In the last 10-20 years we have been able to observe vast swathes of the Universe at different wavelengths, allowing us to build high-sensitivity maps of different projected cosmic properties. The statistical correlation between these properties and the density inhomogeneities that underlie the cosmic large-scale structures can then be used to reconstruct the spatial distribution of fundamental cosmological and astrophysical quantities, as well as their evolution in time. In this talk, I will describe a number of methods used to carry out this kind of tomographic reconstruction, present measurements of fundamental properties (structure growth, gas pressure, star formation rate density) resulting from their application to existing data, and discuss the potential of near-future "Stage-IV" experiments to improve on and benefit from these methods, in their quest to improve our understanding of fundamental physics.
Local contact & organizer: Denise LANZIERI
