  The physical properties of galactic winds are of paramount importance for our
understanding of galaxy formation. Fortunately, they can be constrained using
background quasars passing near star-forming galaxies (SFGs). From the 14
quasar$-$galaxy pairs in our VLT/SINFONI Mgii Program for Line Emitters
(SIMPLE) sample, we reobserved the 10 brightest galaxies in H$_{\alpha}$ with
the VLT/SINFONI with 0.7" seeing and the corresponding quasar with the VLT/UVES
spectrograph. Applying geometrical arguments to these ten pairs, we find that
four are likely probing galactic outflows, three are likely probing extended
gaseous disks, and the remaining three are not classifiable because they are
viewed face-on. In this paper we present a detailed comparison between the
line-of-sight kinematics and the host galaxy emission kinematics for the pairs
suitable for wind studies. We find that the kinematic profile shapes
(asymmetries) can be well reproduced by a purely geometrical wind model with a
constant wind speed, except for one pair (towards J2357$-$2736) that has the
smallest impact parameter b = 6 kpc and requires an accelerated wind flow.
Globally, the outflow speeds are $\sim$ 100 km/s and the mass ejection rates
(or $\dot M _{\rm out}$) in the gas traced by the low-ionization species are
similar to the star formation rate (SFR), meaning that the mass loading factor,
$\eta$ = $\dot M _{\rm out}$/SFR, is $\sim$1.0. The outflow speeds are also
smaller than the local escape velocity, which implies that the outflows do not
escape the galaxy halo and are likely to fall back into the interstellar
medium.
