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We present 23 interferometric images of parsec-scale jet of the quasar PKS1741--03 at 15, 24 and 43 GHz spanning about 13 yr. We model the images as asuperposition of discrete two--dimensional elliptical Gaussian components, withparameters determined by the cross--entropy technique. All the images present aspatially unresolved component (core) and usually two or three componentsreceding from it. The same components were found in simultaneous 24 and 43 GHzmaps, showing the robustness of our model-fitting. The core-shift opacityeffect between these frequencies is weak. We have identified seven componentsmoving along straight lines at constant apparent superluminal speeds($3.5\le\beta_\mathrm{obs}\le 6.1$), with different sky position angles($-186\deg\le \eta\le -125\deg$). The core flux density tracks quite well thefluctuations seen in the historical single-dish light curve at 14.5 GHz, withno measurable delay. The total flux density from the moving jet components isdelayed $\sim$2 yr in relation to the core light curve, roughly the same as thelag between the ejection epoch and the maximum flux density in the light curvesof the jet components. We propose that there are three non-exclusive mechanismsfor producing these delays. From the kinematics of the most robust jetcomponents and the core brightness temperature, we determined the bulk Lorentzfactor ($4.8\le\gamma\le 24.5$) and the jet viewing angle ($0.\deg 35 \le\theta \le 4.\deg 2$); these values agree with previous estimates from thespectral energy distribution of PKS 1741--03 and its radio variability.

Kinematic study of the parsec-scale jet of the quasar PKS 1741--03