An intermediate-mass black hole in the centre of the globular cluster 47
  Tucanae
  Intermediate mass black holes play a critical role in understanding the
evolutionary connection between stellar mass and super-massive black holes.
However, to date the existence of these species of black holes remains
ambiguous and their formation process is therefore unknown. It has been long
suspected that black holes with masses $10^{2}-10^{4}M_{\odot}$ should form and
reside in dense stellar systems. Therefore, dedicated observational campaigns
have targeted globular cluster for many decades searching for signatures of
these elusive objects. All candidates found in these targeted searches appear
radio dim and do not have the X-ray to radio flux ratio predicted by the
fundamental plane for accreting black holes. Based on the lack of an
electromagnetic counterpart upper limits of $2060 M_{\odot}$ and $470
M_{\odot}$ have been placed on the mass of a putative black hole in 47 Tucanae
(NGC 104) from radio and X-ray observations respectively. Here we show there is
evidence for a central black hole in 47 Tuc with a mass of M$_{\bullet}\sim2300
M_{\odot}$$_{-850}^{+1500}$ when the dynamical state of the globular cluster is
probed with pulsars. The existence of an intermediate mass black hole in the
centre of one of the densest clusters with no detectable electromagnetic
counterpart suggests that the black hole is not accreting at a sufficient rate
and therefore contrary to expectations is gas starved. This intermediate mass
black hole might be a member of electromagnetically invisible population of
black holes that are the elusive seeds leading to the formation of supermassive
black holes in galaxies.
