Abstract: 

We focus on understanding how the synchrotron emission morphology of astrophysical jet phenomena is influenced by physical properties of the relativistic plasma within the jet stream. To achieve this, we compare observational data in multi-frequencies with relativistic magnetohydrodynamic jet simulations using the PLUTO code, which are tailored to each specific source. This approach allows us to identify favored intrinsic magnetic field configurations and kinematic properties in the jets from violent black hole sources. To compute polarization using radiative transfer codes, we directly calculate and interpolate the non-thermal particle attributes on a grid in the 3D space. The final set of polarized images include maps of the four Stokes parameters (I, Q, U, and V) and linearly polarized intensity displaying the direction of the magnetic field. Our research examines various astrophysical sources and their jets, including AGN and X-ray binaries. In particular, for X-ray binary sources, we investigate how recollimation shocks form by adjusting the input deck of our simulations. Studying AGN jets across different frequencies, especially in the radio regime, allows us to observe features such as core shift measurements and boundary effects between upstream synchrotron self-absorption and downstream optically thin regions. Centaurus A serves as an ideal laboratory for such studies, allowing observations from low-frequency radio bands (e.g., 1 GHz with the SKA) to higher frequencies (e.g., 230-345 GHz with the EHT). Extending our analysis to higher-energy frequencies, our synthetic polarization maps offer insights into synchrotron polarization levels at high energies, which NASA's Imaging X-ray Polarimetry Explorer (IXPE) mission is now detecting in AGN sources.