PSR J0205+6449 is a X-ray and radio pulsar in supernova remnant 3C 58 . We report on observations of the central region of 3C 58 using the 4.2-m William Herschel Telescope with the intention of identifying the optical counterpart of PSR J0205+6449 and characterising its pulsar wind nebula . Around the pulsar position we identified extended emission with a magnitude of B = 23 \aas@@fstack { m } 97 \pm 0.10 , V = 22 \aas@@fstack { m } 95 \pm 0.05 and R = 22 \aas@@fstack { m } 15 \pm 0.03 consistent with a pulsar wind nebula . From the R-band image we identified three knots with m _ { R } = 24 \aas@@fstack { m } 08 \pm 0.07 ( o1 ) , 24 \aas@@fstack { m } 15 \pm 0.07 ( o2 ) and 24 \aas@@fstack { m } 24 \pm 0.08 ( o3 ) . We confirm the presence of an optical pulsar wind nebula around PSR J0205+6449 and give an upper limit of m _ { R } \approx 24 for the optical magnitude of the pulsar . Furthermore we make the tentative suggestion that our object o1 , with an m _ { R } \approx 24.08 is the optical counterpart . If confirmed the pulsar would have an L _ { R } / L _ { x } \approx 0.004 and an optical efficiency of about 5 % of the Crab pulsar . Such a low efficiency is more consistent with the characteristic age of the pulsar rather than that of SN 1181 .