$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7844fig1.eps}\end{figure}$ Figure 1: Evolutionary tracks for stars with masses ranging from 1 to 120 $M_{\odot }$ for metallicity of 0.02. The box shows the values of $\log(\dot{M})$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7844fig2.eps}\end{figure}$ Figure 2: Dust mass, relative to total (in percent), ejected to the ISM by each stellar mass range during its complete evolution. The solid line represents the model using a typical Salpeter IMF, and the dotted line represents the model for the present-day mass function (PDMF).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{7844fig3.eps}\end{figure}$ Figure 3: Absolute dust mass ejected to the ISM. The modeled ejection by high mass stars (solid thin), low and intermediate mass stars (dashed), and total (solid thick), without dust destruction ( left panel) and considering dust destruction ( right panel).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7844fig1.eps}\end{figure}$	Figure 1: Evolutionary tracks for stars with masses ranging from 1 to 120 $M_{\odot }$ for metallicity of 0.02. The box shows the values of $\log(\dot{M})$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7844fig2.eps}\end{figure}$	Figure 2: Dust mass, relative to total (in percent), ejected to the ISM by each stellar mass range during its complete evolution. The solid line represents the model using a typical Salpeter IMF, and the dotted line represents the model for the present-day mass function (PDMF).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{7844fig3.eps}\end{figure}$	Figure 3: Absolute dust mass ejected to the ISM. The modeled ejection by high mass stars (solid thin), low and intermediate mass stars (dashed), and total (solid thick), without dust destruction ( left panel) and considering dust destruction ( right panel).
Open with DEXTER