All Figures

Figure 1: Spectrum ( left) and image ( right) of PN MeWe 1-10. The exposure time was 900 s for the spectrum as well as for the image. The arrows in the image mark the stars used as astrometric calibrators. The images are given in sky orientation (E is left, N is up). The inner circle encloses the central star of the PN and the outer circle shows the almost perfectly round shape of this nebula. The NE enhancement might be due to ISM interaction, but as the slit of the spectrum does not cover this region, we cannot be sure. The offset of the outer ring with respect to the CSPN strongly encourages this interpretation.

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In the text

	Figure 2: Spectrum ( left) and image ( right) of PN MeWe 1-11. The exposure times were 900 s for the spectrum and for the image. The marks are as described in Fig. 1. The western edge is clearly enhanced. This is most likely due to ISM interaction. But including the somewhat weaker SE dip implies that it might be a signature of a cylindrical structure (see Fig. 5).
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In the text

	Figure 3: Spectrum ( left) and image ( right) of PN MeWe 2-5. The exposure times were 900 s for the spectrum and for the image. The marks are as described in Fig. 1.
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In the text

	Figure 4: The "deconvolution'' of the H and [N II] lines in case of We 1-11. The thin line gives the data, the thin dashed lines the individual lines of the applied fit, using the profile of a nearby night-sky-line, using fixed positions and a fixed ratio of [N II]658.4/[N II]654.8. The thick line gives the total fit.
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In the text

	Figure 5: The spectrum of PN MeWe 1-11 at the western edge. The spectrum changes abruptly with respect to the other parts of the nebula (see text).
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In the text

	Figure 6: The fit of a CLOUDY model (MeWe 1-10). On the abscissa is the luminosity in units of [] and on the ordinate the ratio of .
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In the text