Galaxy formation and evolution is determined by the continuous exchange of gas with the circumgalactic medium (CGM) reservoir: gas is accreted into the disk via dense filamentary structures, but it is also continuously expelled through outflows powered by star formation and AGNs. Only recently have simulations been able to capture the complex multi-phase structure of the CGM, thanks to improved physical modelling and higher resolution. In particular, we focus on the puzzling presence of cold gas (T<10^4 K) in the CGM, adopting a tracking algorithm to study the thermal history of this gas and understand what are the most relevant formation channels. The formation of cold gas at recent epochs appears to be possible thanks to gas cooling via thermal instabilities, while cold CGM gas in high-redshift systems is mostly replenished by cold accretion streams. Furthermore, to compare with observational results, we need to post-process our simulations to reproduce the emission in the most relevant lines, in particular CII, OIII, CO and Lya. We achieve this by adopting state-of-art radiative transfer and chemical models, producing surface brightness maps of simulated galaxies, which are key to guide future observations.
This Friday colloquium will be hybrid. Attendees can therefore participate either in-person or via Zoom. Please join via Zoom at
https://uio.zoom.us/j/69001043754?pwd=cEJpbVE5ci9PdWNtRld2TDNNcGtKdz09
Meeting ID:690 0104 3754
Passcode: PeiseStua3
Attendees will be muted during the colloquium, but will have the opportunity to ask questions at the end by clicking on the "raise hand” button (or send a request via chat).