  In this article, we report high-resolution (~ 0.1" -- 0.3"), high-sensitivity
(~ 50 -100 uJy beam-1) Very Large Array 0.7 and 1.3 cm observations of the
young stellar system IRAS 16293-2422 in rho-Ophiuchus. In the 0.7 cm image,
component A to the south-east of the system looks like its usual binary self.
In the new 1.3 cm image, however, component A2 appears to have split into two
sub-components located roughly symmetrically around the original position of
A2. This change of morphology is likely the result of a recent bipolar
ejection, one of the very first such events observed in a low-mass source. Also
in component A, a marginal detection of 0.7 cm emission associated with the
submillimeter component Ab is reported. If confirmed, this detection would
imply that Ab is a relatively extended dusty structure, where grain coagulation
may already have taken place. With an angular size increasing with frequency,
and an overall spectra index of 2, the emission from component B to the
north-west of the system is confirmed to be dominated by optically thick
thermal dust emission associated with a fairly massive, nearly face-on,
circumstellar disk. In the central region, however, we find evidence for a
modest free-free contribution that originates in a structure elongated roughly
in the east-west direction. We argue that this free-free component traces the
base of the jet driving the large-scale bipolar flow at a position angle of
about 110 degrees that has long been known to be powered by IRAS 16293-2422.
