Kiloparsec view of a typical star-forming galaxy when the Universe was $\sim$1 Gyr old II. Regular rotating disk and evidence for baryon dominance on galactic scales

TL;DR

This study analyzes a star-forming galaxy at redshift 5.5 using ALMA data, revealing a regular rotating disk with high turbulence and a baryon-dominated mass distribution, consistent with galaxy evolution models.

Contribution

First detailed kinematic analysis of a $z=5.5$ galaxy showing a regular rotating disk with baryon dominance on galactic scales.

Findings

Galaxy has a regular rotating disk with high velocity dispersion.

The galaxy is baryon dominated within twice its effective radius.

The observed turbulence aligns with models of gas transport and feedback.

Abstract

We present a kinematic analysis of the main-sequence galaxy HZ4 at $z=5.5$. Our study is based on deep, spatially resolved observations of the [CII] 158 $\mu$m transition obtained with the Atacama Large Millimeter/Submillimeter Array (ALMA). From the combined analysis of the disk morphology, the two-dimensional velocity structure, and forward-modeling of the one-dimensional velocity and velocity dispersion profiles, we conclude that HZ4 has a regular rotating disk in place. The intrinsic velocity dispersion in HZ4 is high ($\sigma_{0}=65.8^{+2.9}_{-3.3}$ km s$^{-1}$), and the ratio between the rotational velocity and the intrinsic velocity dispersion is $V_{\rm rot}/\sigma_{0}=2.2$. These values are consistent with the expectations from the trends of increasing $\sigma_{0}$ and decreasing $V_{\rm rot}/\sigma_{0}$ as a function of redshift observed in main-sequence galaxies up to $z\approx4$. Galaxy evolution models suggest that the high level of turbulence observed in HZ4 can only be achieved if, in addition to stellar feedback, there is radial transport of gas within the disk. Finally, we find that HZ4 is baryon dominated on galactic scales ($\lesssim2\times R_{\rm e}$), with a dark matter fraction at one effective radius of $f_{\rm DM}(R_{\rm e})=0.41^{+0.25}_{-0.22}$. This value is comparable to the dark matter fractions found in lower redshift galaxies that could be the descendants of HZ4: massive ($M_{\star}\approx10^{11}~M_{\odot}$), star-forming galaxies at $z\sim2$, and passive, early type galaxies at $z\approx0$.