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Centimeter continuum emission from protostars offers insight into theinnermost part of the outflows, as shock-ionized gas produces free-freeemission. We observed a complete population of Class 0 and I protostars in thePerseus molecular cloud at 4.1 cm and 6.4 cm with resolution and sensitivitysuperior to previous surveys. From a total of 71 detections, 8 sources exhibitresolved emission at 4.1 cm and/or 6.4 cm. In this paper we focus on thissub-sample, analyzing their spectral indices along the jet, and their alignmentwith respect to the large-scale molecular outflow. Spectral indices for fluxesintegrated toward the position of the protostar are consistent with free-freethermal emission. The value of the spectral index along a radio jet decreaseswith distance from the protostar. For six sources, emission is well alignedwith the outflow central axis, showing that we observe the ionized base of thejet. This is not the case for two sources, where we note misalignment of theemission with respect to the large-scale outflow. This might indicate that theemission does not originate in the radio jet, but rather in an ionized outflowcavity wall or disk surface. For five of the sources, the spectral indicesalong the jet decrease well below the thermal free-free limit of -0.1 with$>2\sigma$ significance. This is indicative of synchrotron emission, meaningthat high energy electrons are being produced in the outflows close to thedisk. This result can have far-reaching implications for the chemicalcomposition of the embedded disks.

The VLA Nascent Disk And Multiplicity Survey of Perseus Protostars (VANDAM). III. Extended Radio Emission from Protostars in Perseus