Warm/Hot Galactic Coronae
by Dr. Yakov Faerman
at Astrophysics and Cosmology Seminar
Wed, 08 Jan 2020, 11:10
Sacta-Rashi Building for Physics (54), room 207
Extended structures of hot gas around galaxies are robust predictions of galaxy formation theory and numerical simulations. X-ray absorption studies of QSO sightlines provide evidence for hot gas around the Milky Way in the form of highly ionized oxygen. Recent observations of metal absorption in the UV show the existence of multiphase gas around L* galaxies in the low redshift universe. Due to the challenging nature of the observations, many questions remain open. Where exactly does the gas reside and what are its properties? What is the extent and the total mass of the corona? These questions are important to our understanding of galaxy evolution and are linked to the properties of gas accretion onto galaxies, star formation, and feedback processes. We construct unified models for the warm/hot corona which successfully reproduce a wide range of observations (UV, X-ray and other). In our models, the corona is a large-scale structure, extending to the virial radius of the MW, and has a significant gas mass, ~1e11 M_sun. We present predictions for absorption and emission observations with future space observatories, such as the ATHENA mission, which will allow to test our models and improve our understanding of the circumgalactic medium.
Created on 01-01-2020 by Zitrin, Adi (zitrin)
Updaded on 01-01-2020 by Zitrin, Adi (zitrin)