Fuzzy dark matter particles are characterized with having such a low mass (log(m/eV) ~ -22) that their de Broglie wavelength becomes relevant on galactic scales (λ ~ kpc). This results in a "quantum pressure" which in turn causes structure suppression below the wavelength scale and to the formation of standing wave cores often referred to as solitons. For these reasons it has been proposed as a solution to the small scales problems of ΛCDM.
The formation of the light elements in the early Universe is strongly related to a series of astronomical and nuclear processes. For this reason, understanding the relation between fundamental parameters and observables can allow us to use our knowledge of nuclear physics and astronomy to constrain cosmological parameters such as number of effective degrees of freedom for radiation and the baryon-to-photon ratio in a way complementary to other observations.
Cosmic strings are one-dimensional topological defects theorized to have formed in a phase-transition in the early Universe. Despite the fact that we know today that strings do not constitute the dominant source of anisotropies, their distinct shape (linear or in loops) and their decay process would leave a perceivable imprint on the CMB. They are often described by a single free parameter the string tension, Gμ.
A systematic treatment of complex mathematical models and of enormous amounts of data requires efficient algorithms and optimized hardware. Part of my research consists in developing and testing the tailored software for the problem at hand. Most of my simulations and modelling tasks are completed on the Niagara supercomputer at the University of Toronto.