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 multi-frequency data, e.g., observed with the Very Long Baseline Array as well as the Imaging X-ray Polarimetry Explorer, with three dimensional relativistic magnetohydrodynamic jet simulations using the PLUTO code. 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 such as RADMC-3D and 3DPOL, we directly calculate and interpolate the non-thermal particle attributes. The final set of both observational and synthetic 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. Studying AGN jets across different frequencies, especially in the radio regime, allows us to observe features such as core shift measurements and magnetic field orientations. We imaged nine blazar sources with DoG-HiT and identified favored magnetic field structures. In particular, for X-ray binary sources, we investigate how recollimation shocks form by adjusting the input deck of our simulations. Hence, extending our analysis to higher-energy frequencies, our synthetic polarization maps offer insights into synchrotron polarization levels, which NASA's Imaging X-ray Polarimetry Explorer (IXPE) mission is now detecting in AGN sources.
