QUBIC experiment:
In the context of the standard cosmological model, the structures of the Universe are formed from small primordial fluctuations. Inflationary models not only predict the spectrum of scalar fluctuations, but also predict a small percentage of tensor fluctuations, or primordial gravitational waves. These gravitational waves leave a particular trace in the polarization of the Cosmic Microwave Background (CMB), called B polarization modes. Measuring this polarization pattern would constitute the first indirect observational evidence of the inflationary period. Currently, there are many observational efforts aimed at measuring this signal, which is not only small, but also heavily contaminated by polarized radiation from our galaxy. The QUBIC (Q & U Bolometric Interferometer for Cosmology) experiment aims at measuring the polarization of the CMB. It presents a novel infrastructure of bolometric interferometer that will observe at 150 and 220 GHz, and stands out among its competitors for combining the sensitivity of bolometric detectors with the high systematic error control characteristic of interferometers. The analysis of data from an experiment of this nature is complicated, but in turn allows the radiation to be separated into additional subfrequencies within each of the bands, and thus obtain a wider spectral coverage than originally thought. This allows contaminants to be better separated from primordial radiation.
Large scale structure:
The primordial perturbations evolve to give rise to the large-scale structure that we observe today in the Universe. The study of the clustering of matter is a valuable tool for testing cosmological models. One way of studying the clustering is through the two-point correlation function, or its analog in Fourier space, the power spectrum. Theoretically, the study of the formation of structures is usually done through numerical N-body simulations, to follow the evolution of perturbations in the nonlinear regime. When these simulations consider only dark matter, they can then be subjected to semi-analytical codes that simulate the formation of galaxies within the dark matter halos generated by the N-body simulation. The treatment of orphan galaxies (those that have lost their dark matter halo during their evolution) is somewhat ambiguous within semi-analytical codes. One possibility is to use the clustering of matter to set limits to possible approaches to deal with orphan galaxies.
Another way to study dark matter deficient galaxies is through cosmological hydrodynamical simulations, where both the baryonic and dark matter can be followed.