The Front-End Electronics Of The Spectrometer Telescope For Imaging X-Rays (Stix) On The Esa Solar Orbiter Satellite

Solar Orbiter is an ESA mission to study the heliosphere in proximity to the Sun, scheduled for launch in January 2017. It carries a suite of ten instruments for comprehensive remote-sensing and in-situ measurements.The Spectrometer Telescope for Imaging X-Rays (STIX), one of the remote sensing instruments, images X-rays between 4 and 150 keV using an Fourier technique. The angular resolution is 7 arcsec and the spectral resolution 1 keV full-width-half-maximum at 6 keV. X-ray detection uses pixelized Cadmium Telluride crystals provided by the Paul Scherrer Institute. The crystals are bonded to read-out hybrids developed by CEA Saclay, called Caliste-SO, incorporating a lownoise, low-power analog front-end ASIC IDeF-X HD. The crystals are cooled to -20 degrees C to obtain very low leakage currents of less than 60 pA per pixel, the prerequisite for obtaining the required spectral resolution.This article briefly describes the mission goals and then details the front-end electronics design and main challenges, resulting in part from the allocation limit in mass of 7 kg and in power of 4W. Emphasis is placed on the design influence of the cooling requirement within the warm environment of a mission approaching the Sun to within the orbit of Mercury. The design for the long-term in-flight energy calibration is also explained.