at $\alpha(2000) = 16^h~ 58^m~ 17\rlap.^s2446 \pm
0\rlap.^s0033; \delta(2000) =  -42^\circ~ 52'~ 08\rlap.^{''}354 \pm 0\rlap.^{''}067$, at $1\rlap.{''}3$ from the center of the jet. The OH maser emission detected by Caswell (1998) is close to the unresolved component associated with this second increase. We can think of three interpretations for this localized flux density increase. One is that we are observing a time-variable source powered by an independent star. There are two arguments against this interpretation: the first is that the sources in this region in general show little variation (see Table 1) and the second is that the source lies exactly in the path of the outflow, suggesting a relation with the jet. This latter fact suggests a second interpretation: we are seeing a discrete, new ejecta from the jet. This interpretation, on its turn, has several difficulties. The first is that, while a similar phenomenon was observed and monitored in the jet associated with HH 80-81 (Martí, Rodríguez, & Reipurth 1995; 1998), in this source the ejection was clearly bipolar, while in IRAS 16547-4247 we would have to consider a monopolar ejection. The second problem is related to the large velocity required for the ejection to move over $1\rlap.{''}3$ 