The better half -- Asymmetric star-formation due to ram pressure in the
  EAGLE simulations
  We use the EAGLE simulations to study the effects of the intra-cluster medium
(ICM) on the spatially resolved star-formation activity in galaxies. We study
three cases of galaxy asymmetry dividing each galaxy in two halves using the
plane (i) perpendicular to the $\rm \texttt{velocity}$ direction,
differentiating the galaxy part approaching to the cluster center, hereafter
dubbed as the "leading half", and the opposite one "trailing half", (ii)
perpendicular to the $\rm \texttt{radial}$ position of the satellite to the
centre of the cluster, (iii) that maximizes the star-formation rate ($\rm SFR$)
difference between the two halves. For (i), we find an enhancement of the $\rm
SFR$, star formation efficiency ($\rm SFE$), and interstellar medium pressure
in the leading half with respect to the trailing one and normal star-forming
galaxies in the EAGLE simulation, and a clear overabundance of gas particles in
their trailing. These results suggest that ram pressure (RP) is boosting the
star formation by gas compression in the leading half, and transporting the gas
to the trailing half. This effect is more pronounced in satellites of
intermediate stellar masses $\rm 10^{9.5-10.5} M_{\odot}$, with gas masses
above $\rm 10^{9} M_{\odot}$, and located within one virial radius or in the
most massive clusters. In (iii) we find an alignment between the velocity and
the vector perpendicular to the plane that maximizes the $\rm SFR$ difference
between the two halves. It suggests that finding this plane in real galaxies
can provide insights into the velocity direction.
