All Figures

$\begin{figure} \par\includegraphics[width=8.5cm]{8879fig1.eps} \end{figure}$ Figure 1: Track 35 showing the position of the particles studied in this work (red numbers). Particles 81 to 90 were extracted from the lower edge of the bulb and particle 92 from the upper edge.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{8879fig2.eps} \end{figure}$ Figure 2: Slice of Stardust aerogel tile C2054 showing track 35 and the position where the aerogel piece away from the track, C2054, 36, was extracted. This position, indicated by the red dot, is more than 3 mm away from the track and at 20 mm depth.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{8879fig3.eps} \end{figure}$ Figure 3: Picture shows particle 84 as a dark spot positioned south of a 50 $\mu$ m long aerogel piece that was extracted with the particle. The squares indicate the apertures used for FTIR analysis; see spectra in Fig. 4.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{8879fig4.ps} \end{figure}$ Figure 4: From bottom to top traces: infrared spectrum of particle 84, see Fig. 3 for sample and background apertures, resp. ``particle 84'' and ``background 1''. The spectrum of ``aerogel next to particle'' was made using ``background 2''. The spectrum of a piece of aerogel outside the particle track is also shown for comparison. The KBr window blank is made using ``background 1'' as sample and ``background 2'' as background.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{8879fig5.eps} \end{figure}$ Figure 5: Picture shows particle 85. The squares indicate the apertures used for FTIR analysis, see spectra in Fig. 6.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8879fig6.ps} \end{figure}$ Figure 6: From bottom to top traces: infrared spectrum of particle 85, see Fig. 3 for sample and background apertures, resp. ``85'' and ``S1''. The other spectra were measured using positions S1 to S4 as samples and B1 to B4 as their backgrounds. The spectrum of a piece of aerogel outside the particle track is also shown for comparison.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm]{8879fig7.ps} \end{figure}$ Figure 7: From bottom to top traces: infrared spectra of Stardust particles 81-87, 89, 90, 92 extracted from track 35, see Fig. 1. Top spectrum corresponds to an aerogel piece that was outside the track. All spectra were normalized in intensity with respect to the bottom spectrum (particle 81).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm]{8879fig8.eps}\par \end{figure}$ Figure 8: From bottom to top traces: 3.4 $\mu$ m infrared feature of Stardust particles 81-87, 89, 90, 92 extracted from track 35, see Fig. 1. Top spectrum corresponds to 3.4 $\mu$ m infrared feature of an aerogel piece that was outside the particle track. Spectra were normalized in intensity with respect to the spectrum of particle 87 (7th trace from bottom), the particle with the highest N[3.4]/N[10] (aliphatic C to Si ratio). For comparison, the 3.4 $\mu$ m feature of Stardust particle C2054, 0, 35, 16, 0 is shown (thin trace, adapted from Sandford et al. 2006).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{8879fig9.ps} \end{figure}$ Figure 9: 3.4 $\mu$ m infrared feature due to CH stretching modes of organic residues (OR) made from ice photoprocessing at 12 K followed by annealing at different temperatures, and that of Stardust particles C2054, 0, 35, 16, 0 (thick trace, adapted from Keller et al. 2006) and 81 (thick dashed trace) overplotted on the same feature of an IDP (labelled R9, adapted from Muñoz Caro et al. 2006).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{8879f10.ps} \end{figure}$ Figure 10: Infrared spectra of an annealed organic residue made by UV irradiation of the H₂O:CH₃OH:NH₃ = 2:1:1 ice mixture. The infrared spectrum of Stardust particle 87 (thick line) is shown for comparison.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{8879f11.eps} \end{figure}$ Figure 11: Raman D and G bands of two Stardust particles (labelled F1_1 and F1_2, adapted from Fig. 1 A of Sandford et al. 2006) after soft smoothing and baseline correction. For comparison, the D and G bands of IDPs N and K2 (adapted from Fig. 3 of Muñoz Caro et al. 2006) are shown. Thin lines are the fits made by addition of two Lorentzians, plotted as dashed lines.
Open with DEXTER

In the text

$\begin{figure} \par\begin{tabular}{r} \par\includegraphics[width=8.5cm]{8879f12t... ...includegraphics[width=8.5cm]{8879f12b.eps}\\ \par\end{tabular}\par \end{figure}$ Figure 12: Top left: a schematic of the expected substructure unit for the a-C:H polymer observed in Stardust grains and many IDPs showing 3 aromatic units depicted in 2 dimensions. Top right: the real structure is not planar because it folds gradually as the number of aromatic units increases. This a-C:H polymer is build up of numerous aromatic units linked by aliphatic chains, which lead to the intricate structure characteristic of a-C:H. Functional groups (OH, C = O, etc.; not shown in this figure) can be inserted in the network. Figure adapted from Muñoz Caro & Dartois (2007). Bottom left: a schematic of the expected substructure unit for the photoproduced a-C:H (analog of the carbonaceous material in diffuse interstellar grains), which was adapted from Dartois et al. (2005). Bottom right: the photoproduced a-C:H polymer is also a complex 3-dimensional structure.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm]{8879fig1.eps} \end{figure}$	Figure 1: Track 35 showing the position of the particles studied in this work (red numbers). Particles 81 to 90 were extracted from the lower edge of the bulb and particle 92 from the upper edge.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm]{8879fig2.eps} \end{figure}$	Figure 2: Slice of Stardust aerogel tile C2054 showing track 35 and the position where the aerogel piece away from the track, C2054, 36, was extracted. This position, indicated by the red dot, is more than 3 mm away from the track and at 20 mm depth.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm]{8879fig3.eps} \end{figure}$	Figure 3: Picture shows particle 84 as a dark spot positioned south of a 50 $\mu$ m long aerogel piece that was extracted with the particle. The squares indicate the apertures used for FTIR analysis; see spectra in Fig. 4.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm]{8879fig5.eps} \end{figure}$	Figure 5: Picture shows particle 85. The squares indicate the apertures used for FTIR analysis, see spectra in Fig. 6.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8879fig6.ps} \end{figure}$	Figure 6: From bottom to top traces: infrared spectrum of particle 85, see Fig. 3 for sample and background apertures, resp. ``85'' and ``S1''. The other spectra were measured using positions S1 to S4 as samples and B1 to B4 as their backgrounds. The spectrum of a piece of aerogel outside the particle track is also shown for comparison.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm]{8879fig7.ps} \end{figure}$	Figure 7: From bottom to top traces: infrared spectra of Stardust particles 81-87, 89, 90, 92 extracted from track 35, see Fig. 1. Top spectrum corresponds to an aerogel piece that was outside the track. All spectra were normalized in intensity with respect to the bottom spectrum (particle 81).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm]{8879f10.ps} \end{figure}$	Figure 10: Infrared spectra of an annealed organic residue made by UV irradiation of the H₂O:CH₃OH:NH₃ = 2:1:1 ice mixture. The infrared spectrum of Stardust particle 87 (thick line) is shown for comparison.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm]{8879f11.eps} \end{figure}$	Figure 11: Raman D and G bands of two Stardust particles (labelled F1_1 and F1_2, adapted from Fig. 1 A of Sandford et al. 2006) after soft smoothing and baseline correction. For comparison, the D and G bands of IDPs N and K2 (adapted from Fig. 3 of Muñoz Caro et al. 2006) are shown. Thin lines are the fits made by addition of two Lorentzians, plotted as dashed lines.
Open with DEXTER