Dynamical Modelling and the Origin of Gas Turbulence in Z~4.5 Galaxies

In recent years, a growing number of regularly rotating galaxy discs have been found at z geq 4. Such systems provide us with the unique opportunity to study the properties of dark matter (DM) halos at these early epochs, the turbulence within the interstellar medium and the evolution of scaling relations. Here, we investigate the dynamics of four gas discs in galaxies at z sim 4.5 observed with ALMA in the CII 158 mu m fine-structure line. We aim to derive the structural properties of the gas, stars and DM halos of the galaxies and to study the mechanisms driving the turbulence in high- z discs. We decomposed the rotation curves into baryonic and DM components within the extent of the CII discs, that is, 3 to 5 kpc. Furthermore, we used the gas velocity dispersion profiles as a diagnostic tool in investigating the mechanisms driving the turbulence in the discs. We obtain total stellar, gas and DM masses in the ranges of $ (M/M_ odot = 10.3 - 11.0$, $9.8 - 11.3$, and $11.2 - 13.3$, respectively. We find dynamical evidence in all four galaxies for the presence of compact stellar components conceivably, stellar bulges. The turbulence present in the galaxies appears to be primarily driven by stellar feedback, negating the necessity for large-scale gravitational instabilities. Finally, we investigate the position of our galaxies in the context of local scaling relations, in particular the stellar-to-halo mass and Tully-Fisher analogue relations.