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A strong hard X‐ray luminosity from a blazar flags the presence of a very powerful jet. If the jet power is in turn related to the mass accretion rate, the most luminous, hard X‐ray blazars should pinpoint the largest accretion rates, and thus the largest black hole masses. These ideas are confirmed by the  Swift  satellite observations of the blazar S5 0014+813, at the redshift   z = 3.366 .  Swift  detected this source with all its three instruments, from the optical to the hard X‐rays. Through the construction of its spectral energy distribution, we are confident that its optical‐ultraviolet (UV) emission is thermal in origin. Associating it with the emission of a standard optically thick geometrically thin accretion disc, we find a black hole mass,   M ∼ 4 × 10 10  M ⊙  , radiating at 40 per cent the Eddington value. The derived mass is among the largest ever found. Super‐Eddington slim discs or thick discs with the presence of a collimating funnel can in principle reduce the black hole mass estimate, but tend to produce spectra bluer than observed.

The blazar S5 0014+813: a real or apparent monster?