All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{1782fig1.eps} % \end{figure}$ Figure 1: The 15 $\mu$ m contour map (red) of Cl 0024+1654 overlaid on a Very Large Telescope image taken in the V band with the FORS2 instrument (ESO program identification: 65.O-0489(A)). Numbers 1 to 30 refer to the 15 $\mu$ m sources in the primary list (Table 2) and sources 1s to 5s label sources from the supplementary list (Table 3). Each set of sources is labelled in order of increasing Right Ascension. Sources ISO_Cl0024_29 and ISO_Cl0024_30 are outside the boundary of the optical map, and have a star and a faint galaxy, respectively, as optical counterparts. Blue circles denote 15 $\mu$ m sources that are spectroscopically confirmed cluster galaxies. Greek letters ( $\alpha \div \delta$ ) identify four gravitationally lensed images of the background galaxy associated with the spectacular giant arcs in the cluster field. North is up and East is to the left. The centre of the ISO map, indicated by a cross, is at RA 00 26 37.5 and Dec 17 09 43.4 (J2000).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1782fig2.eps} \end{figure}$ Figure 2: The fractional distribution of velocities of cluster galaxies in Cl 0024+1654. The counterparts of the cluster members detected at 15 $\mu$ m are displayed in bold. All velocities are in the cluster rest-frame.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{1782fig3.eps} \end{figure}$ Figure 3: SEDs for cluster members in Cl 0024+1654 detected at 15 $\mu$ m. The horizontal axis is the wavelength in the cluster rest frame and the vertical axis is the flux density (in normalized units). The data points are given by black dots and the model fit to the SED by a continuous line.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1782fig4.eps} \end{figure}$ Figure 4: The average SED of 9 ISOCAM cluster sources (the sources from the supplementary list have not been considered). Error bars give the rms values for the flux density. An upper limit of 400 $\mu$ Jy was used for LW2 at 7 $\mu$ m. The solid line shows a model fit (SB+1) to the average SED.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1782fig5.eps} \end{figure}$ Figure 5: The total infrared luminosity distribution for cluster members. The median value for $L_{\rm IR}$ is $\sim$ $1.0\times 10^{11}$ ${L}_\odot$ .
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In the text

$\begin{figure} \par\subfigure[]{\includegraphics[width=7cm,height=7cm,clip]{1782... ...igure[]{\includegraphics[width=7cm,height=7cm,clip]{1782f6b.eps} }\end{figure}$ Figure 6: a) Adaptive Kernel map for cluster members. Black boxes represent the 15 $\mu$ m sources while dots and isodensity contours trace the distribution of component-A galaxies. b) Radial distribution from the centre of component-A galaxies (continuous line) and 15 $\mu$ m cluster galaxies (dashed line) within the region covered by the ISOCAM observations.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=10cm,clip]{1782fig7.eps} \end{figure}$ Figure 7: V - I colour-magnitude diagramme for component-A galaxies (empty circles) within the region mapped by ISOCAM. The eleven 15 $\mu$ m cluster galaxies (filled circles) are identified by their ISO source number from Tables 2 and 3. The V and I magnitudes were not available for source ISO_Cl0024_12. The galaxies in section M, which is defined by V - I < 1.8 and I < 20.4, are BO galaxies. Surprisingly, five of the 15 $\mu$ m sources are in section N and not associated with BO galaxies.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15cm,clip]{1782fig8.eps} \end{figure}$ Figure 8: Miniature maps obtained from HST. The maps are centred on the 15 $\mu$ m source coordinates and labelled with the source number in Tables 2 and 3. The letters M and N at the top right of the images give the positions of the cluster sources in the colour-magnitude diagramme (Fig. 7). All images are $30\times 30$ arcsec². Insets show details of the optical counterpart. North is up, East to the left.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1782fig2.eps} \end{figure}$	Figure 2: The fractional distribution of velocities of cluster galaxies in Cl 0024+1654. The counterparts of the cluster members detected at 15 $\mu$ m are displayed in bold. All velocities are in the cluster rest-frame.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{1782fig3.eps} \end{figure}$	Figure 3: SEDs for cluster members in Cl 0024+1654 detected at 15 $\mu$ m. The horizontal axis is the wavelength in the cluster rest frame and the vertical axis is the flux density (in normalized units). The data points are given by black dots and the model fit to the SED by a continuous line.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1782fig4.eps} \end{figure}$	Figure 4: The average SED of 9 ISOCAM cluster sources (the sources from the supplementary list have not been considered). Error bars give the rms values for the flux density. An upper limit of 400 $\mu$ Jy was used for LW2 at 7 $\mu$ m. The solid line shows a model fit (SB+1) to the average SED.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1782fig5.eps} \end{figure}$	Figure 5: The total infrared luminosity distribution for cluster members. The median value for $L_{\rm IR}$ is $\sim$ $1.0\times 10^{11}$ ${L}_\odot$ .
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$\begin{figure} \par\subfigure[]{\includegraphics[width=7cm,height=7cm,clip]{1782... ...igure[]{\includegraphics[width=7cm,height=7cm,clip]{1782f6b.eps} }\end{figure}$	Figure 6: a) Adaptive Kernel map for cluster members. Black boxes represent the 15 $\mu$ m sources while dots and isodensity contours trace the distribution of component-A galaxies. b) Radial distribution from the centre of component-A galaxies (continuous line) and 15 $\mu$ m cluster galaxies (dashed line) within the region covered by the ISOCAM observations.
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