Young star clusters in the outer disks of LITTLE THINGS dwarf irregular galaxies

TL;DR

This study uses FUV imaging to identify young star-forming regions in the outer disks of dwarf irregular galaxies, revealing ongoing star formation at large radii and examining the relation between gas density and star formation.

Contribution

It provides new observational evidence of star formation in the far outer disks of dwarf irregular galaxies and analyzes the applicability of the Kennicutt-Schmidt relation in these regions.

Findings

Young star clusters are found 1-8 disk scale lengths from galaxy centers.

Star formation rates in outer disks are about 10% of expected rates based on gas density.

Star formation may occur without forming distinct associations at low surface densities.

Abstract

We examine FUV images of the LITTLE THINGS sample of nearby dwarf irregular (dIrr) and Blue Compact Dwarf (BCD) galaxies to identify distinct young regions in their far outer disks. We use these data, obtained with the Galaxy Evolution Explorer satellite, to determine the furthest radius at which in situ star formation can currently be identified. The FUV knots are found at distances from the center of the galaxies of 1 to 8 disk scale lengths and have ages of <20 Myrs and masses of 20 to 1E5 Msolar. The presence of young clusters and OB associations in the outer disks of dwarf galaxies shows that dIrrs do have star formation taking place there in spite of the extreme nature of the environment. Most regions are found where the HI surface density is ~1 Msolar per pc2, although both the HI and dispersed old stars go out much further. This limiting density suggests a cutoff in the ability to form distinct OB associations and perhaps even stars. We compare the star formation rates in the FUV regions to the average rates expected at their radii and beyond from the observed gas, using the conventional correlation for gas-rich regions. The localized rates are typically 10% of the expected average rates for the outer disks. Either star formation in dIrrs at surface densities <1 Msolar per pc2 occurs without forming distinct associations, or the Kennicutt-Schmidt relation over-predicts the rate beyond this point. In the latter case, the stellar disks in the far-outer parts of dIrrs result from scattering of stars from the inner disk.