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$\begin{figure} \par\includegraphics[angle=90,width=9cm,clip]{6714fig1.eps} \end{figure}$ Figure 1: Spectral energy distributions used for the models. From the top downwards these SEDs correspond to the following SED types in the models: normal cold, normal, starburst M 82, starburst, 10 $^{11}~L_{\rm FIR}$ LIG, 10 $^{11.5}~L_{\rm FIR}$ LIG, Cold LIG, Hot ULIRG, Cold ULIRG, Sy1, Sy2.
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In the text

$\begin{figure} \par\includegraphics[width=4cm,clip]{6714fig2.eps}\hspace*{3mm} \includegraphics[width=4cm,clip]{6714fig3.eps}\end{figure}$ Figure 2: Source detected in line below confusion limit. Left: continuum 120 $\mu$ m image of the field. Right: narrow band image of the field at the wavelength at which a 560 $\mu$ Jy 120 $\mu$ m continuum flux source is detected by its line emission. Note that the source is clearly detected in the line image (the rightmost bright pixel, at location (12, 8)) while in the continuum image nothing can be seen because of the confusion noise. Greyscales not the same, but chosen to make this effect clear. The additional source seen to the left in the line image is below our 4.5 $\sigma$ detection threshold.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.2cm,clip]{6714fig4.ps} \includegraphics[angle=90,width=7.1cm,clip]{6714fig5.ps} \end{figure}$ Figure 3: Recovery of Objects, with redshifts, from the FIR data cube. Top: shows the input flux distribution at 120 $\mu$ m from the "truth catalog'' (dotted line) and the sources detected from their line emission as a function of their 120 $\mu$ m continuum flux (solid line) for a 4.5 $\sigma$ line detection threshold and a 1 $\sigma$ noise of 0.4 mJy per channel. The conventional continuum confusion limit of 20 beams per source is shown as a vertical line. Note that many sources below this confusion limit are detected, with sources having continuum fluxes nearly an order of magnitude below the limit being accessible. Bottom: the redshift distribution from the "truth catalog'' for sources brighter than 1 mJy at 120 $\mu$ m (dotted line) and the redshift distribution for sources brighter than 1 mJy at 120 $\mu$ m recovered from the 4.5 $\sigma$ line detected sources. Note that all sources with z<2.5 and $F_{120} > 1~{\rm mJy}$ have been recovered.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=9cm,clip]{6714fig1.eps} \end{figure}$	Figure 1: Spectral energy distributions used for the models. From the top downwards these SEDs correspond to the following SED types in the models: normal cold, normal, starburst M 82, starburst, 10 $^{11}~L_{\rm FIR}$ LIG, 10 $^{11.5}~L_{\rm FIR}$ LIG, Cold LIG, Hot ULIRG, Cold ULIRG, Sy1, Sy2.
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