On central black holes in ultra-compact dwarf galaxies
  CONTEXT: The dynamical mass-to-light (M/L) ratios of massive ultra-compact
dwarf galaxies (UCDs) are about 50% higher than predicted by stellar population
models. AIMS: Here we investigate the possibility that these elevated M/L
ratios are caused by a central black hole (BH), heating up the internal motion
of stars. We focus on a sample of ~50 extragalactic UCDs for which velocity
dispersions and structural parameters have been measured. METHODS: Using
up-to-date distance moduli and a consistent treatment of aperture and seeing
effects, we calculate the ratio Psi=(M/L)_{dyn}/(M/L)_{pop} between the
dynamical and the stellar population M/L of UCDs. For all UCDs with Psi>1 we
estimate the mass of a hypothetical central BH needed to reproduce the observed
integrated velocity dispersion. RESULTS: Massive UCDs (M>10^7 M_*) have an
average Psi = 1.7 +-0.2, implying notable amounts of dark mass in them. We find
that, on average, central BH masses of 10-15% of the UCD mass can explain these
elevated dynamical M/L ratios. The implied BH masses in UCDs range from several
10^5 M_* to several 10^7 M_*. In the M_BH-Luminosity plane, UCDs are offset by
about two orders of magnitude in luminosity from the relation derived for
galaxies. Our findings can be interpreted such that massive UCDs originate from
progenitor galaxies with masses around 10^9 M_*, and that those progenitors
have SMBH occupation fractions of 60-100%. The suggested UCD progenitor masses
agree with predictions from the tidal stripping scenario. Lower-mass UCDs
(M<10^7 M_*) exhibit a bimodal distribution in Psi, suggestive of a coexistence
of massive globular clusters and tidally stripped galaxies in this mass regime.
CONCLUSIONS: Central BHs as relict tracers of tidally stripped progenitor
galaxies are a plausible explanation for the elevated dynamical M/L ratios of
UCDs.
