All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6587fig1.ps}\end{figure}$ Figure 1: H $\alpha$ emission of the LMC HII complex N4A and N4B (from Heydari-Malayeri & Lecavelier des Etangs 1994). The image has been rotated to the same orientation as the ISOCAM-CVF images.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13.5cm,clip]{6587fig2.ps}\end{figure}$ Figure 2: ISOCAM CVF spectra of four different regions of N4A. The regions where the spectra were extracted are shown in each panel on the gray-scale image in the 7.7 $\mu$ m aromatic feature. Note that the steep rise or decrease at the very end of the spectrum is an instrument artifact and should not be considered as real.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,angle=-90,origin=c,clip]{6587fig3.ps}\end{figure}$ Figure 3: Image: map from the Lorentzian fit of the 7.7 $\mu$ m dust emission feature. Gray and black contours: from the map of Gaussian fit in the SIV line and the "pure'' continuum in the LW9 filter (15 $\mu$ m) emission, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,angle=-90,origin=c,clip]{6587fig4.ps}\end{figure}$ Figure 4: Image: map from Lorentzian fit of the 7.7 $\mu$ m dust emission feature. Contours: from the map of Gaussian fit in the NeIII line.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6587fig5.eps}\end{figure}$ Figure 5: NIR Composite map oriented like the ISOCAM images: red is $K_{\rm s}$ , green is H and blue is J. Point sources identified as stars are numbered as in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,height=8.8cm,origin=c,angle=-90,clip]{6587fig6.ps}\end{figure}$ Figure 6: Image: LW9 (15 $\mu$ m) pure continuum emission; Contours = K band.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,height=8.8cm,origin=c,angle=-90,clip]{6587fig7.ps}\end{figure}$ Figure 7: Image: SIV at 10.5 $\mu$ m from the Gaussian fit; Contours = K band. Contours are shown in two colors (black and white) for the purpose of visualization.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,height=8.8cm,origin=c,angle=-90,clip]{6587fig8.ps}\end{figure}$ Figure 8: Image: PAH, 7.7 $\mu$ m feature from the Lorentzian fit; Contours = K band.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,height=8.8cm,angle=-90,origin=c,angle=90,clip]{6587fig9.ps}\end{figure}$ Figure 9: Image: PAH, 7.7 $\mu$ m feature from Lorentzian fit; Contours = NeIII/NeII(+12.7) ratio. Contour values are: 0.7, 1, 2, 3, 4, 5, 6, 7, 8, 9, 10.5.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,height=8.8cm,angle=-90,origin=c,clip]{6587fig10.ps}\end{figure}$ Figure 10: Image: map from the 15 $\mu$ m "pure'' continuum emission. Contours: "pure'' continuum at 6.7 $\mu$ m smoothed to the 15 $\mu$ mresolution.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,height=15cm,angle=-90,origin=c,clip]{6587fig11.ps}\end{figure}$ Figure 11: The 7.7 $\mu$ m PAH emission (filled circle), 5 $\mu$ m and 15 $\mu$ m pure continuum emission (triangles and diamonds, respectively) versus the intensity of the radiation field at 1600 Å ( left panel) and NeIII/NeII ratio that traces the UV hardness ( right panel). Values are above the 3 $\sigma$ for the 3 wavelengths. In the right panel, the maximum at 7.7 $\mu$ m and 5 $\mu$ m have been scaled to the maxima at 15 $\mu$ m to ease the relative comparison among the different emissions.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6587fig12.ps}\end{figure}$ Figure 12: Comparison between the spectrum of the galactic region NGC7023 (thick solid line) and the PDR spectrum of N4 (thin solid line), after being continuum-subtracted. NGC7023 spectrum has been scaled to match the 7.7 $\mu$ m feature of N4.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,height=8.5cm,origin=c]{6587fig13.ps}\end{figure}$ Figure 13: Typical widths of the AFEs obtained by the Lorentzian fit for all N4 (filled circles), the PDR only (solid triangles), and the typical values found with the same fitting technique by Boulanger et al. (1998) in $\rho$ Oph and NGC7023 (open stars).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,height=6.5cm,origin=c]{6587fig14.ps}\end{figure}$ Figure 14: Different dust feature ratios as functions of the ISRF. Upper panel: the 11.3/7.7 $\mu$ m dust feature ratio, which traces the [out of plane C-H]/[vibration C-C] ratio. Bottom panel: the (11-13)/(6.2+7.7) $\mu$ m dust feature ratio, which traces the [out of plane C-H]/[in plane C-C] dust features ratio.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,height=18cm,angle=-90]{6587fig15.eps}\end{figure}$ Figure 15: NIR color-magnitude ( left) and color-color ( right) diagrams of N4 with the IR sources shown as red filled points. For comparison we include the 30 Doradus IR sources as open circles and the N11 IR sources as open squares. In the color-magnitude diagram the upper zero-age main sequence between O3 V and O9 V corresponds to a distance modulus of 18.6 and is indicated by a dashed line. The reddening track for a normal O3 V star is plotted with a dotted line and extends to $A_{\rm V} = 20$ mag. In the color-color diagram, the main-sequence locus from O3 V to M2 V and the cool-giant branch are indicated by a solid line. The reddening tracks for normal O3 V and cool giant stars are plotted as dashed lines, with crosses indicating $A_{\rm V} = 10$ and 20 mag. Sources 1, 4, and 7 show IR excesses that cannot be explained by reddening.
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In the text

$\begin{figure} \includegraphics[angle=-90,width=8.4cm,clip]{6587fig16.ps}\end{figure}$ Figure 16: ISOCAM CVF spectrum of star $\char93$ 4 corresponding to the 15 $\mu$ m pure continuum peak.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6587fig1.ps}\end{figure}$	Figure 1: H $\alpha$ emission of the LMC HII complex N4A and N4B (from Heydari-Malayeri & Lecavelier des Etangs 1994). The image has been rotated to the same orientation as the ISOCAM-CVF images.
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$\begin{figure} \par\includegraphics[angle=-90,width=13.5cm,clip]{6587fig2.ps}\end{figure}$	Figure 2: ISOCAM CVF spectra of four different regions of N4A. The regions where the spectra were extracted are shown in each panel on the gray-scale image in the 7.7 $\mu$ m aromatic feature. Note that the steep rise or decrease at the very end of the spectrum is an instrument artifact and should not be considered as real.
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$\begin{figure} \par\includegraphics[width=8.8cm,angle=-90,origin=c,clip]{6587fig3.ps}\end{figure}$	Figure 3: Image: map from the Lorentzian fit of the 7.7 $\mu$ m dust emission feature. Gray and black contours: from the map of Gaussian fit in the SIV line and the "pure'' continuum in the LW9 filter (15 $\mu$ m) emission, respectively.
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$\begin{figure} \par\includegraphics[width=8.8cm,angle=-90,origin=c,clip]{6587fig4.ps}\end{figure}$	Figure 4: Image: map from Lorentzian fit of the 7.7 $\mu$ m dust emission feature. Contours: from the map of Gaussian fit in the NeIII line.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6587fig5.eps}\end{figure}$	Figure 5: NIR Composite map oriented like the ISOCAM images: red is $K_{\rm s}$ , green is H and blue is J. Point sources identified as stars are numbered as in Table 1.
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$\begin{figure} \par\includegraphics[width=8.8cm,height=8.8cm,origin=c,angle=-90,clip]{6587fig6.ps}\end{figure}$	Figure 6: Image: LW9 (15 $\mu$ m) pure continuum emission; Contours = K band.
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$\begin{figure} \par\includegraphics[width=8.8cm,height=8.8cm,origin=c,angle=-90,clip]{6587fig7.ps}\end{figure}$	Figure 7: Image: SIV at 10.5 $\mu$ m from the Gaussian fit; Contours = K band. Contours are shown in two colors (black and white) for the purpose of visualization.
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$\begin{figure} \par\includegraphics[width=8.8cm,height=8.8cm,origin=c,angle=-90,clip]{6587fig8.ps}\end{figure}$	Figure 8: Image: PAH, 7.7 $\mu$ m feature from the Lorentzian fit; Contours = K band.
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$\begin{figure} \par\includegraphics[width=8.8cm,height=8.8cm,angle=-90,origin=c,angle=90,clip]{6587fig9.ps}\end{figure}$	Figure 9: Image: PAH, 7.7 $\mu$ m feature from Lorentzian fit; Contours = NeIII/NeII(+12.7) ratio. Contour values are: 0.7, 1, 2, 3, 4, 5, 6, 7, 8, 9, 10.5.
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$\begin{figure} \par\includegraphics[width=8.8cm,height=8.8cm,angle=-90,origin=c,clip]{6587fig10.ps}\end{figure}$	Figure 10: Image: map from the 15 $\mu$ m "pure'' continuum emission. Contours: "pure'' continuum at 6.7 $\mu$ m smoothed to the 15 $\mu$ mresolution.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{6587fig12.ps}\end{figure}$	Figure 12: Comparison between the spectrum of the galactic region NGC7023 (thick solid line) and the PDR spectrum of N4 (thin solid line), after being continuum-subtracted. NGC7023 spectrum has been scaled to match the 7.7 $\mu$ m feature of N4.
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$\begin{figure} \par\includegraphics[width=8.5cm,height=8.5cm,origin=c]{6587fig13.ps}\end{figure}$	Figure 13: Typical widths of the AFEs obtained by the Lorentzian fit for all N4 (filled circles), the PDR only (solid triangles), and the typical values found with the same fitting technique by Boulanger et al. (1998) in $\rho$ Oph and NGC7023 (open stars).
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$\begin{figure} \par\includegraphics[width=8.3cm,height=6.5cm,origin=c]{6587fig14.ps}\end{figure}$	Figure 14: Different dust feature ratios as functions of the ISRF. Upper panel: the 11.3/7.7 $\mu$ m dust feature ratio, which traces the [out of plane C-H]/[vibration C-C] ratio. Bottom panel: the (11-13)/(6.2+7.7) $\mu$ m dust feature ratio, which traces the [out of plane C-H]/[in plane C-C] dust features ratio.
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$\begin{figure} \includegraphics[angle=-90,width=8.4cm,clip]{6587fig16.ps}\end{figure}$	Figure 16: ISOCAM CVF spectrum of star $\char93$ 4 corresponding to the 15 $\mu$ m pure continuum peak.
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