DE LUCIA, GABRIELLAGABRIELLADE LUCIA2022-03-222022-03-2220192075-4434http://hdl.handle.net/20.500.12386/31794Previous chapters of this issue have focused on the formation and evolution of cosmic structures under the influence of gravity alone. In order to make a close link between theoretical models of structure formation and observational data, it is necessary to consider the gas-dynamical and radiative processes that drive the evolution of the baryonic components of dark matter halos. These processes cover many orders of magnitude in physical sizes and time-scales and are entangled in a complex network of actions, back-reactions, and self-regulations. In addition, our understanding of them is far from being complete, even when viewed in isolation. This chapter provides a brief review of the techniques that are commonly used to link the physical properties of galaxies with the dark matter halos in which they reside. I discuss the main features of these methods, as well as their aims, limits, and complementarities.ELETTRONICOenArticle10.3390/GALAXIES70200562-s2.0-85069970536https://www.mdpi.com/2075-4434/7/2/56/htmhttps://api.elsevier.com/content/abstract/scopus_id/85069970536FIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation