Observing the surface of Venus after VIRTIS on VEX

Mathematics – Logic

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[5464] Planetary Sciences: Solid Surface Planets / Remote Sensing, [5480] Planetary Sciences: Solid Surface Planets / Volcanism, [5494] Planetary Sciences: Solid Surface Planets / Instruments And Techniques, [6295] Planetary Sciences: Solar System Objects / Venus

Scientific paper

VIRTIS on the ESA mission Venus Express (VEX) was the first instrument to routinely map the surface of Venus using the near infrared windows from orbit. The VIRTIS instrument is the flight spare of the instrument of the same name on the ESA Rosetta comet encounter mission. Originally designed to observe a very cold target far from the Sun, it was adapted to work in the Venus environment. The instruments main purpose on VEX was to study the structure, dynamics and composition of the atmosphere in 3 dimensions. The idea of surface studies were introduced very late in the mission planning and VIRTIS was never specifically adapted for this purpose. For example the wavelength coverage was not optimal and only the long wavelength flank of the main atmospheric window at 1.02µm could be imaged. Despite all issues VIRTIS was an excellent proof-of-concept and far exceeded our expectations. It provided significant new scientific results and may show for example that Venus had volcanic activity in the very recent geological past. After the very successful proof-of-concept it is now time to assess in more details what can be done with NIR observations of Venus. To support this we have been setting up the Planetary Emissivity Laboratory in Berlin which allows taking emissivity measurements in the spectral range of the atmospheric windows at sample temperatures of 500°C. This would provide a baseline for considering new instrument designs for future Venus missions.

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