  We have made a high-resolution VLBI observation of the gamma-ray loud quasar
PKS 1622-297 with the HALCA spacecraft and ground radio telescopes at 5 GHz in
1998 February, almost three years after the source exhibited a spectacular GeV
gamma-ray flare. The source shows an elongated structure toward the west on the
parsec scale. The visibility data are well modeled by three distinct
components; a bright core and two weaker jet components. Comparison with
previous observations confirms that the jet components have an apparent
superluminal motion up to 12.1 h^{-1}c, with the inner jet components having
lower superluminal speeds. We apply the inverse Compton catastrophe model and
derive a Doppler factor, \delta, of 2.45, which is somewhat lower than that of
other gamma-ray loud active galactic nuclei (AGNs), suggesting the source was
in a more quiescent phase at the epoch of our observation. As an alternative
probe of the sub-parsec scale structure, we also present the results from
multi-epoch ATCA total flux monitoring, which indicate the presence of
persistent intraday variability consistent with refractive interstellar
scintillation. We examine the gamma-ray emission mechanism in the light of
these observations.
