Turbulence and Star Formation in a Sample of Spiral Galaxies

TL;DR

This study examines turbulence in spiral galaxies' outer disks using statistical moments of HI data, finding largely uniform turbulence that does not correlate with star formation, and demonstrating the applicability of these methods beyond dwarf galaxies.

Contribution

It applies turbulence statistical analysis methods to spiral galaxies, showing their effectiveness and limitations in understanding star formation processes.

Findings

Gas motions are largely supersonic in sampled galaxies.

Turbulence moments are uniform and do not trace star-forming regions.

Methods are applicable to normal spiral galaxies, not just dwarf galaxies.

Abstract

We investigate turbulent gas motions in spiral galaxies and their importance to star formation in far outer disks, where the column density is typically far below the critical value for spontaneous gravitational collapse. Following the methods of Burkhart et al. (2010) on the Small Magellanic Cloud, we use the third and fourth statistical moments, as indicators of structures caused by turbulence, to examine the neutral hydrogen (HI) column density of a sample of spiral galaxies selected from The HI Nearby Galaxy Survey (THINGS, Walter et al. 2008). We apply the statistical moments in three different methods- the galaxy as a whole, divided into a function of radii and then into grids. We create individual grid maps of kurtosis for each galaxy. To investigate the relation between these moments and star formation, we compare these maps with their far-ultraviolet images taken by the Galaxy Evolution Explorer (GALEX) satellite. We find that the moments are largely uniform across the galaxies, in which the variation does not appear to trace any star forming regions. This may, however, be due to the spatial resolution of our analysis, which could potentially limit the scale of turbulent motions that we are sensitive to greater than ~700 pc. From comparison between the moments themselves, we find that the gas motions in our sampled galaxies are largely supersonic. This analysis also shows that Burkhart et al. (2010)'s methods may be applied not just to dwarf galaxies but also to normal spiral galaxies.