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We present relativistic magnetohydrodynamic (RMHD) simulations of stationaryoverpressured magnetized relativistic jets which are characterized by theirdominant type of energy, namely internal, kinetic, or magnetic. Each model isthreaded by a helical magnetic field with a pitch angle of $45^\circ$ andfeatures a series of recollimation shocks produced by the initial pressuremismatch, whose strength and number varies as a function of the dominant typeof energy. We perform a study of the polarization signatures from these modelsby integrating the radiative transfer equations for synchrotron radiation usingas inputs the RMHD solutions. These simulations show a top-down emissionasymmetry produced by the helical magnetic field and a progressive confinementof the emission into a jet spine as the magnetization increases and theinternal energy of the non-thermal population is considered to be a constantfraction of the thermal one. Bright stationary components associated with therecollimation shocks appear presenting a relative intensity modulated by theDoppler boosting ratio between the pre-shock and post-shock states. Smallviewing angles show a roughly bimodal distribution in the polarization angledue to the helical structure of the magnetic field, which is also responsiblefor the highly stratified degree of linear polarization across the jet width.In addition, small variations of the order of $26^\circ$ are observed in thepolarization angle of the stationary components, which can be used to identifyrecollimation shocks in astrophysical jets.

Total and linearly polarized synchrotron emission from overpressured magnetized relativistic jets