The HI - Star Formation Connection: Open Questions

TL;DR

This paper analyzes star formation in HI-selected galaxies using H-alpha and UV data, revealing correlations with the ISM, variations in flux ratios, and implications for the IMF and galaxy evolution.

Contribution

It provides new observational evidence linking star formation properties to galaxy mass, ISM conditions, and suggests IMF variations as a key factor.

Findings

Strong correlation between R band surface brightness and HI cycling time.

Low mass galaxies are more gaseous and less evolved in stars.

Variations in H-alpha to UV flux ratios suggest IMF or photon escape fraction changes.

Abstract

We show data from the Survey of Ionization in Neutral Gas Galaxies (SINGG) and Survey of Ultraviolet emission in Neutral Gas Galaxies (SUNGG) which survey the star formation properties of HI selected galaxies as traced by H-alpha and ultraviolet emission, respectively. The correlations found demonstrate a strong relationship between the neutral ISM, young massive stars, and the evolved stellar populations. For example the correlation between R band surface brightness and the HI cycling time is tighter than the Kennicutt-Schmidt Star Formation Law. Other scaling relations from SINGG give strong direct confirmation of the downsizing scenario: low mass galaxies are more gaseous and less evolved into stars than high mass galaxies. There are strong variations in the H-alpha to UV flux ratios within and between galaxies. The only plausible explanations for this result are that either the escape fraction of ionizing photons or the upper end of the IMF varies with galaxy mass. We argue for the latter interpretation, although either result has major implications for astrophysics. A detailed dissection of the massive star content in the extended HI disk of NGC2915 provides a consistent picture of continuing star formation with a truncated or steep IMF, while other GALEX results indicate that star formation edges seen in Halpha are not always apparent in the UV. These and other recent results settle some old questions but open many new questions about star formation and its relation to the ISM.