The dark matter halo shape of edge-on disk galaxies - III. Modelling the HI observations: results

TL;DR

This study models HI observations of 8 edge-on disk galaxies to analyze their rotation, velocity dispersion, and HI layer thickness, providing insights into dark halo shapes and galaxy structure.

Contribution

It offers detailed modeling of HI data in edge-on galaxies, revealing consistent flaring profiles and potential perturbations, aiding in constraining dark halo flattening.

Findings

Most galaxies show differential rotation.

HI velocity dispersions range from 6.5 to 7.5 km/s.

Flaring profiles are symmetric with a common shape.

Abstract

This is the third paper in a series in which we attempt to put constraints on the flattening of dark halos in disk galaxies. For this purpose we need to analyse the observed XV diagrams in edge-on galaxies to accurately measure the radial HI surface density, the rotation curve and the HI velocity dispersion. We present the results of the modelling of HI observations of 8 HI-rich, late-type, edge-on galaxies. In all of these we find differential rotation. Most systems display HI velocity dispersions of 6.5 to 7.5 km s$^{-1}$ and all except one show radial structure. There is an increase in the mean HI velocity dispersion with maximum rotation velocity, at least up to 120 km s$^{-1}$. Next we analyse the observations to derive the radial variation of the thickness (flaring) of the HI layer. We find that with the exception of the asymmetric IC5052, all of the galaxies in our sample are good candidates for 3D mass modelling to measure the dark halo shape. The flaring profiles are symmetric and have a common shape, increasing linearly inside the stellar disks and exponential outside where the gravitational potential is dominated by the dark halo. In the best example, UGC7321, we find in the inner regions small deviations from the midplane and accompanying increases in thickness of the HI layer that are possibly a result of perturbations by a relatively strong bar.