All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig1.ps} \end{figure}$ Figure 1: Redshift distribution of the 28 FIRBACK fully identified sources.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig2.ps} \end{figure}$ Figure 2: Optical colors of the identified sources. At the top, we show the ( g' - r')-(U - r') colour-colour diagram, while the bottom gives the (U - r') histogram.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1844fig3.ps} \end{figure}$ Figure 3: 60, 100, 170 color ratios. The continuous line is the ISOPHOT Serendipity Survey (ISS) fit, see text.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1844fig4.ps} \end{figure}$ Figure 4: 170/15 correlation. The diamonds are for $S_{170}>4\sigma$ and the triangle for $3\sigma <S_{170}<4\sigma$ . The continuous line is the best fit for all sources. It has a slope of 170/15=25.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig5.ps} \end{figure}$ Figure 5: Comparison of template SEDs from Dale et al. (2001) ( $\alpha =2.6$ , quiescent case, dashed line; and $\alpha =1$ , active case, continuous line) and Lagache et al. (2003) ("cold galaxy'', triple-dot-long-dashed line) with observed SED's. The dotted line is the observed SED of M 101, the dashed-dotted line the SED of M 82 (curves normalised at 100 $\mu$ m).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig6.ps} \end{figure}$ Figure 6: The results from the fit of the source SEDs with a "cold galaxy'' spectrum from Lagache et al. (2003). The continuous line is the "cold galaxy'' spectrum template, the dashed line the spectrum of M 82.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig7.ps} \end{figure}$ Figure 7: Same as in Fig. 6 for the remaining identified sources.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig8.ps} \end{figure}$ Figure 8: SEDs of those identified sources that have both measured 60 $\rm\mu m$ and 100 $\rm\mu m$ fluxes are fitted with a Dale model. The dashed-dotted line is the Dale model fit, the thin continuous one the "cold galaxy'' spectrum template (Lagache et al. 2003). Both the model and the template have been normalized at 170 $\rm\mu m$ .
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=6cm,angle=270]{spectres/N1-0_jui... ...% \includegraphics[width=6cm,angle=270]{spectres/N1-1_juin99.ps} }\end{figure}$ Figure 9: Spectra of individual objects as examples (FN1-0 and FN1-1). Spectra of further objects are only available in electronic form.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,angle=0]{images/E1_000.ps}\hspace*{2mm} \includegraphics[width=7.7cm,angle=0]{images/E1_001.ps} \end{figure}$ Figure 10: Identification charts of FIRBACK N1 field sources (FN1-0 and FN1-1 as examples). Charts of further objects are only available in electronic form. The error circle for the 170 $\mu$ m ISO source is superposed on the DSS optical image. An ISO 15 $\mu$ m source is marked by a black dot and a radio source by a small open black square.
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In the text

Full version

$\begin{figure} \par\includegraphics[width=6cm,angle=270]{spectres_online/N1-0_ju... ...mm} \includegraphics[width=6cm,angle=270]{spectres_online/N1-4_S.ps}\end{figure}$ Figure 9: Spectra of individual objects.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,angle=270]{spectres_online/N1-6_ju... ...cludegraphics[width=6cm,angle=270]{spectres_online/N1-101_juin99.ps}\end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,angle=270]{spectres_online/N1-11_j... ...ncludegraphics[width=6cm,angle=270]{spectres_online/N1-19_juin99.ps}\end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,angle=270]{spectres_online/N1-21.p... ...mm} \includegraphics[width=6cm,angle=270]{spectres_online/N1-25S.ps}\end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,angle=270]{spectres_online/N1-26.p... ...ncludegraphics[width=6cm,angle=270]{spectres_online/N1-32_juin99.ps}\end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,angle=270]{spectres_online/N1-33.p... ...2mm} \includegraphics[width=6cm,angle=270]{spectres_online/N1-38.ps}\end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,angle=270]{spectres_online/N1-41.p... ...hics[width=6cm,angle=270]{spectres_online/N1-45.ps}\hspace*{4.6cm}} \end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,angle=270]{spectres_online/N1-46_A... ...ncludegraphics[width=6cm,angle=270]{spectres_online/N1-57_juin99.ps}\end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_000.ps... ...{2mm} \includegraphics[width=7.5cm,angle=0]{images_online/E1_005.ps}\end{figure}$ Figure 10: Identification charts of FIRBACK N1 field sources. The error circle for the 170 $\mu$ m ISO source is superposed on the DSS optical image. An ISO 15 $\mu$ m source is marked by a black dot and a radio source by a small open black square.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_006.ps... ...{2mm} \includegraphics[width=7.5cm,angle=0]{images_online/E1_011.ps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_012.ps... ...{2mm} \includegraphics[width=7.5cm,angle=0]{images_online/E1_017.ps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_018.ps... ...{2mm} \includegraphics[width=7.5cm,angle=0]{images_online/E1_023.ps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_024.ps... ...{2mm} \includegraphics[width=7.5cm,angle=0]{images_online/E1_029.ps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_030.ps... ...{2mm} \includegraphics[width=7.5cm,angle=0]{images_online/E1_035.ps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_036.ps... ...{2mm} \includegraphics[width=7.5cm,angle=0]{images_online/E1_041.ps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_042.ps... ...{2mm} \includegraphics[width=7.5cm,angle=0]{images_online/E1_047.ps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_048.ps... ...{2mm} \includegraphics[width=7.5cm,angle=0]{images_online/E1_053.ps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_054.ps... ...s}\\ \includegraphics[width=7.5cm,angle=0]{images_online/E1_057.ps}\end{figure}$ Figure 10: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig1.ps} \end{figure}$	Figure 1: Redshift distribution of the 28 FIRBACK fully identified sources.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig2.ps} \end{figure}$	Figure 2: Optical colors of the identified sources. At the top, we show the ( g' - r')-(U - r') colour-colour diagram, while the bottom gives the (U - r') histogram.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1844fig3.ps} \end{figure}$	Figure 3: 60, 100, 170 color ratios. The continuous line is the ISOPHOT Serendipity Survey (ISS) fit, see text.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1844fig4.ps} \end{figure}$	Figure 4: 170/15 correlation. The diamonds are for $S_{170}>4\sigma$ and the triangle for $3\sigma <S_{170}<4\sigma$ . The continuous line is the best fit for all sources. It has a slope of 170/15=25.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig5.ps} \end{figure}$	Figure 5: Comparison of template SEDs from Dale et al. (2001) ( $\alpha =2.6$ , quiescent case, dashed line; and $\alpha =1$ , active case, continuous line) and Lagache et al. (2003) ("cold galaxy'', triple-dot-long-dashed line) with observed SED's. The dotted line is the observed SED of M 101, the dashed-dotted line the SED of M 82 (curves normalised at 100 $\mu$ m).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig6.ps} \end{figure}$	Figure 6: The results from the fit of the source SEDs with a "cold galaxy'' spectrum from Lagache et al. (2003). The continuous line is the "cold galaxy'' spectrum template, the dashed line the spectrum of M 82.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig7.ps} \end{figure}$	Figure 7: Same as in Fig. 6 for the remaining identified sources.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1844fig8.ps} \end{figure}$	Figure 8: SEDs of those identified sources that have both measured 60 $\rm\mu m$ and 100 $\rm\mu m$ fluxes are fitted with a Dale model. The dashed-dotted line is the Dale model fit, the thin continuous one the "cold galaxy'' spectrum template (Lagache et al. 2003). Both the model and the template have been normalized at 170 $\rm\mu m$ .
Open with DEXTER

$\begin{figure} \par\mbox{\includegraphics[width=6cm,angle=270]{spectres/N1-0_jui... ...% \includegraphics[width=6cm,angle=270]{spectres/N1-1_juin99.ps} }\end{figure}$	Figure 9: Spectra of individual objects as examples (FN1-0 and FN1-1). Spectra of further objects are only available in electronic form.
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$\begin{figure} \par\includegraphics[width=7.7cm,angle=0]{images/E1_000.ps}\hspace*{2mm} \includegraphics[width=7.7cm,angle=0]{images/E1_001.ps} \end{figure}$	Figure 10: Identification charts of FIRBACK N1 field sources (FN1-0 and FN1-1 as examples). Charts of further objects are only available in electronic form. The error circle for the 170 $\mu$ m ISO source is superposed on the DSS optical image. An ISO 15 $\mu$ m source is marked by a black dot and a radio source by a small open black square.
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$\begin{figure} \par\includegraphics[width=6cm,angle=270]{spectres_online/N1-6_ju... ...cludegraphics[width=6cm,angle=270]{spectres_online/N1-101_juin99.ps}\end{figure}$	Figure 9: continued.
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$\begin{figure} \par\includegraphics[width=7.5cm,angle=0]{images_online/E1_006.ps... ...{2mm} \includegraphics[width=7.5cm,angle=0]{images_online/E1_011.ps}\end{figure}$	Figure 10: continued.
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