Understanding the dark side of the Universe with galaxy surveys

2018 edition

Anna Porredon

One of the fundamental goals of Cosmology is to understand how the Universe has evolved to form the distribution of large-scale structures that we observe today. Cosmological models can predict the properties of this distribution given certain values of the cosmological parameters such as the expansion rate of the Universe, the dark energy that accelerates such expansion, the dark matter and baryonic densities, and parameters related to the early Universe.

Over the past two decades, large galaxy surveys such as the Sloan Digital Sky Survey (SDSS; York et al. 2000), the WiggleZ Dark Energy Survey (Blake et al. 2011) and the Baryon Oscillation Spectroscopic Survey (BOSS; Dawson et al. 2013) have enabled to study in detail the large-scale structure of the Universe, and galaxy clustering has become a powerful tool to study galaxy formation and evolution and to tighten constraints on cosmological parameters. This data complements the information coming from cosmic microwave background (CMB) experiments, the most recent and with more quality being the ones collected by the Planck satellite, of the European Space Agency (ESA) (Planck Collaboration: Ade et al. 2015).

Future galaxy surveys will cover larger volumes and will collect images of better quality than those obtained so far. My thesis aims to analyze the distribution of galaxies from the observations of future surveys, such as the Dark Energy Survey (DES), the Dark Energy Spectroscopic Instrument (DESI), Physics of the Accelerating Universe (PAU) and the Euclid satellite from the European Space Agency (ESA).