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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3710fig1.ps} \end{figure}$ Figure 1: Distribution of ELAIS-S1 type-1 and -2 AGN in the z-R-magnitude plane. Best fit linear solutions ( $\pm$ 1 $\sigma$ ) in the log(z)-R space are shown as dotted lines for type-1 AGN and as dashed lines for type-2 AGN. The R-magnitude and redshift distributions are shown in the left and bottom panels respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{3710fig2.ps} \end{figure}$ Figure 2: Adopted mid-IR spectral energy distributions (SEDs) for type-2 sources ( top panel) and the corresponding k-corrections as a function of redshift computed for the ISOCAM-LW3 filter ( bottom panel).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{3710fig3.ps} \end{figure}$ Figure 3: Distribution in the L₁₅- z space of the total sample of mid-IR type-1 and 2 AGN. The mid-IR luminosity for type-2 sources has been computed applying the Circinus k-correction (see text, Sect. 3.1). The dotted, dashed and dot-dashed lines represent the flux limits at 0.1, 1.0 and 300 mJy respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3710fig4.ps} \end{figure}$ Figure 4: Type-1 AGN local (z=0.1, continuous line) and high redshift (z=1.2, dash-dotted line) best fits to the 15 $~\mu$ m Luminosity Function assuming a redshift dependent faint slope (Fit "B'', top panel) and a PLE model (Fit "A'', bottom panel). Open circles represent the observed space density of the local population (dominated mainly by RMS sources) while filled circles represent the observed space density of the high redshift population (dominated by ELAIS sources). Poissonian errors at 1 $\sigma$ confidence level are shown. The dark-grey shaded areas (quite narrow and thus barely visible) represent the uncertainty introduced by the assumptions used to estimate the optical incompleteness of the samples, while the light-grey shaded areas correspond to the 1 $\sigma$ errors of the best fit parameters of the LF (see Sect. 3.2).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3710f5a.ps}\hspace*{2mm} \includegraphics[width=8.6cm,clip]{3710f5b.ps} \end{figure}$ Figure 5: Left: mid-IR integral counts for type-1 AGN. Shaded areas show the RMS and ELAIS observed counts, while symbols (triangle, star and diamonds) represent the ISO-Deep surveys. The thick solid line gives the predicted counts from the variable slope fit model ("B''). Expectations from the fixed faint slope model ("A'') are plotted as a dashed line. All errors in the observed distributions are quoted at the 1 $\sigma$ level and given by Poisson statistics. The bottom panel show the 1 $\sigma$ relative error on the predicted counts due to the uncertainties on the best fit parameters of the LF (see text). Line types have the same meaning as in the above panel. Right: redshift distribution for type-1 AGN. The histogram represents the total number of observed sources in each redshift interval. Shaded regions outline the ISOCAM contribution, while the open histogram accounts for the contribution from IRAS sources. The lines are the predictions from the best fit model ("B''): thick dash-dotted for IRAS, thick dashed for ISO population, while the continuous thick line gives their sum. The expected distributions for the "A'' model are plotted as above but using thin lines. The bottom panel shows the relative errors of the predictions for the entire mid-IR population (IRAS + ISO) only.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3710f6a.ps}\hspace*{2mm} \includegraphics[width=8.4cm,clip]{3710f6b.ps} \end{figure}$ Figure 6: Observed and best fit LF for type-2 AGN at $\langle z\rangle =0.05$ (continuous line) and $\langle z\rangle=0.35$ (dash-dotted line). The solutions with a redshift dependent faint slope, assuming a NGC 1068 ("D''; left panel) and Circinus ("F''; right panel) k-corrections, are shown. Symbols and shaded areas as in Fig. 4. Due to the small redshift intervals used, and for the sake of clarity, the plots have been divided into two panels for the low-redshift ( top) and intermediate-z sources ( bottom). At intermediate-z, the thin line shows the low-z best fit.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3710f7a.ps}\hspace*{2mm} \includegraphics[width=8.4cm,clip]{3710f7b.ps} \end{figure}$ Figure 7: Left: observed and predicted integral counts for type-2 sources using the the two representative SED: NGC 1068 (thin dashed for the "C'' model and thin continuous for the "D'' model) and Circinus (thick dashed for the "E'' model and thick continuous for the "F'' model). Right: observed and predicted type-2 AGN redshift distribution for the different models mentioned before. Lines as in left panel. Symbols and shaded area in both panels as in Fig. 5. Errors reported in the lower section of both panels have been computed and plotted as described in Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3710f8a.ps}\par\vspace*{3mm} \includegraphics[width=8cm,clip]{3710f8b.ps} \end{figure}$ Figure 8: Luminosity-redshift distribution of the type-1 ( top) and type-2 ( bottom) AGN. Shaded areas represents the fraction of incompleteness due to the optical spectroscopic limits. Contours range from 75% (black) to 95% (light-gray) of the total area lost and have a 5% step between them. For type-1 AGN $\sim$ 4 missed sources are expected within z=[0.1, 1.2]. Most missed type-2 AGN are only expected with ${\rm log}~L_{15}>44.5$ at z>0.7, a redshift range outside the current analysis (see text). Only $\sim$ 1 missed type-2 source is expected to lie within z=[0.3,0.5] and L₁₅=[43.5,45.0]. Dotted lines in both panels show three representative flux limits at 1, 4 and 300 mJy.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3710fig9.ps} \end{figure}$ Figure 9: Comparison of LFs at 25 $~\mu$ m. The derived 15 $~\mu$ m LF for type-1 (model "B'') and type-2 (Circinus SED, model "F'') AGN, converted to 25 $~\mu$ m luminosities, are compared with the global AGN LF from Xu et al. (2003). The comparison is made in two different redshift intervals: z=0.1( top panel) and z=0.6 ( bottom panel). The values for the parameters of the LFs are reported in Table 3.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{3710f10.ps} \end{figure}$ Figure 10: The expected Spitzer MIPS integral counts for AGN at 24 $~\mu$ m based on our best fit models (thick dashed for type-1, thick dot-dashed for type-2 and thick continuous line for the total). The panels represent different combinations of type-1 and type-2 models from Table 2. Left: models "B'' and "F'' for type-1 and type-2 respectively. Central: models "A'' and "E''. Right: models "B'' and "E''. For comparison, the expectations from the different AGN classes derived by Silva et al. (2004) are also shown (type-1: thin dashed line; type-2: thin dot-dashed; Total: thin continuous). The total AGN contribution by Xu et al. (2003) is represented by a thin triple-dot-dashed line. The light-grey shaded areas represent the expected flux range at 24 $\mu$ m of a source with a 15 $\mu$ m flux of 1 mJy given the assumed type-1 and type-2 SED.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3710fig1.ps} \end{figure}$	Figure 1: Distribution of ELAIS-S1 type-1 and -2 AGN in the z-R-magnitude plane. Best fit linear solutions ( $\pm$ 1 $\sigma$ ) in the log(z)-R space are shown as dotted lines for type-1 AGN and as dashed lines for type-2 AGN. The R-magnitude and redshift distributions are shown in the left and bottom panels respectively.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{3710fig2.ps} \end{figure}$	Figure 2: Adopted mid-IR spectral energy distributions (SEDs) for type-2 sources ( top panel) and the corresponding k-corrections as a function of redshift computed for the ISOCAM-LW3 filter ( bottom panel).
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{3710fig3.ps} \end{figure}$	Figure 3: Distribution in the L₁₅- z space of the total sample of mid-IR type-1 and 2 AGN. The mid-IR luminosity for type-2 sources has been computed applying the Circinus k-correction (see text, Sect. 3.1). The dotted, dashed and dot-dashed lines represent the flux limits at 0.1, 1.0 and 300 mJy respectively.
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