Stellar Population Constraints on the Dark Matter Content and Origin of Ultra-Compact Dwarf Galaxies

TL;DR

This study analyzes the stellar populations and dark matter content of ultra-compact dwarf galaxies in the Fornax cluster, providing insights into their origins and challenging some assumptions about their dark matter presence.

Contribution

It offers new spectroscopic data and analysis of UCDs, supporting formation scenarios like tidal stripping and galaxy mergers, and discusses their stellar populations and dark matter content.

Findings

UCDs have little dark matter based on stellar and dynamical mass comparison.

UCDs are more metal-rich than expected for their luminosity, deviating from early-type galaxy relations.

The Kroupa IMF aligns stellar and dynamical masses better than Salpeter for UCD3.

Abstract

We analyse intermediate-resolution VLT FLAMES/Giraffe spectra of six ultra-compact dwarf (UCD) galaxies in the Fornax cluster. We obtained velocity dispersions and stellar population properties by full spectral fitting against PEGASE.HR models. Objects span a large range of metallicities (-0.95 to -0.23 dex), 4 of them are older than 8 Gyr. Comparison of the stellar and dynamical masses suggests that UCDs have little dark matter at best. For one object, UCD3, the Salpeter initial mass function (IMF) results in the stellar mass significantly exceeding the dynamical one, whereas for the Kroupa IMF the values coincide. Although, this object may have peculiar dynamics or/and stellar populations, the Kroupa IMF seems more realistic. We find that UCDs lie well above the metallicity-luminosity relation of early-type galaxies. The same behaviour is demonstrated by some of the massive Milky Way globular clusters, known to contain composite stellar populations. Our results support two following UCD formation scenarii: (1) tidal stripping of nucleated dwarf elliptical galaxies; (2) formation of tidal superclusters in galaxy mergers. We also discuss some of the alternative channels of the UCD formation binding them to globular clusters.