Carlos Frenk (ICC, Durham), Simon White (MPA, Garching)

Computer simulations have played a central role in the development of the current structure formation paradigm, the LCDM model. Early simulations of large-scale structure demonstrated the viability of the model, and subsequent developments have enabled ever more precise observational tests. Today's simulations address aspects of cosmic structure, from the innermost structure of dark matter halos, through the visible properties of galaxies and galaxy clusters to the matter distribution on cosmological scales. Simulations are an indispensible tool for testing the validity of the underlying assumptions of LCDM: cold dark matter, dark energy and the inflationary perturbation spectrum.

The ability to model the evolution of baryons in simulations has been a major growth area over the past decade, either through full gasdynamic simulations or through semi-analytic modelling. Mock catalogues from simulations are now routinely used to to link astronomical data to physical models.

The purpose of this session is to bring together experts in simulation of cosmological structure formation to discuss new developments in numerical techniques, particularly in cosmological gasdynamics, as well as recent numerical work addressing galaxy formation, dark matter physics and large-scale structure.

Poster Session A runs from Tuesday 27th March to Wendesday 28th March 2012