Star Formation Models for the Dwarf Galaxies NGC 2915 and NGC 1705

TL;DR

This study evaluates star formation models in dwarf galaxies NGC 2915 and NGC 1705, demonstrating that rotational shear significantly influences star formation activity, with models incorporating shear matching observations well.

Contribution

It introduces a star formation model based on HI kinematics characterized by rotational shear, providing a better explanation for star formation in dwarf galaxies than traditional stability criteria.

Findings

Standard Toomre Q parameter fails to predict star-forming regions.

Two-fluid instability models show parts of the inner disk are unstable.

Rotational shear models match observed star formation patterns accurately.

Abstract

Crucial to a quantitative understanding of galaxy evolution are the properties of the inter-stellar medium that regulate galactic-scale star formation activity. We present here the results of a suite of star formation models applied to the nearby blue compact dwarf galaxies NGC 2915 and NGC 1705. Each of these galaxies has a stellar disk embedded in a much larger, essentially star-less HI disk. These atypical stellar morphologies allow for rigorous tests of star formation models that examine the effects on star formation of the HI, stellar and dark matter mass components, as well as the kinematics of the gaseous and stellar disks. We use far ultra-violet and 24 micron imaging from the Galaxy Evolution Explorer and the Spitzer Infrared Nearby Galaxies Survey respectively to map the spatial distribution of the total star formation rate surface density within each galaxy. New high-resolution HI line observations obtained with the Australia Telescope Compact Array are used to study the distribution and dynamics of each galaxy's neutral inter-stellar medium. The standard Toomre Q parameter is unable to distinguish between active and non-active star forming regions, predicting the HI disks of the dwarfs to be sub-critical. Two-fluid instability models incorporating the stellar and dark matter components of each galaxy, in addition to the gaseous component, yield portions of the inner disk unstable. Finally, a formalisation in which the HI kinematics are characterised by the rotational shear of the gas produces models that very accurately match the observations. This suggests the time available for perturbations to collapse in the presence of rotational shear to be an important factor governing galactic-scale star formation.