  We have developed a new tool to analyse galaxies in the EAGLE simulations as
close as possible to observations.We investigated the evolution of their
kinematic properties by means of the angular momentum proxy parameter,$
\lambda_{Re} $for galaxies with $M_{*} \ge 5 \times 10^{9} M_{\odot}$ in the
RefL0100N1504 simulation up to redshift two (z = 2). Galaxies in the simulation
show a wide variety of kinematic features, similiar to those found in
integral-field spectroscopic studies. At z=0 the distribution of galaxies in
the ${\lambda}_{Re}-{\epsilon}$ plane is also in good agreement with results
from observations. Scaling relations at z = 0 indicate that there is critical
mass, $M_{crit} = 10^{10.3} M_{\odot}$, that divides two different regimes when
we include the ${\lambda}_{Re}$ parameter. The simulation shows that the
distribution of galaxies in the ${\lambda}_{Re}-{\epsilon}$ plane evolves with
time until z = 2 when galaxies are equally distributed both in ${\lambda}_{Re}$
and ${\epsilon}$. We studied the evolution of ${\lambda}_{Re}$ with time and
found that there is no connection between the angular momentum at z = 2 and z =
0. All systems reach their maximum ${\lambda}_{Re}$ at z = 1 and then steadily
lose angular momentum regardless of their merger history, except for the high
star-forming systems that sustain that maximum value over time. The evolution
of the Re in galaxies that have not experienced any merger in the last 10 Gyr
can be explained by their level of gas accretion.
