Simulation: LOS velocities of the cold gas (first from left), the LOS contributions of the radial (second from left) and perturbations to the tangential (third from left) components of the in-plane velocities of the star-forming gas particles, as well as the total LOS residual velocities (fourth from left). The scalebars indicate the size of 0$\stackrel{″}{.}$5 at z ≈ 1.52, while the solid and dashed black lines indicate the PA of the galaxy and the bar, respectively. While the overall pattern in the LOS residual velocity field is dominated by the contribution of the radial component, the tangential perturbations contribute significantly, especially in the region close to the major axis. In regions on both the leading and trailing side of the bar, the opposite signs of the radial and tangential contributions, lead to a possible damping of the total residual amplitudes.