Internal Kinematics of UM 461 and CTS 1020
  We have used integral field spectroscopy to study the internal kinematics of
the H\,{\sc ii} galaxies CTS 1020 and UM 461. We based our analysis on the
velocity and velocity dispersion maps, and intensity-velocity dispersion
($I-\sigma$) and velocity-velocity dispersion ($V_r-\sigma$) diagrams. We found
that the motion in both star-forming knots of UM 461 has different patterns,
suggesting a weak kinematical connection between the knots. The overall
kinematics of the galaxy is probably affected by stellar feedback. CTS 1020 has
an ordered motion with a gradient compatible with a disc rotating at $\sim50$
km s$^{-1}$, though the velocity field is disturbed. In both galaxies the
highest and lowest $\sigma$ values are distributed in the outer parts and are
associated with the diffuse gas that permeates the galaxies. UM 461 has a
ring-like structure with small regions of increasing $\sigma$ in the eastern
knot, which resemble what we could expect in a collect and collapse scenario of
star formation. We found that UM 461 seems to be more susceptible to stellar
feedback, whereas in CTS 1020 the gravitational potential dominates.
