Missions from space for high-resolution earth observation (including greenhouse gases monitoring) require optical sensors covering both Visible channels and the Short Wavelength InfraRed band (SWIR). For SWIR optical sensors, the current approach in Europe is HgCdTe N/P sensors cooled to cryogenic temperature. SWIRup is aiming at developing an alternative photosensitive material to current HgCdTe N/P sensors. It will focus on InGaAs/GaAsSb super-lattice lattice matched to InP substrate, named III-V. The objective is to push the cut off wavelength up to 2,5µm (currently limited to 1,7) adding SWIR bands to the common VISIBLE channels generally proposed on instruments dedicated to earth observation from space. The SWIRup sensor technologies will also provide alternatives to HgCdTe N/P detectors for commercial applications in the SWIR spectral range, such as hyperspectral imaging systems (for airborne, field applications) and Lidar (or active imaging applications). The 2nd objective is to achieve high operating temperature for focal plane arrays, to be the closest possible to room temperature (230 to 290K) compared to the typical 200-210K for current HgCdTe detectors. This will eliminate cryogenic cooling, improving miniaturization, power reduction, efficiency and versatility of the optical payloads, all of which could provide room for increased functionality. The SWIRup technology will be compared to the current reference II-VI technology which is the HgCdTe P/N material, leading to a technology prioritization by type of application, as each material has its own advantages. This II-VI material, already optimized for cooled astronomical application, will be improved to work at higher temperature. The proposal includes the manufacturing and tests of 2D arrays with sensitive module using the new III-V technology and with the II-VI technology. Reaching TRL5 at the end, the highest performance of the 2 technologies will enter industrialization phase and be integrated.

Massive stars are extreme cosmic engines, enriching their environments with chemically processed material throughout their entire life-time, and triggering star and planet formation. Despite their importance for the cosmic evolution, their evolutionary path up to their deaths as spectacular supernova explosions is most uncertain due to the lack of precise knowledge of the physical mechanisms behind mass eruptions. We wish to establish a multidisciplinary, international network of researchers from Europe, Asia, and South America with expertise in a variety of disciplines, and with background in both theory and observations. Our ultimate goal is to enlighten the processes that trigger mass loss in massive stars during extreme phases of their evolution. We will develop cutting-edge numerical codes suitable to describe the chemical and dynamical evolution of the stars, their winds, and their large-scale environments. In addition, we will initiate global observing campaigns utilizing facilities at major renowned observatories in combination with our national facilities, and exploit public archives from ground-based and space missions to acquire an outstanding set of urgently needed highest quality data. Confronting predictions from the numerical models with the observations will empower us to derive the first extensive and comprehensive set of precise physical parameters. The acquired results will significantly enhance our knowledge and lead to major advancements in all related fields. The bulk of exchanges will be undertaken by Early Stage Researchers and young Post-docs, who will be educated and trained in modern observing and data analyzing techniques and in high-performance computation, equipping them with excellent skills for their future careers. We will organize schools and workshops to share knowledge and to communicate and disseminate our results, which will be major breakthroughs and support the leading role of Europe in Astronomy.