J1427-4206.-The core is 0.25 mas in size. There is extended emission to the
north and east (Tingay et al. 2002).
3.3.14. 1424-418 This is one of the most compact radio sources in our
sample. The radio data show a jet extending 1" to the west of a
compact core before becoming diffuse (Fig. 1n). We detect no associated
extended X-ray emission.
PKS 1424-418 (Fig. 1o).--This is a highly optically polarized quasar (Impey &
Tapia 1988, 1990). An accurate redshift measurement of z=1.524 was made by
Stickel et al. (1989). Data on PKS 1424-418 from the 2.3 GHz SHEVE observations
were modeled by two circular components separated by 23 mas (Preston et
al. 1989). Our VLBI image shows two components separated by ~3 mas. Assuming the
stronger component is the core, the position angle of the weaker component is
260^deg^, significantly different from the reported value for the two 2.3 GHz
components of 236^deg^/284^deg^ (Preston et al. 1989). There is a difference in
alignment of 90^deg^ between the VLBI and VLA structures. Using the model
results, we obtain a very flat spectral index of -0.04 for the central core. For
comparison, we calculated a spectral index of 0.20 from the correlated flux
density measured at 2.3 and 8.4 GHz (Robertson et al. 1993). An asymmetry was
also inferred from those data.