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Radio emission from protostellar jets is usually dominated by free-freeemission from thermal electrons. However, in some cases, it has been proposedthat non-thermal emission could also be present. This additional contributionfrom non-thermal emission has been inferred through negative spectral indicesat centimeter wavelengths in some regions of the radio jets. In the case of HH80-81, one of the most powerful protostellar jets known, linearly polarizedemission has also been detected, revealing that the non-thermal emission is ofsynchrotron nature from a population of relativistic particles in the jet. Thisresult implies that an acceleration mechanism should be taking place in someparts of the jet. Here, we present new high sensitivity and high angularresolution radio observations at several wavelengths (in the 3-20 cm range) ofthe HH80-81 radio jet. These new observations represent an improvement insensitivity and angular resolution by a factor of $\sim$10 with respect toprevious observations. This allows us to resolve the morphology of the radiojet, and to study the different emission mechanisms involved through spectralindex maps. We conclude that synchrotron emission in this jet arises from anextended component detected at low frequencies and from the termination pointsof the jet, where strong shocks against the ambient medium can produceefficient particle acceleration.

The Highly Collimated Radio Jet of HH 80-81: Structure and Non-Thermal Emission