All Figures

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{2305fig1.eps} } \end{figure}$ Figure 1: The 3.85-4.10 $\mu$ m spectra of four stars LMC oxygen-rich stars. For comparison, a spectrum of the Galactic giant star g Her, and a model spectrum of SiO bands, are also shown. Wavelength of ²⁸SiO, ²⁹SiO, ³⁰SiO bands are indicated. 10 $\sigma$ errors are plotted as dots.
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In the text

$\begin{figure} \par {\includegraphics[width=8.05cm,clip]{2305fig2.eps} } \end{figure}$ Figure 2: The spectrum of one of the oxygen-rich stars, IRAS 05148-6730, which covers the entire L-band. For comparison, a spectra of g Her, and OH and SiO models are also plotted. 10 $\sigma$ errors are plotted as dots.
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In the text

$\begin{figure} \par {\includegraphics[width=8.05cm,clip]{2305fig3.eps} } \end{figure}$ Figure 3: The spectrum of IRAS 05128-6455, compared the spectrum of the galactic oxygen-rich Mira, Z Cyg ( $R\sim 300$ ; Matsuura et al. 2002a), which shows H₂O and SiO bands. Deep continuous absorption shortwards of 3.8 $\mu$ m in IRAS 05128-6455 is due to H₂O. SiO bands may be detected, although the band strength is almost the same as the noise level. A small dip at 3.2 $\mu$ m is the OH Q-band.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{2305fig4.eps} } \end{figure}$ Figure 4: The equivalent width of the SiO bands. For Galactic stars, supergiants and Mira variables sources are shown by different symbols. Semi-regular variables and unknown variable types are plotted as "others''.
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In the text

$\begin{figure} \par {\includegraphics[width=16.2cm,clip]{2305fig5.eps} } \end{figure}$ Figure 5: ISAAC spectra of carbon-rich AGB stars in LMC. Molecule bands, in particular the 3.1 $\mu$ m C₂H₂+HCN, 3.5 $\mu$ m HCN, and 3.8 $\mu$ m, probably C₂H₂ bands, are indicated. 10 $\sigma$ errors are plotted as dots.
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In the text

$\begin{figure} \par {\includegraphics[width=16.8cm,clip]{2305fig6.eps} } \end{figure}$ Figure 6: Same as Fig. 5, but for carbon-rich stars in SMC and SgrD.
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In the text

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{2305fig7.ps} } \end{figure}$ Figure 7: The flattened spectra of the carbon-rich stars, compared with the CH model spectrum and with the ISO/SWS spectrum of TX Psc. The CH line list is taken from Jørgensen et al. (1996). The relative intensities of the CH lines in the model are not always comparable to the observed ones, especially around 3.5 and 3.8 $\mu$ m, because of other opacity sources such as the HCN and C₂H₂ bands.
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In the text

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{2305fig8.eps} } \end{figure}$ Figure 8: The spectrum of SMC-S2, and smoothed spectrum to 1/10th of the original wavelength resolution. The 3.3 $\mu$ m PAH band is detected. (The 3.308-3.320 $\mu$ m region is removed because of strong telluric lines.) 10 $\sigma$ errors are plotted as dots.
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In the text

$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{2305fig9.eps} } \end{figure}$ Figure 9: The HCN equivalent widths of EW_3.5. The symbols show the host galaxies of the samples.
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In the text

$\begin{figure} \par {\includegraphics[width=8.1cm,clip]{2305f10.eps} } \end{figure}$ Figure 10: The C₂H₂ equivalent widths of EW_3.8.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{2305f11.eps} } \end{figure}$ Figure 11: The HCN and C₂H₂ equivalent widths of EW_3.1.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{2305f12.eps} } \end{figure}$ Figure 12: The equivalent width of SiO bands as a function of metallicity. The model is from Aringer et al. (1997), and Galactic data are from Aringer et al. (1999).
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In the text

$\begin{figure} \par {\includegraphics[width=16cm,clip]{2305f13.eps} } \end{figure}$ Figure 13: Abundance of molecules calculated with the chemical model. The abundance is normalized by H+H₂ pressure. The left side is for $\rm [Z/H]=-0.3$ (approximate LMC metallicity), and the right for [Z/H] = 0.0 (solar metallicity). All elemental abundances are scaled to the metallicity, except carbon, which is set relative to the oxygen abundance using the C/O ratio. The temperature is 2500 K for both panels.
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In the text

$\begin{figure} \par {\includegraphics[width=16cm,clip]{2305f14.eps} } \end{figure}$ Figure 14: Same as Fig.13, but as a function of temperature. The C/O ratio is 1.1 for both panels.
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In the text

$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{2305fig1.eps} } \end{figure}$	Figure 1: The 3.85-4.10 $\mu$ m spectra of four stars LMC oxygen-rich stars. For comparison, a spectrum of the Galactic giant star g Her, and a model spectrum of SiO bands, are also shown. Wavelength of ²⁸SiO, ²⁹SiO, ³⁰SiO bands are indicated. 10 $\sigma$ errors are plotted as dots.
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$\begin{figure} \par {\includegraphics[width=8.05cm,clip]{2305fig2.eps} } \end{figure}$	Figure 2: The spectrum of one of the oxygen-rich stars, IRAS 05148-6730, which covers the entire L-band. For comparison, a spectra of g Her, and OH and SiO models are also plotted. 10 $\sigma$ errors are plotted as dots.
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$\begin{figure} \par {\includegraphics[width=8cm,clip]{2305fig4.eps} } \end{figure}$	Figure 4: The equivalent width of the SiO bands. For Galactic stars, supergiants and Mira variables sources are shown by different symbols. Semi-regular variables and unknown variable types are plotted as "others''.
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$\begin{figure} \par {\includegraphics[width=16.2cm,clip]{2305fig5.eps} } \end{figure}$	Figure 5: ISAAC spectra of carbon-rich AGB stars in LMC. Molecule bands, in particular the 3.1 $\mu$ m C₂H₂+HCN, 3.5 $\mu$ m HCN, and 3.8 $\mu$ m, probably C₂H₂ bands, are indicated. 10 $\sigma$ errors are plotted as dots.
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$\begin{figure} \par {\includegraphics[width=16.8cm,clip]{2305fig6.eps} } \end{figure}$	Figure 6: Same as Fig. 5, but for carbon-rich stars in SMC and SgrD.
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$\begin{figure} \par {\includegraphics[width=8.2cm,clip]{2305fig8.eps} } \end{figure}$	Figure 8: The spectrum of SMC-S2, and smoothed spectrum to 1/10th of the original wavelength resolution. The 3.3 $\mu$ m PAH band is detected. (The 3.308-3.320 $\mu$ m region is removed because of strong telluric lines.) 10 $\sigma$ errors are plotted as dots.
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$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{2305fig9.eps} } \end{figure}$	Figure 9: The HCN equivalent widths of EW_3.5. The symbols show the host galaxies of the samples.
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$\begin{figure} \par {\includegraphics[width=8.1cm,clip]{2305f10.eps} } \end{figure}$	Figure 10: The C₂H₂ equivalent widths of EW_3.8.
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$\begin{figure} \par {\includegraphics[width=8cm,clip]{2305f11.eps} } \end{figure}$	Figure 11: The HCN and C₂H₂ equivalent widths of EW_3.1.
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$\begin{figure} \par {\includegraphics[width=8cm,clip]{2305f12.eps} } \end{figure}$	Figure 12: The equivalent width of SiO bands as a function of metallicity. The model is from Aringer et al. (1997), and Galactic data are from Aringer et al. (1999).
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$\begin{figure} \par {\includegraphics[width=16cm,clip]{2305f14.eps} } \end{figure}$	Figure 14: Same as Fig.13, but as a function of temperature. The C/O ratio is 1.1 for both panels.
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