Ray-Tracing in Relativistic Jet Simulations: A Polarimetric Study of
  Magnetic Field Morphology and Electron Scaling Relations
  The jets emanating from the centers of active galactic nuclei (AGN) are among
the most energetic objects in the universe. Investigating how the morphology of
the jet's synchrotron emission depends on the magnetic nature of the jet's
relativistic plasma is fundamental to the comparison between numerical
simulations and the observed polarization of relativistic jets. Through the use
of 3D relativistic magnetohydrodynamic (RMHD) jet simulations (computed using
the PLUTO code) we study how the jet's synchrotron emission depends upon the
morphology of the jet's magnetic field structure. Through the application of
polarized radiative transfer and ray-tracing (via the RADMC-3D code) we create
synthetic radio maps of the jet's total intensity as well as the linearly and
circularly polarized intensity for each jet simulation. In particular, we
create synthetic ray-traced images of the jet's polarized synchrotron emission
when the jet carries a predominantly poloidal, helical, and toroidal magnetic
field. We also explore several scaling relations in which the underlying
electron power-law distribution is set proportional to: (i) the jet's thermal
plasma density, (ii) the jet's internal energy density, and (iii) the jet's
magnetic energy density. We find that: (i) the jet emission is edge brightened
when the magnetic field is toroidal in nature and spine brightened when the
magnetic field is poloidal in nature, (ii) the circularly polarized emission
exhibits both negative and positive signs for the toroidal magnetic field
morphology at an inclination of 45{\deg} as well as 5{\deg}, and (iii) the
relativistic jet's emission is largely independent of different emission
scaling relations when the ambient medium is excluded.
