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The origin of ultracompact dwarfs (UCDs), a class of compact stellar systemsdiscovered two decades ago, still remains a matter of debate. Recentdiscoveries of central supermassive black holes in UCDs likely inherited fromtheir massive progenitor galaxies provide support for the tidal strippinghypothesis. At the same time, on statistical grounds, some massive UCDs mightbe representatives of the high luminosity tail of the globular clusterluminosity function. Here we present a detection of a$3.3^{+1.4}_{-1.2}\times10^6\,M_{\odot}$ black hole ($1\sigma$ uncertainty) inthe centre of the UCD3 galaxy in the Fornax cluster, that corresponds to 4 percent of its stellar mass. We performed isotropic Jeans dynamical modelling ofUCD3 using internal kinematics derived from adaptive optics assistedobservations with the SINFONI spectrograph and seeing limited data collectedwith the FLAMES spectrograph at the ESO VLT. We rule out the zero black holemass at the $3\sigma$ confidence level when adopting a mass-to-light ratioinferred from stellar populations. This is the fourth supermassive black holefound in a UCD and the first one in the Fornax cluster. Similarly to otherknown UCDs that harbour black holes, UCD3 hosts metal rich stars enhanced in$\alpha$-elements that supports the tidal stripping of a massive progenitor asits likely formation scenario. We estimate that up to 80 per cent of luminousUCDs in galaxy clusters host central black holes. This fraction should be lowerfor UCDs in groups, because their progenitors are more likely to be dwarfgalaxies, which do not tend to host central black holes.

A 3.5-million Solar Masses Black Hole in the Centre of the Ultracompact Dwarf Galaxy Fornax UCD3