  We present Fabry-Perot observations in the H$\alpha$ and [S II] lines to
study the kinematics of the Magellanic-type dwarf irregular galaxy NGC 1569,
these observations allowed us to computed the H$\alpha$ velocity field of this
galaxy. Doing a detailed analysis of the velocity along the line-of-sight and
H$\alpha$ velocity profiles, we identified the origin of most of the motions in
the innermost parts of the galaxy and discarded the possibility of deriving a
rotation curve that traces the gravitational well of the galaxy. We analysed
the kinematics of the ionised gas around 31 supernova remnants previously
detected in NGC 1569 by other authors, in optical and radio emission. We found
that the H$\alpha$ velocity profiles of the supernova remnants are complex
indicating the presence of shocks. Fitting these profiles with several Gaussian
functions, we computed their expansion velocities which rank from 87 to 188 km
s$^{-1}$ confirming they are supernova remnants. Also, we determined the
physical properties such as electron density, mechanical energy, and kinematic
age for 30 of the 31 supernova remnants and found they are in the radiative
phase with an energy range from 1 to 39$\times$10$^{50}$ erg s$^{-1}$ and an
age from 2.3 to 8.9$\times$10$^4$ yr. Finally, we estimated the Surface
Brightness - Diameter ($\Sigma$-D) Relation for NGC 1569 and obtained a slope
$\beta$ = 1.26$\pm$0.2, comparable with the $\beta$ value obtained for
supernova remnants in galaxies M31 and M33.
