The MErcury Radiometer and Thermal Infrared Imaging Spectrometer (MERTIS) is an instrument to study mineralogy and temperature distribution of Mercury surface in unprecedented quality. MERTIS was proposed in 2003 as payload of the Mercury Planetary Orbiter spacecraft of ESA-JAXA BepiColombo mission and will reach Mercury in 2026. MERTIS will map the whole surface at 500m resolution combining a push-broom IR grating spectrometer (TIS) with a radiometer (TIR) sharing the same optics, instrument electronics and in-flight calibration components for the whole wavelength range of 7-14μm (TIS) and 7-40μm (TIR). Currently we are developing and testing an ingestion, calibration and transformation pipeline for MERTIS data, from raw telemetry level data to calibrated product and high level derived product. Bepicolombo Science Ground Segment (BC-SGS or SGS) is embracing new technologies for the BepiColombo mission and follows the latest NASA/PDS format, the xml based PDS4. We adopt open source languages and well optimized libraries for the underlying processing. The data processing pipeline is fully containerized via Docker to be independent from transition between server/OSs/environment, drastically reducing the integration and testing time. Due to strict infrastructural constrains like spacecraft downlink bandwidth and onboard mass memory, the already complex observation scenario is subject to further optimizations. This complicates the reconstruction process for higher-level products like global maps of emissivity and thermal inertia.
PLATO<sup>1</sup> is an M-class mission of the European Space Agency’s Cosmic Vision program, whose launch is foreseen by 2026. PLAnetary Transits and Oscillations of stars aims to characterize exoplanets and exoplanetary systems by detecting planetary transits and conducting asteroseismology of their parent stars. PLATO is the next generation planetary transit space experiment, as it will fly after CoRoT, Kepler, TESS and CHEOPS; its objective is to characterize exoplanets and their host stars in the solar neighbors. While it is built on the heritage from previous missions, the major breakthrough to be achieved by PLATO will come from its strong focus on bright targets, typically with m<sub>v</sub>≤11. The PLATO targets will also include a large number of very bright and nearby stars, with m<sub>v</sub>≤8. The prime science goals characterizing and distinguishing PLATO from the previous missions are: the detection and characterization of exoplanetary systems of all kinds, including both the planets and their host stars, reaching down to small, terrestrial planets in the habitable zone; the identification of suitable targets for future, more detailed characterization, including a spectroscopic search for biomarkers in nearby habitable exoplanets (e.g. ARIEL Mission scientific case, E-ELT observations from Ground); a full characterization of the planet host stars, via asteroseismic analysis: this will provide the Community with the masses, radii and ages of the host stars, from which masses, radii and ages of the detected planets will be determined.