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Dynamical State of Groups & Clusters​

Using numerical simulations, we develop and apply a technique that can determine the mass growth history of groups and clusters of galaxies. We apply this method to large samples of observed groups and clusters. We then test how observed properties of the galaxies in the groups depend on their merger history, such as star formation activity, stellar and gas dynamics, and morphologies of central galaxies and their satellites.

relaxedvsunrelaxed_groups1

Figure demonstrating how we build up samples of relaxed and unrelaxed groups of galaxies, using a combination of the luminosity gap and central galaxy offset, as shown in Raouf et al. 2019.

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