was not completely clear if the fans formed by sediment deposition on dry crater floors (alluvial fans) or in crater lakes (deltas). CRISM discovered that in the fans' lowermost layers, there are concentrated deposits of clay.[21][22] More clay occurs beyond the end of the fans on the crater floors, and in some cases there is also opal. On Earth, the lowermost layers of deltas are called bottom set beds, and they are made of clays that settled out of inflowing river water in quiet, deep parts of the lakes. This discovery supports the idea that many fans formed in crater lakes where, potentially, evidence for habitable environments could be preserved.

Not all ancient Martian lakes were fed by inflowing valley networks. CRISM discovered several craters on the western slope of Tharsis that contain "bathtub rings" of sulfate minerals and a kind of phyllosilicate called kaolinite. Both minerals can form together by precipitating out of acidic, saline water. These craters lack inflowing valley networks, showing that they were not fed by rivers - instead, they must have been fed by inflowing groundwater.[23][24]

HiRISE image of the "Home Plate" rock outcrop

The identification of hot spring deposits was a priority for CRISM, because hot springs would have had energy (geothermal heat) and water, two basic requirements for life. One of the signatures of hot springs on Earth is deposits of silica. The MER Spirit rover explored a silica-rich deposit called "Home Plate" that is thought to have formed in a hot spring.[25][26] CRISM has discovered other silica-rich deposits in many locations. Some are associated with central peaks of impact craters, which are sites of heating driven by meteor impact. Silica has also been identified on the flanks of volcanic inside the caldera of the Syrtis Major shield volcano, forming light-colored mounds that look like scaled-up versions of Home Plate. Elsewhere, in the westernmost parts of Valles Marineris, near the core of the Tharsis volcanic province, there are sulfate and clay deposits suggestive of "warm" springs. Hot spring deposits are one of the most promising areas on Mars to search for evidence for past life.

Nili Fossae on Mars - largest known carbonate deposit.

One of the leading hypotheses for why ancient Mars was wetter than today is that a thick, carbon dioxide-rich atmosphere created a global greenhouse, that warmed the surface enough for liquid water to occur in large amounts. Carbon dioxide ice in today's polar caps is too limited in volume to hold that ancient atmosphere. If a thick atmosphere ever existed, it was either blown into space by solar wind or impacts, or reacted with silicate rocks to become trapped as carbonates in Mars' crust. One of the goals that drove CRISM's design was to find carbonates, to try to solve this question about what happened to Mars' atmosphere. And one of CRISM's most important discoveries was the identification of carbonate bedrock in Nili Fossae in 2008.[27] Soon thereafter, landed missions to Mars started identifying carbonates on the surface; the Phoenix Mars lander found between 3–5 wt% calcite (CaCO3) at its northern lowland landing site,[28] while the MER Spirit rover identified outcrops rich in magnesium-iron carbonate (16–34 wt%) in the Columbia Hills of Gusev crater.[29] Later CRISM analyses identified carbonates in the rim of Huygens crater which suggested that there could be extensive deposits of buried carbonates on Mars.[30] However, a study by CRISM scientists estimated that all of the carbonate rock on Mars holds less that the present Martian atmosphere worth of carbon dioxide.[31][32] They determined that if a dense ancient Martian atmosphere did exist, it is probably not trapped in the crust.

Crustal Composition

Understanding the composition of Mars' crust and how it changed with time tells us about many aspects of Mars' evolution as a planet, and is a major goal of CRISM. Remote and landed measurements prior to CRISM, and analysis of Martian meteorites, all suggest that the Martian crust is made mostly of basaltic igneous rock composed mostly of feldspar and pyroxene. Images from the Mars Orbiter Camera on MGS showed that in some places the upper few kilometers of the crust is composed of hundreds of thin volcanic lava flows. TES and THEMIS both found mostly basaltic igneous rock, with scattered olivine-rich and even some quartz-rich rocks.

The first recognition of widespread sedimentary rock on Mars came from the Mars Orbiter Camera which found that several areas of the planet - including Valles Marineris and Terra Arabia - have horizontally layered, light-toned rocks. Follow-up observations of those rocks' mineralogy by OMEGA found that some are rich in sulfate minerals, and that other layered rocks around Mawrth Vallis are rich in phyllosilicates.[33] Both class of minerals are signatures of sedimentary rocks. CRISM has used its improved spatial resolution to look for other deposits of sedimentary rock on Mars' surface, and for layers of sedimentary rock buried between layers of volcanic rock in Mars' crust.

Modern Climates

To understand Mars' ancient climate, and whether it might have created environments habitable for life, first we need to understand Mars' climate today. Each mission to Mars has made new advances in understanding its climate. Mars has seasonal variations in the abundances of water vapor, water ice clouds and hazes, and atmospheric dust. During southern summer, when Mars is closest to the Sun (at perihelion), solar heating can raise massive dust storms. Regional dust storms - ones having a 1000-kilometer scale - show surprising repeatability Mars-year to Mars-year. Once every decade or so, they grow into global-scale events. In contrast, during northern summer when Mars is furthest from the Sun (at aphelion), there is an equatorial water-ice cloud belt and very little dust in the atmosphere. Atmospheric water vapor varies in abundance seasonally, with the greatest abundances in each hemisphere's summer after the seasonal polar caps have sublimated into the atmosphere. During winter, both water and carbon dioxide frost and ices form on Mars' surface. These ices form the seasonal and residual polar caps. The seasonal caps - which form each autumn and sublimate each spring - are dominated by carbon dioxide ice. The residual caps - which persist year after year - consist mostly of water ice at the north pole and water ice with a thin veneer (a few 10's of meters thick) of carbon dioxide ice at the south pole.

Mars' atmosphere is so thin and wispy that solar heating of dust and ice in the atmosphere - not heating of the atmospheric gases - is more important in driving weather. Small, suspended particles of dust and water ice - aerosols - intercept 20–30% of incoming sunlight, even under relatively clear conditions. So variations in the amounts of these aerosols have a huge influence on climate. CRISM has taken three major kinds of measurements of dust and ice in the atmosphere: targeted observations whose repeated views of the surface provide a sensitive estimate of aerosol abundance; special global grids of targeted observations every couple of months designed especially to track spatial and seasonal variations; and scans across the planet's limb to show how dust and ice vary with height above the surface.

The south polar seasonal cap has a bizarre variety of bright and dark streaks and spots that appear during spring, as carbon dioxide ice sublimates. Prior to MRO there were various ideas for processes that could form these strange features, a leading model being carbon dioxide geysers.[34][35][36][37][38][39][40][41][42] CRISM has watched the dark spots grow during southern spring, and found that bright streaks forming alongside the dark spots are made of fresh, new carbon dioxide frost, pointing like arrows back to their sources - the same sources as the dark spots. The bright streaks probably form by expansion, cooling, and freezing of the carbon dioxide gas, forming a "smoking gun" to support the geyser hypothesis.

References

  1. ↑ "CRISM Reaches the Red Planet" (Press release). Johns Hopkins University. 2006-03-11. Archived from the original on 2006-06-24. Retrieved 2006-06-16.
  2. ↑ "CRISM Joins Mars' Water Detectives". Astrobiology Magazine. Retrieved 2006-06-16.
  3. 1 2 "Disappearing with a Trace". APL CRISM website. Archived from the original on 2006-04-30. Retrieved 2006-06-16.
  4. ↑ "Instrument Development". APL CRISM website. Archived from the original on 2006-04-30. Retrieved 2006-06-16.
  5. ↑ "CRISM FactSheet" (PDF). APL CRISM website. Archived from the original (PDF) on 2006-05-19. Retrieved 2006-06-16.
  6. ↑ Bibring JP, Langevin Y, Mustard JF, Poulet F, Arvidson R, Gendrin A, Gondet B, Mangold N, Pinet P, Forget F (2006). "Global mineralogical and aqueous mars history derived from OMEGA/Mars express data". Science. 312 (5772): 400–404. Bibcode:2006Sci...312..400B. PMID 16627738. doi:10.1126/science.1122659.
  7. ↑ Murchie, S. et al. 2009. A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter. Journal of Geophysical Research: 114.
  8. ↑ Poulet et al. 2005. Nature 438, 623–627.
  9. ↑ Loizeau et al. 2007. JGR 112, E08S08
  10. ↑ ] Bishop et al. 2008. Science 321, 830.
  11. ↑ Noe Dobrea et al. 2010. JGR 115, E00D19
  12. ↑ Michalski, Noe Dobrea. 2007. Geol. 35, 10.
  13. ↑ Loizeau et al. 2010. Icarus 205, 396-418.
  14. ↑ Farrand et al. 2009. Icarus 204, 478-488.
  15. ↑ Wray et al. 2010. Icarus 209, 416-421
  16. ↑ Bishop et al. 2013. PSS 86, 130-149.
  17. ↑ ] Michalski et al. 2013. Icarus 226, 816-840.
  18. ↑ Michalski et al. 2010. Astrobio. 10, 687-703.
  19. ↑ Le Deit, L., J. Flahaut, C. Quantin, E. Hauber, D. Mège, O. Bourgeois, J. Gurgurewicz, M. Massé, and R. Jaumann (2012), Extensive surface pedogenic alteration of the Martian Noachian crust suggested by plateau phyllosilicates around Valles Marineris, J. Geophys. Res.,117, E00J05, doi:10.1029/2011JE003983.
  20. ↑ Noe Dobrea, E. Z., et al. (2010), Mineralogy and stratigraphy of phyllosilicate-bearing and dark mantling units in the greater MawrthVallis/west Arabia Terra area: Constraints on geological origin, J. Geophys. Res.,115, E00D19, doi:10.1029/2009JE003351
  21. ↑ Grotzinger, J. and R. Milliken (eds.) 2012. Sedimentary Geology of Mars. SEPM
  22. ↑ Milliken, R. and T. Bish. 2010. Sources and sinks of clay minerals on Mars. Philosophical Magazine: 90. 2293-2308
  23. ↑ https://pubs.er.usgs.gov/publication/70035986
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  27. ↑ Ehlmann; Mustard, JF; Murchie, SL; Poulet, F; Bishop, JL; Brown, AJ; Calvin, WM; Clark, RN; et al. (2008). "Orbital identification of carbonate-bearing rocks on Mars". Science. 322 (5909): 1828–1832. Bibcode:2008Sci...322.1828E. PMID 19095939. doi:10.1126/science.1164759.
  28. ↑ Boynton, WV; Ming, DW; Kounaves, SP; Young, SM; Arvidson, RE; Hecht, MH; Hoffman, J; Niles, PB; et al. (2009). "Evidence for Calcium Carbonate at the Mars Phoenix Landing Site" (PDF). Science. 325 (5936): 61–64. Bibcode:2009Sci...325...61B. PMID 19574384. doi:10.1126/science.1172768 (inactive 2017-01-31).
  29. ↑ Morris, RV; Ruff, SW; Gellert, R; Ming, DW; Arvidson, RE; Clark, BC; Golden, DC; Siebach, K; et al. (2010). "Identification of carbonate-rich outcrops on Mars by the Spirit rover" (PDF). Science. 329 (5990): 421–4. Bibcode:2010Sci...329..421M. PMID 20522738. doi:10.1126/science.1189667.
  30. ↑ Some of Mars' Missing Carbon Dioxide May be Buried
  31. ↑ http://www.space.com/30746-mars-missing-atmosphere-lost-in-space.html
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  33. ↑ Bibring JP, Langevin Y, Mustard JF, Poulet F, Arvidson R, Gendrin A, Gondet B, Mangold N, Pinet P, Forget F (2006). "Global mineralogical and aqueous mars history derived from OMEGA/Mars express data". Science. 312 (5772): 400–404. Bibcode: 2006Sci...312..400B. doi:10.1126/science.1122659. PMID 16627738
  34. ↑ Piqueux, Sylvain; Shane Byrne; Mark I. Richardson (8 August 2003). "Sublimation of Mars's southern seasonal CO2 ice cap formation of spiders" (PDF). Journal of Geophysical Research. 180 (E8): 5084. Bibcode: 2003JGRE..108.5084P. doi:10.1029/2002JE002007. Retrieved 5 September 2009.
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  37. ↑ Kieffer, Hugh H. (2003). "Third Mars Polar Science Conference (2003)- Behavior of Solid CO" (PDF). Retrieved 6 September 2009.
  38. ↑ Portyankina, G., ed. (2006). "Fourth Mars Polar Science Conference - Simulations of Geyser-Type Eruptions in Cryptic Region of Martian South" (PDF). Retrieved 11 August 2009.
  39. ↑ Sz. Bérczi; et al., eds. (2004). "Lunar and Planetary Science XXXV (2004) - Stratigraphy of Special Layers – Transient Ones on Permeable Ones: Examples" (PDF). Retrieved 12 August 2009.
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  41. ↑ "NASA Findings Suggest Jets Bursting From Martian Ice Cap". Jet Propulsion Laboratory. NASA. 16 August 2006. Retrieved 11 August 2009.
  42. ↑ C.J. Hansen, N. Thomas, G. Portyankina, A. McEwen, T. Becker, S. Byrne, K. Herkenhoff, H. Kieffer, M. Mellon (2010). "HiRISE observations of gas sublimation-driven activity in Mars’ southern polar regions: I. Erosion of the surface" (PDF). Icarus. 205: 283–295. Bibcode:2010Icar..205..283H. doi:10.1016/j.icarus.2009.07.021. Retrieved 26 July 2010.
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