Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg01.ps} \end{figure}$ Figure 1: DFOSC spectra of M-type supergiants.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg02.ps} \end{figure}$ Figure 2: EMMI spectra of M-type AGB stars, displayed twice on different scales to exploit the full dynamic range of the data.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg03.ps} \end{figure}$ Figure 3: DFOSC spectrum of the S-type star GRV 0519-6700.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{2555fg04.ps} \end{figure}$ Figure 4: EMMI spectra of carbon stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg05.ps} \end{figure}$ Figure 5: EMMI spectrum of the carbon star IRAS 05289-6617.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg06.ps} \end{figure}$ Figure 6: EMMI spectra of two dusty emission-line objects.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg07.ps} \end{figure}$ Figure 7: DFOSC spectrum of the emission-line object Al 50.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg08.ps} \end{figure}$ Figure 8: Mass-loss rate as a function of bolometric luminosity, for M-type stars (circles), MS or S-type stars (triangles), and carbon stars (solid dots). The classical AGB luminosity limit is marked by a vertical dotted line. The long and short-dashed slanted lines mark the classical and multiple-scattering limits to the mass-loss rate (van Loon et al. 1999b).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg09.ps} \end{figure}$ Figure 9: Mass-loss rate as a function of stellar effective temperature. Symbols are the same as in Fig. 8.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{2555fg10.ps} %\end{figure}$ Figure 10: Discrepancies between measured mass-loss rates from modelling of the SED, and the mass-loss rates as predicted from the L, $T_{\rm eff}$ dependence of the mass-loss rate for M-type stars, plotted versus bolometric luminosity a) and stellar effective temperature b). Symbols are the same as in Fig. 8.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg11.ps} \end{figure}$ Figure 11: Discrepancies between the mass-loss rates derived from 60 $\mu$ m flux densities, and the mass-loss rates as predicted from the $\dot{M}(L,T_{\rm eff})$ formula for dust-enshrouded stars in the LMC, plotted versus stellar effective temperature, for stars in the solar neighbourhood (Jura & Kleinmann 1989, 1990, 1992).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg12.ps} \end{figure}$ Figure 12: The Hertzsprung-Russell diagram of bolometric luminosity versus stellar effective temperature (symbols are the same as in Fig. 8). The classical AGB luminosity limit is marked by a horizontal dotted line. Three cool stars just above this limit may be AGB stars whose luminosity is enhanced as a result of Hot Bottom Burning (HBB). Evolutionary tracks from Bertelli et al. (1994) are plotted and labelled by their Main Sequence progenitor mass.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg13.ps} \end{figure}$ Figure 13: The Hertzsprung-Russell diagram for the M-type stars (circles), MS or S-type stars (triangles), and carbon stars (squares), where the sizes of the symbols are logarithmically proportional to the mass-loss rate.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg14.ps} \end{figure}$ Figure 14: Same as Fig. 13, but now the sizes of the symbols are proportional to $(T_{\rm eff}/T_{\rm dust})^2$ , which is a measure of the distance to the star of the dust formation region, $R_{\rm dust}/R_\star$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2555fgA1.ps} \end{figure}$ Figure A.1: DFOSC spectra of galactic M-type stars.

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2555fgA2.ps} \end{figure}$ Figure A.2: EMMI spectrum of the galactic M-type star SY Men.

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg01.ps} \end{figure}$	Figure 1: DFOSC spectra of M-type supergiants.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg02.ps} \end{figure}$	Figure 2: EMMI spectra of M-type AGB stars, displayed twice on different scales to exploit the full dynamic range of the data.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg03.ps} \end{figure}$	Figure 3: DFOSC spectrum of the S-type star GRV 0519-6700.
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$\begin{figure} \par\includegraphics[width=16.8cm,clip]{2555fg04.ps} \end{figure}$	Figure 4: EMMI spectra of carbon stars.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg05.ps} \end{figure}$	Figure 5: EMMI spectrum of the carbon star IRAS 05289-6617.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg06.ps} \end{figure}$	Figure 6: EMMI spectra of two dusty emission-line objects.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg07.ps} \end{figure}$	Figure 7: DFOSC spectrum of the emission-line object Al 50.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg08.ps} \end{figure}$	Figure 8: Mass-loss rate as a function of bolometric luminosity, for M-type stars (circles), MS or S-type stars (triangles), and carbon stars (solid dots). The classical AGB luminosity limit is marked by a vertical dotted line. The long and short-dashed slanted lines mark the classical and multiple-scattering limits to the mass-loss rate (van Loon et al. 1999b).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg09.ps} \end{figure}$	Figure 9: Mass-loss rate as a function of stellar effective temperature. Symbols are the same as in Fig. 8.
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$\begin{figure} \par\includegraphics[width=8.8cm]{2555fg10.ps} %\end{figure}$	Figure 10: Discrepancies between measured mass-loss rates from modelling of the SED, and the mass-loss rates as predicted from the L, $T_{\rm eff}$ dependence of the mass-loss rate for M-type stars, plotted versus bolometric luminosity a) and stellar effective temperature b). Symbols are the same as in Fig. 8.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg11.ps} \end{figure}$	Figure 11: Discrepancies between the mass-loss rates derived from 60 $\mu$ m flux densities, and the mass-loss rates as predicted from the $\dot{M}(L,T_{\rm eff})$ formula for dust-enshrouded stars in the LMC, plotted versus stellar effective temperature, for stars in the solar neighbourhood (Jura & Kleinmann 1989, 1990, 1992).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg13.ps} \end{figure}$	Figure 13: The Hertzsprung-Russell diagram for the M-type stars (circles), MS or S-type stars (triangles), and carbon stars (squares), where the sizes of the symbols are logarithmically proportional to the mass-loss rate.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2555fg14.ps} \end{figure}$	Figure 14: Same as Fig. 13, but now the sizes of the symbols are proportional to $(T_{\rm eff}/T_{\rm dust})^2$ , which is a measure of the distance to the star of the dust formation region, $R_{\rm dust}/R_\star$ .
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