Poster details
Rapid evolution of the most massive galaxies in the Universe
Abstract
Recent observational evidence points to the existence of highly star forming (10,000 Msun/yr), massive galaxies (~1e11 Msun) in large groups (>6) in the early Universe. We showed in our last work that these galaxies go on to form the most massive galaxies in the Universe by z ~ 4. Each of these individual galaxies should produce powerful starbursts, and should contain active galactic nuclei (AGN). While the galaxies merge they begin to build up a hot, X-ray emitting gaseous environment surrounding the final massive system. However, the role of AGN in the merging process and the final massive galaxy is unclear.
We aim to answer the following questions: When do AGN switch on during the merger process and over what timescale are they active? Do they halt star formation? What role do the AGN play in shaping the early circumgalactic medium? And is the gas detectable in X-rays?
To address these questions, we require numerical simulations of massive galaxy evolution in the early Universe. We have already begun preliminary steps of the project, by selecting massive galaxy clusters and simulating their cores at low resolution to z = 2. The preliminary results are exciting and we see huge star formation rates, supermassive black holes, and galaxies by z ~ 3.
We aim to answer the following questions: When do AGN switch on during the merger process and over what timescale are they active? Do they halt star formation? What role do the AGN play in shaping the early circumgalactic medium? And is the gas detectable in X-rays?
To address these questions, we require numerical simulations of massive galaxy evolution in the early Universe. We have already begun preliminary steps of the project, by selecting massive galaxy clusters and simulating their cores at low resolution to z = 2. The preliminary results are exciting and we see huge star formation rates, supermassive black holes, and galaxies by z ~ 3.