  Accretion and ejection sets the outcome of the star and planet formation
process. The mid-infrared wavelength range offers key tracers of those
processes that were difficult to detect and spatially resolve in protostars
until now. We aim to characterize the interplay between accretion and ejection
in the low-mass Class I protobinary system TMC1, comprising two young stellar
objects: TMC1-W and TMC1-E with 85 au separation. With the {\it James Webb}
Space Telescope (JWST) - Mid-Infrared Instrument (MIRI) observations in 5 - 28
$\mu$m range, we measure intensities of emission lines of H$_2$, atoms and
ions, e.g., [Fe II] and [Ne II], and HI recombination lines. We detect H$_2$
outflow coming from TMC1-E, with no significant H$_2$ emission from TMC1-W. The
H$_2$ emission from TMC1-E outflow appears narrow and extends to wider opening
angles with decreasing E$_{up}$ from S(8) to S(1) rotational transitions,
indicating a disk wind origin. The outflow from TMC1-E protostar shows
spatially extended emission lines of [Ne II], [Ne III], [Ar II], and [Ar III],
with their line ratios consistent with UV radiation as a source of ionization.
With ALMA, we detect accretion streamer infalling from $>$ 1000 au scales onto
the TMC1-E component. TMC1-W protostar powers a collimated jet, detected with
[Fe II] and [Ni II] consistent with energetic flow. A much weaker ionized jet
is observed from TMC1-E. TMC1-W is associated with strong emission from
hydrogen recombination lines, tracing the accretion onto the young star.
Observations of a binary Class I protostellar system show that the two
processes are clearly intertwined, with accretion from the envelope onto the
disk influencing a wide-angle wind ejected on disk scales, while accretion from
the protostellar disk onto the protostar is associated with the source
launching a collimated high-velocity jet within the innermost regions of the
disk.
