Institute of Astronomy Galaxies Discussion Group 

• Seiji Fujimoto (Copenhagen)
• Friday 10 December 2021, 11:30-12:30
• via zoom .

To attend this talk, please contact Martin Haehnelt.

The cosmic infrared background light is known to have energy comparable to the optical background light, suggesting the importance of infrared observations to understand the other aspect of the universe obscured by cold materials. In this seminar, I will present our latest research on the formation and evolution of galaxies at z_5-7 in a wide range of scales, including active galactic nuclei ( 100 pc to 5 kpc), and circumgalactic media (CGM; ~5-20 kpc), based on the latest (sub)millimeter observations with ALMA and NOEMA. I will discuss what is taking place in the cold side of the early universe, highlighting three recent discoveries: i) CGM-scale [CII]158um gas halos, ii) differential 3D structures between neutral and ionized gases in the ISM, and iii) a young, transitioning-phase quasar forming in a dust-enshrouded starburst at – in a wide range of scales, including active galactic nuclei ( 100 pc to 5 kpc), and circumgalactic media (CGM; ~5-20 kpc), based on the latest (sub)millimeter observations with ALMA and NOEMA. I will discuss what is taking place in the cold side of the early universe, highlighting three recent discoveries: i) CGM-scale [CII]158um gas halos, ii) differential 3D structures between neutral and ionized gases in the ISM, and iii) a young, transitioning-phase quasar forming in a dust-enshrouded starburst at in a wide range of scales, including active galactic nuclei ( 100 pc to 5 kpc), and circumgalactic media (CGM; ~5-20 kpc), based on the latest (sub)millimeter observations with ALMA and NOEMA. I will discuss what is taking place in the cold side of the early universe, highlighting three recent discoveries: i) CGM-scale [CII]158um gas halos, ii) differential 3D structures between neutral and ionized gases in the ISM, and iii) a young, transitioning-phase quasar forming in a dust-enshrouded starburst at z=7.2.