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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{0385f02.ps}} \end{figure}$ Figure 2: The star formation histories of the GRASIL models used in this paper. Time since galaxy formation is on the x-axis, and SFR (normalised to the maximum value) is on the y-axis. Note the logarithmic x- and y-scale in the top and bottom panel, respectively. Top panel: Es (solid line), Em (dash-dotted line), and El (dashed line) models. Middle panel: Sa (solid line), Sb (dash-dotted line), and Sc (dashed line) models. Bottom panel: Mps (solid line), and Aps (dash-dotted line) models. Models M and A are like models Mps and Aps, respectively, except that they are seen at the time of the starburst (the spike in the figure) rather than 1 Gyr after it. See the text for a detailed description of all models.
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In the text

$\begin{figure} \par\resizebox{7.6cm}{!}{\includegraphics[clip]{0385f03.ps}} \end{figure}$ Figure 3: Top panel: the SFR averaged over the last 1.1 Gyr vs. the SFR averaged over the last 0.1 Gyr, both normalised by the SFR averaged over the entire SFH, for the different GRASIL models, grouped in five classes. Middle panel: the distribution of the best-fit models for the ISOCAM cluster sources in the Nsfr(1.1) vs. Nsfr(0.1) plane. The shading in each box is proportional to the number of best-fit models. Bottom panel: same as the middle panel, but for ISOCAM field sources.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{0385f04.ps}} \end{figure}$ Figure 4: The ISOCAM sources IR luminosities obtained from the best-fit model SEDs plotted vs. the IR luminosities obtained from the K-corrected LW3 luminosities, or, when these are not available, from the K-corrected LW2 luminosities, through the relations of Elbaz et al. (2002). The dashed line is the identity line. Crosses indicate those sources whose SED is best fit by an E-type model.
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In the text

$\begin{figure} \par\resizebox{15cm}{!}{\includegraphics[clip]{0385f05.ps}} \end{figure}$ Figure 5: The observed SEDs of the 27 cluster sources for which we obtain an acceptable fit (dots with 2- $\sigma$ error bars), with the best-fit GRASIL models overlayed (solid lines for sources with spectroscopic z, dashed line for sources with z determined from the model fitting procedure). The rest-frame wavelength, in $\mu$ m, is plotted along the x-axis, and the flux density (in normalized units) is plotted along the y-axis. Upper limits are indicated by arrows. The approximate widths of the LW2 and LW3 bands are indicated.
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{0385f06.ps}} \end{figure}$ Figure 6: The average SED of the 27 ISOCAM cluster sources. Error-bars denote the rms among the flux values. The arrow indicates the upper limit on the LW3 flux value. The approximate widths of the LW2 and LW3 bands are indicated. The 27 SEDs were normalised to the H-band flux density, as estimated from the individual best fit models, before averaging them. The best fit Em10 model SED is also shown (solid line).
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{0385f07.ps}} \end{figure}$ Figure 7: The V₆₀₆-I₈₁₄ vs. $I_{814}-K_{\rm s}$ colour-colour diagram for cluster sources with data from S01. ISOCAM galaxies are plotted as diamonds.
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In the text

$\begin{figure} \par\resizebox{14cm}{!}{\includegraphics[clip]{0385f08.ps}} \end{figure}$ Figure 8: The distributions of $L_{\rm IR}$ and SFR for ISOCAM cluster and field sources. Solid (dashed) histograms show the distributions for sources with (respectively, without) known redshift. Top left panel: the distribution of $L_{\rm IR}$ for cluster sources. Bottom left panel: the distribution of $L_{\rm IR}$ for field sources. Top right panel: the distribution of SFR for cluster sources. Bottom right panel: the distribution of SFR for field sources.
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{0385f09.ps}}\end{figure}$ Figure 9: The ratio of the IR luminosity to the NIR luminosity, $L_{\rm IR}/L_{\rm NIR}$ as a function of $L_{\rm NIR}$ , for ISOCAM sources. Open symbols indicate sources without spectroscopic redshift estimates. Top panel: cluster members. Sources with Nsfr(0.1) >0 are crossed. Bottom panel: field galaxies.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{0385f10.ps}} \end{figure}$ Figure 10: The projected space distribution of ISOCAM cluster sources (filled squares: spectroscopically confirmed members; open squares: sources whose cluster membership is established from the best fit model SED), and of optically-selected cluster sources (isodensity contours). The two crosses indicate the position of the cD (near the centre) and of LPS244, the second brightest cluster galaxy.
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In the text

$\begin{figure} \par\resizebox{7.6cm}{!}{\includegraphics[clip]{0385f11.ps}} \end{figure}$ Figure 11: The rest-frame velocity distribution of optically-selected cluster members (dashed line) and of ISOCAM cluster sources (solid line). Arrows indicate the location in the velocity space of the cD galaxy (at negative velocity) and the 2nd brightest member, LPS244.
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In the text

$\begin{figure} \par\resizebox{15.5cm}{!}{\includegraphics[clip]{0385f12.ps}} \end{figure}$ Figure 12: The observed SEDs of the 14 field sources for which we obtain an acceptable fit (dots with 2- $\sigma$ error bars), with the best-fit GRASIL models overlayed (solid lines for sources with spectroscopic z, dashed line for the source with z determined from the model fitting procedure). The rest-frame wavelength, in $\mu$ m, is plotted along the x-axis, and the flux density (in arbitrary units) is plotted along the y-axis. Upper limits are indicated by arrows. The approximate widths of the LW2 and LW3 bands are indicated.
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{0385f13.ps}} \end{figure}$ Figure 13: The total IR luminosity as a function of redshift for ISOCAM field sources with spectroscopic redshift estimates, detected in the LW3 band. The solid line is the luminosity corresponding to a flux of 0.121 mJy (the 50% completeness limit of the A2218 ISOCAM survey), reduced by a factor 0.6 (the average lensing correction factor), and K-corrected using the average correction for the models that best fit the observed field galaxy SEDs.
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{0385f14.ps}} \end{figure}$ Figure 14: The B-r vs. r colour-magnitude diagram for galaxies in the A2218 field (magnitude and colour data are from LPS). Filled symbols represent ISOCAM sources. Diamonds represent cluster sources (big diamonds: spectroscopically confirmed cluster members; small diamonds: cluster membership established through the SED-fitting procedure). X's identify the ISOCAM sources with a ${\it SFR}> 4~M_{\odot}$ yr^-1. The dashed line is the best-fit cluster colour-magnitude relation. Solid lines delimit the region of the diagram where blue BO galaxies are located.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[clip]{0385f01a.ps}} \end{figure}$ Figure 1: MIR isocontours of ISOCAM sources, at 6.7 and 14.3 $\mu$ m (in blue and red, respectively) overlaid on an optical HST image in the F814W band. Each image is 30 arcsec on a side.
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In the text

$\begin{figure}\par\resizebox{18cm}{!}{\includegraphics[clip]{0385f01b.ps}}\end{figure}$ Figure 1: continued.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{0385f04.ps}} \end{figure}$	Figure 4: The ISOCAM sources IR luminosities obtained from the best-fit model SEDs plotted vs. the IR luminosities obtained from the K-corrected LW3 luminosities, or, when these are not available, from the K-corrected LW2 luminosities, through the relations of Elbaz et al. (2002). The dashed line is the identity line. Crosses indicate those sources whose SED is best fit by an E-type model.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{0385f07.ps}} \end{figure}$	Figure 7: The V₆₀₆-I₈₁₄ vs. $I_{814}-K_{\rm s}$ colour-colour diagram for cluster sources with data from S01. ISOCAM galaxies are plotted as diamonds.
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$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{0385f09.ps}}\end{figure}$	Figure 9: The ratio of the IR luminosity to the NIR luminosity, $L_{\rm IR}/L_{\rm NIR}$ as a function of $L_{\rm NIR}$ , for ISOCAM sources. Open symbols indicate sources without spectroscopic redshift estimates. Top panel: cluster members. Sources with Nsfr(0.1) >0 are crossed. Bottom panel: field galaxies.
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$\begin{figure} \par\resizebox{7.6cm}{!}{\includegraphics[clip]{0385f11.ps}} \end{figure}$	Figure 11: The rest-frame velocity distribution of optically-selected cluster members (dashed line) and of ISOCAM cluster sources (solid line). Arrows indicate the location in the velocity space of the cD galaxy (at negative velocity) and the 2nd brightest member, LPS244.
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$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics[clip]{0385f01a.ps}} \end{figure}$	Figure 1: MIR isocontours of ISOCAM sources, at 6.7 and 14.3 $\mu$ m (in blue and red, respectively) overlaid on an optical HST image in the F814W band. Each image is 30 arcsec on a side.
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$\begin{figure}\par\resizebox{18cm}{!}{\includegraphics[clip]{0385f01b.ps}}\end{figure}$	Figure 1: continued.
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