Massive stars are the cornerstone of the dynamic and chemical evolution of the cosmos, enriching it as they evolve with chemically processed material that is blown away from their surface by energetic winds and eruption processes. Despite their importance, their evolution from cradle to death as spectacular supernova explosions still poses many mysteries due to crucial knowledge gaps in the physical processes taking place in their interior and atmosphere and the mutual influence by close-by siblings. Our ultimate goal is to elucidate the physical properties and evolution of massive stars impacted by companions, as well as their contribution to the generation of gravitational waves. For this, we wish to establish a multidisciplinary, international network of researchers from Europe and America with expertise in various disciplines, and with background in both theory and observations. We will exploit the avalanche of public data archives and develop machine learning algorithms to detect massive stars in binary and multiple systems, classify them, and create statistically meaningful samples for diverse evolutionary states. We will develop progressive methods of signal processing for the analysis of the stellar properties, and cutting-edge numerical codes to unveil the impact of stellar interaction and mass ejection on the evolution of the stars and stellar systems. 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 PhD students and Postdocs, whom we will educate and train in modern observing and data analysing techniques, machine learning algorithms, and in high-performance computing, equipping them with excellent skills for their future careers. We will organise schools, workshops and educational activities to share knowledge as well as disseminate our results, which will be major breakthroughs and will expand Europe's leading role in basic research.

Understanding the Physics of Inflation is one of the key questions in present-day fundamental cosmology. For this purpose, the study of the polarization of the Cosmic Microwave Background (CMB) anisotropies provide a unique probe to the early Universe. However, it is well-known that foreground signals, and in particular emission from our Galaxy, will be the major limiting factor of the possible constraints on the existence of B-modes. This proposal will make use of ESA’s PLANCK satellite mission (30-857 GHz), in combination with the ground-based observations provided by the QUIJOTE experiment (10-20 GHz) and other ancillary radio maps, to address the still open problem of the detailed physical modelling of the radio foregrounds in polarization. This project will provide: a) state-of-the-art legacy maps of the synchrotron and the anomalous microwave emission (AME) in the Northern sky; b) a detailed characterization of the synchrotron spectral index, and the implications for cosmic-rays electron physics; c) a model of the large-scale properties of the Galactic magnetic field; d) a detailed characterization of the AME, including its contribution in polarization; and e) the best complete and statistically significant multi-frequency catalogue (from 10 to 217 GHz) of radio sources in both temperature and polarization. The combination of PLANCK and QUIJOTE will provide reference data products which will be an asset for other sub-orbital experiments, as well as in the preparation of future space missions. Finally, we will also provide specific software tools for a more efficient exploitation of our data products, with functionalities far beyond of the existing ones. These tools will not only allow an advanced visualization, but also they will allow the possibility of carrying out specific predictions/simulations for the design of future B-mode experiments, which we expect it will be widely used by the Cosmology and Astrophysics community.