We present 23 interferometric images of parsec-scale jet of the quasar PKS 1741–03 at 15 , 24 and 43 GHz spanning about 13 yr. We model the images as a superposition of discrete two–dimensional elliptical Gaussian components , with parameters determined by the cross–entropy technique .
All the images present a spatially unresolved component ( core ) and usually two or three components receding from it .
The same components were found in simultaneous 24 and 43 GHz maps , showing the robustness of our model-fitting .
The core-shift opacity effect between these frequencies is weak .
We have identified seven components moving along straight lines at constant apparent superluminal speeds ( 3.5 \la \beta _ { \mathrm { obs } } \la 6.1 ) , with different sky position angles ( -186 \degr \la \eta \la - 125 \degr ) .
The core flux density tracks quite well the fluctuations seen in the historical single-dish light curve at 14.5 GHz , with no measurable delay .
The total flux density from the moving jet components is delayed \sim 2 yr in relation to the core light curve , roughly the same as the lag between the ejection epoch and the maximum flux density in the light curves of the jet components .
We propose that there are three non-exclusive mechanisms for producing these delays .
From the kinematics of the most robust jet components and the core brightness temperature , we determined the bulk Lorentz factor ( 4.8 \la \gamma \la 24.5 ) and the jet viewing angle ( 0 \aas@@fstack { \circ } 35 \la \theta \la 4 \aas@@fstack { \circ } 2 ) ; these values agree with previous estimates from the spectral energy distribution of PKS 1741–03 and its radio variability .