Prof. Sanchayeeta Borthakur

Galaxy growth is an active but slow process. For galaxies to maintain a gas disk at the current epoch after billions of years of converting gas into stars, there must be a pathway for new gas to feed the disks. However, detecting gas flows into galaxies is hard as the gas is faint and slow-moving. One of the most promising regions in the search is the disk-halo interface, where new data uncover signs of gas condensation. In this talk, I will discuss the results from our ongoing DIISC (Deciphering the Interplay between the ISM, Stars, and the CGM) survey, which probes the disk-CGM interface with QSO sightlines. I'll discuss our findings of large extended disks in terms of the signpost of gas accretion and galactic feedback. I will also discuss the prevalence of structures similar to high-velocity clouds and extra-planar gas that are observed in the Milky Way. These gaseous structures represent a pathway for gas accretion into galaxies and can be one of the primary ways galaxy disks grow in the nearby Universe.