Hierarchical Structure Formation and Modes of Star Formation in Hickson Compact Group 31

TL;DR

Hickson Compact Group 31 exhibits early-stage hierarchical structure formation with active, recent star formation, resembling high-redshift galaxies, and is likely to evolve into a low-mass elliptical galaxy within about a billion years.

Contribution

This study provides detailed characterization of star formation and structure in HCG 31, revealing its first epoch of interaction-induced star formation and its potential evolutionary path.

Findings

Star clusters follow universal scaling relations despite environment.

Group is undergoing initial interaction-induced star formation epoch.

F galaxy is a new structure with no old stellar population.

Abstract

The handful of low-mass, late-type galaxies that comprise Hickson Compact Group 31 is in the midst of complex, ongoing gravitational interactions, evocative of the process of hierarchical structure formation at higher redshifts. With sensitive, multicolor Hubble Space Telescope imaging, we characterize the large population of <10 Myr old star clusters that suffuse the system. From the colors and luminosities of the young star clusters, we find that the galaxies in HCG 31 follow the same universal scaling relations as actively star-forming galaxies in the local Universe despite the unusual compact group environment. Furthermore, the specific frequency of the globular cluster system is consistent with the low end of galaxies of comparable masses locally. This, combined with the large mass of neutral hydrogen and tight constraints on the amount of intragroup light, indicate that the group is undergoing its first epoch of interaction-induced star formation. In both the main galaxies and the tidal-dwarf candidate, F, stellar complexes, which are sensitive to the magnitude of disk turbulence, have both sizes and masses more characteristic of z=1-2 galaxies. After subtracting the light from compact sources, we find no evidence for an underlying old stellar population in F -- it appears to be a truly new structure. The low velocity dispersion of the system components, available reservoir of HI, and current star formation rate of ~10 solar masses per year, indicate that HCG31 is likely to both exhaust its cold gas supply and merge within ~1 Gyr. We conclude that the end product will be an isolated, X-ray-faint, low-mass elliptical.