The link between the intergalactic medium (IGM) and galaxies is a key to understand the evolution of baryonic matter and galaxies. Although several observations have identified the presence of IGM-galaxy connection up to several tens comoving Mpc using Lyα forest absorption as a tracer of IGM HI, the understanding of their variations over galactic properties, such as mass, SFR and population, is still limited. In order to shed more light on the connection, we perform cross-correlation analysis between galaxies and IGM HI evaluated from simulations and observations. For simulations, we use the light cone from cosmological hydrodynamic simulations, GADGET3-Osaka. For observations, we use publicly available IGM HI 3D tomography data, CLAMATO (Lee et al. 2016, 2018), and several galaxy catalogs. In this talk, I will present the similarity and distinction of the correlation functions, and discuss Mpc scale HI environments around galaxies depending on their physical properties.
BIO
Ph.D in University of Tokyo (thesis is about the resolved Kennicutt-Schmid law in nearby galaxies)
Postdoc experiences are in Institute of Cosmic Ray Research in University of Tokyo, National Astronomical Observatory of Japan and National Tsing Hua University in Taiwan
Currently is JSPS fellow in University of Tokyo.
Host: Zheng Cai
