Many astronomical space missions observe at wavelengths which are absorbed by the atmosphere, as for example some infrared, ultraviolet or x-ray bands. Especially UV and x-ray optics have very stringent alignment tolerances due to the small wavelengths. Consequently, telescopes and instruments can only be tested at their operational wavelengths under vacuum conditions. Traditional methods for fixing optical elements and subassemblies (eg.

A novel anti-reflection process was demonstrated which improves the quantum efficiency (QE) of a CMOS image sensor, with particular benefits at the ultraviolet (UV) and near infrared (NIR) ends of the electromagnetic spectrum. Also, the dark current and photoresponse non-uniformity (PRNU) were reduced to about 33% and 55%, respectively, of the values for a conventional control sensor. Spatial resolution seemed to be reduced in the NIR, as indicated by MTF measurements, but further investigations are required.

The supra-THz (>3 THz) bands have been recently proposed for low Earth orbit THz remote sounding missions such as LOCUS (Low-Cost Upper-atmosphere Sounder). In order to achieve coherent detection, heterodyne receivers at supra-THz frequencies are under development by integrating in a single waveguide cavity a Schottky based mixers fed by a Quantum Cascade Laser (QCL) as Local Oscillator (LO). Thanks to the QCL, enough LO power is available to drive the mixer.

Plastic marine litter is a very complex global environmental issue, with plastic litter at the sea surface representing only a small fraction of plastic entering the sea. In this respect, the BLUE project investigated the potential of diverse LIDAR techniques (backscatter, fluorescence, Raman) to address the detection of plastic litter not only floating on the sea surface, but also suspended in the first few metres under the surface, with also a focus on detecting microplastics and discriminating plastic from other types of litter. The approach adopted was four-fold:

For plastic detection, characterisation and tracking, we need rich spectral information, ideally hyperspectral data. We would like hyperspectral data up to short-wave infrared (2500 nm) and around 0.5 m ground sample distance. Neither of these characteristics are existent in current Earth observation missions, and will still be difficult to find in future Earth observation missions.

As required for the ATHENA mission, filters with high opacity for IR/Visible/UV light need to be developed to reduce the straylight in these spectra. At the same time, a high transmission in the x-ray band shall be maintained.The experience from recent developments in the semicon industry of producing suitable large size carbon nanotube-based foils, shall be utilized. These foils shall form the support membrane for the required x-ray filters.

• Build and test an engineering model of innovative X-Ray Fluorescence spectrometer for the Moon
• Demonstrated instrument performance over temperature range during thermal-vac campaign
• Reduction of measurement fluctuation from 25.2% to 3.7 %
• Improvement of accuracy thanks to peak selection algorithm
• World record in term of energy resolution with this type of EDXRF instrument
• Free space weather measurement thanks to Time Domain MCA

Thermo-optical coatings are used to control and to protect sensitive surfaces of satellites and spacecrafts. The paints are mostly either black (high alpha) and conducting or they are white (low alpha) and non-conducting. Most paint also do not originate from Europe. COIN COAT is an acronym for COnducting Inert Non-hazardous COATings and wants to overcome the statement that a conducting paint needs to be black.

Assessments to Prepare and De-Risk Technology Developments - Characterisation of a Liquid Crystal on Silicon Based Laser Beam Steerer for Applications in Free Space Optical Satellite Communications in Low Earth Orbit.