  We present MUSE observations of AM1354-250, confirming its status as a
collisional ring galaxy which has recently undergone an interaction, creating
its distinctive shape. We analyse the stellar and gaseous emission throughout
the galaxy finding direct evidence that the gaseous ring is expanding with a
velocity of $\sim$70km.s$^{-1}$ and that star formation is occurring primarily
in HII regions associated with the ring. This star formation activity is likely
triggered by the interaction. We find evidence for several excitation
mechanisms in the gas, including emission consistent with shocked gas in the
expanding ring and a region of LINER-like emission in the central core of the
galaxy. Evidence of kinematic disturbance in both the stars and gas, possibly
also triggered by the interaction, can be seen in all of the velocity maps. The
ring galaxy retains weak spiral structure, strongly suggesting the progenitor
galaxy was a massive spiral prior to the collision with its companion an
estimated $140 \pm 12$ Myr ago.
