The standard model of cosmology has been very successful in describing cosmological observations so far, but with the latest generation of surveys some observational tensions have started to grow significant. If not due to some unknown systematic, this must be accounted for by an extension of the cosmological model, and we consider a particular model that might explain some of the observational features by adding dynamics to the poorly understood dark energy component. Since it ultimately must behave like the standard model on the smallest and largest scales, the extension of the model must only become important at some intermediate region around the size of galaxy clusters, which can be done using non-linearities in the dark energy field equations.
The main work to be presented here is the construction of a simulation pipeline to rigorously explore all implications of such a model, extending on previous work in relaxing conditions of quasi-static evolution and consistently keeping first order perturbations in the metric potentials. I present some of the results of our early investigations and point towards interesting further considerations.
This Friday colloquium will be hybrid. Attendees can therefore participate either in-person or via Zoom. Please join via Zoom at
Meeting ID: 690 0104 3754
Attendees will be muted during the colloquium, but will have the opportunity to ask questions at the end by clicking on the "raise hand” button (or send a request via chat).