  We present MUSE integral field stellar and ionized velocity maps for a sample
of 14 barred galaxies. Most of these objects exhibit "S"-shape iso-velocities
in the bar region indicative of the presence of streaming motions in the
velocity fields. % By applying circular rotation models we observe that bars
leave symmetric structures in the residual maps of the stellar velocity. %which
demonstrates the capabilities of the MUSE instrument for detecting kinematic
bar signatures. % We built non-circular rotation models using the \xs~tool to
characterize the observed velocity fields. In particular we adopt bisymmetric
models and a harmonic decomposition for a bar potential for describing the
non-axisymmetric velocities. We find that both models reproduce the observed
kinematic features. % The position angle of the oval distortion estimated from
the bisymmetric model correlates with the photometric bar position angle
$(\rho_{pearson} = 0.95)$, which suggest that non-circular velocities are
caused by the bar. However because of the low amplitudes of the $s_3$ harmonic
we can not rule out radial flows as possible source. % Because of the weak
detection of \ha~in our objects we are not able to compare gas to stellar
non-circular motions in our sample, although we show that when galaxies are gas
rich the oval distortion is also observed but with larger amplitudes. %
Finally, we do not find evidence that the amplitude of the non-circular motions
is dependent on the bar size, stellar mass or the global SFR.
