Optical IFU spectroscopy of a bipolar microquasar jet in NGC 300
  We recently reported the discovery of a candidate jet-driving microquasar
(S10) in the nearby spiral galaxy NGC 300. However, in the absence of kinematic
information, we could not reliably determine the jet power or the dynamical age
of the jet cavity. Here, we present optical MUSE integral field unit (IFU)
observations of S10, which reveal a bipolar line-emitting jet structure
surrounding a continuum-emitting central source. The optical jet lobes of S10
have a total extent of $\sim$ 40 pc and a shock velocity of $\sim$ 150 km
s$^{-1}$. Together with the jet kinematics, we exploit the MUSE coverage of the
Balmer H$\beta$ line to estimate the density of the surrounding matter and
therefore compute the jet power to be $P_{jet}\approx$ 6.3 $\times$ 10$^{38}$
erg s$^{-1}$. An optical analysis of a microquasar jet bubble and a consequent
robust derivation of the jet power have been possible only in a handful of
similar sources. This study therefore adds valuable insight into microquasar
jets, and demonstrates the power of optical integral field spectroscopy in
identifying and analysing these objects.
