Physical and kinematic conditions of the local merging galaxy NGC 1487
  We present optical VLT/MUSE integral field spectroscopy data of the merging
galaxy NGC 1487. We use fitting techniques to study the ionized gas emission of
this merger and its main morphological and kinematical properties. We measured
flat and sometimes inverted oxygen abundance gradients in the subsystems
composing NGC 1487, explained by metal mixing processes common in merging
galaxies. We also measured widespread star-forming bursts, indicating that
photoionisation by stars is the primary ionization source of the galaxy. The
kinematic map revealed a rotating pattern in the gas in the northern tail of
the system, suggesting that the galaxy may be in the process of rebuilding a
disc. The gas located in the central region has larger velocity dispersion
($\sigma\approx 50$ km s$^{-1}$) than the remaining regions, indicating
kinematic heating, possibly owing to the ongoing interaction. Similar trends
were, however, not observed in the stellar velocity-dispersion map, indicating
that the galaxy has not yet achieved equilibrium, and the nebular and stellar
components are still kinematically decoupled. Based on all our measurements and
findings, and specially on the mass estimates, metallicity gradients and
velocity fields of the system, we propose that NGC 1487 is the result of an
ongoing merger event involving smallish dwarf galaxies within a group, in a
pre-merger phase, resulting in a relic with mass and physical parameters
similar to a dwarf galaxy. Thus, we may be witnessing the formation of a dwarf
galaxy by merging of smaller clumps at z=0.
