All Figures

Figure 1: ACS/HRC image of Car and the Homunculus (Smith et al. 2004) with the aperture positions superimposed (see Table 1). The sections plotted in Figs. 2 and 3 are marked with bold lines. The March 2000 aperture represents the aperture centered on Car. At this same epoch, multiple exposures were recorded with offsets orthogonal to the aperture to map the nebular structure (Ishibashi et al. 2003). We have used these same spectra to estimate the size of the Sr  filament in Sr II, sketched in the right panel.

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In the text

Figure 2: Position-velocity diagrams at the location of the strontium filament seen in several different emission lines, with two different slit orientations. The top row shows spectra taken in March 2000 with the STIS slit at PA =  , and the bottom row shows the same four emission lines obtained in November 2001, with the slit at (see Fig. 1 and Table 1). The four emission lines shown here are ( left to right in both the top and bottom panels): Sr  II 4078, [Ca  II] 7293 (this is actually the average of [Ca  II] 7293 and [Ca  II] 7325), [Ni  II] 7379, and [N  II] 6585. The contours superposed on the Sr  II and [Ni  II] emission are corresponding contours of the [Ca  II] emission at the same dates and slit positions. The horizontal axis shows heliocentric Doppler velocity. In the top and bottom panels, the position marked as zero corresponds roughly to the place where the two slits cross to within about 0 1 (see Fig. 1).

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In the text

Figure 3: 2D spectrum of the filament at two different slit orientations at nearly orthogonal angles, March 2000 and November 2001, respectively. The vertical stretch in the upper panel is 2 5 and in the lower 2''. The horizontal scale covers the region 4200-4300 Å. The aperture width was 0 2 on the sky. The slit positions are shown projected on the Homunculus in Fig. 1 with the plotted regions marked with bold lines.

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In the text

	Figure 4: Upper panel: subsection of STIS nebular spectrum centered upon the Sr  filament. The STIS aperture was used for this spectrum. Lower panel: extracted spectrum of the area, marked on the right hand side of the nebular spectrum in the upper panel. This represents the central position of the Sr  filament.
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In the text

	Figure 5: Lines from Ti II ( upper panel) and Sr II ( lower panel) in the region 3000-10 000 Å for Ti II and 3000-11 000 Å for Sr II. All possible lines are shown in grey and the lines observed in the spectrum are in black. The difference in atomic structure is obvious. Note the different x-scales. The forbidden lines of [Ti II] are not included.
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In the text