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We investigate the brightest regions of the kpc‐scale jet in the powerful radio galaxy 3C 346, using new optical  Hubble Space Telescope  ( HST ) ACS/F606W polarimetry together with  Chandra  X‐ray data and 14.9 and 22.5 GHz Very Large Array (VLA) radio polarimetry. The jet shows a close correspondence between optical and radio morphology, while the X‐ray emission shows a  0.80 ± 0.17 kpc  offset from the optical and radio peak positions. Optical and radio polarimetry show the same apparent magnetic field position angle and fractional polarization at the brightest knot, where the jet undergoes a large kink of almost 70° in the optical and radio images. The apparent field direction here is well aligned with the new jet direction, as predicted by earlier work that suggested the kink was the result of an oblique shock. We have explored models of the polarization from oblique shocks to understand the geometry of the 3C 346 jet, and find that the upstream flow is likely to be highly relativistic  (β u = 0.91 +0.05  −0.07 ) , where the plane of the shock front is inclined at an angle of  η= 51°± 11°  to the upstream flow which is at an angle  θ= 14 +8  −7   deg to our line of sight. The actual deflection angle of the jet in this case is only 22°.

The magnetic field and geometry of the oblique shock in the jet of 3C 346