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

Physical and kinematic conditions of the local merging galaxy NGC 1487