This purely non destructive characterization enables further analyses (e.g. through mass spectrometry) to be performed, and/or to contribute to sample selection to return to Earth. MicrOmega IR is coupled to a visible microscope: MicrOmega VIS. Thus, the MicrOmega instrument is developed by an international consortium: IAS (Orsay, France), LESIA (Meudon, France), CBM (Orléans, France), University Of Bern (Bern, Switzerland), IKI (Moscow, Russia). This instrument (MicrOmega IR, MicrOmega VIS and the electronics) is selected for the ESA Exomars mission (launch scheduled for 2013). MicrOmega IR will be used in a reduced spectral range (0.9 – 2.6 μm), due to power, mass and thermal constraints: however, most minerals and other constituents have diagnostic spectral signature in this range.
A full demonstrator model of ExoMars/MicrOmega IR has been assembled at IAS and we will present the design and the experimental results.
The visible/near-infrared imaging spectrometer OMEGA  on the Mars Express mission (ESA), coupled to the NASA Martian Exploration Rover , has provided a great change in our vision of Mars [3, 4]. In the near future, we will see a new generation of space probes that will land on Mars, will do some sample in situ analysis or will select interesting ones to return to Earth.
In this context, we are developing at IAS an hyperspectral microscopic imager, MicrOmega IR [5, 6]. This instrument will acquire in situ reflectance spectra of Martian samples, at a scale of the grain size (spatial sampling of 20 μm per pixel), in a non destructive way. It will work in the spectral range 0.9 to 4 μm. MicrOmega will illuminate 5 mm-sized sample sequentially in 600 contiguous wavelengh channels, and will take an image on a matrix detector for each channel. In this way, we get an ‘Image Cube’ in which the full spectrum of the viewed area is acquired in each pixel. This will enable us to retrieve the composition of the different phases since each mineral exhibits a unique signature in the near-infrared through specific absorption bands. This non destructive analysis is a good way to select interesting samples for a sample return mission to Earth or for further in situ analysis. This composition enables us to get new clues about the formation and the evolution of Mars.
MicrOmega is based on the development done for the Rosetta/CIVA MI instrument. In order to adapt this design to the environment of Mars, we decided to replace the grating by an acousto-optic tunable filter (AOTF). This device is composed of an optical medium in which the light is diffracted by an acoustic wave. Its major advantage is that it is a completely passive device: no mechanisms, no cut order glass and no slit like in grating monochromator system are required.
This instrument is selected for the mission ESA/ExoMars rover mission  in the reduced spectral range 0.9-2.6 μm due to thermal, mechanical and power constraints. To demonstrate the feasibility of MicrOmega, we have developped at IAS a full breadboard of the instrument in the ExoMars configuration. It is designed to characterise MicrOmega and shows its performances. We describe the breadboard and show the results.
The breadboard of the ExoMars instrument
We realized at IAS a full breadboard of the MicrOmega IR instrument (fig. 1). This breadboard is composed of the instrument demonstrator (highlighted by the red ellipse) and of the ground system equiment that simulates the rover interface and environnement. The instrument is coupled to a radiator which simulates the Rover cold Finger. This radiator is essential to dissipate the output power generated by a thermoelectric cooler (TEC). This TEC cools down the detector to 190 K in order to have a low dark current.
The temperature of this radiator is controlled not to exeed 263 K on the hot plate of the TEC. The whole breadboard is purged under a nitrogen atmosphere and humidity controlled chamber in order to avoid condensation on the breadboard while the radiator temperature is below 273 K.
The detector is a Sofradir Mars SW 320 x 256 pixels, HgCdTe matrix. This detector has a sensibility from 0.9 to 2.6 μm with a cut off wavelength of 2.53. The monochromatic light is generated by an AOTF with its own illumination system (fig. 2). The optics used in the demonstrator are the spare optics from the Rosetta/CIVA MI model. It is a two doublet lens system with a magnification of one.
The optical diagram of the demonstrator is shown in fig. 3. The AOTF illuminates the sample with an incidence angle of 20°. The optical axis of the imaging optics is perpendicular to the surface of the sample. It images the sample directly on the detector.
The aim of the instrument is to measure the reflectance spectra of the samples. To measure them, we proceed as shown in fig. 4. First we acquire an image with the AOTF OFF to get the reflective background. Then we acquire an “image cube” of the sample with the AOTF ON. Finally we repeat the measurement with a reference target; in our case we choose the Lambertian labsphere SPECTRALON, coupled to a great reflectivity up to 98% .
We process the data as follows: first we substract the background to the sample and reference “image cube”. Then we divide the one by the other, pixel per pixel, and we obtain an “image cube”, each pixel containing a spectrum of the areas viewed.
Up to now, we have tested two types of samples: powders and rocks. We selected three types of minerals: clays (nontronite) with narrow and intense absorption bands, sulfates (kieserite) and mafic minerals (pyroxene or olivine) with large bands and characteristic slopes.
The powder was composed of either one component, or two components, or a mixture of both components (an example is shown in fig. 5). This sample was analysed by MicrOmega and the results are shown in fig. 6.
We also test our instrument on a Martian analog. The results show that we have the capability to analyse and identify each mineral in the sample, at the grain size. The fig. 8 and the fig. 9 represent each a map in false colors showing the two different families of minerals presents in our sample: the low calcium pyroxene, and the high calcium pyroxene. This map was obtained using the spectral parameter used for Omega data processing. We calculate the ratio of two bands in the spectrum in order to emphasize one type of minerals. For the High calcium pyroxene, we take the ratio of the 1.6 – 1.7 μm band to the 2.2 - 2.3 μm band and for the low calcium pyroxene, the ratio of the 1.25 – 1.35 μm band to the 1.8 – 1.9 μm band. The two maps show the instrument’s capability to identify the grains of each family.
Extension of the spectral range up to 4 μm
MicrOmega is designed to cover the extended spectral range 0.9 – 4 μm. In this configuration, the whole instrument needs to be cooled down to 150 K in order to reduce the thermal contribution. The problem is that we need to qualify and design the AOTF and all the components of the instrument (detector and optics) to survive such low temperatures. The detector and the optics are not a problem because solutions exist. Nevertheless, up to now, nobody succeed in qualifying an AOTF down to this temperature. A research and technology program, supported by CNES has been launched since several years. The problem was to weld all the materials of the AOTF (transducers, crystal and box) and to still work at 150 K. A solution was found and we tested the technology down to 140 K (fig. 10).
Our tests and results show that the MicrOmega IR has reached its goals: capacity to identify minerals, low power consumption, good signal to noise ratio. Even if all the subsystems used, for example the imaging optics, are not optimized for the instrument, we have demonstrated the feasibility of the instrument.
The next step will be to realise the qualification model of MicrOmega to go through thermal and vibrations tests. The AOTF has already been tested at low temperature and some tests will be done soon in order to qualify it in vibrations. With this qualification model, we will have also to test its full performances and its limits.
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