The images presented in the last section show that these seven compact radio sources
are dominated by 
Jy cores and resolved into core-jet
morphologies. In the cases of PKS 0208-512, 0521-365, and
0637-752, the position angle of the mas-scale structure
seen with VLBI aligns with the position angle of the arcsecond-scale
radio structure, with agreement better than 15 
. In the cases of
PKS 0438-436, 0537-441, and 1514-241, the mas-scale and
arcsecond-scale position angles are significantly misaligned, with agreement
worse than 55 . For PKS 1921-293, no arcsecond-scale radio
emission has been detected, so no comparison between the
mas-scale and arcsecond-scale position angles is possible.
The misalignment angles do not correlate with the statistical
significance of EGRET detectability. PKS 0208-512 and 0537-441 are
strong statistical EGRET detections ( 
significance),
PKS 0521-365 is a weak statistical EGRET detection ( 
significance) and PKS 0438-436, 0637-752, 1514-241, and
1921-293 are EGRET non-detections (Table 4.3). It is important to
repeat that the significance of the EGRET
detection, based on the photon statistics, is being considered here, given that the
identifications of the gamma-ray sources with the radio sources can be made, as Thompson et al. [1995] assert, with high confidence.
The estimates of radio core brightness temperatures for the seven
sources suggest that PKS 0208-512, 0438-438, 0637-752, and 1921-293 are
more highly beamed than PKS 0521-365, and 0537-441, probably requiring Doppler factors of 
2 to explain the 
K source frame brightness temperatures. For PKS 1514-241, a good estimate of the radio core brightness
temperature is not available. However, as for the misalignment angles, the brightness temperatures
for the six sources do not correlate with EGRET detectability (Table
4.3).
Table 4.3: VLBI and EGRET properties of the 7 sources
On the basis of the brightness temperatures and misalignment angles for these seven sources, no strong statement concerning the importance of relativistic beaming for identification by EGRET can be made. Is it possible, however, to increase the number of objects under consideration by examining existing VLBI data in the literature and find trends which could link the gamma-ray and VLBI characteristics of the EGRET-identified sources, or differentiate the EGRET-identified radio sources from radio sources which have not been identified by EGRET?
In investigating these questions the VLBI properties under consideration will be:
1] The apparent speed of components in mas-scale jets.
2] The misalignment of mas-scale and arcsecond-scale jets.
3] Radio core brightness temperatures.
