Centimeter continuum emission from protostars offers insight into the innermost part of the outflows , as shock-ionized gas produces free-free emission .
We observed a complete population of Class 0 and I protostars in the Perseus molecular cloud at 4.1 cm and 6.4 cm with resolution and sensitivity superior to previous surveys .
From a total of 71 detections , 8 sources exhibit resolved emission at 4.1 cm and/or 6.4 cm .
In this paper we focus on this sub-sample , analyzing their spectral indices along the jet , and their alignment with respect to the large-scale molecular outflow .
Spectral indices for fluxes integrated toward the position of the protostar are consistent with free-free thermal emission .
The value of the spectral index along a radio jet decreases with distance from the protostar .
For six sources , emission is well aligned with the outflow central axis , showing that we observe the ionized base of the jet .
This is not the case for two sources , where we note misalignment of the emission with respect to the large-scale outflow .
This might indicate that the emission does not originate in the radio jet , but rather in an ionized outflow cavity wall or disk surface .
For five of the sources , the spectral indices along the jet decrease well below the thermal free-free limit of -0.1 with > 2 \sigma significance .
This is indicative of synchrotron emission , meaning that high energy electrons are being produced in the outflows close to the disk .
This result can have far-reaching implications for the chemical composition of the embedded disks .