Abstract
Our observations have constrained the differences in polarization position angle between the optically and radio bright regions of the jet. If these arise predominantly from regions of different velocity (as in a spine–sheath model), relativistic aberration of the polarization position angle may be large. In order to test such a model is not ruled out by the data, we attempt to model the jet as two components: a central high-velocity spine emitting optical synchrotron radiation, and an outer sheath of radio-emitting plasma. Our model has a magnetic field with components (B x, B ′ y, B ′ z) in the jet frame, where the z-axis is parallel to the jet direction, and the xy-plane is transverse to the jet. For a Lorentz factor γ in the z-direction, and an angle φ between the z-axis and the line of sight, the observer will see a projected magnetic field in the plane of the sky Bu = γB ′ x cosφ + B ′ z sinφ, (1)
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