“Truth emerges more readily from error than from confusion“
This invisible component, so far perceived through its effects on the large scale expansion of the universe, accounts for about 70% of the total cosmic matter content and it is thought to be responsible for the present phase of cosmic accelerated expansion. A puzzling cosmological constant can reproduce the observations thus far available. Alternatively, a variety of scenarios have been proposed. I am interested in studying the phenomenology of dark energy models, the observational effects on the CMB and cosmic structure formation, deriving model parameter constraints from cosmological data analysis and new observational tests of dark energy.
Cosmic Microwave Background
This relic radiation provides unique information on the early distribution of matter in the universe as well as a variety of phenomena that occurred throughout the cosmic evolution. I am interested in the CMB-large scale structure correlations induced by the late distribution of matter in the universe as a way of testing the gravitational processes that have driven the cosmic structure formation and the matter content of the universe.
N-body Simulations & Non-Linear Structures
The late time distribution of Dark Matter in the universe is the result of complex non-linear gravitational phenomena which are primarily studied through numerical N-body simulations. Dark Matter halos, which results of this processes, are the venues in which cooling baryonic gas falls in to form the structures we observe today. I am interested in the use of N-body simulations to study the cosmology dependence of these processes which are key to understanding the formation of stars and galaxies in the universe. I am also interested in complementary theoretical approaches that aim to provide a mathematical model description of the properties of Dark Matter halos.
The statistics of the initial matter density field carries information on the physics of the very early universe. Standard inflationary models predict a Gaussian spectrum of density fluctuations, while high-energy physics inspired scenarios allow for different type of non-Gaussian correlations. I am particularly interested in predicting the signatures that such non-Gaussian models make on the CMB bispectrum and the properties of the distribution of Dark Matter halos in the late time universe, which will be tested by the next generation of experiments in cosmology.
Galaxies are dusty environments, stellar winds, supernova shocks and radiation pressure can drive dust produced in stars in the intergalactic medium. The properties of the population of dust grains in the IGM is yet to be fully understood. Dust can contribute to the presence of metals in the IGM and its thermal structure. I am interested in studying the cosmological implications of IGM dust, the correlations induced in large scale structure observations and the physical modeling of the dust distribution on cosmic scales.