  We present relativistic magnetohydrodynamic (RMHD) simulations of stationary
overpressured magnetized relativistic jets which are characterized by their
dominant type of energy, namely internal, kinetic, or magnetic. Each model is
threaded by a helical magnetic field with a pitch angle of $45^\circ$ and
features a series of recollimation shocks produced by the initial pressure
mismatch, whose strength and number varies as a function of the dominant type
of energy. We perform a study of the polarization signatures from these models
by integrating the radiative transfer equations for synchrotron radiation using
as inputs the RMHD solutions. These simulations show a top-down emission
asymmetry produced by the helical magnetic field and a progressive confinement
of the emission into a jet spine as the magnetization increases and the
internal energy of the non-thermal population is considered to be a constant
fraction of the thermal one. Bright stationary components associated with the
recollimation shocks appear presenting a relative intensity modulated by the
Doppler boosting ratio between the pre-shock and post-shock states. Small
viewing angles show a roughly bimodal distribution in the polarization angle
due to the helical structure of the magnetic field, which is also responsible
for the highly stratified degree of linear polarization across the jet width.
In addition, small variations of the order of $26^\circ$ are observed in the
polarization angle of the stationary components, which can be used to identify
recollimation shocks in astrophysical jets.
