All Figures

$\begin{figure} \par\includegraphics[width=4.45cm,clip]{6044fg1a.eps}\hspace*{2.5mm} \includegraphics[width=4.3cm,clip]{6044fg1b.eps}\end{figure}$ Figure 1: Left: the rest-frame far-IR luminosity distribution of the IDS/ISOCAM sample of 56 galaxies. Here, as in Figs. 2-4, 7, 9, and 11, upper limits are taken into account by exploiting the Kaplan-Mayer estimator and by accounting for K-corrections and dust emission using evolutionary population synthesis models (see text). Right: the rest-frame distribution of the IRAS flux density ratio f₆₀/f₁₀₀, as revised in Mazzei et al. (2001), for the same sample.
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In the text

$\begin{figure} \par\includegraphics[width=6.45cm,clip]{6044fg2.eps}\end{figure}$ Figure 2: The distribution of the rest-frame luminosity ratio, $\log L_{60}/L_{100}$ , for our 56 IDS/ISOCAM sources; red continuous line corresponds to the value $\log L_{60}/L_{100}=-0.08$ (see text).
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{6044fg3.eps}\end{figure}$ Figure 3: The rest-frame far-infrared luminosity distribution for the IDS/ISOCAM sample of 56 galaxies. The separate distributions of warm (24 sources) and cold (32 sources) sub-populations are indicated with the (grey) open and (white) hatched histograms, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=4cm,clip]{6044fg4a.eps}\hspace*{1cm} \includegraphics[width=4cm,clip]{6044fg4b.eps}\end{figure}$ Figure 4: Left: the SFR distribution for our sample of 56 sources. Right: the SFR distribution for warm, 24, and for cold, 32 sources, (grey) open and (white) hatched histograms respectively.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6044fg5.eps}\end{figure}$ Figure 5: The redshift distribution for warm, 24, and for cold, 32 sources, (grey) open and (white) hatched histograms, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=4.25cm,clip]{6044fg6a.eps}\hspace*{5mm} \includegraphics[width=4.25cm,clip]{6044fg6b.eps}\end{figure}$ Figure 6: Left: the rest-frame 60 ${\mu }$ m LF for our sample of 56 IDS/ISOCAM sources (red open squares) compared with LF of IRAS PSCz galaxies from Takeuchi et al. (2003, 2004; blue continuous line) and with LF of Spitzer extragalactic First Look Survey from Frayer et al. (2006) (black open diamonds). The bin size is $\Delta\log L_{60}=0.4$ . Right: LF split into different redshift bins: asterisks (red) for z<0.05, triangles (green) for $0.05\le z < 0.010$ , open circles (blue) for $0.010\le z < 0.015$ , and stars (magenta) for z>0.15.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{6044fg7.eps}\end{figure}$ Figure 7: Distribution of the $\log L_{15}/L_{60}$ ratio for 54 IDS/ISOCAM sources (see text). The bin size is $\Delta(\log L_{15}/L_{60})=0.1$ . The fitting function is a type I Pearson whose parameters, optimized following the Levenberg-Marquardt method (see text), are reported in Table 2; dashed lines show the same curves with one $\sigma$ error in the parameters.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{6044fg8.eps}\end{figure}$ Figure 8: The 15 ${\mu }$ m differential LF (red continuous line) for the IDS/ISOCAM sample (54 sources) compared with that of Pozzi et al. (2004) (blue dashed line and open triangles). The error bars correspond to one $\sigma$ error of the Pearson's curve parameters.
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In the text

$\begin{figure} \par\includegraphics[height=3.8cm,width=3.8cm,clip]{6044fg9a.eps}... ...0.9cm} \includegraphics[height=3.8cm,width=3.7cm,clip]{6044fg9b.eps}\end{figure}$ Figure 9: Left: distribution of the $\log L_{15}/L_{60}$ ratios for starbursts (black continuous line), 22 sources, and spirals (red dashed line), 32 sources, selected on the basis of their far-IR colors. The bin size is $\Delta(\log L_{15}/L_{60})=0.1$ and the parameters of the fitting functions, type I Pearson curves, are in Table 4 together with one $\sigma$ errors. Right: the contribution of such galaxy populations to the rest-frame 15 ${\mu }$ m LF (see Table 5): starbursts (magenta long-dashed dotted line) and spirals (green dot-dashed line). Results are compared with those by Pozzi et al. (2004): starbursts (red short-dashed line) and spirals (blue long-dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{6044fg10.eps}\end{figure}$ Figure 10: The behavior of the $\log L_{15}/L_{R}$ ratio for warm sources (24, red triangles), and for cold sources (32, blue open circles) of IDS/ISOCAM sample; the continuous line corresponds to the least-square fit (see Eq. (6)).
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In the text

$\begin{figure} \par\includegraphics[height=3.8cm,width=3.95cm,clip]{6044fg11a.ep... ...85cm} \includegraphics[height=3.8cm,width=3.8cm,clip]{6044fg11b.eps}\end{figure}$ Figure 11: Left: the distribution of the $\log L_{15}/L_{60}$ ratio for starbursts (black continuous line), 24 sources, and for spirals (red dashed line), 30 sources, selected with the same criterion as Pozzi et al. (2004). The bin sizes are $\Delta(\log L_{15}/L_{60})=0.12$ and 0.1, respectively. The parameters of the fitting functions, type I Pearson curves, are in Table 6. Right: the contribution of such galaxy populations to the rest-frame 15 ${\mu }$ m LF (see Table 7): starbursts (magenta long-dashed dotted line) and spirals (green dot-dashed line). Our results are compared with those by Pozzi et al. (2004): starbursts (red short-dashed line) and spirals (blue long-dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=6.45cm,clip]{6044fg2.eps}\end{figure}$	Figure 2: The distribution of the rest-frame luminosity ratio, $\log L_{60}/L_{100}$ , for our 56 IDS/ISOCAM sources; red continuous line corresponds to the value $\log L_{60}/L_{100}=-0.08$ (see text).
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$\begin{figure} \par\includegraphics[width=6.4cm,clip]{6044fg3.eps}\end{figure}$	Figure 3: The rest-frame far-infrared luminosity distribution for the IDS/ISOCAM sample of 56 galaxies. The separate distributions of warm (24 sources) and cold (32 sources) sub-populations are indicated with the (grey) open and (white) hatched histograms, respectively.
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$\begin{figure} \par\includegraphics[width=4cm,clip]{6044fg4a.eps}\hspace*{1cm} \includegraphics[width=4cm,clip]{6044fg4b.eps}\end{figure}$	Figure 4: Left: the SFR distribution for our sample of 56 sources. Right: the SFR distribution for warm, 24, and for cold, 32 sources, (grey) open and (white) hatched histograms respectively.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6044fg5.eps}\end{figure}$	Figure 5: The redshift distribution for warm, 24, and for cold, 32 sources, (grey) open and (white) hatched histograms, respectively.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{6044fg7.eps}\end{figure}$	Figure 7: Distribution of the $\log L_{15}/L_{60}$ ratio for 54 IDS/ISOCAM sources (see text). The bin size is $\Delta(\log L_{15}/L_{60})=0.1$ . The fitting function is a type I Pearson whose parameters, optimized following the Levenberg-Marquardt method (see text), are reported in Table 2; dashed lines show the same curves with one $\sigma$ error in the parameters.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{6044fg8.eps}\end{figure}$	Figure 8: The 15 ${\mu }$ m differential LF (red continuous line) for the IDS/ISOCAM sample (54 sources) compared with that of Pozzi et al. (2004) (blue dashed line and open triangles). The error bars correspond to one $\sigma$ error of the Pearson's curve parameters.
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$\begin{figure} \par\includegraphics[width=6.2cm,clip]{6044fg10.eps}\end{figure}$	Figure 10: The behavior of the $\log L_{15}/L_{R}$ ratio for warm sources (24, red triangles), and for cold sources (32, blue open circles) of IDS/ISOCAM sample; the continuous line corresponds to the least-square fit (see Eq. (6)).
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