ABSTRACT During a systematic search for supermassive black holes (SMBHs) not in galactic nuclei, we identified the compact, symmetric radio source B3 1715+425 with an emission-line galaxy offset ≈ 8.5 kpc from the nucleus of the brightest cluster galaxy (BCG) in the redshift z = 0.1754 cluster ZwCl 8193. B3 1715+425 is too bright (brightness temperature T b ∼ 3 × 10 10 K at observing frequency ν = 7.6 GHz ) and too luminous (1.4 GHz luminosity L 1.4 GHz ∼ 10 25 W Hz − 1 ) to be powered by anything but an SMBH, but its host galaxy is much smaller ( ∼ 0.9 kpc × 0.6 kpc full width between half-maximum points) and optically fainter (R-band absolute magnitude M r ≈ − 18.2 ) than any other radio galaxy. Its high radial velocity v r ≈ 1860 km s − 1 relative to the BCG, continuous ionized wake extending back to the BCG nucleus, and surrounding debris indicate that the radio galaxy was tidally shredded passing through the BCG core, leaving a nearly naked SMBH fleeing from the BCG with space velocity v ≳ 2000 km s − 1 . The radio galaxy has mass M ≲ 6 × 10 9 M ⊙ and infrared luminosity L IR ∼ 3 × 10 11 L ⊙ close to its dust Eddington limit, so it is vulnerable to further mass loss from radiative feedback.