A series of simulated maps showing the appearance in total intensity o
f flows computed using a recently developed relativistic hydrodynamic
code (Duncan & Hughes) are presented. The radiation transfer calculati
ons were performed by assuming that the flow is permeated by a magneti
c field and fast particle distribution in energy equipartition, with e
nergy density proportional to the hydrodynamic energy density (i.e., p
ressure). We find that relativistic flows subject to strong perturbati
ons exhibit a density structure consisting of a series of nested bow s
hocks, and that this structure is evident in the intensity maps for la
rge viewing angles. However, for viewing angles less than 30 degrees,
differential Doppler boosting leads to a series of knots of emission t
hat lie along the jet axis, similar to the pattern exhibited by many V
LBI sources. The appearance of VLBI knots is determined primarily by t
he Doppler boosting of parts of a more extended flow. To study the evo
lution of a perturbed jet, a time series of maps was produced, and an
integrated flux density light curve created. The light curve shows fea
tures characteristic of a radio-loud AGN: small-amplitude variations a
nd a large outburst. We find that in the absence of perturbations, jet
s with a modest Lorentz factor (similar to 5) exhibit complex intensit
y maps, while faster jets (Lorentz factor similar to 10) are largely f
eatureless. We also study the appearance of kiloparsec jet-counterjet
pairs by producing simulated maps at relatively large viewing angles;
we conclude that observed hot spot emission is more likely to be assoc
iated with the Mach disk than with the outer bow shock.