  We present the ionised gas outflow morphology in the Circinus galaxy using
the Narrow Field Mode (NFM) of the MUSE instrument on board the Very Large
Telescope (VLT). The NFM observations provide a spatial resolution of
$\sim$0.1", corresponding to a physical scale of $\sim$2 pc, one of the highest
spatial resolution achievable using ground-based AO-assisted observations in
the optical wavelengths. The MUSE observations reveal a collimated clumpy
outflow profile originating near the AGN location and extending up to 1.5"
($\sim$30 pc) in the NW direction. The collimated structure then fragments into
two filaments, giving the entire outflowing gas a ``tuning-fork'' morphology.
These structures remain undetected in the lower spatial resolution MUSE Wide
Field Mode data. We explain the origin of this tuning-fork structure to the
interaction of the outflow with a dense clump in the interstellar medium (ISM)
as the outflow propagates outward. The origin of the collimated structure
itself could be from jet-ISM interactions on small scales. These observations
also provide evidence to the origin of the ionised gas filaments previously
observed in the Circinus galaxy out to kiloparsec scales. We find instantaneous
and time-averaged mass outflow rates of 10$^{-2}$ M$_{\odot}$ yr$^{-1}$ and
10$^{-4}$ M$_{\odot}$ yr$^{-1}$, respectively. Based on the star formation rate
in the Circinus galaxy reported in the literature, the observed ionised
outflows are not expected to regulate star formation within the $\sim$100 pc
scales probed by the NFM data.
