Intermediate mass black holes play a critical role in understanding theevolutionary connection between stellar mass and super-massive black holes.However, to date the existence of these species of black holes remainsambiguous and their formation process is therefore unknown. It has been longsuspected that black holes with masses $10^{2}-10^{4}M_{\odot}$ should form andreside in dense stellar systems. Therefore, dedicated observational campaignshave targeted globular cluster for many decades searching for signatures ofthese elusive objects. All candidates found in these targeted searches appearradio dim and do not have the X-ray to radio flux ratio predicted by thefundamental plane for accreting black holes. Based on the lack of anelectromagnetic counterpart upper limits of $2060 M_{\odot}$ and $470M_{\odot}$ 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 isevidence for a central black hole in 47 Tuc with a mass of M$_{\bullet}\sim2300M_{\odot}$$_{-850}^{+1500}$ when the dynamical state of the globular cluster isprobed with pulsars. The existence of an intermediate mass black hole in thecentre of one of the densest clusters with no detectable electromagneticcounterpart suggests that the black hole is not accreting at a sufficient rateand therefore contrary to expectations is gas starved. This intermediate massblack hole might be a member of electromagnetically invisible population ofblack holes that are the elusive seeds leading to the formation of supermassiveblack holes in galaxies.
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