When and how did the multitude of observed exo-planets form? The WANDA project aims at tackling this central question by investigating the origin of the ring-like and asymmetric structures observed in protoplanetary disks, the cradle of planets, and pushing such studies to the distant and massive star-forming regions, the locations that best represent the natal environments of the known exo-planets. The WANDA team will employ a novel multi-wavelength and multi-technique observational approach, based on a combination of high-resolution spectroscopy, spatially resolved integral field spectroscopy, and high spatial resolution imaging at near-infrared and millimeter wavelengths. My on-going Large Program at the Very Large Telescope (VLT), together with my VLT/MUSE data, and additional data to be acquired, will be combined to a number of on-going Large and normal Programs on VLT/SPHERE and ALMA. The three PhD students and two Post-docs hired in the WANDA team will work on four work packages, aimed at answering the following specific questions: - Are large cavities and rings observed in disks related to the presence of substantial winds? - Does the presence of planets in disks leave significant imprint on the accretion of material onto the star? - How do externally photoevaporating winds impact the properties of disks and how can we detect them? - How is planet formation in massive star-forming regions different than in nearby low-mass regions? WANDA will push to find a relation between the observed disk structures and the presence of disk winds, or planets, to guide us to better plan future searches for exo-planets in disks. With a better understanding on how to distinguish winds driven by massive nearby stars from those arising from the disk, WANDA will pave the way to explore massive star-forming regions with current and future telescopes, such as ELT and JWST. The quest to understand our origin in the cosmos will be a significant step closer with the WANDA project.

Galaxy groups play a crucial role in modern cosmology by providing the key test for the predictions of models of large-scale structure and galaxy formation and evolution. This is because their hot gas content, and thus their X-ray appearance, is determined by the fundamental ingredient of the modern cosmological models, i.e. the feedback of the supermassive black hole hosted by the central galaxy. However, differently from galaxy clusters, within this general framework, the predictions of the galaxy group baryonic content very vastly depend on the feedback implementation. For this reason, they are the ideal laboratory to provide the ultimate constraint for anchoring the simulations. At present, there are no observational constraints to guide the theory and to discern among the different scenarios. The aim of the present proposal is to fill this fundamental gap in our understanding by characterizing the galaxy group population in terms of baryonic content, from their hot gas on Mpc scale to their galaxy population properties on kpc scale. The main limitation to doing so, thus far, has been the lack of X-ray observations of galaxy groups, due to the low sensitivities of previous surveys. With CLEVeR we will overcome this by taking advantage of the unprecedented statistics and sensitivity at the group mass scale of the eROSITA All Sky Survey in the X-rays. In addition, we will complement eROSITA data with upcoming 4MOST spectroscopic surveys of galaxy groups in the optical and with ancillary datasets that capture specific physical processes of the feedback and the central galaxy itself, such as MaNGA, MUSE, and LOFAR. With such an ultimate dataset, we will, then, be able to study and constrain all relevant components on all relevant scales to nail down the physics of galaxy groups and of their interaction with black hole feedback and, from there, of the large-scale structure simulations of the Universe.