| Abstract : | A significant portion of galactic baryonic content resides in a diffuse gaseous halo, the Circumgalactic medium (CGM), which surrounds the galactic disk and extends up to the virial radius. It has become apparent from the recent absorption and emission observations that the gas in the CGM is multiphase. Based on their temperatures, these phases are roughly divided into hot (T > 10^6K), warm (10^5-10^6K), and cold phases (< 10^4K). Recent observations also pointed toward the existence of cold gas out to large radii (> 100 kpc) even in the massive haloes. It leads to the well-debated question: how do these massive halos (whose virial temperature is much higher than that of the cold phase) form the cold gas? and how does cold gas exist at such a large radius? Apart from the cold mode accretion from the Intergalactic medium, the satellite galaxy could be responsible for a significant amount of cold gas in the outer CGM. When a satellite galaxy passes through the CGM of the host galaxy, its cold gas can be stripped by ram pressure and mixed with the CGM of the host galaxy. There can also be significant induced cooling in the mixing layer of stripped cold gas and hot CGM. To study these effects, we investigated a suite of isolated galaxy simulations with GIZMO code, using FIRE-2 physics in the simulation runs. In this talk, I will highlight at what amount and by what processes satellites can populate the cold phase of the CGM which will help us connect some dots in the puzzle of the origin of the cold phase of the CGM. |
