  The aim of this work is confirming the optical identification of PSR
B1133+16, whose candidate optical counterpart was detected in Very Large
Telescope (VLT) images obtained back in 2003. We used new deep optical images
of the PSR B1133+16 field obtained with both the 10.4 m Gran Telescopio
Canarias (GTC) and the VLT in the g' and B bands, respectively, to confirm the
detection of its candidate optical counterpart and its coincidence with the
most recent pulsar's radio coordinates. We did not detect any object at the
position of the pulsar candidate counterpart (B~28), measured in our 2003 VLT
images. However, we tentatively detected an object of comparable brightness in
both the 2012 GTC and VLT images, whose position is offset by ~3.03" from that
of the pulsar's candidate counterpart in the 2003 VLT images and lies along the
pulsar's proper motion direction. Accounting for the time span of ~9 years
between the 2012 quasi-contemporary GTC and VLT images and the 2003 VLT one,
this offset is consistent with the yearly displacement of the pulsar due to its
proper motion. Therefore, both the flux of the object detected in the 2012 GTC
and VLT images and its position, consistent with the proper motion-corrected
pulsar radio coordinates, suggest that we have detected the candidate pulsar
counterpart that has moved away from its 2003 discovery position.
