Speaker
Description
The Cosmic Microwave Background (CMB) is an open window to the early Uni-
verse. To compute the CMB Spectrum we need to perturb the FLRW universe since
our universe is no longer homogeneous and isotropic at small scales. Furthermore,
the interaction between photons and electrons induces a perturbation in the photons
temperature. This interaction can be described by the Boltzmann equations. Solving
these equations we can find the CMB Temperature Power Spectrum. On the other
hand, observations from both the sun and our atmosphere strongly suggest that
neutrinos have mass. In this work, we will show how we can compute the quantities
that describe the current percent of matter density, energy density and shape of the
universe for ΛCDM considering massive neutrinos in comparison with the standard
model ΛCDM .
