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 .