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We present and discuss new visual wavelength-range observations of the innerregions of the supernova remnant SNR 0540-69.3 that is located in the LargeMagellanic Cloud (LMC). These observations provide us with more spatial andspectral information than were previously available for this object. We usethese data to create a detailed three-dimensional model of the remnant,assuming linear expansion of the ejecta. With the observations and the model westudy the general three-dimensional structure of the remnant, and the influenceof an active region in the remnant - a "blob" - that we address in previouspapers. We used the fibre-fed integral-field spectrograph VIMOS at the VeryLarge Telescope of the European Southern Observatory. The observations provideus with three-dimensional data in [OIII]5007 and [SII]6717,6731 at an 0.33x0.33spatial sampling and a velocity resolution of about 35 km/s. We decomposed thetwo, partially overlapping, sulphur lines and used them to calculate electrondensities across the remnant at high signal-to-noise ratio. Our analysisreveals a structure that stretches from the position of the "blob", and intothe plane of the sky at a position angle of about 60 degrees. We speculate thatthe pulsar is positioned along this activity axis, where it has a velocityalong the line of sight of a few hundred km/s. The "blob" is most likely aregion of shock activity, as it is mainly bright in [SII]; future observationsof [OII]3729 would be useful to test whether the S/O abundance ratio is higherthan average for that location in the remnant. The striking resemblance inX-rays between the pulsar wind nebula (PWN) of SNR 0540-69.3 and the Crab, incombination with our findings in this paper, suggests that the symmetry axis ispart of a torus in the PWN. (abridged)

Properties of the three-dimensional structure in the central region of the supernova remnant SNR 0540-69.3