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The structure, elemental abundances, physical conditions of the LMC supernovaremnant (SNR) 0540-69.3 and its surroundings were investigated using [O III]imaging and spectroscopy. Several new spectral lines are identified, both incentral filaments and in interstellar clouds shocked by the supernova blastwave. The central lines are redshifted by $440\pm80$ km s$^{-1}$ with respectto the LMC, and the [O III] emission displays a symmetry axis of ring-likestructures which could indicate that the pulsar shares the same generalredshift as the central supernova ejecta. [O II], [S II], [Ar III] and H$\beta$have more compact structures than [O III], and possibly [Ne III]. The average[O III] temperature is $23\,500 \pm 1\,800$ K, and the electron density from [SII] is typically $10^3$ cm$^{-3}$. By mass, the relative elemental abundancesof the central shocked ejecta are ${\rm O:Ne:S:Ar} \approx 1:0.07:0.10:0.02$,consistent with explosion models of $13-20$ solar mass progenitors, and similarto that of SN 1987A, as is also the mixing of hydrogen and helium into thecenter. [O III] is also seen in freely coasting ejecta outside the pulsar-windnebula out to well above $2\,000$ km s$^{-1}$. From this a pulsar age of$\approx 1\,200$ years is estimated. Four filaments of shocked interstellarmedium with a wide range in degree of ionization of iron are identified. Onewas observed in X-rays, and another has a redshift of $85\pm30$ km~s$^{-1}$relative to LMC. From this the electron density of the [O III]-emitting gas isestimated to be $10^3$ cm$^{-3}$. The line of the most highly ionized ion, [FeXIV] $\lambda$5303, likely comes from an evaporation zone in connection withthe radiatively cooled gas emitting, e.g., [O III].

Kinematics, structure and abundances of supernova remnant 0540-69.3