The standard way to extract cosmological information from the large-scale structure is to measure two point functions. This statistic is mostly sensitive to the high density regions, which are highly nonlinear objects. Thus, their clustering properties are highly correlated on small scales and the cosmological information in them is limited.

Stars orbiting in the halo of our galaxy, the Milky Way, are a window into the distribution of dark matter. Tidally disrupting star clusters are especially valuable tracers, because in pristine conditions they produce thin stellar streams of nearly uniform density.

The coming decade will mark a milestone in our understanding of interstellar magnetism: achieving a first reconstruction of the Galactic magnetic field in 3D. This will be crucial for progress in fields such as CMB cosmology and cosmic ray physics. Achieving this goal relies on the combination of (a) high-accuracy data that probe interstellar magnetism and (b) novel algorithms that enable the combination of different datasets. A first step towards this direction can be made through the use of starlight polarization in combination with stellar distances.

In the occasion of the exciting discovery of the electromagnetic counterpart of the GW170817 gravitational wave event, the Dark Energy Survey (DES) collaboration produced a series of studies covering different aspects of the event. In particular, these studies showed that observations of the GW170817 host galaxy can provide information about the formation of the binary neutron star that merged, producing the gravit