Prace Call: 17th
ID: 2018184444, Leader: Maxime Trebitsch
Affiliation: CNRS / Institut d'Astrophysique de Paris, FR
Research Field: Universe Sciences
Collaborators: Karl-Joakim Rosdahl Centre de Recherche Astrophysique de Lyon FR , Harley Katz University of Oxford UK , Taysun Kimm Yonsei University KR , Christophe Pichon CNRS / Institut d'Astrophysique de Paris FR , Yohan Dubois CNRS / Institut d'Astrophysique de Paris FR , Marta Volonteri CNRS / Institut d'Astrophysique de Paris FR , Ricarda Beckmann CNRS / Institut d'Astrophysique de Paris FR , Adrianne Slyz University of Oxford UK , Julien Devriendt University of Oxford UK
Resource Awarded: 20 Mil. core hours on Joliot Curie - SKL
Massive galaxies assembled most of their mass in the first 3 Gyr of evolution of the Universe, before the peak of cosmic star formation. Supermassive black holes powering bright quasars are often found at the centre of these massive galaxies. The intense star formation and the accretion onto central supermassive black holes release a tremendous amount of energy in the surrounding gas via various feedback channels, whether radiative or hydrodynamical, strongly shaping the gas flows in and around galaxies, and will affect all neighbouring galaxies. Some of the the most pressing questions in astrophysics today are related to the formation history of these early galaxies. Understanding how these objects assembled their mass, how their star formation history is tied to the growth history of their central black hole, how they contribute to the chemical enrichment of the Universe, or what is their exact role in the reionization history of the Universe. While upcoming facilities such as the JWST or the next generation of Extremely Large Telescopes will revolutionize our views on these questions, there is an need for theoretical models to help understand future observations. To this end, we introduce the Obelisk project: a radiation-hydrodynamical cosmological simulation of a proto-cluster and its environment until the peak of cosmic star formation at z ~ 2. Combining state-of-the-art numerical cosmological codes with a detailed comparison with observations will enable us to understand better the high redshift Universe.