All Figures

$\begin{figure} \par\mbox{ \includegraphics[width=7cm,clip]{NewFigs/pretty_lw6.ep... ...4mm} \includegraphics[width=7cm,clip]{NewFigs/pretty_sw.eps} } \end{figure}$ Figure 1: ISOCAM and SCUBA images of NGC 1569. Top-left: ISOCAM-LW6 ( $\lambda = 7.75\; \mu$ m, $\rm beam=7.6''$ ), this band traces PAH features. Top-right: ISOCAM-LW3 ( $\lambda = 15\; \mu$ m, $\rm beam=9.9''$ ), this band traces the hot dust continuum. Bottom-left: SCUBA ( $\lambda = 850\; \mu$ m, $\rm beam=15.2''$ ). Bottom-right: SCUBA ( $\lambda = 450\; \mu$ m, $\rm beam=8.5''$ ). These two submm bands trace the cold dust continuum. The field of view is the same for the 4 images and the color table has the same dynamic range. The ISOCAM images have been deconvolved.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3441.f2a.ps}\hspace*{4mm} \includegraphics[width=7cm,clip]{3441.f2b.ps} \end{figure}$ Figure 2: Ratio of hot dust/cold dust. Left: ratio of the ISOCAM-LW3 image (contours, $\lambda = 15\; \mu$ m) to the SCUBA image ( $\lambda = 850\; \mu$ m). Right: ratio of the ISOCAM-LW6 image (contours, $\lambda = 7.75\; \mu$ m) to the SCUBA image ( $\lambda = 850\; \mu$ m). The ISOCAM images have been degraded to the resolution of the SCUBA (850 $\mu$ m) image (15'').
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In the text

$\begin{figure} \par\includegraphics[width=\hsize,clip]{3441.f3.eps} \end{figure}$ Figure 3: Schematic diagram of the model geometry.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3441.f4.eps} \end{figure}$ Figure 4: Algorithm used to compute the SED in a self-consistent way. "UV-opt. Obs.'' are the data contained in Table 3, "IR-mm Obs.'' are the data contained in Table 2, "IR ionic lines'' are from Sect. 3.3.2, "IR-mm SED'' is the modeled dust SED and "Extinction'' is the extinction curve computed by DBP90 after converging to a solution. We iterate on this process to obtain the necessary consistency between emission and extinction.
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In the text

$\begin{figure} \par\includegraphics[width=\textwidth,clip]{3441.f5.eps} \end{figure}$ Figure 5: NGC 1569 observations and modeled SED. The data (Table 2) are indicated by crosses: vertical bars are the errors on the flux values and the horizontal bars indicate the widths of the broadbands. The lines are the dust model and its different components (see Sect. 4.1.1). Diamonds are the model integrated over the observational broadbands and color-corrected. Thus, departures from the model lie where the diamonds deviate from the crosses. The power is expressed in $\rm W~ H^{-1}$ which is $\nu L_\nu$ divided by the number of H atoms ( $L_\nu$ is the monochromatic luminosity).
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In the text

$\begin{figure} \par\includegraphics[width=\textwidth,clip]{3441.f6.eps} \end{figure}$ Figure 6: Global synthesized SED for NGC 1569. The solid line is the total energy of the galaxy: the sum of the dust (dashed line) plus the emerging stellar radiation (dashed-dotted line). For comparison, the dotted line shows the non-extincted stellar radiation.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f7.eps} \end{figure}$ Figure 7: Grain size distribution for the two extreme radius cases ( $R_{\rm eff}^{\rm max}$ and $R_{\rm eff}^{\rm min}$ ) and for the best estimated value, $R_{\rm eff}$ (see Sect. 3.1). It gives the conservative range within which the size distribution can be constrained.
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In the text

$\begin{figure} \par\includegraphics[width=\textwidth,clip]{3441.f8.eps} \end{figure}$ Figure 8: Comparison of the dust SED for NGC 1569 (black) with the Galaxy (grey, from DBP90). In addition to the total dust SED (solid lines), the individual components of the DBP90 dust model also shown for both the Galaxy and NGC 1569. The power is expressed in $\rm W~ H^{-1}$ which is $\nu L_\nu$ divided by the number of H atoms ( $L_\nu$ is the monochromatic luminosity).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f9.eps} \end{figure}$ Figure 9: Size distribution of the grains in NGC 1569 and in the Galaxy. The three thin lines are the mass spectrum of the three dust components of the Galaxy. The bold lines are the mass spectrum of the three dust components of NGC 1569. a is the grain radius and m(a) is the dust mass of the component between a and $a+{\rm d}a$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f10.eps} \end{figure}$ Figure 10: The effects of shocks on the dust size distribution. The solid lines are the mass spectrum of the VSGs which are carbonaceous grains and of the BGs which are silicates, in NGC 1569. The dotted lines show the mass spectra of carbon grains before (straight line) and after (curved line) a shock wave ( $V_{\rm shock} = 100 \;\rm km~ s^{-1}$ ). The dashed lines represents the effect of the $100 \;\rm km~ s^{-1}$ shock on silicate grains (before shock: straight line and after shock: curved line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f11.eps} \end{figure}$ Figure 11: Cooling and photon absorption times computed using Eq. (7). The solid lines are for NGC 1569 and the dashed lines for the Galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{3441.f12.eps} \end{figure}$ Figure 12: Extinction curve for NGC 1569 (black) compared to the Galaxy (grey, from DBP90). The Galactic extinction curve has been scaled down for comparison to that of NGC 1569. The solid lines are the total extinction curve modeled with DBP90. The contributions to the extinction curves from the individual dust components are also shown in dashed lines (PAHs), dotted lines (VSGs) and dashed-dotted lines (BGs). The opacity is expressed as the cross section per H atom.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f13.eps} \end{figure}$ Figure 13: Comparison of various extinction curves. The Galactic curve is from Seaton (1979), the LMC's is the average of Koornneef & Code (1981) and of Nandy et al. (1981) and the SMC's is from Prévot et al. (1984).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f14.eps} \end{figure}$ Figure 14: Synthesized ISRF for NGC 1569 computed with PÉGASE and CLOUDY. The Points with error bars are the observational data from Table 3, the solid black line is the global non-extincted ISRF, the dashed line is the global extincted ISRF and the grey line is the young single-burst component. The extinction curve used is the output from the dust model DBP90.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f15.eps} \end{figure}$ Figure 15: Synthesized ISRF for NGC 1569 (solid line) compared to the Galaxy (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f16.eps} \end{figure}$ Figure 16: Schematic diagram of a clump.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3441.f2a.ps}\hspace*{4mm} \includegraphics[width=7cm,clip]{3441.f2b.ps} \end{figure}$	Figure 2: Ratio of hot dust/cold dust. Left: ratio of the ISOCAM-LW3 image (contours, $\lambda = 15\; \mu$ m) to the SCUBA image ( $\lambda = 850\; \mu$ m). Right: ratio of the ISOCAM-LW6 image (contours, $\lambda = 7.75\; \mu$ m) to the SCUBA image ( $\lambda = 850\; \mu$ m). The ISOCAM images have been degraded to the resolution of the SCUBA (850 $\mu$ m) image (15'').
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$\begin{figure} \par\includegraphics[width=\hsize,clip]{3441.f3.eps} \end{figure}$	Figure 3: Schematic diagram of the model geometry.
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$\begin{figure} \par\includegraphics[width=\textwidth,clip]{3441.f6.eps} \end{figure}$	Figure 6: Global synthesized SED for NGC 1569. The solid line is the total energy of the galaxy: the sum of the dust (dashed line) plus the emerging stellar radiation (dashed-dotted line). For comparison, the dotted line shows the non-extincted stellar radiation.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f7.eps} \end{figure}$	Figure 7: Grain size distribution for the two extreme radius cases ( $R_{\rm eff}^{\rm max}$ and $R_{\rm eff}^{\rm min}$ ) and for the best estimated value, $R_{\rm eff}$ (see Sect. 3.1). It gives the conservative range within which the size distribution can be constrained.
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$\begin{figure} \par\includegraphics[width=\textwidth,clip]{3441.f8.eps} \end{figure}$	Figure 8: Comparison of the dust SED for NGC 1569 (black) with the Galaxy (grey, from DBP90). In addition to the total dust SED (solid lines), the individual components of the DBP90 dust model also shown for both the Galaxy and NGC 1569. The power is expressed in $\rm W~ H^{-1}$ which is $\nu L_\nu$ divided by the number of H atoms ( $L_\nu$ is the monochromatic luminosity).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f9.eps} \end{figure}$	Figure 9: Size distribution of the grains in NGC 1569 and in the Galaxy. The three thin lines are the mass spectrum of the three dust components of the Galaxy. The bold lines are the mass spectrum of the three dust components of NGC 1569. a is the grain radius and m(a) is the dust mass of the component between a and $a+{\rm d}a$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f11.eps} \end{figure}$	Figure 11: Cooling and photon absorption times computed using Eq. (7). The solid lines are for NGC 1569 and the dashed lines for the Galaxy.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f13.eps} \end{figure}$	Figure 13: Comparison of various extinction curves. The Galactic curve is from Seaton (1979), the LMC's is the average of Koornneef & Code (1981) and of Nandy et al. (1981) and the SMC's is from Prévot et al. (1984).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f14.eps} \end{figure}$	Figure 14: Synthesized ISRF for NGC 1569 computed with PÉGASE and CLOUDY. The Points with error bars are the observational data from Table 3, the solid black line is the global non-extincted ISRF, the dashed line is the global extincted ISRF and the grey line is the young single-burst component. The extinction curve used is the output from the dust model DBP90.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f15.eps} \end{figure}$	Figure 15: Synthesized ISRF for NGC 1569 (solid line) compared to the Galaxy (dashed line).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3441.f16.eps} \end{figure}$	Figure 16: Schematic diagram of a clump.
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