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We used optical images taken with the Very Large Telescope (VLT) in the B andV bands to search for the optical counterpart of PSR J1028-5819 or constrainits optical brightness. At the same time, we used an archival Suzakuobservation to confirm the preliminary identification of the pulsar's X-raycounterpart obtained by Swift. Due to the large uncertainty on the pulsar'sradio position and the presence of a bright (V = 13.2) early F-type star at <4", we could not detect its counterpart down to flux limits of B~25.4 and V~25.3, the deepest obtained so far for PSR J1028-5819. From the Suzakuobservations, we found that the X-ray spectrum of the pulsar's candidatecounterpart is best-fit by a power-law with spectral index 1.7 +/- 0.2 and anabsorption column density NH < 10^21 cm-2, which would support the proposedX-ray identification. Moreover, we found possible evidence for the presence ofdiffuse emission around the pulsar. If real, and associated with a pulsar windnebula (PWN), its surface brightness and angular extent would be compatiblewith the expectations for a ~100 kyr old pulsar at the PSR J1028-5819 distance.

VLT Suzaku observations of the Fermi pulsar PSR J1028-5819