Abstrakt
Some ultracompact dwarf galaxies (UCDs) have elevated observed dynamical V-band mass-to-light (M/L-V) ratios with respect to what is expected from their stellar populations assuming a canonical initial mass function (IMF). Observations have also revealed the presence of a compact dark object in the centres of several UCDs, having a mass of a few to 15 percent of the present-day stellar mass of the UCD.
This central mass concentration has typically been interpreted as a supermassive black hole, but can in principle also be a subcluster of stellar remnants. We explore the following two formation scenarios of UCDs: (i) monolithic collapse and (ii) mergers of star clusters in cluster complexes as are observed in massively starbursting regions.
We explore the physical properties of the UCDs at different evolutionary stages assuming different initial stellar masses of the UCDs and the IMF being either universal or changing systematically with metallicity and density according to the integrated Galactic IMF theory. While the observed elevated M/L-V ratios of the UCDs cannot be reproduced if the IMF is invariant and universal, the empirically derived IMF that varies systematically with density and metallicity shows agreement with the observations.
Incorporating the UCD-mass-dependent retention fraction of dark remnants improves this agreement. In addition, we apply the results of N-body simulations to young UCDs and show that the same initial conditions describing the observed M/L-V ratios reproduce the observed relation between the half-mass radii and the present-day masses of the UCDs.
The findings thus suggest that the majority of UCDs that have elevated M/L-V ratios could have formed monolithically with significant remnant-mass components that are centrally concentrated, while those with small M/L-V values may be merged star cluster complexes.