Monday 18 February, 2:30 pm, Curia II
I will discuss results of numerical simulations of the LCDM cosmology constrained to reproduce the large-scale density field in our cosmological neighborhood. I will show that such simulations can be used to address a number of questions, which are difficult to tackle in a traditional approach of using statistical realizations of cosmological density fields. These include kinematics of the local Hubble flow, distribution and possible observational signatures of intergalactic gas, and properties of the Virgo cluster.