Mercury Imaging X-ray spectrometer (MIXS)

The MIXS Instrument

MIXS Diagram
Flight Model MIXS instrument prior to delivery.

The Mercury Imaging X-ray Spectrometer (MIXS) is designed to determine the surface composition of the planet by means of fluorescent X-ray spectroscopy. The Solar Intensity X-ray Spectrometer (SIXS: J. Huovelin, University of Helsinki, PI) is the essential monitor of the solar X-ray flux which, along with solar wind protons, excites the characteristic K-series lines of the elements present in surface material. MIXS is also concerned with the interaction of the solar wind with Mercury’s magnetosphere and exosphere which is expected to produce intensive emission of continuum X-rays.

The MIXS-T channel of the instrument features the first true imaging X-ray telescope to be used in planetary science – realised using microchannel plate (MCP) optics manufactured by Photonis SAS (Brive, France). MIXS-T has an angular resolution of 10 arcminutes, which is sufficient to resolve surface features, dependent on solar flare state, smaller than 20km across. A second, conventional non-imaging collimated channel is provided by MIXS-C with superior grasp to MIXS-T, but no spatial resolution on scales less than the field-of-view 10 degrees. The detectors for both channels are 64 x 64 pixels in a macropixel DEPFET active pixel sensor geometry (Max Planck Semiconductor Laboratory, Munich). The energy resolution of these devices is expected to be sufficient to resolve the K series lines of all the elements of interest. An excellent low-energy detector response opens up the possibility of measuring Fe abundance from the L-alpha line at 0.7 keV.

 

The instruments were named by our Finnish collaborators and the names have a hidden meaning:
MIXS is Finnish for 'Why'?
SIXS is Finnish for 'That's Why!'

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