Modelling the galaxy-halo connection in multi-tracer surveys

by Ginevra Favole (IAC/ULL - Tenerife)

Wednesday 27 Apr 2022, 16:30 → 18:30 Europe/Zurich

zoom only

Sub-Halo Abundance Matching (SHAM) is one of the most popular techniques used to connect galaxies to their host dark matter haloes, enabling us to model the galaxy clustering and weak lensing signals. These are fundamental cosmological probes used to constrain the growth of structure and the Universe expansion history. To be reliable and accurate, SHAM has to incorporate the incompleteness effects of the data sets we want to model, as well as the evolution of their galaxy number density. Past surveys, such as SDSS-I/II or SDSS-III/BOSS, mostly targeted luminous red galaxies (LRGs) at low redshift (z<0.7), providing highly complete samples easy to model with a standard SHAM prescription. More recently, SDSS-IV/eBOSS has opened the path to the new generation of multi-tracer surveys by observing emission line galaxies (ELGs) and quasars (QSOs) out to z=2. The next generation of large-scale structure surveys will observe different populations of galaxies, out to high redshifts, with different levels of completeness. I will discuss possible modifications of the standard SHAM prescription to accurately model the clustering signal of incomplete galaxy samples as a function of their galactic properties.