  We present a comparison of the parameters of accretion disc outflows and the
jet of the broad-line radio galaxy 3C 111 on sub-pc scales. We make use of
published X-ray observations of ultra-fast outflows (UFOs) and new 43GHz VLBA
images to track the jet knots ejection. We find that the superluminal jet
coexists with the mildly relativistic outflows on sub-pc scales, possibly
indicating a transverse stratification of a global flow. The two are roughly in
pressure equilibrium, with the UFOs potentially providing additional support
for the initial jet collimation. The UFOs are much more massive than the jet,
but their kinetic power is probably about an order of magnitude lower, at least
for the observations considered here. However, their momentum flux is
equivalent and both of them are powerful enough to exert a concurrent feedback
impact on the surrounding environment. A link between these components is
naturally predicted in the context of MHD models for jet/outflow formation.
However, given the high radiation throughput of AGNs, radiation pressure should
also be taken into account. From the comparison with the long-term 2-10keV RXTE
light curve we find that the UFOs are preferentially detected during periods of
increasing flux. We also find the possibility to place the UFOs within the
known X-ray dips-jet ejection cycles, which has been shown to be a strong proof
of the disc-jet connection, in analogue with stellar-mass black holes. However,
given the limited number of observations presently available, these relations
are only tentative and additional spectral monitoring is needed to test them
conclusively.
