Daftar Isi: Kinematics and dynamics of molecular gas in high redshift quasars

Daftar Isi:

Molecular hydrogen (H2) is a fundamental component of galaxies, being the most abundant element in molecular clouds, where stars form, and an important source of radiative cooling at low temperature. With the advent of the ALMA telescope, we have started to collect data of the H2 distribution in galaxies with unprecedented resolution. In particular, we are now starting to resolve the distribution of molecular gas in high redshift quasar hosts, and this is giving us important information about the kinematics and dynamics of these systems. However, the large majority of numerical simulations on galactic and cosmological scales still lacks the ability to directly follow the formation and dissociation of H2, and must rely on pre-calibrated sub-grid models to compare the results with observations. I will present a numerical study of the H2 kinematics and dynamics in a massive halo at z=6, expected to be a quasar host, in which I self-consistently follow the evolution of H2 with non-equilibrium chemistry, including gas and dust shielding, H2 self-shielding, star formation, supernova feedback, and extragalactic and local stellar radiation. I will discuss in particular the interplay between the central AGN and its galaxy host, and the launching of outflows, both in the ionised/neutral and molecular phase. I will also show that the apparent obesity of high-redshift massive black holes is due to the gas tracers employed, and not to different intrinsic properties of the systems.