  In this work we present the highest spatial and spectral resolution integral
field observations to date of the bipolar jet from the Orion proplyd 244-440
using MUSE NFM) observations on the VLT. We observed a previously unreported
chain of six distinct knots in a roughly S-shaped pattern, and by comparing
them with HST images we estimated proper motions in the redshifted knots of 9.5
mas yr$^{-1}$ with an inclination angle of $73^{\circ}$, though these
quantities could not be measured for the blueshifted lobe. Analysis of the
[FeII] and [NiII] lines suggests jet densities on the order of $\sim 10^5$
cm$^{-3}$. We propose that the observed S-shaped morphology originates from a
jet launched by a smaller source with $M_\star < 0.2$ M$_{\odot}$ in orbital
motion around a larger companion of $M_\star \simeq 0.5$ M$_{\odot}$ at a
separation of 30-40 au. The measured luminosities of the knots using the
[OI]$\lambda6300$ and [SII]$\lambda6731$ lines were used to estimate a lower
limit to the mass-loss rate in the jet of $1.3 \times 10^{-11}$ M$_{\odot}$
yr$^{-1}$ and an upper limit of $10^{-9}$ M$_{\odot}$ yr$^{-1}$, which is
typical for low-mass driving sources. While the brightness asymmetry between
the redshifted and blueshifted lobes is consistent with external irradiation,
further analysis of the [NiII] and [FeII] lines suggests that photoionization
of the jet is not likely to be a dominant factor, and that the emission is
dominated by collisional excitation. The dynamical age of the jet compared to
the anticipated survival time of the proplyd demonstrates that photoevaporation
of the proplyd occurred prior to jet launching, and that this is still an
active source. These two points suggest that the envelope of the proplyd may
shield the jet from the majority of external radiation, and that
photoionization of the proplyd does not appear to impact the ability of a star
to launch a jet.
