  We present the analysis of the archival Suzaku and Swift X-ray observations
of the young $\gamma$-ray pulsar J1932+1916 field. The data revealed a
point-like object at the $\gamma$-ray position of the pulsar and diffuse X-ray
emission around it. Spectra of the point-like source and diffuse emission are
well-described by absorbed power-law models with spectral parameters typical
for pulsar plus pulsar wind nebula systems. Therefore we suggest that Suzaku
and Swift detected the X-ray counterpart of PSR J1932+1916. Assuming this
interpretation, we constrain the distance to the pulsar in the range of 2-6
kpc. We also suggest possible association of the pulsar with the nearby
supernova remnant G54.4-0.3 and discuss its implications for the pulsar proper
motion, age and distance.
