Le 11 octobre 2019
De 10h30 à 12h00
Jonathan Freundlich
Hebrew University
Galaxy history is marked by a peak of star formation ten billion years ago and a subsequent drop of the star formation rate (SFR) by an order of magnitude. To understand this evolution, it is crucial to probe the gas reservoirs from which stars are formed. With programs observing the molecular gas phase in typical star-forming galaxies at different epochs, I will present how the cosmic evolution of the SFR is mainly driven by that of the molecular gas fraction. During the winding-down of star formation, I will further show that the molecular gas content does not seem to correlate with morphology, suggesting an ongoing supply of molecular gas to compensate for star formation while bulges grow. Although structure formation is primarily driven by dark matter (DM) dynamics in ΛCDM cosmology, gas processes can in turn affect the DM distribution at galactic scales. Using theoretical modelling and simulations, I will discuss how outflow episodes and gas density fluctuations induced by stellar feedback can expand both the DM and the stellar distributions and hence provide a simple understanding of the formation of DM halo cores and ultra-diffuse galaxies. The models developed in this context can further help constrain dark matter models, and in particular fuzzy dark matter since large scale fluctuations of fuzzy DM could similarly heat up stellar structures.