Invited speakers
Violeta González-Pérez. UAM (Madrid, Spain).
Title: DESI 2024 Cosmological Results and model galaxies
Abstract: In this talk I will review the main cosmological results from the first year of data from the Dark Energy Survey Instrument (DESI). Cosmological simulations have played a fundamental role to test analysis pipelines and to better determine the systematic errors we induce by our ignorance on galaxy formation and evolution. One of the cosmological tracers targetted by DESI are galaxies with strong spectral emission, ELGs. These are expected to provide one of the densest data sets and they are being targetted by other Stage-IV surveys such as Euclid. I will describe the effort we are making to better understand these galaxies as cosmological tracers at z~1.
Raul Angulo. DIPC (Donostia, Spain).
Title: Modelling baryons for cosmological inferences.
Abstract: Optimal exploitation of future cosmic probes will rely on a detailed understanding of the connection between dark and visible matter in the universe. In this talk I will discuss several physical approaches to model these connections. By combining with suites of gravity-only simulations, this framework delivers predictions for the observed properties of galaxies and gas as a function of cosmological parameters, which will enable high-precision cosmological inferences.
Carles Sánchez. UAB (Barcelona, Spain).
Title: Exploring and exploiting the Cosmological Potential of Angular Redshift Fluctuations
Abstract: Angular Redshift Fluctuations (ARF) constitute a cosmological observable that provides complementary information to other standard 2D cosmological observables like 2D clustering, galaxy shear, or CMB temperature and lensing potential anisotropies. In this talk, I shall explore the added value of ARF when constraining cosmological parameters in upcoming photometric and spectroscopic redshift surveys, and in combination with state-of-the-art CMB experiments. I will outline the particular case of the local non-Gaussianity parameter f_NL, which we constrain in the Quaia quasar survey, and I will also briefly describe the ARF sensitivity on angular *and* radial BAOs, quantifying the improvement on cosmological constraints when combined with 2D clustering. If time allows, I finally explore the sensitivity of ARF to gravity in and around cosmological voids.
Carlos Hernández-Monteagudo. IAC (Tenerife, Spain).
Title: Pushing the limits of imaging galaxy surveys: Cosmology and astrophysics at higher redshifts
Abstract: In this talk I will discuss how to use data from imaging galaxy surveys and CMB experiments to provide robust cosmological and astrophysical constraints in the regime that lies in between the early and late epochs that source the current tensions in the cosmological model of the Universe, the regime at 1 < z < 3. That epoch is not only key to depict a coherent picture for the evolution of the Universe, but also to understand the formation of stars and galaxies. In the past, the precise characterisation of the
large-scale structure in that epoch was not possible, as the galaxy populations from that period were too faint to be observed reliably. Now, with the current and new generation of galaxy surveys and improved analysis methods, it is time to probe this unexplored period in the evolution of the Universe.
I will discuss how to select and use high-redshift galaxy samples from current or future imaging galaxy surveys, which will then be cross-correlated with maps of the weak gravitational lensing of the CMB and maps of the cosmic infrared background (CIB) and thermal Sunyaev-Zeldovich (tSZ) effect from other experiments.
The combination of galaxy clustering and CMB lensing will provide constraints on the amplitude of matter fluctuations at high redshift, which will be crucial for understanding the growth of structures in that high-redshift period. The cross-correlations with CIB and tSZ maps will provide constraints on star formation rates at an epoch where it peaks in the history of the Universe, and will also be used to study the impact of baryonic physics in the analysis of matter fluctuations from weak gravitational lensing. In this way, the usage of various cross-correlations between different probes will allow us to account for all interdependencies between astrophysical and cosmological effects.