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Figure 1: Top: slit width superposed on a blue image (plate from the "Digitized Sky Survey'') of the system AM 1003-435; bottom: the twelve regions of AM 1003-435 from which spectroscopic information was derived. |
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Figure 2: a) ( Upper panel) Spectrum of the NW nucleus of AM 1003-435 before ( top) the subtraction of the stellar population template S7 ( bottom). ( Lower panel) Spectrum of the NW nucleus after the subtraction of this template. Ordinate in arbitrary units. b) ( Upper panel) Spectrum of the SE nucleus of AM 1003-435 before ( top) the subtraction of the stellar population template S2 ( bottom). ( Lower panel) Spectrum of the SE nucleus after the subtraction of this template. Ordinate in the same arbitrary units as in plot a). |
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Figure 3:
LOG([O III]
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Figure 4:
a) Abundance ratio N(O)/N(H) vs. distance. Open squares correspond to the centre of the SE (region 2) and NW (region 9) nuclear regions. Distances are given with respect to region 9, and are positive towards the Southeast. b) Abundance ratio N(N)/N(H) vs. distance. c) H![]() |
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Figure 5:
( Top) Heliocentric radial velocity distribution along
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Figure 6:
a) Gaussian fitting of the Na I ![]() ![]() ![]() |
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Figure 7:
( Top) Heliocentric radial velocity distribution along
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Figure 8: Evolution of the selected encounter model (Table 3), the stellar component is depicted in the nine upper panels and the gaseous component in the lower panels. Time is shown in Myr in the upper right corner of each frame, with respect to the orbital pericenter. The observed system stage would correspond to the +26.12 Myr frames. |
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